Gas Disks and Supermassive Black Holes in Nearby Radio Galaxies

Gas Disks and Supermassive Black Holes in Nearby Radio Galaxies
Jacob Noel-Storr
Advisors Jacqueline H. van Gorkom
and Stefi A. Baum
Submitted in partial fulfillment of the
requirements for the degree
of Doctor of Philosophy
in the Graduate School of Arts and Sciences.
COLUMBIA UNIVERSITY
2004

c○2004
Jacob Noel-Storr
All Rights Reserved

Abstract
Gas Disks and Supermassive Black Holes in Nearby Radio Galaxies
Jacob Noel-Storr
We present a detailed analysis of a set of medium resolution spectra, obtained by
the Space Telescope Imaging Spectrograph on board the Hubble Space Telescope, of
the emission line gas present in the nuclei of a complete sample of 21 nearby, early-type
galaxies with radio jets (the UGC FR-I sample). For each galaxy nucleus we present
spectroscopic data in the region of Hydrogen-alpha and the derived kinematics.
We find that is 67% of the nuclei the gas appears to be rotating and, with one
exception, the cases where rotation is not seen are either face on or have complex
central morphologies. We find that in 62% of the nuclei the fit to the central spectrum
is improved by the inclusion of a broad component. The broad components have a
mean velocity dispersion of 1349 ± 345 km s −1 and are redshifted from the narrow
line components (assuming an origin in Hydrogen-alpha) by 486 ± 443 km s −1 .
We generated model velocity profiles for the nuclei including no black hole, a
1 × 10 8 solar mass black hole and a 9 × 10 8 solar mass black hole. We compared the

predicted profiles to the observed velocity profiles from the above spectra and found
kinematic signatures compatible with black holes > 1 × 10 8 solar masses in 53% of
the sample (in the remaining galaxies we are unable to rule in or out the presence of
a nuclear black hole). We suspect that flow is a significant factor in the nucleus of
NGC 2329. We found hints of jet-disk interaction in 24% of the sample nuclei and
signs of twists or warps in 19% of the sample nuclei. 24% of the velocity profiles show
signs of multiple distinct kinematic components. We suggest that the gas disks in
nearby radio galaxies are generally not well settled systems in the equitorial plane of
the gravitational potentials.
We characterize the kinematic state of the nuclear gas through three weighted
mean parameters, and find that again the disks appear not to be well settled. We
show evidence of a connection between the stellar and gas velocity dispersions. We
show correlations in the nuclear fluxes from the Radio to the X-ray regimes, suggesting
a common origin (e.g. accretion disks or jet bases) for the nuclear fluxes. We find
agreement with the work of others that the nuclear flux and black hole masses are not
correlated, though the width of the broad components, described above may correlate
with the nuclear flux.

Contents
1 Introduction 1
1.1 Radio galaxies 3
1.2 Nuclear dust and gas 6
1.3 Connections to supermassive black holes 10
1.4 This dissertation 14
2 The UGC FR-I Sample 26
2.1 Sample selection and properties 26
2.2 Multiwavelength observations 28
2.2.1 Radio properties . . . . . . . . . . . . . . . . . . . . . . . . . . . . . 29
2.2.2 Optical properties . . . . . . . . . . . . . . . . . . . . . . . . . . . . . 29
2.3 Stellar Dynamics 30
3 STIS spectroscopy of the emission line gas in the nuclei
i

of nearby FR-I galaxies 57
3.1 Introduction 57
3.2 STIS Observations 58
3.2.1 Data Reduction . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . 61
3.3 Analysis 62
3.3.1 Single Gaussian line fitting . . . . . . . . . . . . . . . . . . . . . . . . 62
3.3.2 Fits with an additional free component . . . . . . . . . . . . . . . . . 65
3.3.3 Quantifying error sources . . . . . . . . . . . . . . . . . . . . . . . . 67
3.4 Individual galaxy descriptions 69
3.5 Interpretation and Discussion 79
3.5.1 Rotators and non-rotators . . . . . . . . . . . . . . . . . . . . . . . . 79
3.5.2 Flux ratios and ionization . . . . . . . . . . . . . . . . . . . . . . . . 83
3.5.3 Are we observing broad lines? . . . . . . . . . . . . . . . . . . . . . . 83
3.5.4 Constraining the line shapes . . . . . . . . . . . . . . . . . . . . . . . 85
3.6 Conclusions 87
4 Modeling gas in gravitational potentials 147
4.1 Introduction 147
4.2 Thin disk models with and without a black hole 149
4.2.1 WFPC2 imaging: stars and dust . . . . . . . . . . . . . . . . . . . . . 150
4.2.2 Flux distributions . . . . . . . . . . . . . . . . . . . . . . . . . . . . 151
ii

4.2.3 Stellar luminosity densities and mass distributions . . . . . . . . . . . 152
4.2.4 Dynamical models . . . . . . . . . . . . . . . . . . . . . . . . . . . . 155
4.2.5 Locating the zero point velocities . . . . . . . . . . . . . . . . . . . . 157
4.2.6 Sensitivity to parameters . . . . . . . . . . . . . . . . . . . . . . . . 158
4.3 Descriptions of individual galaxies 161
4.4 Discussion 172
4.4.1 Description of the central kinematics . . . . . . . . . . . . . . . . . . 172
4.4.2 Settling of the gas into a thin disk . . . . . . . . . . . . . . . . . . . . 174
4.4.3 Drivers of unsettled motion . . . . . . . . . . . . . . . . . . . . . . . 176
4.5 Conclusions 179
5 Nuclear gas kinematics and central engines 234
5.1 Introduction 234
5.2 Global kinematic parameterizations 236
5.2.1 Effects of inclination . . . . . . . . . . . . . . . . . . . . . . . . . . . 238
5.2.2 Correlations between kinematic parameters . . . . . . . . . . . . . . . 242
5.2.3 Relationships to the stellar kinematics . . . . . . . . . . . . . . . . . 244
5.3 The central engines 246
5.3.1 Are the Broad Lines physical? . . . . . . . . . . . . . . . . . . . . . . 247
5.3.2 Correlation of nuclear fluxes . . . . . . . . . . . . . . . . . . . . . . . 249
5.3.3 Correlations between host galaxy and central engine . . . . . . . . . . 250
5.4 Conclusions 252
iii

6 Conclusions 272
6.1 Summary 272
6.2 Future directions 276
References 284
iv

List of Tables
1.1 Properties of various classes of Active Galactic Nuclei. . . . . . . . . 16
1.2 Reliable black hole mass measurements. . . . . . . . . . . . . . . . . . 17
2.1 Properties of the galaxy sample members. . . . . . . . . . . . . . . . 32
2.2 Multiwavelength Fluxes of the UGC FR-I Sample Galaxies. . . . . . . 33
2.3 Stellar velocity dispersions and estimated black hole masses. . . . . . 34
3.1 HST-STIS G750M observing log for this program. . . . . . . . . . . . 89
3.2 HST/STIS Instrumental properties for the configurations used. . . . 90
3.3 Position angles of various axes. . . . . . . . . . . . . . . . . . . . . . 91
3.4 Spectral Lines in the region of Hα. . . . . . . . . . . . . . . . . . . . 92
3.5 NGC 193: Measured Parameters. . . . . . . . . . . . . . . . . . . . . 93
3.6 NGC 315: Measured Parameters. . . . . . . . . . . . . . . . . . . . . 94
3.7 NGC 383: Measured Parameters. . . . . . . . . . . . . . . . . . . . . 95
3.8 NGC 541: Measured Parameters. . . . . . . . . . . . . . . . . . . . . 96
3.9 NGC 741: Measured Parameters. . . . . . . . . . . . . . . . . . . . . 97
3.10 UGC 01841: Measured Parameters. . . . . . . . . . . . . . . . . . . 98
3.11 NGC 2329: Measured Parameters. . . . . . . . . . . . . . . . . . . . 99
3.12 NGC 2892: Measured Parameters. . . . . . . . . . . . . . . . . . . . 100
3.13 NGC 3801: Measured Parameters. . . . . . . . . . . . . . . . . . . . 101
v

3.14 NGC 3862: Measured Parameters. . . . . . . . . . . . . . . . . . . . 102
3.15 UGC 7115: Measured Parameters. . . . . . . . . . . . . . . . . . . . 103
3.16 NGC 4261: Measured Parameters. . . . . . . . . . . . . . . . . . . . 104
3.17 NGC 4335: Measured Parameters. . . . . . . . . . . . . . . . . . . . 105
3.18 M84 : Measured Parameters. . . . . . . . . . . . . . . . . . . . . . . 106
3.19 NGC 4486: Measured Parameters. . . . . . . . . . . . . . . . . . . . 107
3.20 NGC 5127: Measured Parameters. . . . . . . . . . . . . . . . . . . . 108
3.21 NGC 5141: Measured Parameters. . . . . . . . . . . . . . . . . . . . 109
3.22 NGC 5490: Measured Parameters. . . . . . . . . . . . . . . . . . . . 110
3.23 NGC 7052: Measured Parameters. . . . . . . . . . . . . . . . . . . . 111
3.24 UGC 12064: Measured Parameters. . . . . . . . . . . . . . . . . . . 112
3.25 NGC 7626: Measured Parameters. . . . . . . . . . . . . . . . . . . . 113
3.26 Effect of making various fit parameters free. . . . . . . . . . . . . . . 114
3.27 Presence of a Nuclear Broad Line. . . . . . . . . . . . . . . . . . . . . 115
3.28 Fits to the central pixel for each galaxy, including broad lines. Kinematics.
. . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . 116
3.29 Fits to the central pixel for each galaxy, including broad lines. Fluxes. 117
3.30 Kinematic estimators within 100 pc of the nucleus. . . . . . . . . . . 118
3.31 Comparison of broad line statistics . . . . . . . . . . . . . . . . . . . 119
3.32 Kinematic parameters measured using various free-parameter sets. . 120
4.1 Disk inclinations and dust masses. . . . . . . . . . . . . . . . . . . . 182
4.2 STIS PSF Parameters. . . . . . . . . . . . . . . . . . . . . . . . . . 183
4.3 Luminosity density fit parameters. . . . . . . . . . . . . . . . . . . . 184
4.4 Mass to light ratio (Υ) estimates for sample galaxies. . . . . . . . . . 185
4.5 Best fitting velocity offsets. . . . . . . . . . . . . . . . . . . . . . . . 186
4.6 Black hole signatures in the central kinematics. . . . . . . . . . . . . 187
vi

5.1 Weighted mean kinematic parameters. . . . . . . . . . . . . . . . . . 255
5.2 Correlation of X-ray flux with other nuclear flux parameters. . . . . 256
5.3 Correlations between kinematic parameters and nuclear fluxes. . . . . 257
vii

List of Figures
1.1 A cartoon radio galaxy. . . . . . . . . . . . . . . . . . . . . . . . . . . 18
1.2 An example of an FR-I and an FR-II radio galaxy . . . . . . . . . . . 19
1.3 The Unified Scheme for Active Galactic Nuclei. . . . . . . . . . . . . 20
1.4 Non uniform dust disks in NGC 383. . . . . . . . . . . . . . . . . . . 21
1.5 The segregation of AGNs based on the circumnuclear gas disk. . . . . 22
1.6 Feeding the central engine. . . . . . . . . . . . . . . . . . . . . . . . . 23
1.7 Velocity cusp in the nucleus of M87. . . . . . . . . . . . . . . . . . . . 24
1.8 The M• − σc relation. . . . . . . . . . . . . . . . . . . . . . . . . . . . 25
2.1 Optical continuum image of the nuclear region of NGC 193. . . . . . 35
2.2 Optical continuum image of the nuclear region of NGC 315. . . . . . 36
2.3 Optical continuum image of the nuclear region of NGC 383. . . . . . 37
2.4 Optical continuum image of the nuclear region of NGC 541. . . . . . 38
2.5 Optical continuum image of the nuclear region of NGC 741. . . . . . 39
2.6 Optical continuum image of the nuclear region of UGC 1841. . . . . . 40
2.7 Optical continuum image of the nuclear region of NGC 2329. . . . . . 41
2.8 Optical continuum image of the nuclear region of NGC 2892. . . . . . 42
2.9 Optical continuum image of the nuclear region of NGC 3801. . . . . . 43
2.10 Optical continuum image of the nuclear region of NGC 3862. . . . . . 44
2.11 Optical continuum image of the nuclear region of UGC 7115. . . . . . 45
viii

2.12 Optical continuum image of the nuclear region of NGC 4261. . . . . . 46
2.13 Optical continuum image of the nuclear region of NGC 4335. . . . . . 47
2.14 Optical continuum image of the nuclear region of M84. . . . . . . . . 48
2.15 Optical continuum image of the nuclear region of NGC 4486. . . . . . 49
2.16 Optical continuum image of the nuclear region of NGC 5127. . . . . . 50
2.17 Optical continuum image of the nuclear region of NGC 5141. . . . . . 51
2.18 Optical continuum image of the nuclear region of NGC 5490. . . . . . 52
2.19 Optical continuum image of the nuclear region of NGC 7052. . . . . . 53
2.20 Optical continuum image of the nuclear region of UGC 12064. . . . . 54
2.21 Optical continuum image of the nuclear region of NGC 7626. . . . . . 55
2.22 The M• − σc relation. . . . . . . . . . . . . . . . . . . . . . . . . . . . 56
3.1 Key to observation and fit data plots. . . . . . . . . . . . . . . . . . . 121
3.2 Observation and fit data for NGC 193 . . . . . . . . . . . . . . . . . 122
3.3 Observation and fit data for NGC 315 . . . . . . . . . . . . . . . . . 123
3.4 Observation and fit data for NGC 383 . . . . . . . . . . . . . . . . . 124
3.5 Observation and fit data for NGC 541 . . . . . . . . . . . . . . . . . 125
3.6 Observation and fit data for NGC 741 . . . . . . . . . . . . . . . . . 126
3.7 Observation and fit data for UGC 1841 . . . . . . . . . . . . . . . . . 127
3.8 Observation and fit data for NGC 2329 . . . . . . . . . . . . . . . . . 128
3.9 Observation and fit data for NGC 2892 . . . . . . . . . . . . . . . . . 129
3.10 Observation and fit data for NGC 3801 . . . . . . . . . . . . . . . . . 130
3.11 Observation and fit data for NGC 3862 . . . . . . . . . . . . . . . . . 131
3.12 Observation and fit data for UGC 7115 . . . . . . . . . . . . . . . . . 132
3.13 Observation and fit data for NGC 4261 . . . . . . . . . . . . . . . . . 133
3.14 Observation and fit data for NGC 4335 . . . . . . . . . . . . . . . . . 134
ix

3.15 Observation and fit data for NGC 4374 . . . . . . . . . . . . . . . . . 135
3.16 Observation and fit data for NGC 4486 . . . . . . . . . . . . . . . . . 136
3.17 Observation and fit data for NGC 5127 . . . . . . . . . . . . . . . . . 137
3.18 Observation and fit data for NGC 5141 . . . . . . . . . . . . . . . . . 138
3.19 Observation and fit data for NGC 5490 . . . . . . . . . . . . . . . . . 139
3.20 Observation and fit data for NGC 7052 . . . . . . . . . . . . . . . . . 140
3.21 Observation and fit data for UGC 12064 . . . . . . . . . . . . . . . . 141
3.22 Observation and fit data for NGC 7626 . . . . . . . . . . . . . . . . . 142
3.23 Difference in mean velocity within 100 pc of each side of the nucleus . 143
3.24 Difference in mean velocity within 100 pc of each side of the nucleus . 144
3.25 Mean gas velocity dispersion within 100 pc of the nucleus . . . . . . . 145
3.26 [N II] against Hα fluxes for the UGC FR-I sample members . . . . . . 146
4.1 Data-Model residuals with varying velocity offsets for NGC 193. . . . 188
4.2 Data-Model residuals with varying velocity offsets for NGC 315. . . . 189
4.3 Data-Model residuals with varying velocity offsets for NGC 383. . . . 190
4.4 Data-Model residuals with varying velocity offsets for NGC 541. . . . 191
4.5 Data-Model residuals with varying velocity offsets for NGC 741. . . . 192
4.6 Data-Model residuals with varying velocity offsets for UGC 1841. . . 193
4.7 Data-Model residuals with varying velocity offsets for NGC 2329. . . 194
4.8 Data-Model residuals with varying velocity offsets for NGC 2892. . . 195
4.9 Data-Model residuals with varying velocity offsets for NGC 3862. . . 196
4.10 Data-Model residuals with varying velocity offsets for NGC 4335. . . 197
4.11 Data-Model residuals with varying velocity offsets for M84. . . . . . . 198
4.12 Data-Model residuals with varying velocity offsets for NGC 4486. . . 199
4.13 Data-Model residuals with varying velocity offsets for NGC 5127. . . 200
x

4.14 Data-Model residuals with varying velocity offsets for NGC 5141. . . 201
4.15 Data-Model residuals with varying velocity offsets for NGC 5490. . . 202
4.16 Data-Model residuals with varying velocity offsets for NGC 7052. . . 203
4.17 Data-Model residuals with varying velocity offsets for UGC 12064. . . 204
4.18 Data-Model residuals with varying velocity offsets for NGC 7626. . . 205
4.19 Effect of changing the STIS PSF. . . . . . . . . . . . . . . . . . . . . 206
4.20 Central observations of M87. . . . . . . . . . . . . . . . . . . . . . . . 207
4.21 Varying Υ, q ′ and i in models of NGC 193. . . . . . . . . . . . . . . . 208
4.22 Varying Υ, q ′ and i in models of NGC 4335. . . . . . . . . . . . . . . 209
4.23 Observed and modeled velocity profiles for NGC 193. . . . . . . . . . 210
4.24 Observed and modeled velocity profiles for NGC 315. . . . . . . . . . 211
4.25 Observed and modeled velocity profiles for NGC 383. . . . . . . . . . 212
4.26 Observed and modeled velocity profiles for NGC 541. . . . . . . . . . 213
4.27 Observed and modeled velocity profiles for NGC 741. . . . . . . . . . 214
4.28 Observed and modeled velocity profiles for UGC 1841. . . . . . . . . 215
4.29 Observed and modeled velocity profiles for NGC 2329. . . . . . . . . 216
4.30 Observed and modeled velocity profiles for NGC 2892. . . . . . . . . 217
4.31 Observed and modeled velocity profiles for NGC 3862. . . . . . . . . 218
4.32 Observed and modeled velocity profiles for NGC 4261. . . . . . . . . 219
4.33 Observed and modeled velocity profiles for NGC 4335. . . . . . . . . 220
4.34 Observed and modeled velocity profiles for M84. . . . . . . . . . . . . 221
4.35 Observed and modeled velocity profiles for NGC 4486. . . . . . . . . 222
4.36 Observed and modeled velocity profiles for NGC 5127. . . . . . . . . 223
4.37 Observed and modeled velocity profiles for NGC 5141. . . . . . . . . 224
4.38 Observed and modeled velocity profiles for NGC 5490. . . . . . . . . 225
4.39 Observed and modeled velocity profiles for NGC 7052. . . . . . . . . 226
xi

4.40 Observed and modeled velocity profiles for UGC 12064. . . . . . . . . 227
4.41 Observed and modeled velocity profiles for NGC 7626. . . . . . . . . 228
4.42 NGC 4335, observations with jet locations indicated. . . . . . . . . . 229
4.43 NGC 7626, observations with jet locations indicated. . . . . . . . . . 230
4.44 NGC 193, observations with jet locations indicated. . . . . . . . . . . 231
4.45 UGC 12064, observations with jet locations indicated. . . . . . . . . . 232
4.46 The M• − σc relation with UGC FR-I black hole limits indicated. . . 233
5.1 Difference in weighted mean velocity within 100 pc on each side of the
nucleus in the central slit as a function of dust axis ratio. . . . . . . . 258
5.2 Weighted mean gas velocity dispersion along the central slit of each
galaxy as a function of dust axis ratio. . . . . . . . . . . . . . . . . . 259
5.3 Weighted mean point-to-point variations in gas velocity along the central
slit as a function of dust disk axis ratio. . . . . . . . . . . . . . . 260
5.4 σ100 2 /∆ 2 100
as a function of dust axis ratio. . . . . . . . . . . . . . . . 261
5.5 σ100 as a function of ∆100 for the sample nuclei. . . . . . . . . . . . . 262
5.6 ɛ100 as a function of ∆100 for the sample nuclei. . . . . . . . . . . . . 263
5.7 ɛ100 as a function of σ100 for the sample nuclei. . . . . . . . . . . . . . 264
5.8 ∆100 for each nucleus as a function of the central stellar velocity dispersion
(σc). . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . 265
5.9 σ100 for each nucleus as a function of the central stellar velocity dispersion
(σc). . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . 266
5.10 ɛ100 for each nucleus as a function of the central stellar velocity dispersion
(σc). . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . 267
5.11 σ100 2 /∆2 100 for each nucleus as a function of the central stellar velocity
dispersion (σc). . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . 268
5.12 Correlations between nuclear fluxes. . . . . . . . . . . . . . . . . . . . 269
5.13 Nuclear SEDs for 5 of the UGC FR-I sample galaxies. . . . . . . . . . 270
5.14 Model SEDs for M87. . . . . . . . . . . . . . . . . . . . . . . . . . . . 271
xii

Acknowledgments
First I would like, of course, to thank my parents, Jenny and Peter, and my entire
family. I must also thank my scientific collaborators, without whom this thesis would
not have been even remotely possible: Gijs Verdoes Kleijn, Stefi Baum, Jacqueline
van Gorkom, Chris O’Dea, Roeland van der Marel, Tim de Zeeuw, and Marcella
Carollo. I also thank many wonderful astronomers for discussions on these topics -
in particular Aaron Barth and Dave Axon, and also Johann Knapen, Luis Ho and
Thaisa Storchi-Bergmann for organizing fantastic conferences that have taken me
from start to finish of this thesis.
Everyone that I have known in the astronomy department, you have been fantastic.
In particular thanks to Aeree Chung and Stephen Muchovej, your friendship is very
important to me... and we will always have Rio! I also want to give particular thanks
to Millie Kramer-Garcia for being possibly the most outstanding, amazing, awesome
department administrator in the history of the entire universe. Probably without you
none of us graduate students would make it past one week of grad school.
Mark Wainer, Simon Stam, Daniel Baker and Alex Vitti – thank you guys so
much for always keeping me going, and for keeping me smiling. Your friendship has
been outstanding, and I will value it forever.
I want to thank fantastic friends that I have had through the years – Ethan
Hurdus, Neil Corbett, Jon Doyle, Stuart Laverack, Eileen Brain, Jackie Bletcher,
Jonathan Bletcher, Adam Pogash, Daniel Pogash, Carrie Johnston, Lucy Edge, Abi
Bralee, Tzu-Ching Chang, Andy Jacobowitz, Karen Vanlandingham, Ben Clissold,
Solomon Meltser, Gina Brissenden, and John Drury – Just for being amazing people.
Gareth Repton, Jon Soyt, Matt Schoen, Steven Turner, Adam Simon, Daniel
Bryer, Eric Lunin, Ariel Stukalin, Cliff Shapiro, Seth Kahn, Scott Menke, Ben Silverman,
James Dawson, Isaac Gerstein, Peter Plant, Freddie Claro, Stephen Conlon,
Brian Bolin, Alex Chval, Andrew Prouty, T.J. Wagner, Jake Skinner, Michael
Seiler, Billie Swift, Heather Groch, Dan Balick, Tim Mendenko, Jeff Wincek, Charles
Stanton-Jones, Eilat Glikman, Suvi Gezari, Andreea Petric, Jen Donovan, Mark Dijkstra,
Sarah Tuttle, Ben Johnson, and Antara Basu-Zych – You guys rule! (James
Dawson, you have been the man through the last few weeks of getting this dissertation
written - Thanks dude).
Everyone else I didn’t have space to write about – Thank you all too!!
Thank you.
xiii

To:
Lofty
Jenny, Peter
Everyone who has ever set foot at Camp Watonka and made it feel like home year
after year, and especially all of my campers.
and Spencer and Ceci... In 21 years I expect to be reading your PhD theses!
xiv

Chapter 1
Introduction
The relationship between quiescent and active early type galaxies bears on our un-
derstanding of black holes and their role in the active nuclei of galaxies, and on the
evolution of galactic nuclei along with their host galaxies. Nearby early-type galaxies
with radio jets provide an opportunity to gain an understanding of the conditions in
a galaxy which lead to the formation of a radio-active nucleus and of the physics of
the regions which harbor the black hole and jet-formation regimes.
In this dissertation, we present a detailed analysis of the kinematics of the emission
line gas in the nuclei of a complete sample of nearby, radio galaxies. This forms a
part of a larger, coordinated, multi-wavelength study of the same sample, which is
described in the next chapter.
1

The study of radio galaxies addresses some important astrophysical questions that
pertain to the nature of active galaxies in general:
• How does fuel get into the central engine? How do active and inactive galaxies
differ in terms of fuel and fueling?
• What connections exist between host galaxies, central engines and central su-
permassive black holes?
• How do radio galaxies fit into ‘unified schemes’ that describe various types of
active galaxy?
In this chapter we will first introduce the reader to radio galaxies, which are strong
radio sources associated with luminous elliptical galaxies, next our discussion moves
inwards to focus on the gas and dust that has been found in many of radio galaxy
nuclei. We increase magnification still further as we go on to talk about the search
for supermassive black holes and the connections they have to the galaxy as a whole,
particularly relationships between the black hole masses (M•) and the large scale
stellar kinematics. We close by outlining the contents of this dissertation.
2

1.1 Radio galaxies
A radio galaxy can produce a jet-lobe, radio wavelength emitting, structure on mega-
parsec scales, emerging from a central engine that resides in an active region no more
than a few milli-parsecs in size. The radio emission is well understood to be from
synchrotron radiation, but the processes involved in fueling and collimating the ra-
dio jets are yet to be explained (Lynden-Bell, 2001). The energy that powers the
radio jets is typically believed to be produced during the accretion of material onto
a central supermassive black hole (e.g., Lynden-Bell, 1969). The formation of such
well organized large scale jet structures is some of the most compelling evidence for
the necessity of supermassive black holes as an ingredient in the makeup of a radio
galaxy (Rees, 1984).
Radio emission can be detected even from relatively quiescent galaxies, such
as the Milky Way, on the level of around 10 37 erg s −1 . Active galaxies (such as
Seyferts or starburst galaxies) radiate at around 10 37 erg s −1 , and radio galaxies (and
also quasars) extend this energy output range to beyond 10 45 erg s −1 (∼ 10 12 L⊙)
(Burke & Graham-Smith, 1997). An active galaxy central engine capable of releas-
ing ∼ 0.1Mfuelc 2 of infalling fuel as radiation would need to be fueled at a rate of
∼> 1 M⊙ yr −1 to maintain this luminosity.
3

The ‘cartoon view’ of a typical radio galaxy structure contains a bright core from
which emanate two jets of radio emitting material which terminate in two large radio
lobes. (Figure 1.1 shows such a cartoon view). Two classes of radio galaxy were
defined by Fanaroff & Riley (1974) based on the morphology of the radio emission.
Fanaroff-Riley Class I galaxies (FR-Is) are brightest at the inner jets, with emission
that becomes gradually fainter out into the radio lobes, while in the more powerful
FR-II galaxies, hot spots at the outer edges of the radio lobes dominate the emission.
Owen & Ledlow (1997) present observations of many radio galaxies, illustrating of
course that there are many inadequacies in such a simplified viewpoint; in Figure 1.2
we present examples of a typical FR-I and FR-II galaxy from their sample.
Radio galaxies belong to the class of galaxies that have Active Galactic Nuclei
(AGN) which are characterized by large energy outputs from very small regions in
their cores. Commonly, the ‘Unified Scheme’ (Urry & Padovani, 1995) is used to
explain different properties of the different types of AGN and the connections between
them, principally by observing the model from varying orientations. A representation
of an AGN according to the unified scheme is shown in Figure 1.3. Various types of
AGN and their properties are listed in Table 1.1. The type of AGN and host galaxy
are also linked, radio galaxies being almost exclusively found in early-type (elliptical
or S0) galaxies.
4

This thesis focuses on a sample of nearby radio galaxies (see Chapter 2). The
sample is complete out to redshifts of 7000 km s −1 (100 Mpc) in the northern hemi-
sphere, and contains only FR-I galaxies, as no FR-IIs are found in this volume (there
is only one FR-II within 7000 km s −1 , Centaurus A, which is in the southern sky at a
declination of ∼ −43 ◦ ). Radio galaxies and BL-Lacs provide a high energy contrast to
Seyfert galaxies and LINERs (Low Ionization Narrow line Emission Region galaxies),
and may be close cousins of the Quasars observed at higher redshifts.
Both FR-I and FR-II galaxies have jets that are well collimated on all scales,
though FR-Is tend to be more prone to having twisted and ‘blobby’ jets while FR-IIs
tend to have straighter more uniform jets (see Bridle, 1984). The accepted paradigm
is that the jets start out at relativistic velocities in both FR-Is and FR-IIs, but that
in FR-Is the jets then decelerate on scales less than ∼ 1 kpc. (Bridle & Perley,
1984, provide a review of the phenomenology of extragalactic jets). The most elegant
demonstration that flow may actually takes place along the jets is presented by Biretta
et al. (1999), who while monitoring the jet of M87 over four years were able to trace
the motion of blobs of emission, providing compelling evidence that some type of flow
does occur along the jets.
Baum et al. (1995) describe various differences in the populations of FR-I and FR-
5

II galaxies. They note that at the same host galaxy magnitude or radio luminosity
FR-IIs can produce and order of magnitude more optical line emission than FR-Is.
This led them to conclude that FR-IIs were predominantly ionized by continuum
sources in the AGN, while in FR-Is the host galaxy may also play an important
role in the ionization of the emission line gas. Following earlier work by Rees et al.
(1982), Baum et al. (1995) also propose that FR-I galaxies may be produced when
the central engine is fed at a lower accretion rate and FR-IIs are produced when the
fuel is being accreted more quickly. Understanding the fueling of the central engines
of nearby radio galaxies, or at least better understanding the kinematic nature of the
fuel sources, may lead to greater understanding of the physical mechanisms driving
this dichotomy.
1.2 Nuclear dust and gas
Though when observed on the sky elliptical galaxies can appear smooth and largely
featureless, the Hubble Space Telescope (HST) was able to resolve dust and gas fea-
tures present in their central regions (Jaffe et al., 1993; Ford et al., 1994). Central
emission line dust and gas disks are detected in about 20% of all giant ellipticals,
and virtually all nearby radio galaxies that harbor kiloparsec scale radio jets (e.g.
van Dokkum & Franx, 1995; Verdoes Kleijn et al., 1999; Capetti et al., 2000; de Koff
6

et al., 2000; Tomita et al., 2000; Tran et al., 2001; Laine et al., 2003). This dust and
gas presumably provides a bulk of the fuel for the central engine.
The kinematics of the disk are not well understood, and important questions
remain regarding the importance of non-circular motions (such as turbulence, inflow,
outflow, winds, etc...). It is also of interest whether these disks are short lived or
long lived, and whether they are providing fuel to the central engine or playing a
role in the collimation of the jets. Disks have been identified that are non-uniform in
continuum light and are surrounded by arcs, filaments, and diffuse absorbing clumps,
suggesting that the dust (and by association the gas) in the cores of these galaxies is
not dynamically settled (for example, Martel et al., 2000, ; Figure 1.4).
Assuming that this gas and dust indeed provides the primary fuel source of the
central engine, a long standing problem is the ‘fueling problem’ – that is how to
remove the large angular momentum of the gas in a disk and get it into the central
engine. This problem is described in a well known cartoon by Phinney (1994) of a
baby being fed by a huge (angular momentum) spoon into its tiny mouth (Figure 1.6).
Also, typical findings are that 60% of quiescent early-type galaxies have detections
of emission line gas (e.g. Philips et al., 1986; Goudfrooij et al., 1994) and about 40%
have nuclear dust (e.g. van Dokkum & Franx, 1995; Tran et al., 2001). Despite the
7

apparent presence of fuel, these galaxies fail to produce radio jets or any significant
nuclear activity.
Unified schemes (see above) suggest that the ionized gas disk not intersect the
photo-ionization cone of the central engine, which would require that the disks be
shock ionized (Doptia et al., 1997). An investigation of the ionization structure of the
disk, and any variations, can therefore reveal properties important to understanding
and confirming the position of FR-I galaxies in such schemes. The nature of the gas
disks is differentiated between the different types of AGN with key parameters being
the gas mass, the black hole mass and the star formation rate. Different AGN can be
plotted as a function of these parameters as represented in Figure 1.5. Radio Galaxies
have large black hole masses, low star formation rates and relatively low gas masses
so would fall into the same region of this plot as occupied by the quasars (QSOs).
Different fueling mechanism may operate to bring the fuel into the center depending
on these parameters (see Wada, 2004, for a recent review).
Asymmetries in galaxy potentials can induce dynamical resonances that perturb
the gas dynamics in the central regions. Hydrodynamical simulations (e.g., Ma-
ciejewski, 2004) show that these resonances, and the resulting perturbations in the
gas motions, can be governed primarily by the central black hole and on scales much
8

larger than the generally expected sphere of influence (see Equation 1.1 below). These
results may imply that the central black hole is able to have kinematic influences far
into the gas disk, and may even be able to regulate flow (and hence the fueling of the
central engine) though these mechanisms.
The nuclear gas and dust may be perturbed by sources unrelated to the gravita-
tional potential of the galaxy, for example interactions with jets, starburst activity
and galactic mergers, each of which could have considerable consequences for the
kinematics of the gas, and the organization of structures in the central regions of
these galaxies.
Solórzano-Iñarrea et al. (2001) suggest that the emission line gas may be affected
by jet induced shocks even in sources where the radio emission structures are much
larger in extent than the regions of emission line gas (as is the case for the radio
galaxies described in this thesis). It would take a certain amount of misalignment
between jet and disk for such interactions to be possible, and such large misalignments
between disks and jets may be observed in some radio galaxies (Schmitt et al., 2002;
Verdoes Kleijn & de Zeeuw, 2004).
Starbursts and AGN go hand in hand in many galactic nuclei (Beckman, 2001)
and episodes of star burst activity could induce shocks into the gas disks, having a
9

pronounced effect of the observed kinematics. The gas in the emission line disk is
an obvious source of fuel for any starburst activity that may have taken place, which
would have had dramatic consequences for the disk kinematics the remnants of which
may not be fast to dissipate. Galactic mergers in the evolutionary history of the radio
galaxy would also have disrupted the gas: both by the addition of new gas into the
disk and by tidal disruption of the gas by the merging galaxy.
1.3 Connections to supermassive black holes
Current evidence suggests that all galaxies may have a central supermassive black
hole and that the mass of this black hole is a strong function of the mass and lumi-
nosity of the mass spheroid in which it presently resides (for example, Kormendy &
Richstone, 1995), and an even stronger function of the central stellar velocity disper-
sion (Ferrarese & Merritt, 2000; Gebhardt et al., 2000a; Merritt & Ferrarese, 2001;
Tremaine et al., 2002). It is not clear what drives these relationships or whether they
are the same for active and quiescent galaxies. Since black hole growth and nuclear
activity are causally related, scatter in these relationships can, in principle, put limits
on the frequency and duration of nuclear activity in galaxies.
Four principle methods exist for the direct measurement of black hole masses. The
10

most reliable is, of course, by the measurement of the proper motions and accelerations
of the stars in the closest orbits to the black hole. This has now been achieved in
the nucleus of our own galaxy (Ghez et al., 1998; Melia & Falcke, 2001; Reid et al.,
2003; Ghez et al., 2003), though this will be the only case where we can make these
measurements. Kinematics of water masers in the inner nuclei also provide what
appear to be very robust measurements of the black hole mass (Greenhill & Gwinn,
1997; Herrnstein et al., 1999), though cases with suitable maser organization and
orientation prove hard to find. For larger samples, one must use dynamical modeling
either of the stars or of the gas in the nuclear region of the galaxy.
A black hole of mass M• dominates the gravitational potential inside an angular
‘radius of influence’ given by
θ• ∼ 0. ′′ 1
� M•
10 6 M⊙
� � �
−1 2 �1Mpc �
100km s
σ
D
11
(1.1)
Where θ• is the angular size projected on the sky of the radius of influence of
the black hole, σ is a typical velocity dispersion of stars in the galaxy and D is the
distance to the galaxy in Mpc. For typical nearby galaxies, this radius of influence
will be less than an arcsecond, so that the Hubble Space Telescope is required to make
the necessary observations.
The mass of the black hole may be sought by modeling the observed line of sight

velocity distribution of the stars in a galaxy by superimposing collections of stellar
orbits and a range of different black hole masses to determine the best fitting model
velocity profile, using χ 2 minimization techniques. The most reliable models must
include the Energy, Angular Momentum and Third-Integral of motion, and are there-
fore known as ‘three-integral’ models. While mass estimates obtained through these
means are often taken to be the most reliable, Valluri et al. (2004) remind us that we
do not know if orbits that physically exist in a galaxy are being selected to generate
the models, and that the errors in the fitting procedure are not normally distributed,
but more represent a range of equally acceptable values.
Finally, in what seems the most straightforward method at the outset, the mass
of a central black hole can be measured through the induced cusp in the rotation
velocities of gas in the nucleus of the galaxy (see Figure 1.7). State of the art models
do not account for dissipative effects or non-circular, coplanar motions and these
deviations from the circular thin disk model have important consequences for the
determination of black hole masses. Understanding these motions in the nuclei of
galaxies will allow further progress to be made in this field.
With the advent of HST, and the arrival of the necessary angular resolution to
probe scales of interest to black hole hunters, early emission line spectra of a few
12

galaxies were obtained with the Faint Object Spectrograph (FOS). FOS was a single
aperture spectrograph and therefore rather inefficient for mapping velocity fields,
however early results were encouraging and showed that the kinematic signatures of
black holes could indeed be detected in the nuclei of some galaxies (Harms et al.,
1994; Ferrarese et al., 1996; van der Marel & van den Bosch, 1998; Ferrarese & Ford,
1999). The Space Telescope Imaging Spectrograph (STIS, see Brown et al., 2002) was
installed on board HST in 1997 making it possible to obtain long slit spectra of the gas
disks in galactic nuclei, and map out the velocity fields with much greater efficiency,
spatial coverage and resolution. Though the velocity fields may now be mapped much
more precisely, we will see later in this thesis that the observed velocity fields are not
those of uniform, circular disks, but rather pose more of a challenge to interpret.
We show the most reliable black hole determinations to date, as assessed by
Tremaine et al. (2002), in Table 1.2. The means of determination of each M• (by
those methods described briefly above) are also indicated. These data are plotted
in Figure 1.8 against the stellar velocity dispersion in the inner parts of each galaxy
(σc) showing the conspicuous correlation between these two parameters that was first
noted by Ferrarese & Merritt (2000) and Gebhardt et al. (2000a).
The scales on which σc are measured are much larger than the nuclear regions
13

where the black hole dominates the potential, so the relationship implies a connection
between the formation and evolution of galaxies and the black holes they harbor.
Models describing this linked co-evolution, growing the systems that we observe today
from ‘seed’ black holes and small bulges, are beginning to provide some theoretical
frameworks to explain the observed correlations (Silk & Rees, 1998; Ostriker, 2000;
Haehnelt & Kauffmann, 2000; Adams et al., 2001). This type of co-evolution scenario
may also indicate that other connections between the central engine and large scale
host galaxy may exist.
1.4 This dissertation
In this dissertation we present investigations into a complete sample of nearby radio
galaxies, based primarily on spectroscopic observations obtained from the Hubble
Space Telescope. We set out to work towards answering the following questions:
• What is the nature of the spectra observed from the emission line gas in the
nuclei of nearby radio galaxies?
• What can be said about the masses of the black holes in these radio galaxies
based on the gas kinematics?
• How is the gas organized in the central regions?
14

• What connections can be found between the central engines and that gas?
Understanding these matters in nearby galaxies, where we are able to probe on
scales that may be meaningful in terms of the physical processes that take place, may
allow us in future to gain insights into how AGN relate to each other, and how we
might make more meaningful interpretations of data we receive from more distant
sources where we do not have the resolution to probe the nuclei in such detail.
In Chapter 2, we will describe the selection of our sample of 21, nearby, radio-loud
elliptical galaxies, and summarize some previous observational work on the sample. In
Chapter 3, we describe the Hubble Space Telescope (HST) spectroscopic observations
we obtained of the sample galaxies, and present the resulting data set. In Chapter 4
we discuss work we have carried out on modeling the gas in the gravitational potential
of the galaxies, with and without black holes, and in Chapter 5 we go on to discuss
the global kinematic state of the nuclear gas, some properties of the central engines
and possible connections between the two. We present a summary of our conclusions
and a description of future directions for this work in Chapter 6.
15

Table 1.1. Properties of various classes of Active Galactic Nuclei.
Type Broad Lines Narrow Lines Radio
(1) (2) (3) (4)
Radio-loud Quasars � � Loud
Radio-quiet Quasars � � Weak
Broad-line Radio Galaxies � � Loud
Narrow-line Radio Galaxies × � Loud
BL-Lacs × × Loud
Seyfert-1 � � Weak
Seyfert-2 × � Weak
LINERS × � No
Note. — Col. (1): Name of the type of AGN; Cols. (2-3): Are broad and
narrow gas emission lines present?; Col. (4): Is the AGN radio loud?
References. — Adapted from Table 1.2 of Krolik (1999)
16

Table 1.2. Reliable black hole mass measurements.
Name Type M• Method σ∗ Reference
(M ⊙ ) (km s −1 )
(1) (2) (3) (4) (5) (6)
Milky Way SBbc 1.8 × 10 6 s, p 103 (1)
M32 E2 2.5 × 10 6 s, 3I 75 (2)
M31 Sb 4.5 × 10 7 s 160 (3),(4),(5)
NGC 821 E4 3.7 × 10 7 s, 3I 209 (6),(7)
NGC 1023 SB0 4.4 × 10 7 s, 3I 205 (8)
NGC 1068 Sb 1.5 × 10 7 m 151 (9)
NGC 2778 E2 1.4 × 10 7 s, 3I 175 (6),(7)
NGC 2787 SB0 4.1 × 10 7 g 140 (10)
NGC 3115 S0 1.0 × 10 9 s 230 (11)
NGC 3245 S0 2.1 × 10 8 g 205 (12)
NGC 3377 E5 1.0 × 10 8 s, 3I 145 (6),(13)
NGC 3379 E1 1.0 × 10 8 s, 3I 206 (14)
NGC 3384 S0 1.6 × 10 7 s, 3I 143 (6),(7)
NGC 3608 E2 1.9 × 10 8 s, 3I 182 (6),(7)
NGC 4258 Sbc 3.9 × 10 7 m, a 130 (15)
NGC 4261 E2 5.2 × 10 8 g 315 (16)
NGC 4291 E2 3.1 × 10 8 s, 3I 242 (6),(7)
NGC 4342 S0 3.0 × 10 8 s, 3I 225 (17)
NGC 4459 S0 7.0 × 10 7 g 186 (10)
NGC 4473 E5 1.1 × 10 8 s, 3I 190 (6),(7)
NGC 4486 E0 3.0 × 10 9 g 375 (18),(19)
NGC 4564 E3 5.6 × 10 7 s, 3I 162 (6),(7)
NGC 4596 SB0 7.8 × 10 7 g 152 (10)
NGC 4649 E1 5.6 × 10 7 s, 3I 385 (6),(7)
NGC 4697 E4 1.7 × 10 8 s, 3I 177 (6),(7)
NGC 4742 E4 1.4 × 10 7 s, 3I 90 (20)
NGC 5845 E3 2.4 × 10 8 s, 3I 234 (6)
NGC 6251 E2 5.3 × 10 8 g 290 (21)
NGC 7052 E4 3.3 × 10 8 g 266 (22)
NGC 7457 S0 3.5 × 10 6 s, 3I 67 (6),(7)
IC 1459 E3 2.5 × 10 9 s, 3I 340 (23)
Note. — Data from Tremaine et al. (2002). Col. (1): Galaxy Name; Col. (2): Morphological Type; Col.
(3): Determined black hole mass; Col. (4): Method used, g - gas dynamics, m - maser dynamics, s - stars,
3I - three integral modeling, a - maser accelerations, p - proper motions; Col. (5): Central stellar velocity
dispersion; Col. (6): Reference for the Black Hole Mass
References. — Black Hole Mass References: (1) Chakrabarty & Saha (2001); (2) Verolme et al. (2002);
(3) Tremaine (1995); (4) Kormendy & Bender (1999); (5) Bacon et al. (2001); (6) Gebhardt et al. (2003); (7)
Pinkney et al. (2003); (8) Bower et al. (2001); (9) Greenhill & Gwinn (1997); (10) Sarzi et al. (2001); (11)
Kormendy et al. (1996); (12) Barth et al. (2001); (13) Kormendy et al. (1998); (14) Gebhardt et al. (2000b);
(15) Herrnstein et al. (1999); (16) Ferrarese et al. (1996); (17) Cretton & van den Bosch (1999); (18) Harms
et al. (1994); (19) Macchetto et al. (1997); (20) Kaiser, in preparation; (21) Ferrarese & Ford (1999); (22)
van der Marel & van den Bosch (1998); (23) Cappellari et al. (2002).
17

Lobe
Jet
Core
Optical galaxy
Jet
Lobe
Figure 1.1 A cartoon view of a radio galaxy showing the core, jets and lobes as observed
at radio wavelengths, a typical size scale for the elliptical host galaxy observed
at visible wavelengths is also indicated.
18

Figure 1.2 An example of a FR-I (left) and a FR-II (right) radio galaxy, observed at
20 cm wavelengths by Owen & Ledlow (1997). The FR-I is characterized by bright
jets, closest to the nucleus, while the FR-II has bright radio lobes.
19

Black Hole
Obscuring Torus
Jet
Jet
Broad Line
Clouds
Narrow Line Region
Obscuring Torus
Accretion Disk
Figure 1.3 A representation of the unified scheme for the central engine of active
galactic nuclei (AGN); different classes of AGN would be observed by viewing the
model from different angles. (after Urry & Padovani, 1995).
20

Figure 1.4 From Martel et al. (2000): The dust disk in the nucleus of NGC 383
showing intriguing morphological structures in the dust distribution.
21

Figure 1.5 From Wada (2004), the segregation of various types of AGNs from the
point of view of the circumnuclear gas disk.
22

Figure 1.6 The famous cartoon by Phinney (1994) capturing the essence of the fueling
problem in AGN: getting the food with the large (angular momentum) spoon into
the small (area and angular momentum) mouth.
23

Figure 1.7 Cusp in velocities in the nuclear region of M87. Dotted line indicates the
continuum flux. (figure from Macchetto et al., 1997).
24

M BH (M Sun)
10 10
10 9
10 8
10 7
10 6
60 70 80 90100 200 300 400
σ c (km s -1 )
Figure 1.8 Measured black hole masses (MBH) as a function of central stellar velocity
dispersion (σc) for reliable determinations summarized by Tremaine et al. (2002).
The line indicates the fit M• = 1.3 × 10 8 M⊙(σc/200) 4.72 . (*) indicates masses determined
from stellar dynamical modeling; (◦) indicates masses determined from gas
kinematics; and (△) indicates masses determined from MASER kinematics.
25

Chapter 2
The UGC FR-I Sample
In this Chapter we introduce the UGC FR-I galaxy sample, which is the central
sample of galaxies discussed in this dissertation. We briefly discuss the radio and
optical properties of the sample, and present some stellar kinematical data which
relates to relationships between black hole mass and properties of the host galaxies.
2.1 Sample selection and properties
Our galaxy sample (the UGC FR-I sample) contains all 21 nearby (vr < 7000 km s −1 ),
elliptical or S0 galaxies in the declination range −5 ◦ < δ < 70 ◦ in the UGC catalog
(Nilson, 1973, limits magnitude mB < 14. m 6 and angular size θp > 1. ′ 0) that are
extended radio-loud sources (larger than 10 ′′ at 3σ on VLA A-Array maps, which
crudely ensures that the sources are extended, and brighter than 150 mJy from single
26

dish flux density measurements at 1400 MHz). The source information is shown in
Table 2.1. The selection criteria result in a complete sample of nearby radio galaxies
with jets.
This complete sample was drawn from a catalog of 176 radio-loud galaxies con-
structed by Condon & Broderick (1988), by position coincidence of radio identifica-
tions in the Green Bank 1400 MHz sky maps and galaxies in the UGC catalog. All
of the galaxies fall into the Fanaroff & Riley (1974) Type-I (FR-I) radio classification
(see Xu et al., 2000, for a description of the radio properties of our sample); i.e. they
are low luminosity radio galaxies, with jets that are brightest nearest to the nucleus.
(In contrast, FR-II galaxies are more powerful radio sources, and have bright spots
at the far edges of their radio lobes, the only FR-II within 7000 km s −1 is the radio
galaxy Cen-A, which is in the southern sky.)
The combination of selecting extended sources and early type galaxies results in
the primary energy source of each galaxy in the sample falling into ‘monster’ rather
than ‘starburst’ classification of Condon & Broderick (1988) based on their infra-red
to radio flux ratios (for example, see Heckman et al., 1983)
u ≡ log
27
� �
S60µm
≪ 1.6, (2.1)
S1400MHz

and infra-red spectral gradients
αIR ≡
log (S60µm/S25µm)
log (60/25)
2.2 Multiwavelength observations
28
< +1.25. (2.2)
Prior to the work presented in this dissertation, imaging of the galaxies had been car-
ried out at various wavelengths with a variety of instruments. The fluxes of the UGC
FR-I nuclei in various wave-bands are given in Table 2.2. Particular attention has
been paid to the sample at radio and optical wavelengths, and we briefly summarize
those results below. We describe spectroscopic observations of the nuclei, that we
obtained using HST, in Chapter 3. In Figures 2.1 to 2.21 we show continuum optical
images of the central region of each galaxy – indicating the directions of the galaxy
major axes and radio jet axes, along with the positions of the spectroscopic slits (see
Chapter 3). The orientations of the slits compared to morphological features of the
nuclei are explained in the individual description of the observations given in §3.4 and
offsets are given in Table 3.3. For the majority of cases the STIS slits were aligned
within 10 ◦ of the galaxy major axis.

2.2.1 Radio properties
Radio observations of the sample galaxies were obtained using both the Very Large Ar-
ray (VLA; Wrobel, et al., in preparation) and the Very Large Baseline Array (VLBA),
descriptions of the radio morphology are given for each galaxy in §3.4. Xu et al. (2000)
report the results of a program using the VLBA to observe 17 of the UGC FR-I sam-
ple galaxies at 1.67 GHz. At a resolution of ∼ 10 × 4 mas, five galaxies showed only
an unresolved radio core, 10 galaxies showed core-jet structures, and two galaxies
showed twin-jet structures. Comparing the VLBA jets (on parsec scales) to the VLA
jets (on kiloparsec scales) they found that the VLBA and VLA jets are well aligned
and that the jet-to-counterjet surface brightness ratios, or the sidedness, decreases
systematically with increasing distance along the jet. Xu et al. (2000) attribute the
sidedness of the jets to the Doppler boosting effect, and its decline to the deceleration
of the jets.
2.2.2 Optical properties
A photometric analysis of the nuclei of the UGC FR-I sample galaxies was performed
by Verdoes Kleijn et al. (1999), based on observations made using the WFPC2 in-
strument on board HST (the photometric analyses of UGC 7115 and UGC 12064 are
29

presented in Appendix A of Verdoes Kleijn et al., 2002a). Verdoes Kleijn et al. (1999)
obtained V - and I-band images and narrow-band images centered on the Hα + [N II]
emission lines. They found that although obscuration by dust prevents satisfactory
determinations of the central cusp slopes, that the data suggest that most of the
sample galaxies have shallow cores.
Dust is detected in all but two galaxies and central emission line gas is detected in
all of the galaxies in the sample. There are a wide variety of central dust morphologies,
ranging from central disks to lanes and irregular distributions; the dust morphologies
for each individual source are described in §3.4.
2.3 Stellar Dynamics
We estimate the central stellar velocity dispersion (σc) within one eighth of the effec-
tive radius (re/8) using the relationship
� �
σap
σc
=
30
� �−0.04 rap
, (2.3)
re/8
as described by Jørgensen et al. (1995) and basing σap on ground based measure-
ments from various sources as referenced in Table 2.3.
We found the effective radii of the sample nuclei using the WFPC2 imaging de-

scribed by Verdoes Kleijn et al. (1999), and fitting a r 1/4 -law profile of the form
I = I0 exp (−7.67(x/re) 0.25 − 1) (2.4)
to the stellar surface brightness profile outside of the break radius.
This procedure to find σc follows the same prescription as Ferrarese & Merritt
(2000). Using their relationship between σc and M• (Merritt & Ferrarese, 2001):
M• = 1.30 × 10 8 M⊙
�
σc
200kms −1
31
� 4.72
, (2.5)
we estimate values of M• for our sample galaxies. The stellar velocity dispersions
and black hole mass estimates are listed in Table 2.3, where we also give measured
black hole masses for the 5 sample galaxies for which such data exist. The five
measured black hole masses are plotted on a M• − σc diagram including all reliable
black hole masses (cf Figure 1.8) in Figure 2.22.
Variations of this relationship give different values for M•, however for our pur-
poses in this dissertation we will give black hole mass estimates based on the above
relationship and remind the reader that the masses may vary somewhat from these
values.

Table 2.1. Properties of the galaxy sample members.
NGC UGC Other Names Type vsys STIS Scale MB log(L1400) Axis Ratio
(km s −1 ) (pc/pixel) (mag) (W Hz −1 ) b/a
(1) (2) (3) (4) (5) (6) (7) (8) (9)
193 408 E-S0 4342.5 15.0 -21.0 23.93 (0.18)
315 597 E 5092.5 17.6 -22.6 24.10 0.23
383 689 3C 31 E-S0 4890.0 16.9 -22.2 24.51 0.77
541 1004 E 5497.5 19.0 -21.7 23.94 0.91
741 1413 E 5265.0 18.2 -22.6 23.85 · · ·
1841 3C 66B E 6360.0 22.0 -22.5 24.94 ∼ 0.98
2329 3695 E-S0 5725.0 19.8 -21.9 23.76 0.68
2892 5073 E 6810.0 23.6 -21.1 23.36 · · ·
3801 6635 S0 3255.0 11.3 -20.8 23.49 (0.12)
3862 6723 3C 264 E 6330.0 21.9 -21.7 24.75 ∼ 0.99
7115 E 6787.5 23.5 -21.0 23.94 ∼ 0.95
4261 7360 3C 270 E 2212.5 7.7 -21.5 24.40 0.46
4335 7455 E-S0 4672.5 16.2 -21.6 23.11 0.41
4374 7494 M84, 3C 272.1 S0 1155.0 4.0 -20.9 23.35 (0.15)
4486 7654 M87, 3C 274 E 1155.0 4.0 -22.2 24.90 · · ·
5127 8419 E 4830.0 16.7 -21.3 24.08 (0.25)
5141 8433 S0 5302.5 18.4 -21.0 23.80 (0.25)
5490 9058 E 5790.0 20.1 -21.7 23.79 (0.35)
7052 11718 E 4155.0 14.4 -21.0 23.04 0.30
12064 3C 449 E-S0 5122.5 17.7 -20.8 24.38 0.54
7626 12531 E 3495.0 12.1 -21.7 23.37 (0.17)
Note. — Col. (1): NGC number where available; Col. (2): Upsalla General
Catalog (UGC) number; Col. (3): Alternative names; Col. (4): From the NASA
Extragalactic Database (NED); Col. (5): Measured from the stellar kinematics
(from NED); Col. (6): Parsecs per unbinned STIS pixel; Col. (7): Absolute blue
magnitude from Condon & Broderick (1988); Col. (8): Radio Luminosity from
Condon & Broderick (1988); Col. (9): Dust disk axis ratio from Verdoes Kleijn
et al. (1999), numbers in parentheses indicate a dust lane where the width:length
ratio is given instead.
32

Table 2.2. Multiwavelength Fluxes of the UGC FR-I Sample Galaxies.
Galaxy Vnuc Inuc VLBApeak VLApeak X-raysoft X-rayhard
(mJy/b.a.) (mJy/b.a.) (erg cm −2 s −1 ) (erg cm −2 s −1 )
(1) (2) (3) (4) (5) (6) (7)
NGC 193 6.20 × 10 −18 1.10 × 10 −17 29.8 40.0 · · · · · ·
NGC 315 3.30 × 10 −17 4.70 × 10 −17 224 396 4.63 × 10 −13 9.61 × 10 −13
NGC 383 2.40 × 10 −17 1.80 × 10 −17 44.1 89.0 3.91 × 10 −14 6.78 × 10 −14
NGC 541 7.50 × 10 −18 7.40 × 10 −18 1.90 8.00 · · · · · ·
UGC 1841 5.20 × 10 −17 3.70 × 10 −17 112 131 2.37 × 10 −13 8.79 × 10 −14
NGC 2329 1.70 × 10 −16 1.20 × 10 −16 49.7 117 · · · · · ·
NGC 2892 1.60 × 10 −17 1.40 × 10 −17 15.3 22.0 · · · · · ·
NGC 3862 1.90 × 10 −16 1.40 × 10 −16 123 386 · · · · · ·
UGC 7115 3.40 × 10 −17 3.40 × 10 −17 · · · · · · · · · · · ·
NGC 4261 3.80 × 10 −18 1.00 × 10 −17 67.4 165 9.64 × 10 −14 9.86 × 10 −13
NGC 4335 2.50 × 10 −17 3.00 × 10 −17 9.20 15.0 · · · · · ·
NGC 4374 6.20 × 10 −17 7.30 × 10 −17 106 112 1.89 × 10 −13 8.94 × 10 −14
NGC 4486 6.40 × 10 −16 3.20 × 10 −16 1570 3600 · · · · · ·
NGC 5127 · · · · · · 3.90 7.00 · · · · · ·
NGC 5141 9.50 × 10 −18 1.40 × 10 −17 35.5 71.0 · · · · · ·
NGC 5490 6.70 × 10 −19 4.00 × 10 −18 20.0 41.0 · · · · · ·
NGC 7052 · · · · · · 2.79 × 10 1 36.0 · · · · · ·
UGC 12064 · · · 3.10 × 10 −17 · · · · · · · · · · · ·
NGC 7626 3.70 × 10 −18 1.10 × 10 −17 12.5 23.0 · · · · · ·
Note. — Col. (1): Galaxy Name; Cols. (2-3): The nuclear point source V and
I fluxes (from WFPC2 imaging) in (erg s −1 cm −2 ˚A −1 ); Cols. (4-5) Peak fluxes in
the radio core from VLBA and VLA observations; Cols. (5-6) Unabsorbed X-ray
fluxes from the nucleus in soft (0.02 - 2 keV) and hard (2 - 10 keV) bands from
Chandra observations.
References. — Cols. 2-3: Verdoes Kleijn et al. (2002a); Cols. 4-5: Xu et al.
(2000); Cols. 6-7 E. Colbert (Private Communication).
33

Table 2.3. Stellar velocity dispersions and estimated black hole masses.
Galaxy σmeas Ref. rap re σc M• MF01 M•Meas. Ref.
(km s −1 ) (arcsec) (arcsec) (km s −1 ) (10 8 M⊙) (10 8 M⊙)
NGC 193 · · · · · · · · · 25.90 · · · · · · · · · · · ·
NGC 315 357 (1) 1.48 62.78 334 14.6 · · · · · ·
NGC 383 311 (1) 1.48 22.65 303 9.24 · · · · · ·
NGC 541 225 (1) 1.48 21.34 220 2.03 · · · · · ·
NGC 741 284 (1) 1.48 47.01 269 5.24 · · · · · ·
UGC 1841 382 (10) Re · · · 352 18.6 · · · · · ·
NGC 2329 274 (1) 1.48 26.81 265 4.92 · · · · · ·
NGC 2892 · · · · · · · · · 33.51 · · · · · · · · · · · ·
NGC 3801 225 (2) Re? · · · 207 1.53 · · · · · ·
NGC 3862 263 (1) 1.48 12.87 264 4.66 · · · · · ·
UGC 7115 198 (3) 3.39 13.63 204 1.41 · · · · · ·
NGC 4261 306 (1) 1.48 38.25 292 7.75 5.4 (5)
NGC 4335 282 (9) 2Re · · · 252 3.9 ≤ 1.0 (9)
NGC 4374 304 (1) 1.48 43.87 288 7.30 4.3 (6)
NGC 4486 383 (1) 4.50 113.87 366 22.5 35.7 (7)
NGC 5127 198 (3) 3.39 48.12 194 1.11 · · · · · ·
NGC 5141 · · · · · · · · · 15.13 · · · · · · · · · · · ·
NGC 5490 305 (1) 1.48 15.39 302 9.07 · · · · · ·
NGC 7052 270 (4) ∼ Re · · · 248 3.62 3.7 (8)
UGC 12064 233 (10) Re · · · 214 1.80 · · · · · ·
NGC 7626 244 (1) 1.48 34.16 234 2.72 · · · · · ·
Note. — Measured stellar velocity dispersions are shown, with the source
reference indicated. These have then been adapted to yield σc based on measurements
of re from our WFPC2 data (see text). The relation of Merritt &
Ferrarese (2001) was then used to yield estimates of the black hole masses.
References. — (1) Davies et al. (1987); (2) Di Nella et al. (1995); (3) Tonry
& Davis (1981); (4) Wagner et al. (1988); (5) Ferrarese et al. (1996); (6) Maciejewski
& Binney (2001); (7) Macchetto et al. (1997); (8) van der Marel & van
den Bosch (1998); (9) Verdoes Kleijn et al. (2002b); (10) Balcells et al. (1995);
(11) van der Marel & van den Bosch (1998).
34

0.5"
Figure 2.1 Optical continuum image of the nuclear region of NGC 193. The position
of the spectroscopic slits used in the observing program described in Chapter 3 are
indicated. The dashed line indicates the galaxy major axis position angle, the dotted
line indicates the direction of the radio jet. A north-east indicator is shown.
35

0.5"
Figure 2.2 Optical continuum image of the nuclear region of NGC 315. The position
of the spectroscopic slits used in the observing program described in Chapter 3 are
indicated. The dashed line indicates the galaxy major axis position angle, the dotted
line indicates the direction of the radio jet. A north-east indicator is shown.
36

0.5"
Figure 2.3 Optical continuum image of the nuclear region of NGC 383. The position
of the spectroscopic slits used in the observing program described in Chapter 3 are
indicated. The dashed line indicates the galaxy major axis position angle, the dotted
line indicates the direction of the radio jet. A north-east indicator is shown.
37

0.5"
Figure 2.4 Optical continuum image of the nuclear region of NGC 541. The position
of the spectroscopic slits used in the observing program described in Chapter 3 are
indicated. The dashed line indicates the galaxy major axis position angle, the dotted
line indicates the direction of the radio jet. A north-east indicator is shown.
38

0.5"
Figure 2.5 Optical continuum image of the nuclear region of NGC 741. The position
of the spectroscopic slits used in the observing program described in Chapter 3 are
indicated. The dashed line indicates the galaxy major axis position angle, the dotted
line indicates the direction of the radio jet. A north-east indicator is shown.
39

0.5"
Figure 2.6 Optical continuum image of the nuclear region of UGC 1841. The position
of the spectroscopic slits used in the observing program described in Chapter 3 are
indicated. The dashed line indicates the galaxy major axis position angle, the dotted
line indicates the direction of the radio jet. A north-east indicator is shown.
40

0.5"
Figure 2.7 Optical continuum image of the nuclear region of NGC 2329. The position
of the spectroscopic slits used in the observing program described in Chapter 3 are
indicated. The dashed line indicates the galaxy major axis position angle, the dotted
line indicates the direction of the radio jet. A north-east indicator is shown.
41

0.5"
Figure 2.8 Optical continuum image of the nuclear region of NGC 2892. The position
of the spectroscopic slits used in the observing program described in Chapter 3 are
indicated. The dashed line indicates the galaxy major axis position angle, the dotted
line indicates the direction of the radio jet. A north-east indicator is shown.
42

0.5"
Figure 2.9 Optical continuum image of the nuclear region of NGC 3801. The position
of the spectroscopic slits used in the observing program described in Chapter 3 are
indicated. The dashed line indicates the galaxy major axis position angle, the dotted
line indicates the direction of the radio jet. A north-east indicator is shown.
43

0.5"
Figure 2.10 Optical continuum image of the nuclear region of NGC 3862. The position
of the spectroscopic slits used in the observing program described in Chapter 3 are
indicated. The dashed line indicates the galaxy major axis position angle, the dotted
line indicates the direction of the radio jet. A north-east indicator is shown.
44

0.5"
Figure 2.11 Optical continuum image of the nuclear region of UGC 7115. The position
of the spectroscopic slit used in the observing program described in Chapter 3 are
indicated. The dashed line indicates the galaxy major axis position angle, the dotted
line indicates the direction of the radio jet. A north-east indicator is shown.
45

0.5"
Figure 2.12 Optical continuum image of the nuclear region of NGC 4261. The position
of the spectroscopic slits used in the observing program described in Chapter 3 are
indicated. The dashed line indicates the galaxy major axis position angle, the dotted
line indicates the direction of the radio jet. A north-east indicator is shown.
46

0.5"
Figure 2.13 Optical continuum image of the nuclear region of NGC 4335. The position
of the spectroscopic slits used in the observing program described in Chapter 3 are
indicated. The dashed line indicates the galaxy major axis position angle, the dotted
line indicates the direction of the radio jet. A north-east indicator is shown.
47

0.5"
Figure 2.14 Optical continuum image of the nuclear region of M84. The position
of the spectroscopic slits used in the observing program described in Chapter 3 are
indicated. The dashed line indicates the galaxy major axis position angle, the dotted
line indicates the direction of the radio jet. A north-east indicator is shown.
48

0.5"
Figure 2.15 Optical continuum image of the nuclear region of NGC 4486. The position
of the spectroscopic slits used in the observing program described in Chapter 3 are
indicated. The dashed line indicates the galaxy major axis position angle, the dotted
line indicates the direction of the radio jet. A north-east indicator is shown.
49

0.5"
Figure 2.16 Optical continuum image of the nuclear region of NGC 5127. The position
of the spectroscopic slits used in the observing program described in Chapter 3 are
indicated. The dashed line indicates the galaxy major axis position angle, the dotted
line indicates the direction of the radio jet. A north-east indicator is shown.
50

0.5"
Figure 2.17 Optical continuum image of the nuclear region of NGC 5141. The position
of the spectroscopic slits used in the observing program described in Chapter 3 are
indicated. The dashed line indicates the galaxy major axis position angle, the dotted
line indicates the direction of the radio jet. A north-east indicator is shown.
51

0.5"
Figure 2.18 Optical continuum image of the nuclear region of NGC 5490. The position
of the spectroscopic slits used in the observing program described in Chapter 3 are
indicated. The dashed line indicates the galaxy major axis position angle, the dotted
line indicates the direction of the radio jet. A north-east indicator is shown.
52

0.5"
Figure 2.19 Optical continuum image of the nuclear region of NGC 7052. The position
of the spectroscopic slits used in the observing program described in Chapter 3 are
indicated. The dashed line indicates the galaxy major axis position angle, the dotted
line indicates the direction of the radio jet. A north-east indicator is shown.
53

0.5"
Figure 2.20 Optical continuum image of the nuclear region of UGC 12064. The
position of the spectroscopic slits used in the observing program described in Chapter
3 are indicated. The dashed line indicates the galaxy major axis position angle, the
dotted line indicates the direction of the radio jet. A north-east indicator is shown.
54

0.5"
Figure 2.21 Optical continuum image of the nuclear region of NGC 7626. The position
of the spectroscopic slits used in the observing program described in Chapter 3 are
indicated. The dashed line indicates the galaxy major axis position angle, the dotted
line indicates the direction of the radio jet. A north-east indicator is shown.
55

M BH (M Sun)
10 10
10 9
10 8
10 7
10 6
60 70 80 90100 200 300 400
σ c (km s -1 )
Figure 2.22 Measured black hole masses (MBH) as a function of central stellar velocity
dispersion (σc) for reliable determinations summarized by Tremaine et al. (2002). The
line indicates the fit M• = 1.3 ×10 8 M⊙(σc/200) 4.72 . (*) indicates masses determined
from stellar dynamical modeling; (◦) indicates masses determined from gas kinematics;
and (△) indicates masses determined from MASER kinematics. The members of
the UGC FR-I sample which have previous black hole mass measurements are shown
as black squares (�).
56

Chapter 3
STIS spectroscopy of the emission
line gas in the nuclei of nearby
FR-I galaxies
This chapter originally appeared as part of Noel-Storr et al. (2003).
3.1 Introduction
We present the results of the analysis of a set of medium resolution spectra, obtained
by the Space Telescope Imaging Spectrograph on board the Hubble Space Telescope,
of the emission line gas present in the nuclei of a complete sample of 21 nearby, early-
type galaxies with radio jets (the UGC FR-I Sample). For each galaxy nucleus we
present spectroscopic data in the region of Hα and the derived kinematics.
57

We find that in 67% of the nuclei the gas appears to be rotating and, with one
exception, the cases where rotation is not seen are either face on or have complex
central morphologies. We find that in 62% of the nuclei the fit to the central spectrum
is improved by the inclusion of a broad component. The broad components have a
mean velocity dispersion of 1349 ± 345 km s −1 and are redshifted from the narrow
line components (assuming an origin in Hα) by 486 ± 443 km s −1 .
The chapter is organized as follows. In section 2 we describe the sample and in
section 3 we describe the STIS spectroscopic observations and the data reduction. In
section 4 we describe our analysis procedures. We present our initial interpretations
in section 5 and draw conclusions in section 6. We use a Hubble constant of H0 =
50km s −1 Mpc −1 throughout.
3.2 STIS Observations
In program 8236 we used HST/STIS (see Kimble, et al., 1998) to take spectra of the
19 sample members not previously or concurrently observed by others. Observations
were carried out at both medium (for 19/19 galaxies) and low (for 4/19 galaxies) res-
olution, with the G750M and the G430L and G750L gratings respectively. Our medium
resolution observation log is shown in Table 3.1. We will present the low resolution
58

spectra in a future paper. We include in our analysis similar medium resolution data
obtained by R. Green and collaborators for the nucleus of M84 (program 7124, see
Bower et al., 1998) and H. Ford and collaborators for the nucleus of M87 (program
8666) to complete the data set for UGC FR-I galaxies.
In our program, we observed each galaxy in three parallel, adjacent slit positions.
For each slit position we obtained two exposures with a shift of 0. ′′ 202800 (4 unbinned
STIS Pixels) along the slit direction to enable us to more efficiently remove detector
effects (bad pixels, etc.). In the case of UGC 7115 we observed in only one slit position
- we sacrificed STIS observing time to make WFPC2 observations of this galaxy as
it had not been included in our earlier WFPC2 program.
The data for M87 (NGC 4486) were obtained in a similar manner to our own.
In the case of M84 (NGC 4374) the observation pairs were not shifted along the slit
direction, thus some detector effects may remain, though will be much less significant
thanks to the far greater signal to noise.
We list the instrumental properties of the STIS configurations used in Table 3.2.
Panel (a) of Figures 3.2 to 3.22 (see key in Figure 3.1) shows the location of the STIS
slits on each galaxy observed, along with the position angles of the galaxy major axes
and radio-jet axes. For the majority of cases the STIS slits were aligned within 10 ◦
59

of the galaxy major axes (Table 3.3), with the exceptions that we note below.
In the cases of NGC 741 [∆PA(gal, slit) = 19.4 ◦ ] and NGC 2892 [∆PA(gal, slit) =
22 ◦ ] more freedom in orientation was allowed to provide reasonable observing win-
dows.
In NGC 3862 and UGC 7115 the position angles of the galaxy major axes are
hard to determine, we decided to position the slits approximately perpendicular to
the radio jets [∆PA(jet, slit) = 92.3 ◦ & 110.4 ◦ , respectively]. The central major axis
is also hard to determine in NGC 541, where the central isophotes rotate consid-
erably. In this case we chose to use a slit position somewhere around the mean of
the isophotal position angles with considerable leeway given to allow for reasonable
observing windows.
For UGC 12064 the slits were aligned along the major axis of the prominent dust
disk, which is offset from the galaxy major axis by ∼ 50 ◦ .
The slits in M84 were positioned approximately perpendicular to the radio jet,
which lies close to the major axis of the nuclear gas. For NGC 4486 (M87) the slits
were positioned to follow certain morphological structures across the nuclear regions.
60

3.2.1 Data Reduction
We used the standard STIS calibration pipeline (calstis, see Brown et al., 2002) to
perform bias, dark and flat-field corrections using the best available reference files.
We used calstis version 2.13 (26-April-2002) throughout the data reduction 1 .
We shifted the rows of alternating observations by 4 pixels, so that they were
properly aligned with their counterparts and combined them using the STSDAS rou-
tine ocrreject. We cleaned co-incident cosmic rays and negative bad pixels, which
would not be caught by ocrreject, using the NOAO/IRAF task cosmicrays. At
each step we carefully investigated the effects of varying task parameters to insure we
were not damaging valid data while removing most cosmic rays.
We made use of the STIS calibration pipeline tasks wavecal and x2d to perform
wavelength calibration and image rectification respectively. The error introduced by
rectifying after shifting one of the images is ∼ < 0.05 pixels (which is ∼ < 1.3 km s −1 at
6750˚A).
Panel (b) of Figures 3.2 to 3.22 (see key in Figure 3.1) shows (i) the central strip
1 We found that significant variations in measured parameters could be introduced by using different
calstis versions. Versions 2.4 and 2.13 produce consistent results, while intermediate versions
do not.
61

of the reduced spectrum for each slit position observed on each galaxy, along with
(ii) Gaussian line fits to the same (see §4.1).
3.3 Analysis
In this section we describe the line fitting that we carried out on each spectral row
of each reduced CCD spectral image, firstly with a single Gaussian per spectral line
(§4.1) and secondly with the inclusion of an additional free component (§4.2). In
§4.3 we discuss the sizes of the errors on quoted parameters from various sources. In
§4.4 we describe each of the UGC FR-I sample members in turn. For each galaxy
we define the central spectrum as the row with the greatest integrated flux after the
data reduction. We list the row numbers in the final x2d image corresponding to the
central spectrum in Table 3.1.
3.3.1 Single Gaussian line fitting
In the G750M spectra we expect to find the emission lines in the vicinity of Hα that are
listed in Table 3.4. We used wavelengths from the recent measurements of Wallerstein
et al. (2001) and converted from air to vacuum wavelengths using the IAU standard
formula
62

λvac − λair
λair
= 6.4328 × 10 −5 +
2.94981 × 10−2
146 − (104 2.5540 × 10−4
2 +
/λair)
41 − (10 4 /λair) 2.
63
(3.1)
Using one Gaussian to represent each of these five lines we obtain a set of 7 free
parameters to fit: the continuum flux level, velocity (vr), velocity dispersion (σ), and
the fluxes of each line. The flux of [N II]6550 was fixed in a ratio of 1:3 with the
flux of [N II]6585 based on the transition probabilities derived from atomic physics
(Osterbrock, 1989).
We used a χ 2 minimization routine (using Levenberg-Marquardt iterations, see
Press et al., 1992) to fit the Gaussian template to the observed spectra. The applica-
tion of this fitting technique and development of this routine are described by van der
Marel & van den Bosch (1998). Formal errors are drawn from the covariance matrix
of the fit. As we do not expect the noise in each spectrum to be normally-distributed
after the steps of wavelength calibration and two-dimensional rectification, these error
values should be treated strictly as the formal fit errors under the understanding that
the size of the real errors may be somewhat different (see §4.3 below).
From this point on we only consider data points where the formal errors from
the fits meet the following criteria, allowing us to exclude unreliable data points
originating from poorly constrained fits:

∆F(Hα)
F(Hα)
∆σ < 50 km s −1
64
(3.2)
< 0.75 (3.3)
where ∆σ and ∆F(Hα) are the errors in velocity dispersion and line flux respec-
tively. The main constraint arises from the limit on the velocity dispersion error. The
very large flux error allowed is in place to remove only the few remaining bad data
points where the profile very precisely fits the noise.
In Panel (e) of Figures 3.2 to 3.22 (see key in Figure 3.1) we show profiles of (i)
radial velocity, (ii) velocity dispersion, (iii) [N II]6585 line flux and (iv) [N II] / Hα
ratios resulting from this fitting procedure for each of our sample galaxies. These
profiles are combined and visualized in 2D for each galaxy in Panel (c) of Figures 3.2
to 3.22.
We present the fit data in Tables 3.5 to 3.25, where the errors given are the formal
errors from the fit. In these tables Column (1) is the row number of the portion of the
spectrum fitted. Column (2) shows the offset along the slit direction in arcseconds
from the row with the greatest integrated flux. Columns (3) and (4) give the radial
velocities (vr) and gas velocity dispersions (σgas) respectively. Column (5) gives the

line flux of the Hα line and columns (6) and (7) show its ratio against the fluxes of
the [N II]6585 and [S II]total (the total flux of the two [S II] lines) respectively. Column
(8) gives the reduced χ 2 (R 2 ) value of the resulting fit.
We repeated the fit for the central row of the galaxy NGC 4335 varying the set of
free parameters in order to estimate the reliability of the fits that we had used. We
found that the fit was stable to within one formal error on all quoted parameters when
the velocities, velocity dispersions and fluxes of all parameters were fit independently.
The signal to noise falls off rapidly outside of the very nuclear regions so it is not
possible to consistently run fits with a large number of free parameters. The results
for the nucleus of NGC 4335 satisfy us that we are justified in fixing the parameters
in the manner that we have chosen, without adding any obvious biases to our results.
3.3.2 Fits with an additional free component
In many cases, as the very central pixels are reached the fit begins to do a poorer
job of matching the observed profile. In an attempt to improve the fit to the narrow
centers of the lines we tested a fit for the central spectrum of each galaxy including
an additional fit component with independent velocity, velocity dispersion and flux,
along with the original set of five Gaussians. The fits to the central spectra are
shown in Panel (d) of Figures 3.2 to 3.22 (see key in Figure 3.1), (i) excluding and
65

(ii) including the additional component.
We assessed the effectiveness of including this component in each galaxy based
on (1) an improvement in the mean of the absolute value of the residuals from the
fit ≥ 5% (2) an improvement in the reduced χ 2 value of the fit such that (R 2 1 −
R 2 2 )/R2 1
≥ 0.15 and (3) an improvement judged by eye in the fit compared to the
data. We assigned a score to each galaxy, with one point available for each of the
three categories. We consider scores of 2 or 3 to be indicative of the presence of a
broad component, a score of 1 indicates the possibility of a broad component, while
we treat a score of 0 as a none detection. The three parameters and scores are listed
in Table 3.27.
We find an additional free component improves the fit in 62% (N = 13) of the
sample galaxies. In the cases of NGC 2329 and NGC 3862 the component appears to
represent a non-flat continuum. The kinematic parameters for each galaxy including
the additional free component are listed in Table 3.28 and the flux parameters in
Table 3.29. We present further interpretation of the nature and origin of the features
fit by the additional free component in §5.3.
66

3.3.3 Quantifying error sources
The STIS data handbook (Brown et al., 2002) gives the following absolute and relative
accuracies applicable to this work: A wavelength absolute calibration error (∆λ offset)
of 0.1 to 0.3 pixels (2.6 to 7.7 km s −1 at 6500˚A) within an exposure, and from 0.2 to
0.5 pixels (5.1 to 12.8 km s −1 at 6500˚A) between exposures. An absolute photometry
error of 5% and a relative photometry error of 2% within a single exposure assuming
a wide slit observation. 5 µm variations in slit width along the slit lengths could
result in variations of up to 20% in flux along the 0. ′′ 1 slit.
In Verdoes Kleijn et al. (2002a) Hα + [N II] fluxes were presented for each nucleus
in the sample. The values presented there agree well with the values we find here,
certainly given our limited ability to extract comparable apertures and within the
20% potential flux errors noted above.
In Section 1 we indicated that a 1.3 km s −1 error could be incorporated into the
final data as a result of shifting the spectra for image combination and cosmic ray
rejection. This shift is insignificant compared to other error sources.
In Table 3.26 we showed that by allowing different free parameters within the
single-Gaussian-per-line fit produced changes in the measurement in velocity of ∼
67

8 km s −1 and of ∼ 16 km s −1 in velocity dispersion for the nucleus of NGC 4335.
In Table 3.32 we show the effect on the measured velocities and velocity dispersions
of the various components for each of the models described in the previous section,
again for the case of NGC 4335. This illustrates that the measured velocities of the
narrow lines may vary by up to ∼ 20 km s −1 (and velocity dispersions by as much as
∼ 110 km s −1 ) when additional components in the line shape are taken into account.
In the nuclei of NGC 383 and NGC 4335 (representing cases with blended and
less blended lines respectively) we repeated the narrow line fit to the central spec-
trum with 286 different combinations of input velocity and velocity dispersion; vary-
ing the velocities over a range of 2000 km s −1 and the velocity dispersions over a
range of 6000 km s −1 . In the case of NGC 4335 we found that the velocity varied
by ±10.91 km s −1 and the velocity dispersion by just ±0.02 km s −1 . In the case of
NGC 383 we found that the velocity varied by ±13.04 km s −1 and the velocity disper-
sion by just ±3.76 km s −1 . There was a systematic effect relating input and output
velocities in both cases.
We conclude that reasonable estimates of the genuine errors on each of our mea-
sured parameters are: 5% - 10% on fluxes (dominated by the effects of variations along
the narrow slits and the STIS absolute calibration); and ∼ 20 km s −1 on velocities
68

and velocity dispersions (dominated by the fit model dependency of the results).
3.4 Individual galaxy descriptions
Below, we give descriptions of each member of the UGC FR-I sample in turn. The
galaxy classifications are taken from the NASA Extragalactic Database, which lists
references in which the terms used are described. Descriptions of dust properties and
radio sources are as presented by Verdoes Kleijn et al. (1999) and Xu et al. (2000)
respectively.
NGC 193 (UGC 408) This S0 galaxy has a complex gas morphology with two
lanes apparent in the central regions (the most clearly defined lane has a width :
length = 0.18). It has a core-jet radio morphology on VLA and VLBA scales. The
STIS slits were aligned parallel to the galaxy major axis. The central kinematic and
flux properties are listed in Table 3.5; the gas does not exhibit a regular rotation
curve, though it does appear dominated by systematic rather than random motions.
The fit to the central spectrum is improved by the addition of a broad component.
Data for this galaxy are shown in Figure 3.2 (see key in Figure 3.1 for an explanation
of these plots).
69

NGC 315 (UGC 597) This elliptical galaxy has a nuclear dust disk (b/a = 0.23).
It has a core-jet radio morphology on VLA and VLBA scales. The STIS slits were
aligned parallel to the galaxy major axis. The central kinematic and flux properties
are listed in Table 3.6; the gas appears to be in organized motion, possibly regular
rotation. The fit to the central spectrum is improved by the addition of a broad
component. Data for this galaxy are shown in Figure 3.3 (see key in Figure 3.1 for
an explanation of these plots).
NGC 383 (UGC 689) This S0 galaxy has a nuclear dust disk (b/a = 0.77). It
has a core-jet radio morphology on VLBA scales, and a twin-jet morphology on VLA
scales. The STIS slits were aligned parallel to the galaxy major axis. The central
kinematic and flux properties are listed in Table 3.7; the gas exhibits a regular rotation
profile. In the negative offset side slit there is a dip in the velocity dispersion profile
at a position close to the nucleus. The fit to the central spectrum is improved by the
addition of a broad component. Data for this galaxy are shown in Figure 3.4 (see key
in Figure 3.1 for an explanation of these plots).
NGC 541 (UGC 1004) This cD S0 galaxy has a nuclear dust disk (b/a = 0.91). It
has a radio core on VLBA scales and a core-jet morphology on VLA scales. The STIS
70

slits were aligned to a mean of the position angles of the central isophotes measured
from our WFPC/2 images, which vary considerably. We allowed considerable flexibil-
ity in position angle to enable reasonable observing windows. The central kinematic
and flux properties are listed in Table 3.8; the gas does not exhibit a regular rotation
profile. The fit to the central spectrum is not significantly improved by the addition
of a broad component, though the fit improves somewhat when judged by eye. Data
for this galaxy are shown in Figure 3.5 (see key in Figure 3.1 for an explanation of
these plots).
NGC 741 (UGC 1413) This E0 galaxy has no apparent nuclear dust. It has a
radio core on VLBA scales and a core-jet morphology on VLA scales. The STIS slits
were aligned approximately parallel to the galaxy major axis, however a certain degree
of freedom was allowed in slit placement to allow reasonable observing windows. The
central kinematic and flux properties are listed in Table 3.9. Very few points had
sufficient signal to noise to obtain good fits in these data, it has not been included
in further analysis of global kinematic properties. The fit to the central spectrum is
not improved by the addition of a broad component. Data for this galaxy are shown
in Figure 3.6 (see key in Figure 3.1 for an explanation of these plots).
71

UGC 1841 This elliptical galaxy has a nuclear dust disk (b/a ∼ 0.98). It has a
core-jet radio morphology on VLBA and VLA scales. The STIS slits were aligned
parallel to the galaxy major axis. The central kinematic and flux properties are listed
in Table 3.10; the gas does not exhibit a regular rotation profile. The fit to the central
spectrum is improved by the addition of a broad component. Data for this galaxy
are shown in Figure 3.7 (see key in Figure 3.1 for an explanation of these plots).
NGC 2329 (UGC 3695) This S0 galaxy has a nuclear dust disk (b/a = 0.68).
It has a core-jet radio morphology on VLBA and VLA scales. The STIS slits were
aligned parallel to the galaxy major axis. The central kinematic and flux properties
are listed in Table 3.11; the gas does not exhibit a regular rotation profile. The
fit to the central spectrum is improved by the addition of a broad component which
appears to represent a non-flat continuum in this case. Data for this galaxy are shown
in Figure 3.8 (see key in Figure 3.1 for an explanation of these plots).
NGC 2892 (UGC 5073) This elliptical galaxy has no apparent nuclear dust. It
has a radio core on VLBA scales and a twin-jet morphology on VLA scales. The
STIS slits were aligned approximately parallel to the galaxy major axis, however a
certain degree of freedom was allowed in slit placement to allow reasonable observing
72

windows. The central kinematic and flux properties are listed in Table 3.12; the gas
does not exhibit a regular rotation profile. The fit to the central spectrum is not
significantly improved by the addition of a broad component. Data for this galaxy
are shown in Figure 3.9 (see key in Figure 3.1 for an explanation of these plots).
NGC 3801 (UGC 6635) This S0/a galaxy has a complex nuclear dust morphol-
ogy with a large scale dust lane (width : length = 0.12). It has a twin-jet radio
morphology on VLA scales. The STIS slits were aligned parallel to the galaxy major
axis. The central kinematic and flux properties are listed in Table 3.13; the gas does
not exhibit a regular rotation profile. The fit to the central spectrum is not signif-
icantly improved by the addition of a broad component. Data for this galaxy are
shown in Figure 3.10 (see key in Figure 3.1 for an explanation of these plots).
NGC 3862 (UGC 6723) This elliptical galaxy has a nuclear dust disk (b/a ∼
0.99). It has a core-jet radio morphology on VLBA and VLA scales. The STIS slits
were aligned approximately perpendicular to the radio jet as the nuclear isophotal
position angles are poorly constrained. The central kinematic and flux properties are
listed in Table 3.14; the gas does not exhibit a regular rotation profile. The fit to the
central spectrum is improved by the addition of a broad component which appears to
73

epresent a non-flat continuum in this case. Data for this galaxy are shown in Figure
3.11 (see key in Figure 3.1 for an explanation of these plots).
UGC 7115 This elliptical galaxy has a nuclear dust disk (b/a ∼ 0.95). It has a
core-jet radio morphology on VLA scales. The STIS slit were aligned approximately
perpendicular to the radio jet as the nuclear isophotal position angles are poorly con-
strained, a certain degree of freedom was allowed in slit placement to allow reasonable
observing windows. This galaxy was observed in only one slit position, as we also
required WFPC2 observations of this target in order to measure the central photo-
metric properties (see Verdoes Kleijn et al., 2002a). The central kinematic and flux
properties are listed in Table 3.15; the gas exhibits a regular rotation profile. The
fit to the central spectrum is not significantly improved by the addition of a broad
component. Data for this galaxy are shown in Figure 3.12 (see key in Figure 3.1 for
an explanation of these plots).
NGC 4261 (UGC 7360) This E2-3 galaxy has a nuclear dust disk (b/a = 0.46).
It has a twin-jet radio morphology on VLBA and VLA scales. The STIS slits were
aligned parallel to the galaxy major axis. The central kinematic and flux properties
are listed in Table 3.16. The nucleus of this galaxy lies closer to one of the side slits
74

(slit one) than the central position, however it is still possible to see a clear rotation
curve along that slit. The fit to the central spectrum is improved by the addition of
a broad component. Data for this galaxy are shown in Figure 3.13 (see key in Figure
3.1 for an explanation of these plots).
NGC 4335 (UGC 7455) This elliptical galaxy has a nuclear dust disk (b/a =
0.41). It has a radio core on VLBA scales and a twin-jet morphology on VLA scales.
The STIS slits were aligned parallel to the galaxy major axis. The central kinematic
and flux properties are listed in Table 3.17; the gas exhibits a regular rotation profile.
In the positive offset side slit there is a dip in the velocity dispersion profile at the
position closest to the nucleus. See also Verdoes Kleijn et al. (2002b). The fit to the
central spectrum is improved by the addition of a broad component. Data for this
galaxy are shown in Figure 3.14 (see key in Figure 3.1 for an explanation of these
plots).
NGC 4374 (M84; UGC 7494) This E1 galaxy has a nuclear dust lane (width :
length = 0.15). It has a core-jet radio morphology on VLBA scales, and a twin-jet
morphology on VLA scales. The STIS slits were aligned approximately perpendicular
to the radio jets, which lies close to the major axis of the emission line gas. The
75

central kinematic and flux properties are listed in Table 3.18; the gas exhibits a
regular rotation profile. See also Bower et al. (1998). The fit to the central spectrum
is not significantly improved the addition of a broad component. Data for this galaxy
are shown in Figure 3.15 (see key in Figure 3.1 for an explanation of these plots).
NGC 4486 (M87; UGC 7654) This elliptical galaxy has an irregular nuclear dust
morphology. It has a core-jet radio morphology on VLBA and VLA scales. The STIS
slits were aligned to trace morphological features in the emission line gas across the
nuclear region of this galaxy. The central kinematic and flux properties are listed in
Table 3.19; the gas exhibits a regular rotation profile. The fit to the central spectrum
is improved by the addition of a broad component. Data for this galaxy are shown
in Figure 3.16 (see key in Figure 3.1 for an explanation of these plots).
NGC 5127 (UGC 8419) This elliptical peculiar galaxy has a nuclear dust lane
(width : length = 0.25). It has a radio core on VLBA scales and a twin-jet morphol-
ogy on VLA scales. The STIS slits were aligned parallel to the galaxy major axis.
The central kinematic and flux properties are listed in Table 3.20; the gas exhibits a
regular rotation profile. The fit to the central spectrum is not significantly improved
by the addition of a broad component. Data for this galaxy are shown in Figure 3.17
76

(see key in Figure 3.1 for an explanation of these plots).
NGC 5141 (UGC 8433) This S0 galaxy has a nuclear dust lane (width : length =
0.25). It has a core-jet radio morphology on VLBA scales and a twin-jet morphology
on VLA scales. The STIS slits were aligned parallel to the galaxy major axis. The
central kinematic and flux properties are listed in Table 3.21; the gas exhibits a
regular rotation profile. The fit to the central spectrum is improved by the addition
of a broad component. Data for this galaxy are shown in Figure 3.18 (see key in
Figure 3.1 for an explanation of these plots).
NGC 5490 (UGC 9058) This elliptical galaxy has a nuclear dust lane (width :
length = 0.35). It has a core-jet radio morphology on VLBA scales and a twin-jet
morphology on VLA scales. The STIS slits were aligned parallel to the galaxy major
axis. The central kinematic and flux properties are listed in Table 3.22; the gas does
not exhibit a regular rotation profile. The fit to the central spectrum is improved by
the addition of a broad component. Data for this galaxy are shown in Figure 3.19
(see key in Figure 3.1 for an explanation of these plots).
77

NGC 7052 (UGC 11718) This elliptical galaxy has a nuclear dust disk (b/a =
0.30). It has a twin-jet radio morphology on VLBA scales and a core-jet morphology
on VLA scales. The STIS slits were aligned parallel to the galaxy major axis. The
central kinematic and flux properties are listed in Table 3.23; the gas exhibits a regular
rotation profile. The fit to the central spectrum is not significantly improved by the
addition of a broad component. Data for this galaxy are shown in Figure 3.20 (see
key in Figure 3.1 for an explanation of these plots).
UGC 12064 This S0 galaxy has a nuclear dust disk (b/a = 0.54). It has a twin-jet
radio morphology on VLA scales. The STIS slits were aligned parallel to the dust
disk major axis. The central kinematic and flux properties are listed in Table 3.24;
the gas exhibits a regular rotation profile. The fit to the central spectrum is improved
by the addition of a broad component. Data for this galaxy are shown in Figure 3.21
(see key in Figure 3.1 for an explanation of these plots).
NGC 7626 (UGC 12531) This elliptical peculiar galaxy has a nuclear dust lane
(width : length = 0.17). It has a core-jet radio morphology on VLBA scales and
a twin-jet morphology on VLA scales. The STIS slits were aligned parallel to the
galaxy major axis. The central kinematic and flux properties are listed in Table 3.25;
78

the gas exhibits a regular rotation profile. The fit to the central spectrum is improved
by the addition of a broad component. Data for this galaxy are shown in Figure 3.22
(see key in Figure 3.1 for an explanation of these plots).
3.5 Interpretation and Discussion
In our initial interpretation we have focussed on understanding the general parameters
of the data set. We will undertake more detailed analyses in future work that we
outline in §6 below. Here, we first describe the categorization of sources as rotating
and non-rotating systems based on the observed kinematics (§5.1). We then discuss
the ionization states of the nuclear regions (§5.2). We go on to discuss the presence
of broad components in these nuclei and a more detailed analysis of the line shapes
(§5.3).
3.5.1 Rotators and non-rotators
By inspecting maps of the central kinematics and the velocity profiles along each slit
(as presented above in figures 3.2 to 3.22), we have classified, by eye, the galaxies
into two classes: rotators and non-rotators. Rotators are systems where we see pat-
terns reminiscent of rotation curves; in non-rotators we find no such patterns - the
79

kinematics seem either irregular or organized in some manner that does not represent
regular rotation. We do not include NGC 741 in discussions of kinematics as very
few points were well fit during our analysis. We classify 67% (N = 14/21) of the
UGC FR-I galaxies as rotators. 73% of galaxies with dust disks (N = 8/11), 100%
of galaxies with dust lanes (N = 5/5) and 50% of galaxies with complex dust or no
dust (N = 2/4) are rotators.
We have made use of the mean velocity dispersion
σ100pc = 1
N
80
�
σi : xi ≤ 100pc, (3.4)
and the difference in mean velocities on each side of the nucleus
�
��
� ⎛
� 1 �
∆100pc = �
� vi : −100pc ≤ xi < 0 − ⎝
� N1 i
1
⎞�
�
�
�
vj : 0 < xj ≤ 100pc⎠�
�
N2 j
�
i
(3.5)
within 100 pc of the brightest pixel as illustrative of the global kinematic pa-
rameters along the central slit 2 . These parameters are shown in Table 3.30 for each
galaxy, along with the mean properties for each class of galaxy. In Figure 3.23 we
2 For NGC 4261 we used the offset slit closest to the nucleus as explained above.

show the relationship between the two parameters for each galaxy. It is clear that
the non-rotators lie at the bottom of the ∆100pc distribution, so it is conceivable that
irregular motions conceal any remaining signs of rotation in these cases. We note that
we detect rotation in all cases where the disk is ∼ > 25 ◦ from face on, other than those
cases where the dust morphology is highly irregular. The only exception is NGC 5490
where the signal to noise was particularly poor.
In Figure 3.24 we show the values of ∆100pc plotted as a function of dust disk axis
ratio, or dust lane width to length ratio; if the dust were all in circular disks this
would be an indicator of disk inclination. We included lines showing an indication
of the projection of several values of ∆100pc at different disk inclinations through the
relation
�
�
�
�
∆obs ≈ ∆int.sini ≈ ∆int × 1 −
81
� �2 b
, (3.6)
a
Where ∆obs is the observed ∆100pc parameter at a given inclination, ∆int is the
presumed intrinsic rotation of the disk and b/a is the axis (or width:length) ratio.
This is not a rigorously valid means of projecting these values, but it serves our
purposes of illustration here.

It is easy to see that the non-rotators with face on disks would have to be intrinsi-
cally rotating very fast for their rotation to register over the random motions in these
cases. From the observations of systems at greater inclinations we have no cause to
expect any disks to be rotating that fast. In a similar manner we plot the values of
σ100pc against dust disk axis ratio, or dust lane width to length ratio in Figure 3.25.
Here we see no clear trend in velocity dispersion with axis ratio.
We find no significant systematic differences between the typical values σ100pc be-
tween the two classes. Using the Kolmogorov-Smirnov Test to assess the two groups
we find a probability of 0.93 that the distributions of velocity dispersions were drawn
from the same underlying distribution. Applying the same test to the ∆100pc param-
eter gives only a 0.08 probability that these were drawn from the same distribution.
This evidence suggests to us that rotators and non-rotators represent the same
type of kinematic systems, with observational effects such as inclination and dust
properties limiting our ability to detect the rotation of those systems where we do
not. We conclude that a model of a rotating gas disk with significant random motions
is compatible with all of the observations.
82

3.5.2 Flux ratios and ionization
In Figure 3.26 we show the [N II] flux as a function of Hα narrow line flux for each
central spectrum. The values are compatible with values typically found for photo-
ionization and shock models (see, for example, Doptia et al., 1997). The unusually
low ratios shown in two nuclei (NGC 383 and M84) are likely a consequence of the
high degree of blending of the lines in these observations (see panel (d) of Figures 3.4
and 3.15), rather than any underlying physics.
While we are satisfied that our data have not produced any results that are in-
compatible with reasonable parameters, detailed modeling is required to understand
the various ionization mechanisms at work in each individual case. We intend to
undertake this type of modeling and present the outcomes in future work.
3.5.3 Are we observing broad lines?
The fit to the central spectrum is improved in 62% of the galaxies by the inclusion
of an additional free Gaussian component (see §4.2). Each of these fits resulted in
the supplementary component being centered redwards of the Hα line with a velocity
dispersion between about two and ten times that of the narrow lines; thus we describe
this feature as a broad fit component. We identify these broad components in 73%
83

of galaxies with dust disks (N=8/11), 60% of galaxies with dust lanes (N=3/5), 67%
of galaxies with irregular dust (N=2/3) and 0% of galaxies with no dust (N=0/2).
If we make a flux cut in Hα we find broad components in 40% of nuclei with
1×10 −15 ≤ F(Hα) ≤ 1×10 −14 , in 55% of nuclei with 1×10 −14 ≤ F(Hα) ≤ 5×10 −14
and in 100% of nuclei with F(Hα) ≥ 5 × 10 −14 . This detection trend with flux is
reflected in Figure 3.26. This suggests that the detection of nuclear broad components
is somewhat flux (and therefore signal to noise) dependent across the sample.
The broad components could originate either as an artifact of attempting to fit
Gaussians to non-Gaussian line profiles, or from a physical source – such as a broad
line region or a change in the characteristics of the gas as the inner regions of the
disk are approached.
We detect broad components only in the central few pixels, this could be a con-
sequence of either the fall in signal to noise or that the component is an unresolved
source. It is important to note as a consequence of this, that fitting single Gaus-
sians to each line samples a different part of the line shape as the central pixels are
approached.
In Table 3.31 we show the mean properties of the broad components and compare
84

them to the samples of LINERS by Ho et al. (1997) and Radio Galaxies summarized
by Sulentic et al. (2000). These comparisons show that our broad components are
compatible with the broad lines seen in LINERs and that the observed offsets from
the narrow line components are compatible with those observed in samples of radio
loud galaxies.
3.5.4 Constraining the line shapes
In order to better establish the line shape, we investigated the profiles from the nucleus
of NGC 4335, which has a relatively good signal to noise and relatively non-blended
lines (Verdoes Kleijn et al., 2002b).
We first investigated the profile of the two [S II] lines, as they are less entangled
than the Hα + [N II] complex. We fit these two lines with a varying number of
Gaussians per line. The minimum in the reduced χ 2 parameter resulting from each
of these fits lay between two and three Gaussians per line. We extended the two
Gaussian per line model to fit the entire profile of the five emission lines. By then
testing various sets of free parameters we were able to discover an optimal set.
Fitting these models quickly illustrated that the additional broad component is a
very strongly favored feature; in any case where it was possible for the parameters to
85

contrive to create a broad component they did so. Table 3.32 shows the kinematic pa-
rameters and reduced χ 2 values from five combinations of fit parameters that produce
distinct fits. These were:
1. Narrow lines only: The original 5 Gaussian model (one Gaussian for each of
the following 5 lines: [N II]6550, Hα, [N II]6585, [S II]6718, [S II]6733), with a single
value of velocity and velocity dispersion for all lines.
2. Additional broad component: The same as the Narrow lines only model, with an
additional broad component, with an independent velocity, velocity dispersion
and flux.
3. Flux-constrained Broad Bases (i): The same as model 2, with an additional set
of 5 Gaussians, representing the broader wings (Broad Bases). This new set of
lines had a single velocity and velocity dispersion and the velocity was fixed to
be the same as for the other lines. The fluxes of each line in the second set of
Gaussians was fixed at a constant ratio to its counterpart in the first set, based
on the mean ratio measured in the fit of two Gaussians per line to the two [S II]
lines as described above.
4. Flux-constrained Broad Bases (ii): The same as model 3, however in this case
the velocity of the set of broad bases was allowed to vary from that of the narrow
86

lines.
5. Flux-unconstrained Broad Bases: the same as model 3, however in this case the
lines in both sets were able to vary independently in flux, other than the fixed
1:3 ratio between the two [N II] lines in each set.
We conclude, as the Flux-constrained Broad Bases (ii) model not only produces
the most satisfying fit judged by eye, but also the lowest reduced χ 2 value, that this
model is likely to most closely represent the line profile present in the central regions.
The broad bases in this case are able to represent an asymmetric red wing on each
line, but they do not reduce the importance of the broad component in the fit.
3.6 Conclusions
In this chapter we presented the medium resolution spectra of the 21 galaxies in our
UGC FR-I sample, obtained by ourselves and others using STIS. Data were obtained
for three parallel slit positions on each nucleus (other than UGC 7115, which was
observed in only one slit position).
We find that all nuclei are compatible with a single kinematic description: a
rotating gas disk, where random motions are always important. We observe patterns
87

eminiscent of rotation in 67% of the nuclei, in the remainder the non-detection can be
accounted for as the systems are either face on, have complex central morphologies (as
judged from the nuclear dust distribution) or, in the case of NGC 5490, particularly
poor signal to noise.
We find that the inclusion of an additional fit component with unconstrained
parameters improves our fit to the nuclear spectrum in 62% of the galaxies, where
it fits in every case as a broad component in the vicinity of Hα and [N II]. The
detection of the broad component is related to the line flux (and therefore the signal
to noise). The broad components have a mean velocity dispersion of 1349±345 km s −1
and are redshifted from the narrow line components (assuming an origin in Hα) by
486 ± 443 km s −1 .
The broad component could be a consequence of non-Gaussian line profiles with
broad wings, which would be biased toward the brightest [N II] line (redwards of
Hα). However, our more detailed analysis of line shape shows that it is very hard
to reproduce this effect by including broad (even asymmetric) wings on each line,
suggesting the broad component may indeed have a physical origin.
The measured Hα to [N II] ratios for the narrow components in the central spectra
are consistent with standard photo-ionization or shock-ionization models (for example,
Doptia et al., 1997) other than two examples where the lines are highly blended
and may be leading us to misleading fits in the very center.
88

Table 3.1. HST-STIS G750M observing log for this program.
Galaxy Visit ID Aperture Offsets Exposure times Brightest Row
( ′′ ) (seconds)
(1) (2) (3) (4) (5) (6)
NGC 193 o5ee01 52x0.2 -0.20, 0.00, +0.20 1700, 1300, 1560 300
NGC 315 o5ee02 52x0.1 -0.10, 0.00, +0.10 1082, 1000, 1098 598
NGC 383 o5ee03 52x0.1 -0.10, 0.00, +0.10 1082, 1000, 1098 599
NGC 541 o5ee04 52x0.2 -0.20, 0.00, +0.20 1442, 1300, 1500 300
NGC 741 o5ee05 52x0.2 -0.20, 0.00, +0.20 1667, 1145, 1500 300
UGC 1841 o5ee06 52x0.2 -0.20, 0.00, +0.20 1870, 1300, 1560 300
NGC 2329 o5ee07 52x0.2 -0.20, 0.00, +0.20 1967, 1245, 1560 300
NGC 2892 o5ee09 52x0.2 -0.20, 0.00, +0.20 2037, 1300, 1560 299
NGC 3801 o5ee10 52x0.2 -0.20, 0.00, +0.20 1699, 1292, 1560 305
NGC 3862 o5ee11 52x0.2 -0.20, 0.00, +0.20 900, 731, 1066 300
UGC 7115 o5ee22 52x0.2 0.00 2058 299
NGC 4261 o5ee12 52x0.1 -0.10, 0.00, +0.10 994, 1000, 1000 601
NGC 4335 o5ee13 52x0.2 -0.20, 0.00, +0.20 2154, 1300, 1560 300
NGC 4374 o3wn01 52x0.2 -0.20, 0.00, +0.20 2245, 2600, 2600 600
NGC 4486 o67z01/2 52x0.2 -0.20, 0.00, +0.20 1708, 1380, 1708 601
NGC 5127 o5ee15 52x0.2 -0.20, 0.00, +0.20 1660, 1000, 1500 303
NGC 5141 o5ee16 52x0.2 -0.20, 0.00, +0.20 1968, 1300, 1560 300
NGC 5490 o5ee17 52x0.2 -0.20, 0.00, +0.20 1590, 1300, 1560 299
NGC 7052 o5ee18 52x0.1 -0.10, 0.00, +0.10 1747, 1300, 1500 600
UGC 12064 o5ee20 52x0.1 -0.10, 0.00, +0.10 1532, 1000, 1500 599
NGC 7626 o5ee19 52x0.2 -0.20, 0.00, +0.20 1905, 1263, 1560 300
Note. — Col. (1): NGC/UGC Number; Col. (2): Root name for
the HST visit and data sets; Col. (3): HST/STIS aperture used; Col.
(4): Slit positions with offsets perpendicular to the slit direction, given
relative to the central slit position. UGC 7115 was observed in only
one position. Further data not included here is available for NGC 4374
(M84) and NGC 4486 (M87); Col. (5): Exposure times in each offset
position. For each position two observations were obtained separated
by 0. ′′ 2028 along the direction of the slit, the combined exposure time is
shown; Col. (6): Row number in the final x2d file of the brightest row.
89

Table 3.2. HST/STIS Instrumental properties for the configurations used.
Grating Aperture Slit Width Binning Wavelength Covered λ Scale Spatial Scale
( ′′ ) (˚A ... ˚A) (˚A/ pixel) ( ′′ / pixel)
(1) (2) (3) (4) (5) (6) (7)
G750M 52x0.1 0.1 2 × 1 6482 ... 7054 1.108 0.05
G750M 52x0.2 0.2 2 × 2 6482 ... 7054 1.108 0.1
G750M 52x0.2 (M84) 0.2 1 × 1 6295 ... 6867 0.554 0.05
G750M 52x0.2 (M87) 0.2 1 × 1 6295 ... 6867 0.554 0.05
Note. — Col. (1): HST/STIS Grating Used; Col. (2): HST/STIS Aperture
Used; Col. (3): The slit width of the chosen aperture; Col. (4): The degree
of on chip binning used given as binaxis1× binaxis2 (wavelength by spatial
binning); Col. (5): The minimum and maximum wavelengths on the CCD chip
at that central wavelength position; Col. (6) The wavelength scale per binned
pixel; Col. (7) The spatial scale per binned pixel. Further details of HST/STIS
configurations can be found in Kimble, et al. (1998).
90

Table 3.3. Position angles of various axes.
Galaxy Major Axis Radio Axis Dust Axis STIS Slits Target ∆PA
( ◦ N ↩→ E) ( ◦ N ↩→ E) ( ◦ N ↩→ E) ( ◦ N ↩→ E) ( ◦ )
(1) (2) (3) (4) (5) (6) (7)
NGC 193 58 104 0 57.9 � M.Ax. 0.1
NGC 315 39 130 40 -143.8 � M.Ax. 2.8
NGC 383 144 162 138 144.1 � M.Ax. 0.1
NGC 541 143 76 · · · -85.6 · · · · · ·
NGC 741 92 · · · · · · -107.4 � M.Ax. † 19.4
UGC 1841 91 50 · · · 90.0 � M.Ax. 1.0
NGC 2329 171 150 174 170.8 � M.Ax. 0.2
NGC 2892 164 52 · · · 142.0 � M.Ax. † 22.0
NGC 3801 121 121 24 121.1 � M.Ax. 0.1
NGC 3862 25 30 · · · 122.3 ⊥ Jet 2.3
UGC 7115 91 116 175 -174.4 ⊥ Jet † 20.4
NGC 4261 155 87 163 157.9 � M.Ax. 2.9
NGC 4335 156 82 158 -32.5 � M.Ax. 8.5
NGC 4374 128 1 79 104.0 ⊥ Jet 13.0
NGC 4486 128 112 · · · 164.7 · · · · · ·
NGC 5127 68 118 48 68.0 � M.Ax. 0.0
NGC 5141 65 12 88 71.9 � M.Ax. 6.9
NGC 5490 1 75 143 -173.9 � M.Ax. 5.1
NGC 7052 64 23 65 63.6 � M.Ax. 0.4
UGC 12064 39 11 171 170.6 � Dust 0.4
NGC 7626 171 44 167 170.8 � M.Ax. 0.2
Note. — Col. (1): NGC/UGC Name; Col. (2): Position angles of the major axes just
outside the central dust distributions; Col. (3): Position angles of the radio jet axes on
arcsecond scales or smaller; Col. (4): Position angles of the central dust distributions;
Col. (5): Position angles of the STIS slits on the nucleus; Col. (6): The target orientation
of the STIS slits (� M.Ax.: Parallel to the Major Axis; � Dust: Parallel to the Dust
Axis; ⊥ Jet: Perpendicular to the radio jet; † Additional flexibility allowed to reduce
scheduling constraints); Col. (7): Offset in degrees of the STIS slits from the target
orientation.
References. — Data for Columns 3 - 5 taken from Verdoes Kleijn, et al. (1999)
91

Table 3.4. Spectral Lines in the region of Hα.
Ion Ref. Transition λair λvac
(˚A) (˚A)
(1) (2) (3) (4) (5)
[N II] (a) 3 P1 − 1 D2 6548.05 6549.86
Hα (b) 6562.80 6564.61
[N II] (a) 3 P2 − 1 D2 6583.39 6585.21
[S II] (a) 4 S3/2 − 2 D5/2 6716.44 6718.29
[S II] (a) 4 S3/2 − 2 D3/2 6730.81 6732.67
Note. — Col. (1): Ion responsible for the line;
Col. (2): Wavelength reference; Col. (3): Transition
configuration terms; Col. (4): Air wavelength;
Col. (5): Vacuum wavelength. Note
that the value for Hα is computed from the intensity
weighted mean of fine structure lines at
λair = 6562.7247 and λair = 6562.8516 with relative
intensities of 120 and 180 respectively.
References. — (a) Wallerstein, et al. (2001);
(b) Reader & Corliss (1998)
92

Table 3.5. NGC 193: Measured Parameters.
Row Y-Offset vr σgas F(Hα/10 −16 ) F([NII]6585) F([SII]total) R 2
( ′′ ) (km s −1 ) (km s −1 ) (erg s −1 cm −2 Hz −1 ) F(Hα) F(Hα)
Slit 1: X-Offset -0.2 ′′
2 -0.9128 4334 ± 30 135 ± 30 6.6 ± 2.9 1.7 ± 0.9 1.2 ± 0.7 3.79
3 -0.8114 4270 ± 30 121 ± 32 6.9 ± 3.3 1.5 ± 1.0 0.2 ± 0.3 3.17
4 -0.7099 4323 ± 22 124 ± 23 10.6 ± 4.0 1.5 ± 0.7 0.1 ± 0.2 3.90
5 -0.6085 4390 ± 7 40 ± 7 7.8 ± 2.3 1.4 ± 0.6 0.1 ± 0.2 3.23
6 -0.5071 4602 ± 42 233 ± 41 12.9 ± 4.5 0.0 ± 0.3 1.8 ± 0.8 2.83
7 -0.4057 4371 ± 10 67 ± 10 7.4 ± 2.3 1.5 ± 0.6 1.2 ± 0.5 3.67
8 -0.3043 4402 ± 9 48 ± 9 6.2 ± 2.2 1.1 ± 0.5 0.9 ± 0.5 3.46
9 -0.2028 4369 ± 23 210 ± 18 24.7 ± 4.4 1.2 ± 0.3 1.3 ± 0.3 3.28
10 -0.1014 4344 ± 9 132 ± 9 12.5 ± 2.8 2.9 ± 0.7 3.0 ± 0.7 3.49
11 0.0000 4336 ± 7 121 ± 7 18.3 ± 2.8 2.8 ± 0.5 2.2 ± 0.4 3.66
12 0.1014 4340 ± 8 128 ± 8 18.6 ± 2.9 2.7 ± 0.5 1.6 ± 0.3 3.50
13 0.2028 4374 ± 6 85 ± 6 18.0 ± 2.7 1.8 ± 0.3 1.1 ± 0.2 3.11
14 0.3043 4343 ± 7 86 ± 7 19.2 ± 3.1 1.3 ± 0.3 1.0 ± 0.2 2.77
15 0.4057 4298 ± 14 97 ± 14 8.0 ± 2.6 2.6 ± 1.0 0.2 ± 0.3 2.52
16 0.5071 4309 ± 10 64 ± 10 8.0 ± 2.3 1.5 ± 0.6 1.0 ± 0.4 3.05
17 0.6085 4303 ± 8 66 ± 8 9.9 ± 2.3 1.7 ± 0.5 0.9 ± 0.3 2.96
18 0.7099 4317 ± 6 47 ± 6 13.3 ± 2.7 0.5 ± 0.2 0.6 ± 0.2 2.95
19 0.8114 4331 ± 8 45 ± 7 10.8 ± 2.9 0.6 ± 0.3 0.2 ± 0.1 3.50
20 0.9128 4390 ± 31 169 ± 29 5.7 ± 3.1 3.2 ± 1.9 1.6 ± 1.1 3.42
Slit 0: X-Offset 0.0 ′′
1 -1.0142 4425 ± 41 164 ± 38 7.2 ± 4.0 2.5 ± 1.6 0.4 ± 0.5 2.62
4 -0.7099 4336 ± 10 75 ± 10 10.5 ± 3.1 1.9 ± 0.7 0.8 ± 0.4 2.41
5 -0.6085 4353 ± 10 96 ± 10 13.4 ± 3.1 1.9 ± 0.5 1.4 ± 0.4 2.58
6 -0.5071 4345 ± 18 163 ± 17 22.8 ± 4.5 1.2 ± 0.3 1.0 ± 0.3 2.81
7 -0.4057 4391 ± 22 178 ± 18 22.4 ± 4.7 1.0 ± 0.3 1.7 ± 0.4 2.86
8 -0.3043 4331 ± 39 223 ± 31 17.3 ± 4.9 1.4 ± 0.5 1.6 ± 0.6 2.78
9 -0.2028 4551 ± 15 274 ± 12 54.9 ± 6.3 2.3 ± 0.3 2.1 ± 0.3 2.61
10 -0.1014 4560 ± 10 444 ± 9 205.9 ± 13.8 3.2 ± 0.2 2.0 ± 0.2 3.16
11 0.0000 4481 ± 7 437 ± 6 316.4 ± 16.3 3.5 ± 0.2 1.8 ± 0.1 3.89
12 0.1014 4308 ± 5 178 ± 4 74.1 ± 5.0 2.5 ± 0.2 1.6 ± 0.1 2.87
13 0.2028 4339 ± 10 135 ± 9 16.0 ± 3.4 2.2 ± 0.6 3.4 ± 0.8 2.33
14 0.3043 4323 ± 12 109 ± 11 10.1 ± 3.0 2.1 ± 0.8 3.5 ± 1.2 2.67
15 0.4057 4336 ± 9 51 ± 8 11.2 ± 3.0 0.9 ± 0.4 0.3 ± 0.2 2.50
16 0.5071 4288 ± 26 159 ± 25 17.0 ± 4.4 1.0 ± 0.4 0.9 ± 0.4 2.88
17 0.6085 4314 ± 25 137 ± 24 7.9 ± 3.3 2.4 ± 1.2 1.9 ± 1.0 2.97
18 0.7099 4331 ± 15 80 ± 16 11.4 ± 3.6 1.0 ± 0.5 0.3 ± 0.2 2.90
20 0.9128 4110 ± 28 158 ± 24 11.4 ± 3.5 0.1 ± 0.3 2.3 ± 0.9 2.96
21 1.0142 4483 ± 39 200 ± 33 8.7 ± 3.8 3.0 ± 1.5 0.7 ± 0.6 2.86
Slit 2: X-Offset +0.2 ′′
1 -1.0142 4366 ± 10 75 ± 9 11.1 ± 2.7 1.4 ± 0.4 0.4 ± 0.2 3.19
2 -0.9128 4380 ± 10 80 ± 10 8.5 ± 2.4 1.8 ± 0.6 1.1 ± 0.4 3.07
7 -0.4057 4450 ± 13 101 ± 13 4.6 ± 2.5 3.5 ± 2.0 3.7 ± 2.1 2.81
8 -0.3043 4466 ± 9 84 ± 9 4.2 ± 2.2 4.2 ± 2.3 5.0 ± 2.7 2.91
9 -0.2028 4449 ± 11 91 ± 11 6.7 ± 2.4 2.1 ± 0.9 3.0 ± 1.2 2.83
10 -0.1014 4453 ± 7 84 ± 7 9.6 ± 2.6 3.3 ± 1.0 1.8 ± 0.6 2.91
11 0.0000 4433 ± 7 87 ± 7 9.3 ± 2.6 3.8 ± 1.2 2.4 ± 0.7 2.78
12 0.1014 4385 ± 7 77 ± 7 10.8 ± 2.5 2.5 ± 0.7 1.4 ± 0.4 2.67
13 0.2028 4386 ± 14 131 ± 15 5.2 ± 2.7 6.5 ± 3.5 1.9 ± 1.1 2.56
14 0.3043 4411 ± 8 61 ± 8 8.3 ± 2.3 1.7 ± 0.6 1.3 ± 0.5 2.61
15 0.4057 4421 ± 20 107 ± 19 10.6 ± 3.5 1.1 ± 0.5 0.9 ± 0.4 2.66
16 0.5071 4342 ± 22 83 ± 23 6.1 ± 2.8 1.1 ± 0.7 1.1 ± 0.7 2.77
17 0.6085 4413 ± 44 114 ± 44 3.7 ± 2.8 2.2 ± 2.0 0.4 ± 0.7 2.96
21 1.0142 4112 ± 35 130 ± 34 5.6 ± 2.8 0.1 ± 0.4 2.0 ± 1.2 3.34
93

Table 3.6. NGC 315: Measured Parameters.
Row Y-Offset vr σgas F(Hα/10 −16 ) F([NII]6585) F([SII]total) R 2
( ′′ ) (km s −1 ) (km s −1 ) (erg s −1 cm −2 Hz −1 ) F(Hα) F(Hα)
Slit 1: X-Offset -0.1 ′′
1 -0.5071 4827 ± 22 70 ± 21 39.1 ± 17.8 0.0 ± 0.3 0.5 ± 0.4 1.67
7 -0.2028 4884 ± 34 161 ± 31 52.2 ± 19.8 1.2 ± 0.6 1.2 ± 0.6 1.90
8 -0.1521 4943 ± 33 175 ± 29 33.0 ± 17.3 3.0 ± 1.7 2.7 ± 1.6 1.93
9 -0.1014 4866 ± 32 193 ± 27 62.0 ± 19.8 2.4 ± 0.9 1.0 ± 0.4 1.65
10 -0.0507 4905 ± 37 272 ± 32 88.4 ± 25.3 2.4 ± 0.8 0.9 ± 0.4 1.84
11 0.0000 4917 ± 28 302 ± 24 151.2 ± 29.4 2.5 ± 0.6 1.3 ± 0.3 1.83
12 0.0507 4814 ± 48 485 ± 44 60.7 ± 45.0 8.3 ± 6.3 3.0 ± 2.3 1.90
13 0.1014 4882 ± 36 337 ± 35 61.7 ± 28.1 5.4 ± 2.6 2.2 ± 1.1 1.88
14 0.1521 5041 ± 8 65 ± 8 55.6 ± 13.8 1.6 ± 0.5 0.9 ± 0.3 1.64
15 0.2028 5036 ± 14 66 ± 13 42.2 ± 15.7 1.3 ± 0.6 0.5 ± 0.3 1.51
16 0.2535 5079 ± 17 79 ± 17 45.6 ± 17.0 1.2 ± 0.6 0.5 ± 0.3 1.45
17 0.3043 5069 ± 12 59 ± 11 65.0 ± 19.4 0.1 ± 0.2 0.6 ± 0.3 1.68
18 0.3550 5053 ± 8 43 ± 7 25.4 ± 9.9 0.5 ± 0.4 2.1 ± 1.0 1.46
20 0.4564 5283 ± 11 42 ± 11 18.7 ± 10.4 0.4 ± 0.5 1.6 ± 1.1 1.28
Slit 0: X-Offset 0.0 ′′
1 -0.5071 4880 ± 43 174 ± 40 58.9 ± 22.8 0.9 ± 0.5 0.7 ± 0.4 1.36
2 -0.4564 4800 ± 31 160 ± 29 98.9 ± 26.6 0.7 ± 0.3 0.1 ± 0.2 1.65
4 -0.3550 4860 ± 38 166 ± 36 63.5 ± 22.0 1.2 ± 0.6 0.4 ± 0.3 1.55
5 -0.3043 4853 ± 30 183 ± 27 96.9 ± 23.9 1.1 ± 0.4 0.6 ± 0.3 1.47
6 -0.2535 4878 ± 26 206 ± 22 90.1 ± 21.7 1.8 ± 0.5 1.5 ± 0.4 1.62
7 -0.2028 4915 ± 18 162 ± 16 72.1 ± 17.8 2.0 ± 0.6 2.1 ± 0.6 1.63
8 -0.1521 4921 ± 26 263 ± 19 228.1 ± 29.8 1.3 ± 0.2 0.9 ± 0.2 1.38
9 -0.1014 4873 ± 19 347 ± 16 442.4 ± 43.7 2.1 ± 0.2 0.9 ± 0.1 1.79
10 -0.0507 4824 ± 9 354 ± 8 992.3 ± 53.0 2.2 ± 0.1 1.1 ± 0.1 2.39
11 0.0000 4835 ± 9 528 ± 7 899.0 ± 108.2 7.1 ± 0.9 1.8 ± 0.2 3.84
12 0.0507 4906 ± 9 457 ± 8 1314.6 ± 83.9 3.6 ± 0.2 0.9 ± 0.1 2.94
13 0.1014 4819 ± 28 438 ± 26 479.8 ± 62.2 1.9 ± 0.3 0.7 ± 0.1 1.89
14 0.1521 5124 ± 22 204 ± 18 156.1 ± 26.6 1.3 ± 0.3 0.8 ± 0.2 1.37
15 0.2028 5172 ± 33 172 ± 29 81.8 ± 22.6 0.9 ± 0.4 0.9 ± 0.4 1.74
17 0.3043 4957 ± 38 213 ± 29 117.9 ± 25.8 0.8 ± 0.3 0.7 ± 0.2 1.84
19 0.4057 5218 ± 14 60 ± 14 47.4 ± 16.3 0.7 ± 0.4 0.4 ± 0.3 1.49
20 0.4564 5060 ± 24 102 ± 24 60.6 ± 20.9 0.0 ± 0.2 0.6 ± 0.3 1.58
21 0.5071 5185 ± 8 39 ± 8 15.8 ± 8.5 1.1 ± 0.9 2.8 ± 1.7 1.78
Slit 2: X-Offset +0.1 ′′
3 -0.4057 4971 ± 26 164 ± 24 97.2 ± 22.4 0.8 ± 0.3 0.3 ± 0.2 1.60
4 -0.3550 4889 ± 22 154 ± 20 72.4 ± 17.4 1.2 ± 0.4 1.2 ± 0.4 1.67
5 -0.3043 4868 ± 18 169 ± 16 66.0 ± 16.7 2.5 ± 0.7 1.8 ± 0.5 1.67
6 -0.2535 4977 ± 12 136 ± 11 61.9 ± 14.8 3.0 ± 0.8 1.8 ± 0.5 1.83
7 -0.2028 4956 ± 16 222 ± 13 143.8 ± 20.6 2.1 ± 0.4 1.4 ± 0.3 1.69
8 -0.1521 4944 ± 11 208 ± 9 145.5 ± 18.8 3.2 ± 0.5 2.0 ± 0.3 1.56
9 -0.1014 4897 ± 7 214 ± 5 320.3 ± 22.0 2.6 ± 0.2 1.5 ± 0.1 1.96
10 -0.0507 4880 ± 5 239 ± 4 597.9 ± 27.9 2.8 ± 0.2 1.4 ± 0.1 1.99
11 0.0000 4883 ± 4 251 ± 3 712.0 ± 30.2 3.2 ± 0.2 1.4 ± 0.1 1.90
12 0.0507 4953 ± 6 263 ± 4 657.0 ± 31.9 3.0 ± 0.2 1.2 ± 0.1 2.04
13 0.1014 4984 ± 8 242 ± 6 378.2 ± 26.5 2.9 ± 0.2 1.1 ± 0.1 2.30
14 0.1521 5021 ± 17 244 ± 13 198.5 ± 24.1 2.3 ± 0.3 1.2 ± 0.2 1.54
15 0.2028 5014 ± 43 273 ± 33 136.9 ± 28.1 1.2 ± 0.3 0.9 ± 0.3 1.68
17 0.3043 5097 ± 35 191 ± 30 49.1 ± 17.4 2.3 ± 1.0 1.0 ± 0.5 1.70
18 0.3550 5165 ± 45 190 ± 40 65.0 ± 21.8 0.8 ± 0.4 0.7 ± 0.4 1.94
19 0.4057 5256 ± 40 218 ± 31 108.3 ± 26.6 0.9 ± 0.3 0.4 ± 0.2 1.56
20 0.4564 5313 ± 50 222 ± 45 97.2 ± 30.9 0.4 ± 0.3 0.5 ± 0.3 1.71
21 0.5071 5169 ± 41 190 ± 35 63.9 ± 20.5 1.6 ± 0.7 0.1 ± 0.3 1.76
94

Table 3.7. NGC 383: Measured Parameters.
Row Y-Offset vr σgas F(Hα/10 −16 ) F([NII]6585) F([SII]total) R 2
( ′′ ) (km s −1 ) (km s −1 ) (erg s −1 cm −2 Hz −1 ) F(Hα) F(Hα)
Slit 1: X-Offset -0.1 ′′
2 -0.4564 4953 ± 7 37 ± 7 9.5 ± 5.5 3.4 ± 2.2 3.6 ± 2.4 1.40
3 -0.4057 4880 ± 21 105 ± 21 21.6 ± 10.0 2.4 ± 1.3 1.6 ± 1.1 1.58
4 -0.3550 4923 ± 41 184 ± 38 29.1 ± 13.5 2.4 ± 1.3 0.1 ± 0.7 1.62
5 -0.3043 4915 ± 30 163 ± 28 42.5 ± 14.2 1.9 ± 0.8 0.1 ± 0.4 1.86
6 -0.2535 4952 ± 24 201 ± 20 95.3 ± 17.3 1.3 ± 0.3 0.6 ± 0.3 1.91
7 -0.2028 4945 ± 18 205 ± 15 116.8 ± 16.9 1.5 ± 0.3 1.1 ± 0.3 1.48
8 -0.1521 4957 ± 13 173 ± 11 112.3 ± 14.9 1.7 ± 0.3 1.0 ± 0.2 1.68
9 -0.1014 5046 ± 16 248 ± 12 156.8 ± 18.2 2.1 ± 0.3 0.9 ± 0.2 1.64
10 -0.0507 5086 ± 11 269 ± 9 235.4 ± 20.0 2.6 ± 0.3 1.3 ± 0.2 1.65
11 0.0000 5135 ± 7 235 ± 5 274.4 ± 18.7 3.1 ± 0.2 1.3 ± 0.1 1.90
12 0.0507 5186 ± 7 223 ± 5 275.3 ± 18.6 2.7 ± 0.2 1.0 ± 0.1 2.04
13 0.1014 5201 ± 13 239 ± 10 157.2 ± 17.6 2.6 ± 0.3 1.0 ± 0.2 1.48
14 0.1521 5263 ± 40 306 ± 35 64.9 ± 20.0 3.1 ± 1.1 0.5 ± 0.5 1.34
17 0.3043 5166 ± 40 126 ± 40 31.0 ± 14.3 0.8 ± 0.6 0.6 ± 0.7 1.76
18 0.3550 5216 ± 25 87 ± 25 26.6 ± 11.7 0.3 ± 0.3 1.6 ± 1.0 1.58
20 0.4564 4457 ± 30 137 ± 29 40.8 ± 14.6 1.2 ± 0.6 0.4 ± 0.5 1.60
21 0.5071 5285 ± 7 37 ± 7 33.6 ± 9.2 0.4 ± 0.2 0.5 ± 0.3 1.70
Slit 0: X-Offset 0.0 ′′
1 -0.5071 4909 ± 19 94 ± 19 55.7 ± 18.5 0.8 ± 0.4 0.3 ± 0.3 1.68
2 -0.4564 4750 ± 33 140 ± 32 49.6 ± 18.0 1.0 ± 0.5 0.5 ± 0.5 1.68
3 -0.4057 4796 ± 16 93 ± 15 57.9 ± 15.5 1.0 ± 0.4 0.8 ± 0.4 1.72
4 -0.3550 4905 ± 41 212 ± 33 70.8 ± 21.1 1.4 ± 0.5 0.2 ± 0.4 1.71
5 -0.3043 4987 ± 24 149 ± 23 59.9 ± 17.9 1.6 ± 0.6 0.2 ± 0.4 1.56
6 -0.2535 4873 ± 24 213 ± 23 36.6 ± 16.8 5.0 ± 2.4 2.4 ± 1.4 1.76
7 -0.2028 4865 ± 11 182 ± 10 140.6 ± 18.8 2.2 ± 0.4 0.6 ± 0.2 1.89
8 -0.1521 4874 ± 15 319 ± 14 263.4 ± 29.6 2.7 ± 0.3 1.0 ± 0.2 2.08
9 -0.1014 4939 ± 16 464 ± 15 501.0 ± 54.0 3.1 ± 0.4 1.1 ± 0.2 2.17
10 -0.0507 4924 ± 21 798 ± 13 359.0 ± 186.5 13.3 ± 6.9 3.8 ± 2.0 2.99
11 0.0000 5266 ± 44 924 ± 28 5274.1 ± 587.9 0.6 ± 0.1 0.3 ± 0.1 2.68
13 0.1014 5258 ± 16 311 ± 15 181.2 ± 28.0 3.1 ± 0.5 0.7 ± 0.2 1.83
14 0.1521 5299 ± 29 288 ± 29 40.4 ± 22.6 5.9 ± 3.4 0.4 ± 0.8 1.80
15 0.2028 5188 ± 27 159 ± 26 46.7 ± 18.3 2.1 ± 0.9 0.2 ± 0.5 1.69
18 0.3550 4537 ± 57 265 ± 44 67.6 ± 22.3 1.7 ± 0.7 0.5 ± 0.5 1.47
19 0.4057 5193 ± 24 135 ± 24 58.6 ± 18.6 1.2 ± 0.5 0.4 ± 0.4 1.53
20 0.4564 5239 ± 22 108 ± 21 23.9 ± 13.3 2.8 ± 1.7 0.6 ± 0.9 1.76
21 0.5071 5069 ± 11 38 ± 10 22.4 ± 10.1 0.5 ± 0.4 1.5 ± 1.0 1.36
Slit 2: X-Offset +0.1 ′′
1 -0.5071 4871 ± 8 39 ± 7 45.1 ± 13.5 0.4 ± 0.2 0.2 ± 0.2 1.48
2 -0.4564 4865 ± 18 89 ± 18 38.1 ± 12.8 1.4 ± 0.6 0.2 ± 0.4 1.74
4 -0.3550 4855 ± 12 54 ± 12 26.0 ± 10.1 1.5 ± 0.8 0.1 ± 0.5 2.26
5 -0.3043 4813 ± 16 79 ± 16 48.2 ± 15.6 0.7 ± 0.4 0.4 ± 0.3 1.77
6 -0.2535 4777 ± 8 64 ± 8 53.1 ± 11.6 1.3 ± 0.4 0.6 ± 0.3 1.97
7 -0.2028 4813 ± 8 105 ± 8 40.0 ± 10.5 5.2 ± 1.5 1.4 ± 0.6 1.79
8 -0.1521 4857 ± 9 145 ± 9 98.8 ± 14.3 2.6 ± 0.5 1.2 ± 0.3 1.91
9 -0.1014 4922 ± 20 289 ± 17 203.9 ± 24.9 2.0 ± 0.3 1.1 ± 0.2 1.67
10 -0.0507 4967 ± 11 257 ± 8 333.5 ± 25.0 2.0 ± 0.2 0.6 ± 0.1 1.76
11 0.0000 5083 ± 22 406 ± 21 290.3 ± 38.2 2.4 ± 0.4 0.9 ± 0.2 1.53
12 0.0507 5169 ± 35 420 ± 34 245.2 ± 42.5 1.8 ± 0.4 0.7 ± 0.2 1.82
13 0.1014 5229 ± 19 190 ± 18 69.8 ± 16.8 2.6 ± 0.7 0.8 ± 0.4 1.65
18 0.3550 4761 ± 16 64 ± 15 34.8 ± 12.3 0.0 ± 0.3 0.9 ± 0.6 1.75
19 0.4057 5278 ± 23 82 ± 23 15.8 ± 10.7 2.4 ± 1.9 1.4 ± 1.5 1.66
20 0.4564 5122 ± 47 179 ± 43 28.2 ± 15.5 2.2 ± 1.4 1.5 ± 1.3 1.84
21 0.5071 5260 ± 11 59 ± 11 40.4 ± 12.3 1.0 ± 0.4 0.1 ± 0.3 1.81
95

Table 3.8. NGC 541: Measured Parameters.
Row Y-Offset vr σgas F(Hα/10 −16 ) F([NII]6585) F([SII]total) R 2
( ′′ ) (km s −1 ) (km s −1 ) (erg s −1 cm −2 Hz −1 ) F(Hα) F(Hα)
Slit 1: X-Offset -0.2 ′′
2 -0.9128 5600 ± 41 188 ± 35 11.4 ± 4.5 1.6 ± 0.8 1.1 ± 0.6 2.73
5 -0.6085 5516 ± 4 51 ± 4 29.4 ± 4.0 0.4 ± 0.1 0.2 ± 0.1 3.11
6 -0.5071 5528 ± 6 60 ± 6 26.7 ± 4.1 0.5 ± 0.2 0.2 ± 0.1 3.27
7 -0.4057 5535 ± 7 54 ± 6 21.5 ± 3.9 0.7 ± 0.2 0.4 ± 0.1 2.86
8 -0.3043 5195 ± 7 43 ± 7 3.2 ± 1.8 4.5 ± 2.8 1.9 ± 1.3 2.36
9 -0.2028 5220 ± 23 142 ± 22 4.7 ± 3.2 5.6 ± 4.1 4.3 ± 3.1 2.66
10 -0.1014 5297 ± 19 140 ± 18 11.6 ± 4.1 2.8 ± 1.1 1.2 ± 0.6 2.34
11 0.0000 5389 ± 15 168 ± 14 17.6 ± 4.3 4.1 ± 1.1 0.0 ± 0.2 2.61
12 0.1014 5451 ± 8 63 ± 8 4.4 ± 2.3 6.6 ± 3.6 2.6 ± 1.5 2.57
13 0.2028 5442 ± 13 107 ± 14 13.6 ± 3.5 2.4 ± 0.8 0.7 ± 0.3 2.34
14 0.3043 5419 ± 5 104 ± 5 38.3 ± 3.8 1.8 ± 0.2 1.1 ± 0.2 2.85
15 0.4057 5401 ± 4 66 ± 4 34.2 ± 3.8 0.8 ± 0.1 0.7 ± 0.1 2.70
16 0.5071 5390 ± 6 63 ± 6 22.6 ± 3.5 0.9 ± 0.2 0.2 ± 0.1 3.38
17 0.6085 5379 ± 11 80 ± 11 11.4 ± 2.9 1.2 ± 0.4 1.3 ± 0.4 3.38
18 0.7099 5403 ± 11 69 ± 11 9.0 ± 2.7 1.3 ± 0.5 1.1 ± 0.5 2.57
19 0.8114 5497 ± 20 77 ± 21 5.4 ± 2.6 1.4 ± 0.9 1.1 ± 0.8 2.49
20 0.9128 5742 ± 21 47 ± 20 5.1 ± 3.0 0.0 ± 0.3 0.4 ± 0.5 3.00
Slit 0: X-Offset 0.0 ′′
5 -0.6085 5485 ± 7 45 ± 6 17.6 ± 3.7 0.3 ± 0.1 0.2 ± 0.1 2.10
6 -0.5071 5498 ± 5 43 ± 4 25.2 ± 4.1 0.1 ± 0.1 0.1 ± 0.1 2.59
7 -0.4057 5471 ± 5 29 ± 4 13.4 ± 3.0 0.6 ± 0.2 0.1 ± 0.1 2.98
9 -0.2028 5406 ± 24 163 ± 22 13.0 ± 4.3 2.2 ± 0.9 2.1 ± 0.8 2.26
10 -0.1014 5597 ± 23 362 ± 21 78.5 ± 11.2 2.6 ± 0.4 1.0 ± 0.2 2.78
11 0.0000 5459 ± 16 336 ± 13 138.3 ± 11.7 2.0 ± 0.2 0.4 ± 0.1 2.44
12 0.1014 5402 ± 23 164 ± 21 21.6 ± 5.2 1.7 ± 0.5 0.3 ± 0.2 2.54
13 0.2028 5331 ± 8 38 ± 8 8.7 ± 2.8 0.7 ± 0.3 0.7 ± 0.4 2.60
14 0.3043 5377 ± 8 55 ± 7 14.5 ± 3.2 0.9 ± 0.3 0.6 ± 0.2 2.73
15 0.4057 5372 ± 3 36 ± 3 26.1 ± 3.5 0.4 ± 0.1 0.3 ± 0.1 2.54
16 0.5071 5360 ± 8 77 ± 8 27.2 ± 4.4 0.3 ± 0.1 0.5 ± 0.1 2.51
17 0.6085 5250 ± 32 117 ± 31 4.5 ± 2.9 0.7 ± 0.8 3.1 ± 2.3 2.28
20 0.9128 5411 ± 14 47 ± 14 5.5 ± 2.6 0.1 ± 0.3 0.9 ± 0.7 2.62
Slit 2: X-Offset +0.2 ′′
1 -1.0142 5503 ± 24 84 ± 22 8.2 ± 3.4 0.8 ± 0.5 0.5 ± 0.4 3.02
2 -0.9128 5039 ± 38 160 ± 36 8.9 ± 3.7 0.2 ± 0.3 1.4 ± 0.8 2.87
6 -0.5071 5484 ± 8 73 ± 8 20.5 ± 3.6 0.5 ± 0.2 0.6 ± 0.2 3.47
7 -0.4057 5382 ± 11 107 ± 11 33.3 ± 5.0 0.2 ± 0.1 0.4 ± 0.1 3.15
8 -0.3043 5428 ± 11 108 ± 11 27.5 ± 4.5 0.9 ± 0.2 0.2 ± 0.1 2.56
9 -0.2028 5383 ± 9 68 ± 8 14.0 ± 3.1 1.2 ± 0.4 0.9 ± 0.3 2.62
10 -0.1014 5371 ± 17 110 ± 17 16.4 ± 4.0 0.9 ± 0.3 1.0 ± 0.3 2.34
11 0.0000 5410 ± 20 106 ± 20 19.5 ± 5.4 0.1 ± 0.2 0.6 ± 0.2 2.79
12 0.1014 5292 ± 17 117 ± 17 19.6 ± 4.5 1.1 ± 0.3 0.2 ± 0.2 2.62
13 0.2028 5312 ± 3 27 ± 4 16.1 ± 3.8 0.5 ± 0.2 0.3 ± 0.1 2.63
14 0.3043 5324 ± 5 49 ± 5 20.2 ± 3.4 0.5 ± 0.1 0.3 ± 0.1 2.89
15 0.4057 5330 ± 6 55 ± 5 19.9 ± 3.1 0.5 ± 0.1 0.5 ± 0.1 2.85
16 0.5071 5346 ± 6 54 ± 5 22.0 ± 3.5 0.2 ± 0.1 0.3 ± 0.1 2.85
17 0.6085 5343 ± 6 42 ± 6 12.9 ± 2.9 0.1 ± 0.1 0.4 ± 0.2 2.60
19 0.8114 5275 ± 20 75 ± 19 9.2 ± 3.3 0.0 ± 0.2 0.4 ± 0.3 2.60
20 0.9128 4453 ± 26 144 ± 24 11.4 ± 3.0 0.1 ± 0.2 1.4 ± 0.5 2.37
96

Table 3.9. NGC 741: Measured Parameters.
Row Y-Offset vr σgas F(Hα/10 −16 ) F([NII]6585) F([SII]total) R 2
( ′′ ) (km s −1 ) (km s −1 ) (erg s −1 cm −2 Hz −1 ) F(Hα) F(Hα)
Slit 1: X-Offset -0.2 ′′
2 -0.9128 5337 ± 33 86 ± 31 5.6 ± 3.5 0.0 ± 0.3 1.2 ± 0.9 2.41
3 -0.8114 5309 ± 28 125 ± 28 15.0 ± 5.3 0.1 ± 0.2 0.6 ± 0.3 2.69
6 -0.5071 5303 ± 32 190 ± 29 7.1 ± 4.2 4.1 ± 2.6 1.3 ± 1.0 3.00
7 -0.4057 5465 ± 23 100 ± 22 7.5 ± 3.8 1.8 ± 1.1 0.8 ± 0.6 3.08
12 0.1014 5686 ± 20 138 ± 19 11.9 ± 3.9 1.7 ± 0.7 1.9 ± 0.7 2.83
13 0.2028 5616 ± 41 192 ± 37 9.5 ± 4.7 2.4 ± 1.4 0.6 ± 0.5 3.50
18 0.7099 5252 ± 42 181 ± 41 9.6 ± 4.2 0.1 ± 0.3 1.5 ± 0.8 3.33
19 0.8114 5317 ± 10 37 ± 10 10.5 ± 3.9 0.3 ± 0.2 0.0 ± 0.1 2.94
Slit 0: X-Offset 0.0 ′′
2 -0.9128 5091 ± 54 168 ± 49 13.7 ± 6.4 0.7 ± 0.5 0.5 ± 0.4 2.12
6 -0.5071 5164 ± 0 3 ± 0 0.1 ± 0.0 2.4 ± 0.0 0.4 ± 2.1 2.45
11 0.0000 5706 ± 26 424 ± 24 57.2 ± 14.4 4.2 ± 1.1 1.8 ± 0.5 2.40
12 0.1014 5882 ± 52 361 ± 47 25.8 ± 10.3 2.8 ± 1.2 1.3 ± 0.7 2.22
13 0.2028 5163 ± 28 96 ± 28 7.6 ± 4.1 0.7 ± 0.6 1.5 ± 1.0 2.15
Slit 2: X-Offset +0.2 ′′
10 -0.1014 5559 ± 32 96 ± 30 12.1 ± 5.8 0.4 ± 0.4 0.3 ± 0.3 2.40
11 0.0000 5608 ± 21 122 ± 20 22.4 ± 6.3 0.7 ± 0.3 0.3 ± 0.2 2.92
14 0.3043 5171 ± 10 61 ± 10 4.2 ± 2.3 0.9 ± 0.7 3.5 ± 2.1 2.63
97

Table 3.10. UGC 01841: Measured Parameters.
Row Y-Offset vr σgas F(Hα/10 −16 ) F([NII]6585) F([SII]total) R 2
( ′′ ) (km s −1 ) (km s −1 ) (erg s −1 cm −2 Hz −1 ) F(Hα) F(Hα)
Slit 1: X-Offset -0.2 ′′
1 -1.0142 6626 ± 13 87 ± 13 10.6 ± 2.6 1.0 ± 0.3 0.4 ± 0.2 4.21
2 -0.9128 6276 ± 27 172 ± 25 5.5 ± 2.4 3.5 ± 1.7 1.3 ± 0.9 4.16
5 -0.6085 6444 ± 7 60 ± 7 13.1 ± 2.6 0.8 ± 0.2 0.3 ± 0.2 4.90
6 -0.5071 6258 ± 47 289 ± 35 22.2 ± 4.6 1.0 ± 0.3 1.1 ± 0.3 4.45
7 -0.4057 6416 ± 9 115 ± 9 6.9 ± 2.1 4.6 ± 1.5 1.5 ± 0.6 4.76
8 -0.3043 6411 ± 7 137 ± 7 9.3 ± 2.2 5.8 ± 1.5 2.9 ± 0.8 4.34
9 -0.2028 6379 ± 13 234 ± 10 48.3 ± 4.0 1.5 ± 0.2 0.5 ± 0.1 3.53
10 -0.1014 6155 ± 29 574 ± 25 28.0 ± 11.2 7.2 ± 2.9 3.0 ± 1.3 4.58
11 0.0000 6228 ± 10 316 ± 8 85.7 ± 5.9 2.5 ± 0.2 1.0 ± 0.1 4.20
12 0.1014 6305 ± 8 212 ± 7 38.8 ± 3.5 2.5 ± 0.3 1.1 ± 0.2 4.32
13 0.2028 6088 ± 47 426 ± 47 12.8 ± 5.8 4.4 ± 2.1 0.6 ± 0.6 4.56
14 0.3043 6369 ± 36 155 ± 32 4.1 ± 2.4 3.2 ± 2.0 0.3 ± 0.9 4.48
15 0.4057 6458 ± 24 95 ± 23 3.4 ± 2.0 1.7 ± 1.2 2.3 ± 1.7 5.04
16 0.5071 6725 ± 19 57 ± 19 5.2 ± 2.4 0.4 ± 0.3 0.4 ± 0.4 3.89
17 0.6085 6433 ± 32 125 ± 32 3.2 ± 2.0 2.7 ± 2.0 0.9 ± 1.1 5.27
19 0.8114 6617 ± 20 84 ± 20 9.2 ± 3.8 0.4 ± 0.3 0.1 ± 0.3 3.96
20 0.9128 6320 ± 22 112 ± 21 4.8 ± 1.9 2.3 ± 1.1 1.1 ± 0.7 4.76
Slit 0: X-Offset 0.0 ′′
3 -0.8114 6350 ± 12 68 ± 11 4.0 ± 2.2 3.9 ± 2.4 0.4 ± 0.7 3.40
4 -0.7099 6339 ± 23 125 ± 23 14.1 ± 4.2 1.1 ± 0.4 0.5 ± 0.3 2.62
6 -0.5071 6276 ± 21 169 ± 19 9.2 ± 3.6 4.4 ± 1.9 1.1 ± 0.7 2.43
7 -0.4057 6371 ± 15 163 ± 14 16.3 ± 3.8 3.0 ± 0.8 0.1 ± 0.3 3.18
8 -0.3043 6428 ± 10 164 ± 10 22.8 ± 3.9 3.2 ± 0.6 0.9 ± 0.3 3.83
9 -0.2028 6329 ± 10 278 ± 8 110.7 ± 7.2 1.9 ± 0.2 1.1 ± 0.1 3.44
10 -0.1014 6337 ± 7 596 ± 6 215.6 ± 26.7 9.1 ± 1.1 3.2 ± 0.4 4.16
11 0.0000 6305 ± 5 592 ± 4 1001.2 ± 37.8 3.0 ± 0.1 1.1 ± 0.1 4.79
13 0.2028 6322 ± 26 260 ± 21 26.3 ± 5.2 2.2 ± 0.5 0.3 ± 0.2 3.46
14 0.3043 6126 ± 27 176 ± 26 5.2 ± 3.3 5.2 ± 3.5 2.8 ± 2.1 2.94
15 0.4057 6451 ± 31 105 ± 31 5.1 ± 3.0 1.6 ± 1.1 1.6 ± 1.2 3.10
17 0.6085 6407 ± 36 104 ± 33 10.6 ± 4.8 0.2 ± 0.2 0.5 ± 0.4 3.84
Slit 2: X-Offset +0.2 ′′
1 -1.0142 6449 ± 35 172 ± 33 7.7 ± 3.1 2.0 ± 1.0 0.7 ± 0.6 4.02
3 -0.8114 6303 ± 12 109 ± 12 4.6 ± 2.1 4.8 ± 2.3 3.8 ± 1.9 3.60
6 -0.5071 6394 ± 10 85 ± 10 12.3 ± 2.7 1.5 ± 0.4 0.9 ± 0.3 3.62
7 -0.4057 6393 ± 5 72 ± 4 7.1 ± 1.9 5.2 ± 1.5 1.3 ± 0.5 3.12
8 -0.3043 6412 ± 5 111 ± 5 17.2 ± 2.6 3.9 ± 0.6 0.9 ± 0.3 3.54
9 -0.2028 6388 ± 5 120 ± 5 25.7 ± 3.1 2.4 ± 0.3 1.6 ± 0.3 4.25
10 -0.1014 6390 ± 6 166 ± 6 42.1 ± 3.7 2.2 ± 0.2 1.5 ± 0.2 3.76
11 0.0000 6363 ± 6 150 ± 6 46.0 ± 3.8 1.5 ± 0.2 1.1 ± 0.1 3.04
12 0.1014 6415 ± 10 165 ± 9 21.3 ± 3.4 2.8 ± 0.5 1.1 ± 0.3 4.05
14 0.3043 6328 ± 20 123 ± 20 7.3 ± 2.6 2.4 ± 1.0 0.5 ± 0.6 4.44
17 0.6085 6204 ± 14 79 ± 14 6.7 ± 2.3 1.8 ± 0.8 0.1 ± 0.5 3.44
18 0.7099 6450 ± 44 268 ± 39 7.3 ± 3.6 3.6 ± 1.9 1.0 ± 0.9 3.65
20 0.9128 6391 ± 27 120 ± 27 7.7 ± 2.9 0.0 ± 0.2 1.9 ± 1.0 3.41
21 1.0142 6118 ± 7 45 ± 7 9.7 ± 2.3 0.4 ± 0.2 0.5 ± 0.3 3.95
98

Table 3.11. NGC 2329: Measured Parameters.
Row Y-Offset vr σgas F(Hα/10 −16 ) F([NII]6585) F([SII]total) R 2
( ′′ ) (km s −1 ) (km s −1 ) (erg s −1 cm −2 Hz −1 ) F(Hα) F(Hα)
Slit 1: X-Offset -0.2 ′′
2 -0.9128 6017 ± 7 52 ± 7 13.0 ± 2.6 0.4 ± 0.1 0.3 ± 0.2 3.27
3 -0.8114 5709 ± 49 164 ± 48 4.6 ± 2.7 1.7 ± 1.2 1.7 ± 1.4 2.73
4 -0.7099 5752 ± 52 284 ± 40 28.8 ± 5.7 0.4 ± 0.2 0.2 ± 0.2 3.24
5 -0.6085 5973 ± 10 67 ± 11 8.9 ± 2.3 1.2 ± 0.4 0.5 ± 0.3 3.19
6 -0.5071 5989 ± 13 59 ± 12 8.8 ± 3.1 0.5 ± 0.3 0.8 ± 0.4 2.98
7 -0.4057 5493 ± 26 112 ± 26 7.4 ± 2.7 1.2 ± 0.6 0.6 ± 0.5 3.33
8 -0.3043 5816 ± 39 223 ± 30 12.7 ± 3.8 2.1 ± 0.7 0.2 ± 0.4 3.04
9 -0.2028 5810 ± 20 154 ± 20 9.5 ± 3.2 3.3 ± 1.3 0.2 ± 0.5 2.53
10 -0.1014 5763 ± 13 133 ± 13 16.6 ± 3.6 2.3 ± 0.6 0.7 ± 0.4 2.67
11 0.0000 5747 ± 13 150 ± 12 16.0 ± 3.2 3.4 ± 0.8 0.5 ± 0.4 2.51
12 0.1014 5775 ± 19 201 ± 16 25.0 ± 4.0 1.8 ± 0.4 0.1 ± 0.2 2.94
13 0.2028 5855 ± 26 170 ± 22 9.4 ± 3.0 2.7 ± 1.0 0.9 ± 0.6 2.90
14 0.3043 5678 ± 8 29 ± 7 2.8 ± 1.2 1.6 ± 0.9 1.0 ± 0.9 3.03
18 0.7099 5748 ± 32 137 ± 31 6.4 ± 2.6 1.6 ± 0.8 0.6 ± 0.7 3.22
Slit 0: X-Offset 0.0 ′′
1 -1.0142 5898 ± 23 74 ± 23 3.7 ± 2.6 2.2 ± 1.8 2.0 ± 2.0 1.93
5 -0.6085 6063 ± 10 38 ± 11 5.3 ± 2.5 1.2 ± 0.8 0.4 ± 0.6 2.34
6 -0.5071 5877 ± 28 129 ± 28 11.8 ± 4.2 0.1 ± 0.3 1.9 ± 0.9 2.50
7 -0.4057 5943 ± 12 79 ± 11 11.8 ± 3.3 1.8 ± 0.7 1.1 ± 0.5 2.20
9 -0.2028 5819 ± 9 104 ± 9 20.5 ± 4.3 2.6 ± 0.6 1.7 ± 0.5 2.17
10 -0.1014 5795 ± 5 268 ± 5 96.0 ± 9.6 6.6 ± 0.7 2.2 ± 0.3 3.19
11 0.0000 5789 ± 4 301 ± 4 348.6 ± 13.8 3.0 ± 0.1 1.1 ± 0.1 3.82
12 0.1014 5735 ± 2 61 ± 2 30.4 ± 4.1 3.7 ± 0.6 0.1 ± 0.2 4.66
14 0.3043 5627 ± 16 76 ± 16 13.3 ± 4.5 0.7 ± 0.4 0.3 ± 0.4 2.64
20 0.9128 5782 ± 45 146 ± 43 12.2 ± 5.1 0.6 ± 0.4 0.2 ± 0.5 2.23
21 1.0142 5770 ± 38 111 ± 37 4.1 ± 3.0 2.5 ± 2.1 0.6 ± 1.4 2.25
Slit 2: X-Offset +0.2 ′′
1 -1.0142 5643 ± 37 154 ± 35 8.9 ± 3.4 1.4 ± 0.7 0.5 ± 0.6 2.15
2 -0.9128 5560 ± 7 32 ± 10 6.7 ± 2.9 0.4 ± 0.3 0.4 ± 0.4 2.48
8 -0.3043 5905 ± 5 53 ± 5 21.3 ± 3.3 0.5 ± 0.1 0.7 ± 0.2 2.64
9 -0.2028 5830 ± 21 195 ± 20 11.6 ± 3.8 3.9 ± 1.4 1.2 ± 0.7 2.69
10 -0.1014 5875 ± 9 119 ± 9 25.0 ± 3.8 1.9 ± 0.4 0.1 ± 0.2 2.94
11 0.0000 5844 ± 10 123 ± 10 24.2 ± 4.0 1.8 ± 0.4 1.0 ± 0.3 2.44
12 0.1014 5839 ± 6 82 ± 6 20.7 ± 3.3 1.8 ± 0.4 0.6 ± 0.2 2.66
13 0.2028 5742 ± 12 77 ± 12 12.5 ± 3.1 1.1 ± 0.4 0.5 ± 0.3 2.25
14 0.3043 5700 ± 8 45 ± 8 10.9 ± 2.9 0.7 ± 0.3 0.2 ± 0.3 2.58
15 0.4057 5631 ± 10 39 ± 9 6.5 ± 2.4 0.5 ± 0.3 0.3 ± 0.4 2.59
17 0.6085 5774 ± 30 157 ± 29 4.8 ± 2.8 4.0 ± 2.5 0.5 ± 1.1 2.71
19 0.8114 5841 ± 20 60 ± 20 5.3 ± 2.7 0.6 ± 0.5 0.9 ± 0.8 2.43
20 0.9128 5742 ± 13 59 ± 13 5.4 ± 2.2 1.6 ± 0.8 0.5 ± 0.7 2.61
99

Table 3.12. NGC 2892: Measured Parameters.
Row Y-Offset vr σgas F(Hα/10 −16 ) F([NII]6585) F([SII]total) R 2
( ′′ ) (km s −1 ) (km s −1 ) (erg s −1 cm −2 Hz −1 ) F(Hα) F(Hα)
Slit 1: X-Offset -0.2 ′′
1 -1.0142 6843 ± 8 25 ± 6 1.4 ± 0.9 1.1 ± 0.9 4.9 ± 3.6 3.48
3 -0.8114 6649 ± 13 76 ± 12 15.2 ± 3.6 0.1 ± 0.1 0.4 ± 0.2 3.31
4 -0.7099 6895 ± 22 143 ± 22 7.9 ± 2.5 1.8 ± 0.7 1.2 ± 0.7 3.43
6 -0.5071 6700 ± 20 71 ± 20 3.1 ± 1.9 2.0 ± 1.5 0.6 ± 1.0 3.25
8 -0.3043 6905 ± 14 81 ± 13 10.1 ± 2.7 0.9 ± 0.3 0.3 ± 0.3 3.19
9 -0.2028 6912 ± 23 71 ± 23 5.7 ± 2.7 0.5 ± 0.4 1.0 ± 0.7 3.18
11 0.0000 6844 ± 9 98 ± 9 10.4 ± 2.7 2.5 ± 0.7 0.5 ± 0.4 3.17
12 0.1014 6868 ± 12 99 ± 12 3.9 ± 2.9 5.8 ± 4.4 2.5 ± 2.1 2.98
13 0.2028 6935 ± 9 85 ± 10 3.6 ± 2.1 5.5 ± 3.4 3.6 ± 2.4 2.94
15 0.4057 6856 ± 8 35 ± 7 3.0 ± 1.4 1.8 ± 1.0 1.7 ± 1.3 2.95
16 0.5071 6891 ± 4 36 ± 3 8.0 ± 1.7 1.5 ± 0.4 0.3 ± 0.3 2.74
19 0.8114 6674 ± 22 71 ± 22 6.7 ± 2.8 0.0 ± 0.2 0.4 ± 0.4 3.38
21 1.0142 6931 ± 13 31 ± 13 3.4 ± 2.0 0.2 ± 0.3 0.1 ± 0.5 3.43
Slit 0: X-Offset 0.0 ′′
1 -1.0142 6734 ± 46 157 ± 44 5.8 ± 3.7 2.1 ± 1.6 1.2 ± 1.2 2.11
3 -0.8114 6665 ± 27 66 ± 26 7.1 ± 3.9 0.2 ± 0.3 0.5 ± 0.6 2.21
9 -0.2028 6962 ± 24 206 ± 21 26.6 ± 5.4 1.5 ± 0.4 0.1 ± 0.3 2.25
10 -0.1014 6844 ± 19 354 ± 18 28.1 ± 7.8 5.9 ± 1.7 1.4 ± 0.5 2.24
11 0.0000 6938 ± 7 453 ± 6 240.9 ± 17.0 4.3 ± 0.3 1.1 ± 0.1 2.44
12 0.1014 6947 ± 10 452 ± 9 259.5 ± 17.3 2.8 ± 0.2 0.5 ± 0.1 2.96
21 1.0142 6956 ± 33 81 ± 34 4.1 ± 2.9 1.5 ± 1.6 0.3 ± 1.1 1.98
Slit 2: X-Offset +0.2 ′′
3 -0.8114 6894 ± 28 65 ± 26 4.3 ± 2.7 0.0 ± 0.4 1.7 ± 1.4 2.70
4 -0.7099 7218 ± 44 147 ± 43 3.8 ± 2.9 3.0 ± 2.6 0.1 ± 1.2 1.70
5 -0.6085 6902 ± 34 134 ± 31 15.9 ± 5.5 0.0 ± 0.1 0.2 ± 0.3 2.70
7 -0.4057 6801 ± 21 92 ± 21 7.4 ± 3.0 1.5 ± 0.8 0.3 ± 0.6 2.44
10 -0.1014 6963 ± 43 260 ± 37 11.0 ± 4.7 2.9 ± 1.4 1.2 ± 0.9 2.22
11 0.0000 6840 ± 13 169 ± 12 38.5 ± 5.1 1.1 ± 0.2 0.2 ± 0.2 2.62
12 0.1014 6890 ± 10 138 ± 9 16.2 ± 3.3 3.2 ± 0.7 0.7 ± 0.4 2.52
13 0.2028 6957 ± 17 183 ± 17 5.8 ± 3.3 7.7 ± 4.6 1.0 ± 1.3 2.55
14 0.3043 6938 ± 26 135 ± 26 5.8 ± 3.0 2.9 ± 1.7 0.4 ± 0.9 2.42
15 0.4057 6899 ± 26 54 ± 25 4.3 ± 2.9 0.5 ± 0.6 0.4 ± 0.8 2.46
16 0.5071 6980 ± 38 213 ± 32 9.4 ± 4.0 2.6 ± 1.3 0.8 ± 0.8 2.17
17 0.6085 7064 ± 8 42 ± 8 3.2 ± 1.7 3.4 ± 2.0 0.4 ± 0.9 2.46
100

Table 3.13. NGC 3801: Measured Parameters.
Row Y-Offset vr σgas F(Hα/10 −16 ) F([NII]6585) F([SII]total) R 2
( ′′ ) (km s −1 ) (km s −1 ) (erg s −1 cm −2 Hz −1 ) F(Hα) F(Hα)
Slit 1: X-Offset -0.2 ′′
2 -0.9128 3372 ± 40 89 ± 40 3.7 ± 2.2 0.0 ± 0.3 0.2 ± 0.6 3.00
3 -0.8114 3436 ± 16 57 ± 16 4.3 ± 1.7 0.4 ± 0.3 0.4 ± 0.5 3.49
4 -0.7099 3468 ± 9 46 ± 9 3.4 ± 1.2 1.0 ± 0.5 1.7 ± 0.9 3.59
7 -0.4057 3476 ± 9 48 ± 9 1.5 ± 1.0 1.0 ± 0.9 7.5 ± 5.2 3.41
9 -0.2028 3325 ± 13 161 ± 12 25.4 ± 3.3 0.9 ± 0.2 0.8 ± 0.2 3.78
10 -0.1014 3383 ± 10 143 ± 9 20.8 ± 2.9 1.7 ± 0.3 0.8 ± 0.2 3.66
11 0.0000 3378 ± 12 142 ± 11 15.6 ± 2.8 1.9 ± 0.4 1.3 ± 0.3 3.01
12 0.1014 3345 ± 17 148 ± 17 14.5 ± 2.9 1.0 ± 0.3 1.1 ± 0.4 3.50
14 0.3043 3471 ± 16 74 ± 17 2.5 ± 1.5 3.1 ± 2.2 2.1 ± 1.7 3.23
17 0.6085 3317 ± 26 113 ± 24 8.0 ± 2.7 1.0 ± 0.5 0.3 ± 0.4 3.53
20 0.9128 3190 ± 19 56 ± 20 2.9 ± 1.6 0.9 ± 0.7 0.9 ± 0.9 3.17
Slit 0: X-Offset 0.0 ′′
2 -0.9128 3510 ± 26 124 ± 26 6.3 ± 2.5 1.7 ± 0.8 1.4 ± 0.8 2.76
3 -0.8114 3461 ± 17 57 ± 17 3.4 ± 1.8 1.2 ± 0.8 1.4 ± 1.2 2.43
6 -0.5071 3448 ± 18 157 ± 17 11.5 ± 2.8 2.5 ± 0.7 0.3 ± 0.4 2.51
8 -0.3043 3438 ± 12 75 ± 12 4.7 ± 2.0 2.6 ± 1.3 2.5 ± 1.3 2.02
9 -0.2028 3486 ± 12 146 ± 12 16.0 ± 3.0 2.1 ± 0.5 1.6 ± 0.4 2.55
10 -0.1014 3510 ± 12 174 ± 11 25.0 ± 3.7 2.0 ± 0.4 1.1 ± 0.3 2.56
11 0.0000 3498 ± 12 163 ± 12 25.8 ± 4.1 1.8 ± 0.4 1.1 ± 0.3 2.32
12 0.1014 3451 ± 14 129 ± 14 9.9 ± 3.1 3.1 ± 1.1 2.3 ± 0.9 2.72
13 0.2028 3397 ± 20 125 ± 20 10.8 ± 3.3 1.5 ± 0.6 1.1 ± 0.6 2.27
14 0.3043 3425 ± 31 208 ± 26 22.9 ± 4.7 0.9 ± 0.3 0.2 ± 0.3 2.20
17 0.6085 2822 ± 37 205 ± 36 21.4 ± 5.4 0.1 ± 0.1 0.7 ± 0.3 2.57
19 0.8114 3194 ± 28 108 ± 28 9.7 ± 3.5 0.1 ± 0.2 0.7 ± 0.5 2.43
20 0.9128 3184 ± 38 164 ± 38 13.8 ± 4.3 0.1 ± 0.2 0.5 ± 0.4 2.71
21 1.0142 3263 ± 47 180 ± 44 11.2 ± 4.1 0.5 ± 0.3 0.8 ± 0.5 2.66
Slit 2: X-Offset +0.2 ′′
2 -0.9128 3405 ± 17 53 ± 17 3.5 ± 1.7 0.7 ± 0.5 0.8 ± 0.7 2.96
3 -0.8114 3455 ± 15 47 ± 15 3.7 ± 1.6 0.6 ± 0.4 0.1 ± 0.4 2.64
4 -0.7099 3506 ± 10 39 ± 10 1.3 ± 0.9 3.4 ± 2.7 1.9 ± 1.9 2.44
5 -0.6085 3388 ± 16 67 ± 16 3.5 ± 1.6 0.1 ± 0.3 2.5 ± 1.4 2.43
7 -0.4057 3447 ± 19 119 ± 19 8.6 ± 2.4 0.5 ± 0.2 2.4 ± 0.8 2.75
8 -0.3043 3456 ± 11 102 ± 10 15.3 ± 2.9 0.7 ± 0.2 1.3 ± 0.3 2.62
9 -0.2028 3522 ± 12 93 ± 12 6.4 ± 1.9 2.1 ± 0.7 2.1 ± 0.8 2.93
10 -0.1014 3640 ± 17 138 ± 17 11.2 ± 2.6 1.0 ± 0.3 2.1 ± 0.6 2.70
11 0.0000 3611 ± 18 140 ± 18 8.7 ± 2.4 1.4 ± 0.5 2.8 ± 0.9 2.98
12 0.1014 3518 ± 19 121 ± 19 7.2 ± 2.3 1.1 ± 0.5 2.9 ± 1.1 2.93
13 0.2028 3441 ± 8 38 ± 8 5.9 ± 1.9 0.5 ± 0.3 0.6 ± 0.4 2.52
14 0.3043 3456 ± 9 63 ± 9 10.1 ± 2.2 0.5 ± 0.2 0.9 ± 0.4 2.43
15 0.4057 3451 ± 9 59 ± 9 7.8 ± 1.9 0.8 ± 0.3 1.5 ± 0.5 2.31
20 0.9128 3482 ± 18 99 ± 19 4.7 ± 1.8 1.8 ± 0.8 2.0 ± 1.0 2.90
101

Table 3.14. NGC 3862: Measured Parameters.
Row Y-Offset vr σgas F(Hα/10 −16 ) F([NII]6585) F([SII]total) R 2
( ′′ ) (km s −1 ) (km s −1 ) (erg s −1 cm −2 Hz −1 ) F(Hα) F(Hα)
Slit 1: X-Offset -0.2 ′′
1 -1.0142 6244 ± 13 48 ± 13 9.5 ± 4.4 0.6 ± 0.4 1.1 ± 0.8 2.10
5 -0.6085 6452 ± 9 56 ± 8 23.3 ± 5.4 0.4 ± 0.2 0.1 ± 0.2 2.22
6 -0.5071 6464 ± 5 43 ± 5 20.7 ± 4.2 0.7 ± 0.2 1.0 ± 0.3 1.94
7 -0.4057 6450 ± 5 43 ± 4 34.1 ± 5.5 0.2 ± 0.1 0.1 ± 0.1 2.25
8 -0.3043 6451 ± 9 78 ± 9 23.7 ± 4.9 1.3 ± 0.4 0.4 ± 0.3 2.07
9 -0.2028 6457 ± 8 80 ± 8 20.3 ± 4.9 2.0 ± 0.6 0.7 ± 0.4 2.30
10 -0.1014 6486 ± 13 149 ± 13 10.2 ± 5.1 7.7 ± 4.0 1.9 ± 1.4 2.36
11 0.0000 6468 ± 13 214 ± 12 42.7 ± 7.7 3.1 ± 0.6 1.2 ± 0.4 2.41
12 0.1014 6408 ± 9 87 ± 9 29.0 ± 5.4 1.3 ± 0.3 0.7 ± 0.3 2.36
13 0.2028 6438 ± 8 77 ± 8 32.2 ± 5.6 0.8 ± 0.2 0.3 ± 0.2 2.26
14 0.3043 6455 ± 5 47 ± 5 29.4 ± 4.9 0.2 ± 0.1 0.9 ± 0.3 2.27
15 0.4057 6460 ± 7 51 ± 7 21.1 ± 4.7 0.7 ± 0.2 0.4 ± 0.3 1.96
16 0.5071 6472 ± 6 38 ± 6 13.9 ± 3.9 0.8 ± 0.3 0.7 ± 0.4 2.10
17 0.6085 6478 ± 10 49 ± 9 10.8 ± 3.7 1.2 ± 0.5 0.4 ± 0.5 2.31
18 0.7099 6573 ± 18 66 ± 18 10.2 ± 4.5 0.9 ± 0.6 1.1 ± 0.8 1.95
21 1.0142 6463 ± 10 40 ± 10 5.6 ± 2.9 0.0 ± 0.4 3.3 ± 2.2 2.23
Slit 0: X-Offset 0.0 ′′
4 -0.7099 6525 ± 19 50 ± 19 7.6 ± 4.7 1.0 ± 0.9 0.5 ± 0.9 1.75
5 -0.6085 6510 ± 7 38 ± 8 17.5 ± 5.4 0.4 ± 0.2 0.6 ± 0.4 1.70
6 -0.5071 6503 ± 7 43 ± 7 10.1 ± 3.7 2.1 ± 0.9 1.1 ± 0.7 1.82
7 -0.4057 6512 ± 7 52 ± 6 21.3 ± 5.0 1.3 ± 0.4 0.3 ± 0.3 1.81
8 -0.3043 6520 ± 7 52 ± 7 14.0 ± 4.3 1.9 ± 0.7 1.4 ± 0.7 1.88
9 -0.2028 6520 ± 10 116 ± 10 39.4 ± 7.4 1.8 ± 0.4 0.2 ± 0.2 2.34
10 -0.1014 6605 ± 6 267 ± 6 84.9 ± 13.8 9.4 ± 1.6 3.7 ± 0.7 3.40
11 0.0000 6441 ± 4 302 ± 3 854.0 ± 25.6 2.4 ± 0.1 1.0 ± 0.1 4.21
12 0.1014 6474 ± 6 197 ± 6 18.8 ± 8.2 17.9 ± 7.8 0.7 ± 0.8 4.59
13 0.2028 6487 ± 15 147 ± 15 11.5 ± 5.8 6.2 ± 3.3 0.1 ± 0.9 2.01
14 0.3043 6526 ± 6 49 ± 6 20.9 ± 4.8 1.1 ± 0.3 0.6 ± 0.3 1.90
16 0.5071 6603 ± 44 199 ± 37 20.5 ± 7.9 1.5 ± 0.7 0.0 ± 0.5 1.96
17 0.6085 6511 ± 28 95 ± 28 10.6 ± 5.8 1.4 ± 1.0 0.4 ± 0.7 1.76
Slit 2: X-Offset +0.2 ′′
1 -1.0142 6364 ± 50 235 ± 40 14.1 ± 5.9 2.1 ± 1.0 0.4 ± 0.6 1.90
3 -0.8114 6480 ± 14 51 ± 13 5.6 ± 3.2 1.8 ± 1.2 0.9 ± 0.9 2.27
4 -0.7099 6526 ± 5 40 ± 5 5.6 ± 2.3 3.7 ± 1.7 1.8 ± 1.0 2.43
5 -0.6085 6536 ± 7 46 ± 7 12.8 ± 3.5 1.1 ± 0.4 0.1 ± 0.3 2.27
6 -0.5071 6541 ± 8 65 ± 8 18.3 ± 4.1 1.2 ± 0.3 0.3 ± 0.3 2.32
7 -0.4057 6527 ± 5 74 ± 5 12.7 ± 3.5 3.8 ± 1.1 0.8 ± 0.5 2.81
8 -0.3043 6554 ± 7 77 ± 7 16.0 ± 3.6 2.2 ± 0.6 1.3 ± 0.5 2.32
9 -0.2028 6551 ± 14 149 ± 14 15.1 ± 4.7 3.6 ± 1.2 1.1 ± 0.6 2.33
10 -0.1014 6625 ± 9 102 ± 8 13.9 ± 3.8 3.5 ± 1.1 2.5 ± 0.9 2.61
11 0.0000 6603 ± 10 118 ± 9 28.3 ± 5.1 2.0 ± 0.4 0.5 ± 0.3 1.99
12 0.1014 6581 ± 20 214 ± 18 26.8 ± 5.8 2.5 ± 0.6 1.1 ± 0.5 2.45
13 0.2028 6435 ± 34 235 ± 29 23.6 ± 6.3 1.8 ± 0.6 0.7 ± 0.4 2.06
14 0.3043 6450 ± 64 263 ± 49 26.0 ± 7.9 0.9 ± 0.4 0.5 ± 0.4 2.12
15 0.4057 6568 ± 6 46 ± 5 23.8 ± 4.4 0.5 ± 0.1 0.2 ± 0.2 1.99
16 0.5071 6530 ± 7 55 ± 7 15.6 ± 3.5 1.0 ± 0.3 1.3 ± 0.5 2.44
102

Table 3.15. UGC 7115: Measured Parameters.
Row Y-Offset vr σgas F(Hα/10 −16 ) F(N II6585) F(S IItotal) R 2
( ′′ ) (km s −1 ) (km s −1 ) (erg s −1 cm −2 Hz −1 ) F(Hα) F(Hα)
Slit 0: X-Offset 0.0 ′′
5 -0.6085 6792 ± 17 63 ± 18 5.7 ± 2.7 1.0 ± 0.7 0.6 ± 0.5 2.59
6 -0.5071 6886 ± 9 49 ± 8 8.4 ± 2.5 1.0 ± 0.4 0.5 ± 0.3 2.90
7 -0.4057 6863 ± 6 57 ± 6 15.8 ± 3.0 0.8 ± 0.2 0.7 ± 0.2 2.65
8 -0.3043 6897 ± 7 64 ± 7 15.1 ± 2.9 1.2 ± 0.3 0.6 ± 0.2 2.84
9 -0.2028 6914 ± 9 107 ± 9 17.1 ± 3.8 2.3 ± 0.6 0.9 ± 0.3 2.53
10 -0.1014 6963 ± 10 271 ± 9 74.7 ± 6.9 2.6 ± 0.3 1.1 ± 0.1 2.48
11 0.0000 6801 ± 9 496 ± 7 372.8 ± 19.3 2.4 ± 0.1 1.4 ± 0.1 2.79
12 0.1014 6625 ± 13 545 ± 10 138.7 ± 20.7 5.6 ± 0.8 2.3 ± 0.4 3.86
13 0.2028 6669 ± 8 224 ± 7 62.4 ± 5.0 2.3 ± 0.2 0.9 ± 0.1 2.92
15 0.4057 6639 ± 8 69 ± 8 3.1 ± 1.9 5.6 ± 3.7 4.7 ± 3.1 2.78
16 0.5071 6661 ± 5 40 ± 6 5.7 ± 1.8 1.9 ± 0.7 0.7 ± 0.4 2.42
103

Table 3.16. NGC 4261: Measured Parameters.
Row Y-Offset vr σgas F(Hα/10 −16 ) F([NII]6585) F([SII]total) R 2
( ′′ ) (km s −1 ) (km s −1 ) (erg s −1 cm −2 Hz −1 ) F(Hα) F(Hα)
Slit 1: X-Offset -0.1 ′′
1 -0.5071 2442 ± 17 126 ± 16 77.3 ± 19.6 1.6 ± 0.5 1.0 ± 0.4 1.62
2 -0.4564 2324 ± 17 149 ± 17 68.2 ± 18.7 2.3 ± 0.7 1.2 ± 0.5 1.62
3 -0.4057 2388 ± 14 114 ± 13 43.0 ± 15.6 3.3 ± 1.3 1.8 ± 0.8 1.54
4 -0.3550 2365 ± 16 186 ± 15 94.8 ± 20.8 2.7 ± 0.7 1.5 ± 0.4 1.45
5 -0.3043 2357 ± 11 193 ± 10 174.7 ± 23.0 2.5 ± 0.4 0.7 ± 0.2 1.83
6 -0.2535 2377 ± 7 195 ± 6 223.3 ± 23.1 3.3 ± 0.4 1.4 ± 0.2 1.64
7 -0.2028 2393 ± 6 237 ± 5 381.4 ± 27.7 3.4 ± 0.3 1.4 ± 0.1 1.91
8 -0.1521 2360 ± 7 343 ± 7 864.7 ± 48.2 2.8 ± 0.2 1.0 ± 0.1 2.24
9 -0.1014 2216 ± 7 463 ± 6 948.5 ± 69.4 5.0 ± 0.4 1.7 ± 0.1 1.96
10 -0.0507 2079 ± 7 461 ± 6 936.9 ± 69.3 5.0 ± 0.4 1.6 ± 0.1 2.17
11 0.0000 2038 ± 11 459 ± 10 491.7 ± 57.1 5.1 ± 0.6 1.4 ± 0.2 1.68
12 0.0507 2071 ± 20 406 ± 19 263.9 ± 43.1 3.5 ± 0.6 1.1 ± 0.2 1.85
13 0.1014 2099 ± 35 341 ± 32 84.0 ± 30.4 4.3 ± 1.6 1.7 ± 0.7 1.59
14 0.1521 2187 ± 29 239 ± 24 62.6 ± 21.5 3.7 ± 1.4 1.4 ± 0.7 1.68
18 0.3550 2142 ± 22 123 ± 22 52.5 ± 17.3 1.5 ± 0.6 0.9 ± 0.5 1.90
20 0.4564 2020 ± 34 119 ± 34 35.0 ± 16.8 1.5 ± 1.0 0.1 ± 0.5 1.50
21 0.5071 2021 ± 22 99 ± 22 45.1 ± 16.2 1.3 ± 0.6 0.1 ± 0.3 1.73
Slit 0: X-Offset 0.0 ′′
1 -0.5071 2327 ± 27 112 ± 26 33.6 ± 17.5 2.3 ± 1.4 0.4 ± 0.5 1.93
2 -0.4564 2283 ± 22 155 ± 21 51.3 ± 18.9 3.0 ± 1.3 0.7 ± 0.5 1.89
3 -0.4057 2274 ± 20 152 ± 18 46.9 ± 18.1 3.1 ± 1.3 2.6 ± 1.1 1.33
4 -0.3550 2216 ± 13 141 ± 12 71.3 ± 18.5 3.2 ± 0.9 1.8 ± 0.6 1.64
5 -0.3043 2233 ± 14 164 ± 13 84.7 ± 19.9 2.7 ± 0.7 2.2 ± 0.6 1.77
6 -0.2535 2249 ± 18 191 ± 15 125.0 ± 23.4 2.2 ± 0.5 0.4 ± 0.2 2.05
7 -0.2028 2280 ± 12 139 ± 12 118.2 ± 20.7 1.8 ± 0.4 0.5 ± 0.2 1.71
8 -0.1521 2243 ± 13 189 ± 11 161.9 ± 23.5 2.1 ± 0.4 1.0 ± 0.2 1.77
9 -0.1014 2210 ± 11 182 ± 10 83.5 ± 19.1 5.0 ± 1.2 2.8 ± 0.7 1.72
10 -0.0507 2194 ± 11 205 ± 10 91.9 ± 21.1 5.6 ± 1.4 2.4 ± 0.6 1.98
11 0.0000 2140 ± 18 290 ± 17 70.1 ± 25.7 8.2 ± 3.1 4.3 ± 1.7 1.71
12 0.0507 2184 ± 14 194 ± 12 68.1 ± 20.3 4.9 ± 1.5 3.6 ± 1.1 1.67
13 0.1014 2189 ± 15 147 ± 16 40.8 ± 16.1 5.0 ± 2.1 1.8 ± 0.9 1.58
14 0.1521 2156 ± 11 79 ± 11 41.0 ± 13.1 2.6 ± 1.0 1.3 ± 0.6 1.79
15 0.2028 2212 ± 15 84 ± 15 33.1 ± 13.8 2.2 ± 1.1 1.7 ± 0.9 1.86
Slit 2: X-Offset +0.1 ′′
1 -0.5071 2341 ± 18 116 ± 17 73.2 ± 20.6 1.6 ± 0.6 0.3 ± 0.3 1.74
2 -0.4564 2300 ± 17 135 ± 17 76.0 ± 20.4 2.1 ± 0.7 0.4 ± 0.3 1.54
3 -0.4057 2261 ± 17 131 ± 16 79.8 ± 20.2 2.0 ± 0.6 0.5 ± 0.3 1.44
4 -0.3550 2212 ± 22 214 ± 18 127.7 ± 25.1 2.1 ± 0.5 0.9 ± 0.3 1.61
5 -0.3043 2228 ± 20 163 ± 18 57.2 ± 19.1 3.1 ± 1.2 2.0 ± 0.8 1.83
6 -0.2535 2317 ± 15 110 ± 15 63.7 ± 18.3 1.7 ± 0.6 1.4 ± 0.5 1.52
7 -0.2028 2308 ± 15 83 ± 15 31.6 ± 14.8 2.7 ± 1.5 1.2 ± 0.8 1.54
8 -0.1521 2244 ± 22 167 ± 20 85.7 ± 21.9 1.9 ± 0.6 1.0 ± 0.4 1.52
9 -0.1014 2271 ± 12 144 ± 11 73.4 ± 17.9 3.3 ± 0.9 2.1 ± 0.6 1.59
10 -0.0507 2223 ± 9 125 ± 8 97.9 ± 18.0 2.8 ± 0.6 1.5 ± 0.4 1.33
11 0.0000 2243 ± 11 139 ± 11 93.6 ± 18.9 2.9 ± 0.7 1.3 ± 0.3 1.48
12 0.0507 2251 ± 9 103 ± 9 37.2 ± 16.5 6.0 ± 2.8 2.4 ± 1.2 1.94
13 0.1014 2199 ± 19 170 ± 18 26.7 ± 19.0 8.4 ± 6.1 3.6 ± 2.7 1.39
15 0.2028 1984 ± 49 251 ± 38 49.4 ± 21.9 3.1 ± 1.5 2.4 ± 1.2 1.63
16 0.2535 2091 ± 34 161 ± 31 66.0 ± 21.6 1.1 ± 0.5 1.0 ± 0.5 1.63
20 0.4564 2022 ± 24 90 ± 24 21.6 ± 14.0 2.3 ± 1.8 1.6 ± 1.3 1.60
104

Table 3.17. NGC 4335: Measured Parameters.
Row Y-Offset vr σgas F(Hα/10 −16 ) F([NII]6585) F([SII]total) R 2
( ′′ ) (km s −1 ) (km s −1 ) (erg s −1 cm −2 Hz −1 ) F(Hα) F(Hα)
Slit 1: X-Offset -0.2 ′′
1 -1.0142 4955 ± 12 94 ± 12 5.4 ± 1.6 2.3 ± 0.8 0.8 ± 0.5 2.80
3 -0.8114 4943 ± 7 92 ± 7 13.0 ± 1.9 1.8 ± 0.3 0.8 ± 0.3 2.81
4 -0.7099 4915 ± 9 107 ± 9 14.3 ± 2.2 1.7 ± 0.3 1.0 ± 0.3 2.37
5 -0.6085 4928 ± 7 84 ± 7 8.5 ± 1.9 2.9 ± 0.7 1.3 ± 0.5 2.29
6 -0.5071 4967 ± 6 83 ± 6 13.7 ± 2.2 2.0 ± 0.4 0.3 ± 0.2 2.15
7 -0.4057 4947 ± 5 85 ± 5 20.8 ± 2.6 1.7 ± 0.3 0.8 ± 0.2 1.84
8 -0.3043 4904 ± 8 111 ± 8 19.2 ± 3.1 2.2 ± 0.4 1.0 ± 0.3 2.20
9 -0.2028 4807 ± 10 160 ± 9 29.5 ± 4.0 2.3 ± 0.4 1.0 ± 0.3 2.43
10 -0.1014 4711 ± 7 174 ± 6 41.4 ± 4.4 2.8 ± 0.3 0.5 ± 0.2 2.06
11 0.0000 4639 ± 5 163 ± 5 45.9 ± 4.2 3.1 ± 0.3 0.9 ± 0.2 2.34
12 0.1014 4606 ± 6 158 ± 6 36.3 ± 3.9 3.0 ± 0.4 0.6 ± 0.2 2.14
13 0.2028 4540 ± 6 109 ± 6 15.5 ± 3.0 3.4 ± 0.7 0.4 ± 0.3 2.50
14 0.3043 4507 ± 6 83 ± 6 6.1 ± 2.3 5.4 ± 2.1 1.0 ± 0.7 3.17
16 0.5071 4471 ± 10 100 ± 10 8.3 ± 2.0 2.4 ± 0.7 0.7 ± 0.4 2.72
17 0.6085 4416 ± 29 227 ± 25 9.4 ± 2.9 2.4 ± 0.8 0.7 ± 0.5 2.99
18 0.7099 4476 ± 18 129 ± 18 9.0 ± 2.3 1.3 ± 0.4 1.0 ± 0.4 3.24
20 0.9128 4526 ± 17 97 ± 18 7.0 ± 2.1 1.0 ± 0.4 0.5 ± 0.4 3.04
21 1.0142 4531 ± 21 138 ± 22 6.3 ± 2.0 1.2 ± 0.5 1.7 ± 0.7 3.68
Slit 0: X-Offset 0.0 ′′
1 -1.0142 4940 ± 11 80 ± 11 9.7 ± 2.5 1.4 ± 0.5 0.8 ± 0.4 2.16
2 -0.9128 4928 ± 8 70 ± 8 7.0 ± 2.1 2.5 ± 0.9 1.5 ± 0.7 2.21
3 -0.8114 4912 ± 6 60 ± 6 15.7 ± 2.7 1.1 ± 0.2 1.0 ± 0.3 2.18
4 -0.7099 4910 ± 5 55 ± 5 17.8 ± 2.8 0.9 ± 0.2 0.8 ± 0.2 2.31
5 -0.6085 4906 ± 7 61 ± 7 17.0 ± 3.1 0.9 ± 0.2 0.9 ± 0.3 2.01
6 -0.5071 4890 ± 22 170 ± 21 12.9 ± 4.2 2.7 ± 1.0 1.7 ± 0.8 1.88
7 -0.4057 4865 ± 20 207 ± 19 12.8 ± 4.8 4.7 ± 1.9 1.7 ± 1.0 1.62
8 -0.3043 4800 ± 10 133 ± 10 27.1 ± 4.9 2.4 ± 0.5 1.1 ± 0.4 1.66
9 -0.2028 4749 ± 8 162 ± 7 42.6 ± 5.8 3.0 ± 0.5 1.7 ± 0.3 1.56
10 -0.1014 4683 ± 4 210 ± 3 155.9 ± 8.1 3.0 ± 0.2 1.3 ± 0.1 2.19
11 0.0000 4619 ± 3 248 ± 2 337.3 ± 10.3 2.6 ± 0.1 1.0 ± 0.1 3.21
12 0.1014 4568 ± 3 220 ± 3 206.9 ± 8.2 2.7 ± 0.1 1.0 ± 0.1 2.19
13 0.2028 4531 ± 5 134 ± 5 47.9 ± 5.2 3.3 ± 0.4 1.2 ± 0.2 1.72
14 0.3043 4493 ± 8 131 ± 8 28.0 ± 4.7 2.7 ± 0.5 1.1 ± 0.3 1.98
15 0.4057 4376 ± 17 168 ± 17 22.7 ± 5.1 2.0 ± 0.5 0.6 ± 0.3 2.11
16 0.5071 4372 ± 22 175 ± 21 18.7 ± 4.7 2.0 ± 0.6 0.8 ± 0.4 2.39
17 0.6085 4406 ± 17 148 ± 17 17.0 ± 4.0 1.9 ± 0.5 1.1 ± 0.4 2.28
18 0.7099 4383 ± 13 123 ± 14 12.2 ± 3.2 2.2 ± 0.7 1.6 ± 0.6 2.16
19 0.8114 4438 ± 23 159 ± 23 8.8 ± 3.2 2.5 ± 1.1 1.6 ± 0.8 2.54
Slit 2: X-Offset +0.2 ′′
1 -1.0142 4683 ± 53 259 ± 49 5.1 ± 3.6 3.2 ± 2.4 3.5 ± 2.8 2.72
4 -0.7099 4883 ± 14 67 ± 14 6.0 ± 2.3 1.5 ± 0.7 0.3 ± 0.5 2.69
5 -0.6085 4767 ± 14 103 ± 15 9.7 ± 2.9 1.9 ± 0.7 1.1 ± 0.6 2.17
7 -0.4057 4725 ± 13 114 ± 12 16.2 ± 4.0 1.8 ± 0.5 0.7 ± 0.4 1.95
8 -0.3043 4713 ± 13 109 ± 12 13.5 ± 3.7 2.2 ± 0.7 1.1 ± 0.5 1.74
9 -0.2028 4673 ± 8 82 ± 8 8.4 ± 3.2 4.4 ± 1.8 1.5 ± 0.9 1.72
10 -0.1014 4654 ± 5 76 ± 5 11.8 ± 3.0 4.3 ± 1.2 1.9 ± 0.7 1.95
11 0.0000 4605 ± 5 83 ± 5 12.2 ± 3.2 4.8 ± 1.3 1.4 ± 0.6 1.74
12 0.1014 4550 ± 5 94 ± 6 13.7 ± 3.4 5.0 ± 1.3 1.4 ± 0.6 1.94
13 0.2028 4509 ± 6 115 ± 6 22.4 ± 3.7 3.7 ± 0.7 0.9 ± 0.3 1.70
14 0.3043 4504 ± 11 145 ± 10 12.6 ± 3.7 4.8 ± 1.5 1.6 ± 0.7 1.85
15 0.4057 4481 ± 19 158 ± 18 13.8 ± 3.9 2.4 ± 0.8 0.8 ± 0.5 1.75
16 0.5071 4329 ± 6 54 ± 6 14.9 ± 2.9 1.0 ± 0.3 0.4 ± 0.2 1.68
17 0.6085 4325 ± 7 58 ± 7 12.0 ± 3.1 1.2 ± 0.4 0.4 ± 0.3 2.24
18 0.7099 4352 ± 14 128 ± 14 5.8 ± 2.6 4.6 ± 2.2 3.4 ± 1.8 2.51
19 0.8114 4345 ± 10 78 ± 10 5.3 ± 2.1 2.9 ± 1.3 1.7 ± 1.0 2.20
21 1.0142 4476 ± 34 152 ± 34 4.3 ± 2.7 2.7 ± 1.9 0.9 ± 1.1 3.22
105

Table 3.18. M84 : Measured Parameters.
Row Y-Offset vr σgas F(Hα/10 −16 ) F([NII]6585) F([SII]total) R 2
( ′′ ) (km s −1 ) (km s −1 ) (erg s −1 cm −2 Hz −1 ) F(Hα) F(Hα)
Slit 1: X-Offset -0.2 ′′
1 -0.5071 1088 ± 7 89 ± 8 19.3 ± 3.2 1.9 ± 0.4 0.9 ± 0.3 1.33
2 -0.4564 1071 ± 6 88 ± 6 14.4 ± 2.8 3.2 ± 0.7 1.6 ± 0.4 1.28
3 -0.4057 1064 ± 7 95 ± 7 21.7 ± 3.3 2.2 ± 0.4 1.0 ± 0.2 1.36
4 -0.3550 1061 ± 6 101 ± 6 31.6 ± 3.6 1.9 ± 0.3 1.1 ± 0.2 1.22
5 -0.3043 1068 ± 5 118 ± 5 45.4 ± 4.0 1.9 ± 0.2 0.9 ± 0.1 1.34
6 -0.2535 1106 ± 4 126 ± 4 53.1 ± 3.9 2.5 ± 0.2 1.2 ± 0.1 1.39
7 -0.2028 1102 ± 3 115 ± 3 67.7 ± 4.0 2.2 ± 0.2 1.1 ± 0.1 1.42
8 -0.1521 1102 ± 2 102 ± 2 65.0 ± 3.6 2.3 ± 0.2 1.5 ± 0.1 1.54
9 -0.1014 1099 ± 2 124 ± 2 79.8 ± 3.9 2.5 ± 0.1 1.6 ± 0.1 1.50
10 -0.0507 1076 ± 2 137 ± 2 104.9 ± 4.1 2.7 ± 0.1 1.8 ± 0.1 1.65
11 0.0000 1026 ± 2 178 ± 2 150.0 ± 4.9 2.5 ± 0.1 1.8 ± 0.1 1.58
12 0.0507 944 ± 2 197 ± 2 168.1 ± 5.2 2.5 ± 0.1 1.8 ± 0.1 1.61
13 0.1014 878 ± 2 190 ± 2 153.1 ± 5.1 2.7 ± 0.1 1.7 ± 0.1 1.33
14 0.1521 856 ± 3 200 ± 2 131.4 ± 5.0 2.8 ± 0.1 1.8 ± 0.1 1.24
15 0.2028 865 ± 3 184 ± 2 113.5 ± 4.9 2.8 ± 0.1 1.8 ± 0.1 1.23
16 0.2535 855 ± 4 175 ± 3 87.5 ± 4.7 2.5 ± 0.2 1.8 ± 0.1 1.31
17 0.3043 839 ± 5 158 ± 4 56.8 ± 4.3 2.6 ± 0.2 1.9 ± 0.2 1.42
18 0.3550 846 ± 5 141 ± 5 46.2 ± 4.0 2.4 ± 0.2 1.6 ± 0.2 1.33
19 0.4057 881 ± 6 160 ± 6 43.3 ± 4.1 2.5 ± 0.3 1.6 ± 0.2 1.24
20 0.4564 900 ± 6 143 ± 6 33.0 ± 3.8 3.0 ± 0.4 2.0 ± 0.3 1.34
21 0.5071 913 ± 5 126 ± 5 27.0 ± 3.5 3.2 ± 0.5 2.3 ± 0.4 1.26
Slit 0: X-Offset 0.0 ′′
1 -0.5071 1148 ± 7 118 ± 7 31.6 ± 3.7 1.4 ± 0.2 1.2 ± 0.2 1.30
2 -0.4564 1156 ± 7 148 ± 7 28.0 ± 3.5 2.3 ± 0.3 1.9 ± 0.3 1.30
3 -0.4057 1202 ± 5 140 ± 5 32.9 ± 3.4 2.4 ± 0.3 1.6 ± 0.2 1.47
4 -0.3550 1224 ± 4 138 ± 4 46.1 ± 3.6 2.1 ± 0.2 1.4 ± 0.1 1.40
5 -0.3043 1238 ± 4 156 ± 3 60.6 ± 3.9 2.3 ± 0.2 1.6 ± 0.1 1.33
6 -0.2535 1269 ± 3 173 ± 3 86.3 ± 4.1 2.3 ± 0.1 1.5 ± 0.1 1.45
7 -0.2028 1322 ± 3 192 ± 2 115.7 ± 4.4 2.6 ± 0.1 1.8 ± 0.1 1.58
8 -0.1521 1376 ± 2 224 ± 2 190.2 ± 5.2 2.7 ± 0.1 1.9 ± 0.1 1.78
9 -0.1014 1420 ± 2 305 ± 2 380.0 ± 8.1 2.6 ± 0.1 1.6 ± 0.0 2.35
10 -0.0507 1383 ± 4 483 ± 3 633.2 ± 20.0 3.2 ± 0.1 1.7 ± 0.1 3.95
11 0.0000 1107 ± 11 883 ± 5 761.1 ± 81.3 4.8 ± 0.5 2.4 ± 0.3 5.07
12 0.0507 751 ± 10 779 ± 5 402.9 ± 60.4 7.3 ± 1.1 3.9 ± 0.6 4.03
13 0.1014 754 ± 4 415 ± 4 377.8 ± 14.0 3.0 ± 0.1 1.9 ± 0.1 2.33
14 0.1521 786 ± 5 319 ± 4 175.4 ± 7.8 2.9 ± 0.1 1.9 ± 0.1 2.12
15 0.2028 869 ± 6 258 ± 5 106.9 ± 6.0 2.4 ± 0.2 1.4 ± 0.1 1.67
16 0.2535 934 ± 5 188 ± 4 74.5 ± 4.9 2.1 ± 0.2 1.2 ± 0.1 1.30
17 0.3043 963 ± 4 141 ± 4 58.2 ± 4.3 1.9 ± 0.2 1.1 ± 0.1 1.36
18 0.3550 979 ± 3 105 ± 3 37.1 ± 3.5 2.4 ± 0.3 1.3 ± 0.2 1.37
19 0.4057 975 ± 4 101 ± 3 40.0 ± 3.6 2.0 ± 0.2 1.0 ± 0.1 1.37
20 0.4564 960 ± 3 94 ± 3 36.8 ± 3.4 2.0 ± 0.2 1.2 ± 0.2 1.28
21 0.5071 958 ± 3 83 ± 3 33.6 ± 3.3 2.0 ± 0.2 1.2 ± 0.2 1.56
Slit 2: X-Offset +0.2 ′′
1 -0.5071 1266 ± 6 122 ± 5 38.3 ± 3.7 1.6 ± 0.2 1.2 ± 0.2 1.27
2 -0.4564 1261 ± 5 126 ± 5 34.4 ± 3.5 2.1 ± 0.3 1.4 ± 0.2 1.30
3 -0.4057 1249 ± 5 138 ± 5 34.1 ± 3.5 2.7 ± 0.3 1.3 ± 0.2 1.30
4 -0.3550 1256 ± 5 150 ± 4 34.5 ± 3.6 3.3 ± 0.4 2.2 ± 0.3 1.33
5 -0.3043 1251 ± 4 169 ± 4 49.4 ± 3.9 3.1 ± 0.3 2.0 ± 0.2 1.40
6 -0.2535 1276 ± 4 170 ± 4 61.0 ± 4.1 2.8 ± 0.2 1.6 ± 0.1 1.49
7 -0.2028 1266 ± 3 162 ± 3 71.6 ± 4.2 2.5 ± 0.2 1.4 ± 0.1 1.41
8 -0.1521 1239 ± 3 150 ± 3 79.4 ± 4.3 2.3 ± 0.1 1.3 ± 0.1 1.31
9 -0.1014 1208 ± 3 147 ± 3 71.4 ± 4.4 2.2 ± 0.2 1.4 ± 0.1 1.41
10 -0.0507 1159 ± 4 163 ± 3 59.6 ± 4.6 2.7 ± 0.2 1.7 ± 0.2 1.39
11 0.0000 1126 ± 3 140 ± 3 71.3 ± 4.3 2.1 ± 0.1 1.4 ± 0.1 1.42
12 0.0507 1105 ± 3 136 ± 3 63.5 ± 4.1 2.1 ± 0.2 1.5 ± 0.1 1.28
13 0.1014 1086 ± 4 140 ± 4 54.8 ± 4.1 2.2 ± 0.2 1.1 ± 0.1 1.27
14 0.1521 1060 ± 4 118 ± 4 46.0 ± 3.8 2.1 ± 0.2 1.2 ± 0.1 1.32
15 0.2028 1035 ± 4 111 ± 4 36.1 ± 3.7 2.2 ± 0.3 1.4 ± 0.2 1.22
16 0.2535 1039 ± 4 102 ± 4 41.1 ± 3.7 1.8 ± 0.2 1.1 ± 0.2 1.40
17 0.3043 1006 ± 4 97 ± 4 45.0 ± 4.1 1.5 ± 0.2 0.7 ± 0.1 1.55
18 0.3550 986 ± 4 96 ± 4 34.2 ± 3.9 1.9 ± 0.3 0.9 ± 0.2 1.36
19 0.4057 980 ± 4 90 ± 4 36.8 ± 4.0 1.4 ± 0.2 0.7 ± 0.1 1.27
20 0.4564 983 ± 4 74 ± 3 36.5 ± 3.7 1.2 ± 0.2 0.7 ± 0.1 1.28
21 0.5071 998 ± 5 90 ± 5 30.3 ± 3.7 1.5 ± 0.2 0.8 ± 0.2 1.28
106

Table 3.19. NGC 4486: Measured Parameters.
Row Y-Offset vr σgas F(Hα/10 −16 ) F([NII]6585) F([SII]total) R 2
( ′′ ) (km s −1 ) (km s −1 ) (erg s −1 cm −2 Hz −1 ) F(Hα) F(Hα)
Slit 1: X-Offset -0.2 ′′
1 -0.5071 1535 ± 14 374 ± 12 113.0 ± 17.5 3.9 ± 0.6 2.4 ± 0.4 1.93
2 -0.4564 1634 ± 12 376 ± 10 252.0 ± 19.7 2.0 ± 0.2 1.4 ± 0.1 2.10
3 -0.4057 1775 ± 5 266 ± 4 353.6 ± 14.4 1.7 ± 0.1 1.3 ± 0.1 2.18
4 -0.3550 1765 ± 4 256 ± 3 352.3 ± 14.1 2.0 ± 0.1 1.4 ± 0.1 1.89
5 -0.3043 1755 ± 5 274 ± 4 332.3 ± 14.4 2.2 ± 0.1 1.5 ± 0.1 1.90
6 -0.2535 1788 ± 3 274 ± 2 477.4 ± 15.6 2.5 ± 0.1 1.6 ± 0.1 2.33
7 -0.2028 1850 ± 2 235 ± 1 794.4 ± 16.2 2.4 ± 0.1 1.5 ± 0.0 2.68
8 -0.1521 1842 ± 1 206 ± 1 1109.7 ± 17.9 2.4 ± 0.0 1.5 ± 0.0 2.81
9 -0.1014 1814 ± 1 191 ± 0 1301.5 ± 18.2 2.3 ± 0.0 1.3 ± 0.0 3.34
10 -0.0507 1789 ± 1 191 ± 1 1101.6 ± 17.5 2.2 ± 0.0 1.2 ± 0.0 3.37
11 0.0000 1720 ± 1 211 ± 1 894.9 ± 17.9 2.0 ± 0.0 1.1 ± 0.0 2.53
12 0.0507 1587 ± 2 251 ± 2 744.3 ± 19.3 1.9 ± 0.1 1.0 ± 0.0 2.89
13 0.1014 1411 ± 3 304 ± 3 611.7 ± 19.7 2.4 ± 0.1 1.3 ± 0.1 2.98
14 0.1521 1287 ± 4 308 ± 3 536.7 ± 18.8 2.6 ± 0.1 1.6 ± 0.1 2.42
15 0.2028 1195 ± 3 259 ± 2 450.5 ± 15.5 2.6 ± 0.1 1.7 ± 0.1 1.83
16 0.2535 1115 ± 2 197 ± 2 423.7 ± 12.7 2.4 ± 0.1 1.6 ± 0.1 2.20
17 0.3043 1106 ± 2 180 ± 2 311.2 ± 11.1 2.7 ± 0.1 1.8 ± 0.1 1.84
18 0.3550 1120 ± 2 171 ± 2 257.4 ± 10.6 2.5 ± 0.1 1.6 ± 0.1 1.69
19 0.4057 1115 ± 3 149 ± 2 193.4 ± 9.6 2.3 ± 0.1 1.6 ± 0.1 1.87
20 0.4564 1115 ± 3 145 ± 3 139.1 ± 8.8 2.4 ± 0.2 1.8 ± 0.1 1.81
21 0.5071 1112 ± 5 166 ± 5 93.9 ± 8.8 3.2 ± 0.3 1.9 ± 0.2 1.84
Slit 0: X-Offset 0.0 ′′
1 -0.5071 1451 ± 7 212 ± 6 189.2 ± 14.2 1.8 ± 0.2 1.3 ± 0.1 1.64
2 -0.4564 1469 ± 4 191 ± 4 200.7 ± 13.1 2.4 ± 0.2 1.8 ± 0.1 1.72
3 -0.4057 1497 ± 3 197 ± 2 406.8 ± 15.6 2.1 ± 0.1 1.5 ± 0.1 2.01
4 -0.3550 1521 ± 2 201 ± 2 582.5 ± 17.4 1.9 ± 0.1 1.3 ± 0.0 1.97
5 -0.3043 1532 ± 2 205 ± 2 655.5 ± 17.7 2.1 ± 0.1 1.3 ± 0.0 2.11
6 -0.2535 1526 ± 2 217 ± 1 802.6 ± 19.7 2.1 ± 0.1 1.2 ± 0.0 2.53
7 -0.2028 1548 ± 2 253 ± 2 883.2 ± 22.4 2.2 ± 0.1 1.2 ± 0.0 2.63
8 -0.1521 1525 ± 3 301 ± 2 1378.4 ± 30.7 2.1 ± 0.1 1.0 ± 0.0 3.91
9 -0.1014 1378 ± 3 422 ± 3 2160.2 ± 48.2 2.2 ± 0.1 1.1 ± 0.0 3.38
10 -0.0507 1128 ± 7 681 ± 5 1781.4 ± 108.3 4.3 ± 0.3 1.5 ± 0.1 3.29
11 0.0000 1109 ± 6 612 ± 6 3500.2 ± 102.1 1.8 ± 0.1 0.8 ± 0.0 7.08
12 0.0507 1142 ± 18 920 ± 10 4026.6 ± 258.4 1.2 ± 0.1 0.4 ± 0.0 7.24
13 0.1014 940 ± 8 628 ± 7 1372.2 ± 58.2 2.3 ± 0.1 0.7 ± 0.0 3.91
14 0.1521 948 ± 6 395 ± 5 697.2 ± 26.5 2.5 ± 0.1 1.2 ± 0.1 1.98
15 0.2028 1003 ± 4 277 ± 3 558.2 ± 17.6 2.6 ± 0.1 1.6 ± 0.1 2.13
16 0.2535 1020 ± 2 218 ± 2 622.5 ± 15.2 2.3 ± 0.1 1.5 ± 0.0 2.13
17 0.3043 1007 ± 2 206 ± 2 536.8 ± 13.7 2.3 ± 0.1 1.5 ± 0.0 2.07
18 0.3550 1000 ± 3 193 ± 2 364.7 ± 11.9 2.3 ± 0.1 1.5 ± 0.1 1.95
19 0.4057 1018 ± 4 190 ± 3 266.5 ± 11.5 2.3 ± 0.1 1.4 ± 0.1 1.70
20 0.4564 1047 ± 3 183 ± 3 258.4 ± 11.1 2.2 ± 0.1 1.3 ± 0.1 1.66
21 0.5071 1073 ± 3 156 ± 3 207.0 ± 10.4 2.4 ± 0.1 1.5 ± 0.1 1.47
Slit 2: X-Offset +0.2 ′′
1 -0.5071 1083 ± 10 225 ± 8 143.0 ± 12.0 1.7 ± 0.2 1.2 ± 0.1 1.84
2 -0.4564 1088 ± 9 236 ± 7 132.8 ± 12.0 2.3 ± 0.2 1.4 ± 0.2 1.90
3 -0.4057 1089 ± 8 234 ± 6 158.2 ± 12.2 2.1 ± 0.2 1.5 ± 0.1 1.75
4 -0.3550 1053 ± 8 254 ± 7 152.5 ± 12.1 2.4 ± 0.2 1.7 ± 0.2 1.82
5 -0.3043 1019 ± 9 275 ± 8 165.4 ± 12.9 2.5 ± 0.2 1.6 ± 0.2 2.15
6 -0.2535 1008 ± 11 309 ± 9 197.4 ± 15.1 2.4 ± 0.2 1.5 ± 0.2 2.03
7 -0.2028 1026 ± 12 350 ± 10 209.9 ± 17.3 2.5 ± 0.2 1.7 ± 0.2 1.85
8 -0.1521 1029 ± 12 367 ± 10 216.5 ± 18.4 2.8 ± 0.3 1.7 ± 0.2 2.05
9 -0.1014 1038 ± 11 368 ± 9 261.9 ± 19.6 2.5 ± 0.2 1.7 ± 0.2 2.39
10 -0.0507 1038 ± 10 380 ± 8 344.8 ± 21.0 2.3 ± 0.2 1.5 ± 0.1 2.10
11 0.0000 992 ± 10 407 ± 8 364.2 ± 22.6 2.5 ± 0.2 1.6 ± 0.1 2.25
12 0.0507 922 ± 9 395 ± 8 404.9 ± 21.9 2.5 ± 0.2 1.6 ± 0.1 2.23
13 0.1014 869 ± 5 329 ± 5 434.7 ± 18.0 2.8 ± 0.1 1.6 ± 0.1 2.39
14 0.1521 852 ± 4 286 ± 3 499.4 ± 16.4 2.6 ± 0.1 1.4 ± 0.1 2.26
15 0.2028 843 ± 3 239 ± 2 555.4 ± 14.7 2.3 ± 0.1 1.3 ± 0.0 2.16
16 0.2535 864 ± 3 239 ± 2 520.7 ± 14.1 2.1 ± 0.1 1.3 ± 0.0 2.23
17 0.3043 890 ± 3 231 ± 2 483.9 ± 13.5 2.1 ± 0.1 1.4 ± 0.1 2.22
18 0.3550 893 ± 3 213 ± 2 440.6 ± 12.6 2.1 ± 0.1 1.3 ± 0.1 1.87
19 0.4057 880 ± 3 199 ± 2 364.4 ± 11.5 2.3 ± 0.1 1.4 ± 0.1 1.97
20 0.4564 907 ± 3 199 ± 2 322.5 ± 11.1 2.1 ± 0.1 1.4 ± 0.1 1.79
21 0.5071 940 ± 4 203 ± 3 296.1 ± 11.0 2.2 ± 0.1 1.5 ± 0.1 1.79
107

Table 3.20. NGC 5127: Measured Parameters.
Row Y-Offset vr σgas F(Hα/10 −16 ) F([NII]6585) F([SII]total) R 2
( ′′ ) (km s −1 ) (km s −1 ) (erg s −1 cm −2 Hz −1 ) F(Hα) F(Hα)
Slit 1: X-Offset -0.2 ′′
5 -0.6085 4931 ± 17 52 ± 17 4.4 ± 2.3 0.4 ± 0.5 1.3 ± 0.9 3.61
8 -0.3043 4851 ± 10 125 ± 10 11.4 ± 2.8 2.5 ± 0.7 2.7 ± 0.7 3.72
9 -0.2028 4873 ± 9 91 ± 9 5.4 ± 2.2 4.3 ± 1.9 3.5 ± 1.5 3.01
10 -0.1014 4799 ± 8 61 ± 8 6.7 ± 2.1 1.5 ± 0.6 1.8 ± 0.7 3.31
11 0.0000 4919 ± 22 125 ± 22 7.6 ± 2.9 1.8 ± 0.8 1.2 ± 0.6 2.99
12 0.1014 4711 ± 27 161 ± 26 11.1 ± 3.5 1.4 ± 0.6 1.0 ± 0.4 3.59
13 0.2028 4705 ± 10 68 ± 10 9.6 ± 2.5 0.6 ± 0.3 1.4 ± 0.5 3.65
14 0.3043 4663 ± 36 219 ± 31 14.0 ± 4.1 1.0 ± 0.4 1.3 ± 0.5 3.24
17 0.6085 4685 ± 12 75 ± 13 5.9 ± 2.3 2.2 ± 1.0 1.2 ± 0.6 3.17
20 0.9128 4305 ± 12 61 ± 11 8.0 ± 2.4 0.7 ± 0.3 0.7 ± 0.3 3.25
21 1.0142 4360 ± 9 67 ± 9 18.7 ± 4.2 0.0 ± 0.1 0.4 ± 0.1 3.50
Slit 0: X-Offset 0.0 ′′
4 -0.7099 5010 ± 29 97 ± 29 9.7 ± 4.8 1.3 ± 0.8 0.4 ± 0.4 2.02
7 -0.4057 4879 ± 13 174 ± 12 24.8 ± 5.3 2.9 ± 0.7 2.1 ± 0.5 2.07
8 -0.3043 4902 ± 5 157 ± 5 46.6 ± 5.7 4.3 ± 0.6 2.2 ± 0.3 2.01
9 -0.2028 4861 ± 10 173 ± 8 33.1 ± 5.7 3.5 ± 0.7 2.3 ± 0.5 2.15
10 -0.1014 4810 ± 9 95 ± 9 14.4 ± 4.2 3.0 ± 1.0 2.1 ± 0.7 1.96
11 0.0000 4769 ± 8 52 ± 8 10.7 ± 3.5 1.9 ± 0.8 1.1 ± 0.5 1.97
12 0.1014 4747 ± 6 36 ± 7 13.2 ± 4.0 1.0 ± 0.4 0.5 ± 0.3 1.99
13 0.2028 4799 ± 17 83 ± 16 11.6 ± 4.5 0.2 ± 0.3 1.4 ± 0.7 1.92
18 0.7099 4606 ± 34 162 ± 33 8.5 ± 4.6 2.9 ± 1.8 1.1 ± 0.9 1.94
21 1.0142 4422 ± 45 166 ± 41 8.0 ± 4.8 1.8 ± 1.3 1.7 ± 1.2 2.29
Slit 2: X-Offset +0.2 ′′
1 -1.0142 4826 ± 20 19 ± 9 5.3 ± 2.8 0.0 ± 0.2 0.2 ± 0.2 2.64
4 -0.7099 4984 ± 9 56 ± 9 4.9 ± 2.1 2.6 ± 1.3 1.7 ± 0.9 2.37
6 -0.5071 4983 ± 9 72 ± 9 6.9 ± 2.5 3.3 ± 1.4 1.0 ± 0.6 2.41
7 -0.4057 4978 ± 10 86 ± 10 12.1 ± 3.1 2.2 ± 0.7 1.0 ± 0.4 2.36
8 -0.3043 4929 ± 10 90 ± 9 15.9 ± 3.5 1.9 ± 0.5 0.7 ± 0.3 2.24
9 -0.2028 4899 ± 10 76 ± 9 10.1 ± 2.9 2.2 ± 0.8 1.5 ± 0.6 1.91
10 -0.1014 4865 ± 11 77 ± 11 7.5 ± 2.6 1.6 ± 0.8 2.9 ± 1.1 2.53
11 0.0000 4924 ± 32 143 ± 30 10.0 ± 4.1 1.7 ± 0.9 0.7 ± 0.5 2.49
12 0.1014 4918 ± 19 119 ± 19 5.3 ± 3.2 4.8 ± 3.1 0.4 ± 0.6 2.52
13 0.2028 4882 ± 15 88 ± 14 4.6 ± 2.8 4.2 ± 2.7 1.9 ± 1.3 2.50
14 0.3043 4861 ± 14 70 ± 13 4.1 ± 2.5 2.2 ± 1.5 2.4 ± 1.6 2.43
18 0.7099 5121 ± 41 132 ± 39 13.3 ± 5.4 0.1 ± 0.2 0.0 ± 0.2 2.47
19 0.8114 4800 ± 14 68 ± 14 3.0 ± 2.2 1.7 ± 1.4 3.6 ± 2.9 2.91
108

Table 3.21. NGC 5141: Measured Parameters.
Row Y-Offset vr σgas F(Hα/10 −16 ) F([NII]6585) F([SII]total) R 2
( ′′ ) (km s −1 ) (km s −1 ) (erg s −1 cm −2 Hz −1 ) F(Hα) F(Hα)
Slit 1: X-Offset -0.2 ′′
1 -1.0142 5498 ± 15 128 ± 15 6.0 ± 2.4 3.9 ± 1.7 1.4 ± 0.9 2.78
4 -0.7099 5335 ± 26 160 ± 25 5.2 ± 2.6 4.2 ± 2.3 0.5 ± 0.9 2.97
5 -0.6085 5494 ± 10 87 ± 10 8.9 ± 2.3 2.3 ± 0.7 0.8 ± 0.4 2.27
6 -0.5071 5389 ± 20 179 ± 18 7.1 ± 2.8 5.3 ± 2.2 0.7 ± 0.8 2.26
7 -0.4057 5456 ± 23 198 ± 21 10.8 ± 3.3 3.4 ± 1.2 0.6 ± 0.6 2.35
8 -0.3043 5383 ± 12 158 ± 11 12.6 ± 3.0 4.1 ± 1.1 2.1 ± 0.7 2.67
9 -0.2028 5295 ± 7 141 ± 7 25.5 ± 3.3 3.0 ± 0.5 2.3 ± 0.4 2.21
10 -0.1014 5265 ± 3 131 ± 3 50.9 ± 3.6 3.2 ± 0.3 1.5 ± 0.2 2.35
11 0.0000 5282 ± 2 107 ± 2 66.4 ± 3.6 2.9 ± 0.2 1.2 ± 0.1 2.43
12 0.1014 5243 ± 3 105 ± 3 50.2 ± 3.3 2.6 ± 0.2 0.8 ± 0.1 2.66
13 0.2028 5169 ± 2 62 ± 2 22.3 ± 2.5 3.4 ± 0.4 0.7 ± 0.2 2.44
14 0.3043 5123 ± 15 120 ± 15 9.6 ± 2.8 2.8 ± 1.0 0.7 ± 0.5 1.97
15 0.4057 5134 ± 13 80 ± 13 3.5 ± 2.0 4.6 ± 2.8 1.2 ± 1.2 2.10
16 0.5071 5058 ± 22 138 ± 22 18.1 ± 4.1 0.6 ± 0.2 0.5 ± 0.3 2.10
17 0.6085 4932 ± 57 275 ± 42 16.8 ± 4.7 1.4 ± 0.5 0.3 ± 0.4 2.36
18 0.7099 5032 ± 17 96 ± 17 3.1 ± 2.1 5.0 ± 3.7 0.6 ± 1.1 2.15
Slit 0: X-Offset 0.0 ′′
1 -1.0142 5440 ± 26 103 ± 27 6.4 ± 3.2 2.1 ± 1.3 0.8 ± 0.9 2.24
3 -0.8114 5401 ± 15 94 ± 15 8.9 ± 3.1 2.4 ± 1.0 0.5 ± 0.6 2.03
5 -0.6085 5408 ± 14 117 ± 14 6.6 ± 3.0 5.5 ± 2.7 0.6 ± 0.8 2.20
6 -0.5071 5486 ± 20 107 ± 19 12.5 ± 3.8 1.6 ± 0.6 0.4 ± 0.4 2.05
7 -0.4057 5435 ± 17 148 ± 16 20.1 ± 4.3 1.9 ± 0.5 1.3 ± 0.4 1.77
8 -0.3043 5384 ± 13 183 ± 12 22.8 ± 4.6 3.4 ± 0.8 1.6 ± 0.5 1.80
9 -0.2028 5330 ± 5 165 ± 5 73.6 ± 5.2 2.4 ± 0.2 1.2 ± 0.1 1.99
10 -0.1014 5296 ± 3 186 ± 2 191.1 ± 6.8 2.6 ± 0.1 1.1 ± 0.1 2.53
11 0.0000 5228 ± 3 148 ± 3 140.1 ± 6.4 2.4 ± 0.1 0.9 ± 0.1 2.39
12 0.1014 5189 ± 3 106 ± 3 56.4 ± 4.8 3.3 ± 0.3 0.8 ± 0.1 1.71
13 0.2028 5134 ± 7 121 ± 7 30.9 ± 4.3 2.9 ± 0.5 0.6 ± 0.2 1.65
14 0.3043 5088 ± 17 132 ± 16 28.2 ± 5.5 1.0 ± 0.3 0.7 ± 0.3 1.84
15 0.4057 5103 ± 13 112 ± 13 23.5 ± 4.5 1.2 ± 0.3 0.5 ± 0.3 1.81
16 0.5071 4978 ± 50 263 ± 39 22.4 ± 6.3 1.4 ± 0.5 1.0 ± 0.5 2.19
17 0.6085 5344 ± 51 256 ± 41 14.0 ± 5.6 2.3 ± 1.0 1.2 ± 0.8 1.84
18 0.7099 5336 ± 36 213 ± 32 9.4 ± 4.8 3.6 ± 2.0 0.4 ± 0.7 2.21
Slit 2: X-Offset +0.2 ′′
3 -0.8114 5462 ± 15 62 ± 15 6.3 ± 2.6 1.6 ± 0.8 0.3 ± 0.6 2.46
4 -0.7099 5523 ± 17 95 ± 17 15.0 ± 4.0 0.8 ± 0.3 0.2 ± 0.3 2.44
6 -0.5071 5326 ± 22 136 ± 21 4.5 ± 3.1 6.8 ± 4.9 1.1 ± 1.4 1.85
7 -0.4057 5389 ± 16 112 ± 16 9.2 ± 3.2 3.0 ± 1.2 1.7 ± 0.9 2.04
8 -0.3043 5334 ± 15 100 ± 16 16.0 ± 4.0 1.1 ± 0.4 0.7 ± 0.4 2.22
9 -0.2028 5312 ± 7 115 ± 7 35.9 ± 4.1 1.8 ± 0.3 0.7 ± 0.2 1.81
10 -0.1014 5252 ± 4 122 ± 4 52.1 ± 4.1 2.5 ± 0.2 1.2 ± 0.2 2.06
11 0.0000 5215 ± 5 128 ± 5 53.9 ± 4.6 2.0 ± 0.2 0.8 ± 0.1 2.07
12 0.1014 5162 ± 6 112 ± 6 29.2 ± 3.8 2.5 ± 0.4 0.8 ± 0.2 1.98
13 0.2028 5110 ± 9 95 ± 9 14.2 ± 3.0 2.3 ± 0.6 0.8 ± 0.4 1.72
14 0.3043 5032 ± 14 141 ± 13 22.5 ± 4.0 1.6 ± 0.4 0.7 ± 0.3 2.47
15 0.4057 5062 ± 9 89 ± 8 18.1 ± 3.2 1.6 ± 0.4 0.6 ± 0.2 2.36
16 0.5071 5023 ± 19 113 ± 19 13.7 ± 3.7 1.0 ± 0.4 1.0 ± 0.5 2.15
19 0.8114 4973 ± 8 45 ± 8 9.2 ± 2.5 0.8 ± 0.3 0.1 ± 0.3 2.24
21 1.0142 5510 ± 15 42 ± 15 5.5 ± 2.8 0.1 ± 0.3 0.3 ± 0.4 2.74
109

Table 3.22. NGC 5490: Measured Parameters.
Row Y-Offset vr σgas F(Hα/10 −16 ) F([NII]6585) F([SII]total) R 2
( ′′ ) (km s −1 ) (km s −1 ) (erg s −1 cm −2 Hz −1 ) F(Hα) F(Hα)
Slit 1: X-Offset -0.2 ′′
3 -0.8114 5164 ± 33 76 ± 33 5.8 ± 3.5 0.5 ± 0.5 0.3 ± 0.6 2.42
5 -0.6085 5104 ± 7 33 ± 10 9.8 ± 4.1 0.1 ± 0.2 0.6 ± 0.4 2.05
10 -0.1014 5008 ± 16 162 ± 15 16.1 ± 4.4 3.4 ± 1.0 0.8 ± 0.5 2.02
11 0.0000 4999 ± 10 205 ± 9 41.3 ± 5.4 3.3 ± 0.5 0.8 ± 0.2 2.29
12 0.1014 5154 ± 11 261 ± 9 79.9 ± 7.0 2.6 ± 0.3 1.0 ± 0.2 2.29
13 0.2028 5220 ± 9 160 ± 8 29.9 ± 4.4 3.6 ± 0.6 1.5 ± 0.3 1.94
14 0.3043 5204 ± 18 145 ± 18 24.3 ± 5.3 1.3 ± 0.4 0.8 ± 0.3 2.00
16 0.5071 5213 ± 17 63 ± 17 7.9 ± 3.3 1.0 ± 0.6 0.5 ± 0.5 2.07
19 0.8114 5154 ± 17 77 ± 16 11.0 ± 3.4 0.9 ± 0.4 0.2 ± 0.3 2.45
20 0.9128 5002 ± 48 192 ± 39 7.4 ± 3.6 2.4 ± 1.4 1.0 ± 0.9 2.51
Slit 0: X-Offset 0.0 ′′
2 -0.9128 5214 ± 10 34 ± 9 7.0 ± 3.6 0.0 ± 0.2 1.0 ± 0.7 2.21
3 -0.8114 5073 ± 8 39 ± 8 11.4 ± 3.4 0.1 ± 0.2 0.2 ± 0.2 2.37
6 -0.5071 5317 ± 9 38 ± 9 10.6 ± 3.6 0.2 ± 0.2 0.5 ± 0.4 2.20
7 -0.4057 5537 ± 28 115 ± 28 22.9 ± 8.2 0.3 ± 0.2 0.2 ± 0.3 1.79
10 -0.1014 4701 ± 11 280 ± 9 74.4 ± 7.4 3.4 ± 0.4 1.3 ± 0.2 2.24
13 0.2028 5058 ± 16 199 ± 14 40.2 ± 6.6 2.3 ± 0.5 0.7 ± 0.3 2.18
18 0.7099 5491 ± 26 60 ± 25 7.4 ± 4.3 0.2 ± 0.4 0.2 ± 0.5 1.93
21 1.0142 5350 ± 37 131 ± 36 7.7 ± 3.7 1.7 ± 1.1 0.3 ± 0.7 2.43
Slit 2: X-Offset +0.2 ′′
1 -1.0142 5222 ± 13 41 ± 13 6.1 ± 2.7 0.1 ± 0.2 0.1 ± 0.4 2.81
4 -0.7099 5506 ± 8 30 ± 7 −3.1 ± 1.7 1.1 ± 0.8 3.0 ± 2.0 2.38
13 0.2028 5083 ± 6 77 ± 6 15.3 ± 3.0 3.0 ± 0.7 0.4 ± 0.3 1.67
16 0.5071 5228 ± 36 131 ± 36 8.8 ± 4.0 1.5 ± 0.9 0.2 ± 0.6 1.91
110

Table 3.23. NGC 7052: Measured Parameters.
Row Y-Offset vr σgas F(Hα/10 −16 ) F([NII]6585) F([SII]total) R 2
( ′′ ) (km s −1 ) (km s −1 ) (erg s −1 cm −2 Hz −1 ) F(Hα) F(Hα)
Slit 1: X-Offset -0.1 ′′
2 -0.4564 4310 ± 26 153 ± 23 35.8 ± 10.0 1.9 ± 0.7 0.3 ± 0.3 2.33
5 -0.3043 4466 ± 26 186 ± 24 28.5 ± 9.9 3.3 ± 1.3 0.6 ± 0.5 1.94
6 -0.2535 4527 ± 24 179 ± 22 25.7 ± 9.8 4.0 ± 1.7 0.7 ± 0.5 2.75
7 -0.2028 4461 ± 26 241 ± 22 50.7 ± 12.0 2.9 ± 0.8 1.0 ± 0.4 2.97
8 -0.1521 4481 ± 27 281 ± 21 86.0 ± 15.0 2.3 ± 0.5 1.6 ± 0.4 2.15
9 -0.1014 4487 ± 15 285 ± 12 167.2 ± 17.1 2.4 ± 0.3 1.1 ± 0.2 2.62
10 -0.0507 4463 ± 15 413 ± 14 289.4 ± 29.2 3.0 ± 0.3 1.1 ± 0.2 2.31
11 0.0000 4541 ± 17 456 ± 16 354.7 ± 35.1 2.7 ± 0.3 0.8 ± 0.1 2.94
12 0.0507 4722 ± 24 387 ± 22 148.1 ± 24.7 2.8 ± 0.5 0.9 ± 0.2 2.95
16 0.2535 4173 ± 7 37 ± 6 29.4 ± 7.9 0.4 ± 0.2 0.1 ± 0.2 2.29
18 0.3550 4130 ± 14 59 ± 13 20.7 ± 8.5 0.1 ± 0.3 1.2 ± 0.6 3.04
19 0.4057 4210 ± 15 54 ± 15 20.2 ± 7.7 0.0 ± 0.2 0.5 ± 0.5 2.56
Slit 0: X-Offset 0.0 ′′
1 -0.5071 4434 ± 8 66 ± 7 87.2 ± 15.5 0.5 ± 0.1 0.4 ± 0.2 1.76
4 -0.3550 4606 ± 21 130 ± 20 37.3 ± 13.6 1.6 ± 0.7 1.8 ± 0.8 1.65
7 -0.2028 4511 ± 22 175 ± 19 59.6 ± 15.7 2.0 ± 0.6 1.6 ± 0.5 2.02
8 -0.1521 4558 ± 19 232 ± 18 48.1 ± 17.2 5.6 ± 2.1 1.5 ± 0.7 1.46
9 -0.1014 4665 ± 14 265 ± 13 110.1 ± 20.7 4.1 ± 0.8 2.3 ± 0.5 1.54
10 -0.0507 4677 ± 10 268 ± 8 244.8 ± 24.5 3.1 ± 0.3 1.3 ± 0.2 2.09
11 0.0000 4772 ± 11 303 ± 9 285.5 ± 29.5 3.1 ± 0.4 0.5 ± 0.1 1.97
12 0.0507 4832 ± 17 346 ± 16 153.1 ± 28.8 4.1 ± 0.8 1.6 ± 0.4 1.91
14 0.1521 3887 ± 25 65 ± 24 21.6 ± 11.3 0.4 ± 0.4 0.4 ± 0.5 1.64
Slit 2: X-Offset +0.1 ′′
1 -0.5071 4468 ± 9 84 ± 9 87.2 ± 14.6 0.5 ± 0.1 0.0 ± 0.1 1.91
2 -0.4564 4479 ± 15 99 ± 15 62.3 ± 13.8 0.4 ± 0.2 0.5 ± 0.2 1.73
3 -0.4057 4561 ± 13 75 ± 13 47.9 ± 12.4 0.7 ± 0.3 0.3 ± 0.2 1.82
4 -0.3550 4572 ± 18 114 ± 17 51.7 ± 13.3 1.3 ± 0.4 0.3 ± 0.2 2.24
5 -0.3043 4576 ± 20 105 ± 19 53.3 ± 14.5 0.6 ± 0.3 0.4 ± 0.2 1.99
6 -0.2535 4582 ± 13 79 ± 13 41.2 ± 10.9 0.9 ± 0.4 0.7 ± 0.3 1.82
7 -0.2028 4536 ± 21 127 ± 21 71.6 ± 16.4 0.2 ± 0.2 0.1 ± 0.2 1.87
8 -0.1521 4641 ± 9 69 ± 9 55.7 ± 11.1 1.0 ± 0.3 0.2 ± 0.2 2.06
9 -0.1014 4667 ± 11 126 ± 11 73.4 ± 12.1 1.8 ± 0.4 0.8 ± 0.2 1.91
10 -0.0507 4670 ± 7 109 ± 7 68.4 ± 10.4 2.3 ± 0.4 1.6 ± 0.3 1.73
11 0.0000 4678 ± 9 137 ± 9 65.2 ± 11.1 2.6 ± 0.5 2.1 ± 0.4 2.11
13 0.1014 4726 ± 13 87 ± 12 14.5 ± 7.5 5.8 ± 3.2 0.9 ± 0.8 1.62
14 0.1521 4759 ± 33 125 ± 33 32.5 ± 13.3 1.1 ± 0.6 0.2 ± 0.3 1.50
16 0.2535 4738 ± 32 132 ± 32 20.8 ± 10.5 1.7 ± 1.1 1.8 ± 1.2 2.30
20 0.4564 3941 ± 15 73 ± 15 11.0 ± 5.9 2.9 ± 1.8 2.6 ± 1.6 1.96
111

Table 3.24. UGC 12064: Measured Parameters.
Row Y-Offset vr σgas F(Hα/10 −16 ) F([NII]6585) F([SII]total) R 2
( ′′ ) (km s −1 ) (km s −1 ) (erg s −1 cm −2 Hz −1 ) F(Hα) F(Hα)
Slit 1: X-Offset -0.1 ′′
2 -0.4564 4876 ± 17 136 ± 17 39.5 ± 10.9 1.8 ± 0.6 1.3 ± 0.5 2.29
3 -0.4057 4971 ± 18 107 ± 18 47.6 ± 11.6 0.4 ± 0.2 0.7 ± 0.3 1.88
4 -0.3550 4962 ± 19 73 ± 19 29.8 ± 10.6 0.1 ± 0.2 0.2 ± 0.3 2.06
5 -0.3043 4880 ± 25 127 ± 25 37.2 ± 11.3 1.0 ± 0.4 0.1 ± 0.3 2.24
6 -0.2535 4868 ± 18 134 ± 16 44.1 ± 10.1 1.7 ± 0.5 0.0 ± 0.3 2.11
7 -0.2028 4940 ± 13 47 ± 12 17.8 ± 7.1 0.5 ± 0.4 0.9 ± 0.6 1.77
8 -0.1521 4957 ± 8 46 ± 8 32.3 ± 8.5 0.4 ± 0.2 0.7 ± 0.3 2.44
9 -0.1014 5015 ± 21 191 ± 18 69.0 ± 13.2 1.6 ± 0.4 0.7 ± 0.3 2.36
10 -0.0507 5085 ± 22 259 ± 20 37.9 ± 13.4 5.4 ± 2.0 2.4 ± 1.0 2.13
11 0.0000 5141 ± 21 248 ± 15 87.6 ± 14.6 2.6 ± 0.5 0.9 ± 0.3 1.81
12 0.0507 5231 ± 26 305 ± 21 93.0 ± 17.7 3.1 ± 0.7 1.2 ± 0.3 1.97
18 0.3550 5121 ± 13 40 ± 12 10.7 ± 5.9 1.4 ± 1.0 0.5 ± 0.7 2.26
Slit 0: X-Offset 0.0 ′′
2 -0.4564 4783 ± 36 174 ± 34 87.6 ± 24.2 0.3 ± 0.2 0.4 ± 0.3 1.63
3 -0.4057 4795 ± 43 157 ± 41 44.9 ± 18.3 1.1 ± 0.6 0.3 ± 0.4 1.63
5 -0.3043 4963 ± 28 82 ± 29 23.2 ± 14.3 1.2 ± 1.0 0.5 ± 0.7 1.56
6 -0.2535 4951 ± 49 189 ± 44 35.9 ± 17.5 1.8 ± 1.1 1.0 ± 0.8 1.41
8 -0.1521 4846 ± 42 245 ± 36 35.5 ± 17.8 3.8 ± 2.1 2.8 ± 1.6 1.63
10 -0.0507 5070 ± 15 341 ± 14 265.0 ± 31.6 3.3 ± 0.4 1.1 ± 0.2 1.25
11 0.0000 5186 ± 15 496 ± 13 304.5 ± 62.6 7.1 ± 1.5 1.7 ± 0.4 1.67
12 0.0507 5207 ± 14 444 ± 13 446.8 ± 53.5 4.3 ± 0.5 1.0 ± 0.2 2.28
13 0.1014 5187 ± 32 320 ± 27 132.7 ± 28.3 2.7 ± 0.7 0.8 ± 0.3 1.73
19 0.4057 5128 ± 30 97 ± 30 43.7 ± 18.4 0.2 ± 0.2 0.2 ± 0.3 1.68
20 0.4564 5170 ± 35 121 ± 34 36.4 ± 16.2 0.3 ± 0.4 1.3 ± 0.9 1.86
21 0.5071 5086 ± 32 79 ± 32 22.2 ± 15.6 1.1 ± 1.1 0.2 ± 0.6 1.71
Slit 2: X-Offset +0.1 ′′
1 -0.5071 5016 ± 38 199 ± 34 23.1 ± 10.8 3.0 ± 1.6 0.9 ± 0.8 1.65
2 -0.4564 4863 ± 8 38 ± 7 29.0 ± 8.2 0.6 ± 0.3 0.0 ± 0.2 1.81
3 -0.4057 4881 ± 41 134 ± 42 14.8 ± 9.4 2.1 ± 1.6 0.2 ± 0.8 1.72
8 -0.1521 4884 ± 18 160 ± 17 21.5 ± 9.0 4.7 ± 2.1 3.2 ± 1.5 1.73
9 -0.1014 4914 ± 19 237 ± 17 47.7 ± 12.1 4.1 ± 1.1 1.8 ± 0.6 1.89
10 -0.0507 4926 ± 15 257 ± 12 96.8 ± 14.1 3.3 ± 0.5 1.1 ± 0.3 1.88
11 0.0000 4939 ± 16 304 ± 14 127.4 ± 17.4 3.3 ± 0.5 1.1 ± 0.2 1.72
14 0.1521 5081 ± 45 199 ± 38 38.5 ± 13.1 1.3 ± 0.6 0.6 ± 0.4 2.36
15 0.2028 5088 ± 23 101 ± 22 41.0 ± 12.5 0.1 ± 0.2 0.5 ± 0.3 2.03
16 0.2535 5197 ± 33 97 ± 33 11.2 ± 7.7 2.1 ± 1.8 1.2 ± 1.3 1.69
18 0.3550 4867 ± 38 143 ± 37 43.4 ± 15.4 0.1 ± 0.2 0.3 ± 0.3 1.75
112

Table 3.25. NGC 7626: Measured Parameters.
Row Y-Offset vr σgas F(Hα/10 −16 ) F([NII]6585) F([SII]total) R 2
( ′′ ) (km s −1 ) (km s −1 ) (erg s −1 cm −2 Hz −1 ) F(Hα) F(Hα)
Slit 1: X-Offset -0.2 ′′
8 -0.3043 3554 ± 30 210 ± 25 17.5 ± 4.1 1.6 ± 0.5 0.5 ± 0.3 2.25
9 -0.2028 3583 ± 22 230 ± 18 22.5 ± 4.2 2.3 ± 0.5 0.4 ± 0.3 2.17
10 -0.1014 3457 ± 13 200 ± 12 34.4 ± 4.1 1.9 ± 0.3 0.9 ± 0.2 2.46
11 0.0000 3378 ± 8 152 ± 8 14.0 ± 3.1 5.1 ± 1.2 1.4 ± 0.5 2.32
12 0.1014 3332 ± 15 185 ± 14 8.6 ± 3.4 6.5 ± 2.6 1.3 ± 0.8 2.51
13 0.2028 3331 ± 18 163 ± 17 20.5 ± 4.0 1.5 ± 0.4 0.4 ± 0.3 2.14
14 0.3043 3295 ± 27 155 ± 27 13.4 ± 4.1 1.3 ± 0.5 0.4 ± 0.4 2.25
16 0.5071 3289 ± 16 63 ± 16 7.9 ± 2.8 0.0 ± 0.2 0.2 ± 0.3 2.89
17 0.6085 3412 ± 36 147 ± 35 9.7 ± 3.5 0.8 ± 0.4 0.1 ± 0.4 2.61
18 0.7099 3572 ± 23 93 ± 23 10.2 ± 3.3 0.1 ± 0.2 0.1 ± 0.3 3.05
19 0.8114 4142 ± 23 170 ± 21 16.7 ± 3.4 1.0 ± 0.3 0.4 ± 0.2 3.42
Slit 0: X-Offset 0.0 ′′
1 -1.0142 3116 ± 34 156 ± 33 4.8 ± 3.0 3.9 ± 2.7 0.5 ± 1.0 2.74
2 -0.9128 3191 ± 43 197 ± 38 8.1 ± 3.8 2.6 ± 1.4 0.5 ± 0.7 2.33
6 -0.5071 3630 ± 39 184 ± 36 6.2 ± 3.9 4.2 ± 2.9 0.3 ± 1.0 2.16
7 -0.4057 3568 ± 10 104 ± 10 7.1 ± 2.9 5.6 ± 2.4 2.0 ± 1.0 1.83
8 -0.3043 3605 ± 9 153 ± 8 34.7 ± 4.3 2.5 ± 0.4 1.3 ± 0.2 1.96
9 -0.2028 3607 ± 5 171 ± 5 65.4 ± 4.8 2.9 ± 0.3 1.2 ± 0.1 1.97
10 -0.1014 3552 ± 4 260 ± 3 217.8 ± 7.7 2.3 ± 0.1 1.0 ± 0.1 2.43
11 0.0000 3446 ± 5 349 ± 5 261.0 ± 11.3 3.2 ± 0.2 1.1 ± 0.1 2.64
12 0.1014 3227 ± 4 223 ± 3 136.0 ± 6.2 2.6 ± 0.1 1.0 ± 0.1 2.58
13 0.2028 3216 ± 6 151 ± 6 44.4 ± 4.3 2.7 ± 0.3 0.9 ± 0.2 2.08
14 0.3043 3235 ± 13 157 ± 13 21.7 ± 4.1 2.5 ± 0.6 0.5 ± 0.3 2.23
16 0.5071 3417 ± 24 95 ± 24 12.4 ± 4.4 0.5 ± 0.3 0.4 ± 0.4 2.32
17 0.6085 3470 ± 16 84 ± 16 7.9 ± 2.9 1.8 ± 0.8 0.3 ± 0.5 2.21
21 1.0142 3136 ± 27 118 ± 28 8.9 ± 3.5 1.1 ± 0.6 1.0 ± 0.7 2.29
Slit 2: X-Offset +0.2 ′′
5 -0.6085 3780 ± 5 29 ± 5 7.0 ± 2.1 0.1 ± 0.2 1.1 ± 0.5 2.06
6 -0.5071 3849 ± 18 69 ± 18 5.6 ± 2.5 0.6 ± 0.5 2.3 ± 1.3 2.84
10 -0.1014 3479 ± 14 181 ± 14 12.0 ± 3.7 5.5 ± 1.8 1.6 ± 0.7 1.97
11 0.0000 3433 ± 6 135 ± 6 33.9 ± 3.7 2.9 ± 0.4 0.8 ± 0.2 2.36
12 0.1014 3405 ± 7 119 ± 7 27.1 ± 3.5 2.4 ± 0.4 0.1 ± 0.2 1.90
15 0.4057 3442 ± 27 185 ± 25 10.7 ± 3.5 2.6 ± 1.0 0.2 ± 0.5 2.42
16 0.5071 3377 ± 10 51 ± 10 6.0 ± 2.1 1.5 ± 0.7 0.3 ± 0.4 2.29
17 0.6085 3391 ± 10 34 ± 11 2.9 ± 1.7 1.3 ± 1.0 1.2 ± 1.1 2.33
18 0.7099 3275 ± 42 163 ± 41 6.9 ± 3.3 1.5 ± 1.0 1.5 ± 1.0 2.19
19 0.8114 3579 ± 15 56 ± 15 3.8 ± 1.9 1.2 ± 0.8 2.2 ± 1.3 2.65
20 0.9128 3518 ± 10 31 ± 10 4.0 ± 1.9 0.3 ± 0.3 1.0 ± 0.7 2.37
113

Table 3.26. Effect of making various fit parameters free.
Fit description vHα v[NII] σHα σ[NII] F([N II]6585) R 2
(km s −1 ) (km s −1 ) (km s −1 ) (km s −1 ) F([N II]6549)
(1) (2) (3) (4) (5) (6) (7)
114
initial parameters 4620 ± 4 249 ± 3 3.0 3.21
vHα free 4616 ± 9 4620 ± 3 249 ± 3 3.0 3.22
σHα free 4619 ± 3 228 ± 9 256 ± 4 3.0 3.21
vHα + σHα free 4618 ± 9 4619 ± 4 228 ± 9 256 ± 4 3.0 3.22
[N II] ratio free 4622 ± 3 248 ± 3 2.32 ± 0.09 3.04
Note. — The measurements shown were made using the central spectral row in the
central slit observed for NGC 4335. Col. (1): Parameters made free, Initially a set of
lines with one velocity and one velocity dispersion was used, with the ratio of the two
[N II] lines fixed to 3.0. The two [S II] lines are fixed in velocity and width to the [N II]
lines in every case; Col. (2-3): The radial velocities of the Hα and [N II] lines; Col.
(3-4): The velocity dispersions of the Hα and [N II] lines; Col. (5): The ratio of the
[N II]6585 and [N II]6549 lines; Col. (6): The reduced χ 2 value of the resulting fit.

Table 3.27. Presence of a Nuclear Broad Line.
Galaxy ∆|residual| R 2 N − R 2 A By eye Score Broad Cpt.
(%) R 2 N
(1) (2) (3) (4) (5) (6)
NGC 193 9.6 0.19 � 3 Yes
NGC 315 25.0 0.46 � 3 Yes
NGC 383 8.7 0.16 ◦ 2 Yes
NGC 541 4.6 0.12 � 1 No
NGC 741 1.9 0.01 ◦ 0 No
UGC 1841 14.7 0.35 � 3 Yes
NGC 2329 9.4 0.32 ◦ 2 *
NGC 2892 2.8 0.09 ◦ 0 No
NGC 3801 0.1 0.01 ◦ 0 No
NGC 3862 8.0 0.22 ◦ 2 *
UGC 7115 2.6 0.09 ◦ 0 No
NGC 4261 7.8 0.22 � 3 Yes
NGC 4335 8.0 0.40 � 3 Yes
NGC 4374 2.4 0.12 ◦ 0 No
NGC 4486 3.4 0.15 � 2 Yes
NGC 5127 -1.5 -0.01 ◦ 0 No
NGC 5141 3.7 0.16 � 2 Yes
NGC 5490 5.2 0.23 � 3 Yes
NGC 7052 4.9 0.04 � 1 No
UGC 12064 6.7 0.11 � 2 Yes
NGC 7626 2.5 0.13 � 2 Yes
Note. — Col. (1): NGC/UGC Identification; Col. (2): Difference in
the mean of the absolute values of the residuals from the fits including
and excluding the additional component; Col. (3): Relative change in
reduced χ 2 value between fits with the narrow lines alone (N) and with
the additional component (A); Col. (4): Could an improvement in the
fit be judged by eye?; Col. (5): Additional component ‘score’, one point
available from each of columns 2 to 6, see text for criteria; Col. (6) Is
an additional broad component useful in the fit based on these results?
An asterisk (*) indicates the component appears to represent a non-flat
continuum.
115

Table 3.28. Fits to the central pixel for each galaxy, including broad lines.
Kinematics.
Galaxy Row vr(NL) vr(BL) σgas(NL) σgas(BL) R 2
(km s −1 ) (km s −1 ) (km s −1 ) (km s −1 )
(1) (2) (3) (4) (5) (6) (7)
NGC 193 11 4417 ± 7 5128 ± 36 277 ± 6 967 ± 21 3.15
NGC 315 11 4830 ± 9 5738 ± 55 406 ± 9 1790 ± 67 2.06
NGC 383 11 5278 ± 54 5568 ± 29 669 ± 39 1367 ± 79 2.25
UGC 1841 11 6409 ± 8 6585 ± 20 436 ± 7 1254 ± 35 3.11
NGC 4261 † 11 2056 ± 9 2703 ± 68 366 ± 12 1079 ± 55 1.69
NGC 4335 11 4618 ± 3 4893 ± 37 188 ± 4 1299 ± 51 1.93
NGC 4486 11 1417 ± 14 1408 ± 28 534 ± 12 1479 ± 42 6.01
NGC 5141 11 5229 ± 3 5356 ± 86 121 ± 4 1223 ± 96 2.01
NGC 5490 11 4733 ± 16 5621 ± 61 377 ± 22 1336 ± 56 1.94
UGC 12064 11 5195 ± 16 5417 ± 90 423 ± 19 1321 ± 168 1.49
NGC 7626 11 3432 ± 7 4083 ± 76 287 ± 10 1126 ± 73 2.29
Note. — †For NGC 4261 slit 1 (offset -0.1 arcsec) was used; Col. (1):
NGC/UGC Number; Col. (2): Central pixel row number referenced from
the earlier data tables for each galaxy; Col. (3): The line of sight velocities
of the narrow line components; Col. (4): The line of sight velocities of the
broad components (where present); Col. (5): The line of sight velocity
dispersions of the narrow line components; Col. (6): The line of sight
velocity dispersions of the broad components (where present); Col. (7):
The reduced χ 2 value of the fit. The parameters were measured by fitting
a models with 5 narrow lines, fixed to each other in velocity and velocity
dispersion and one free broad component, except as noted above. Errors
quoted are the formal errors on the various parameters from the fit.
116

Table 3.29. Fits to the central pixel for each galaxy, including broad lines. Fluxes.
Galaxy F(HαNarrow) F([N II]6585) F([S II]total) F(Broad Line) F([S II]6733)
(ergs −1 cm −2 Hz −1 ) F(HαNarrow) F(HαNarrow) F(HαNarrow) F([S II]6718)
(1) (2) (3) (4) (5) (6)
NGC 193 1.33 ± 0.23 4.21 ± 0.77 3.86 ± 0.71 7.60 ± 1.46 1.18 ± 0.07
NGC 315 9.28 ± 0.77 4.72 ± 0.42 1.81 ± 0.21 4.40 ± 0.51 1.80 ± 0.14
NGC 383 27.72 ± 3.65 0.33 ± 0.18 0.56 ± 0.63 2.14 ± 0.50 0.11 ± 0.12
UGC 1841 7.71 ± 0.46 2.41 ± 0.16 1.39 ± 0.11 2.57 ± 0.28 1.09 ± 0.06
NGC 4261 4.36 ± 1.53 6.76 ± 2.42 3.37 ± 1.23 7.22 ± 2.93 1.55 ± 0.15
NGC 4335 1.33 ± 0.13 4.46 ± 0.44 2.63 ± 0.32 7.54 ± 0.87 1.04 ± 0.08
NGC 4486 44.96 ± 1.53 0.43 ± 0.04 0.59 ± 0.60 1.37 ± 0.11 0.03 ± 0.03
NGC 5141 0.91 ± 0.07 2.95 ± 0.25 1.38 ± 0.22 3.11 ± 0.45 0.97 ± 0.14
NGC 5490 0.25 ± 0.20 14.34 ± 11.64 9.12 ± 7.56 40.54 ± 32.95 1.94 ± 0.38
UGC 12064 0.48 ± 1.14 30.72 ± 72.97 11.16 ± 26.60 32.31 ± 77.41 0.58 ± 0.12
NGC 7626 1.48 ± 0.24 3.80 ± 0.66 1.98 ± 0.38 4.00 ± 1.01 0.95 ± 0.09
Note. — Col. (1): NGC/UGC Number; Col. (2): Hα narrow line flux; Col.
(3): Ratio of the broad line flux to the Hα narrow line flux; Col. (4) Ratio of
the [N II]6585 narrow line flux to the Hα Narrow line flux; Col. (5) Ratio of
the total [S II] flux to the Hα Narrow line flux; Col. (6) Ratio of the [S II]6733
narrow line to the [S II]6718 narrow line. The parameters were measured by
fitting a models with 5 narrow lines, fixed to each other in velocity and velocity
dispersion and one free broad component, except as noted above. Errors quoted
are the formal errors on the various parameters from the fit.
117

Table 3.30. Kinematic estimators within 100 pc of the nucleus.
Galaxy rmax. σnuc. ¯σ100pc ∆100pc
(pc) (km s −1 ) (km s −1 ) (km s −1 )
(1) (2) (3) (4) (5)
Rotators:
NGC 315 · · · 528 290 353
NGC 383 · · · 924 342 434
NGC 2329 · · · 302 145 84
UGC 7115 · · · 497 287 337
NGC 4261 78 459 238 319
NGC 4335 · · · 249 166 307
M 84 41 883 229 669
NGC 4486 41 612 313 607
NGC 5127 · · · 157 148 69
NGC 5141 · · · 149 146 196
NGC 7052 · · · 303 226 945
UGC 12064 · · · 497 308 361
NGC 7626 · · · 350 175 391
Mean 463 ± 254 236 ± 72 390 ± 250
Non-Rotators:
NGC 193 · · · 437 228 253
NGC 541 · · · 336 182 266
UGC 1841 · · · 593 378 16
NGC 2892 · · · 453 338 118
NGC 3801 · · · 163 143 113
NGC 3862 · · · 303 182 130
NGC 5490 · · · 680 240 358
Mean 381 ± 147 242 ± 95 149 ± 95
Note. — Col. (1): Galaxy ID; Col. (2): Where the radius away from the central
pixel used was less than 100 pc the radius is indicated here; Col. (3): The velocity
dispersion of the very central spectrum; Col. (4): The mean velocity dispersion
within 100 pc of the central position; Col. (5): The difference in mean velocities
within 100 pc to either side of the central spectrum. The galaxies are grouped into
two classes ‘rotators’ and ‘non-rotators’ judged by eye as discussed in the text,
mean values of each parameter are given for each class.
118

Table 3.31. Comparison of broad line statistics
Parameter UGC FR-I sample Sy/LINERs Radio Loud
(1) (2) (3) (4)
< σBL > (km s −1 ) 1295 ± 218 2400 ± 1100 5900 ± 3700
< σNL > (km s −1 ) 371 ± 153 · · · · · ·
< vNL − vBL > (km s −1 ) −435 ± 335 · · · −500 ± 1200
Note. — The mean velocity dispersions of broad and narrow lines and
offsets of broad and narrow lines for three different galaxy samples: Col.(2)
the data presented in this work; Col. (3) A sample of Seyferts and LINERs;
Col. (4) A summary of properties of several sample of radio galaxies.
References. — (3) Ho et al. (1997); (4) Sulentic et al. (2000)
119

Table 3.32.
Model ID Description vr(NL) vr(BB) vr(BC) σgas(NL) σgas(BB) σgas(BC) R 2
(km s −1 ) (km s −1 ) (km s −1 ) (km s −1 ) (km s −1 ) (km s −1 )
(1) (2) (3) (4) (5) (6) (7) (8) (9)
1 Narrow lines only 4620 · · · · · · 249 · · · · · · 3.21
2 (1) + Extra Broad Component 4618 · · · 4893 188 · · · 1299 1.93
3 (2) + Constrained Broad Bases (i) 4616 = 4616 4767 139 354 1565 1.73
4 (2) + Constrained Broad Bases (ii) 4595 4724 4680 139 319 1417 1.60
5 (2) + Unconstrained Broad Bases 4616 = 4616 4764 128 319 1389 1.68
Note. — Col. (1) Model ID (see text); Col. (2): Brief description of the fit; Cols. (3-5): The radial velocities of the
narrow line (NL), broad base (BB) and broad components (BC) respectively; Cols. (6-8): The velocity dispersions of the
narrow line (NL), broad base (BB) and broad components (BC) respectively. Fits were performed on the central row of the
central slit of the observations of NGC 4335; Col. (9): The reduced χ 2 value of the fit.
Table 3.32 Kinematic parameters measured using various free-parameter sets.
120

(a)
(b) (i)
(ii)
(c)
(i) (ii) (iii) (iv)
(d)
(i) (ii)
(e)
(i) (ii) (iii) (iv)
Intensity (erg s −1 cm −2 Å −1 arcsec −2 )
v r (km s −1 )
8•10 −15
6•10 −15
4•10 −15
2•10 −15
4700
4600
4500
4400
4300
4200
4100
0
Reduced 2−D Spectrum
Single Gaussian per Line Fit
v r
X = −0.2
Y (arcsec)
Hα+[NII] & [SII] − Narrow Line Fit
0.91
0.41
−0.10
−0.61
σ gas
v r
+0.2 0.0 −0.2
X (arcsec)
−2•10
6584 6638 6691 6745 6799 6852 6906
Wavelength (Angstroms)
−15
X = 0.0
X = +0.2
−1.01 −0.34 0.34 1.01
Y (arcsec)
σ gas (km s −1 )
500
400
300
200
100
0
X = −0.2
X = 0.0
X = +0.2
−1.01 −0.34 0.34 1.01
Y (arcsec)
Intensity (erg s −1 cm −2 Å −1 arcsec −2 )
F (10 −14 ergs s −1 cm −2 Hz −1 )
8•10 −15
6•10 −15
4•10 −15
2•10 −15
0.5
0.4
0.3
0.2
0.1
0.0
10
8
6
4
2
0
0.4
0.3
0.2
0.1
0
σ gas
+0.2 0.0 −0.2
X (arcsec)
[NII] 6585 Flux
X = −0.2
X = 0.0
X = +0.2
0.0
−0.1
−1.01 −0.34 0.34 1.01
Y (arcsec)
F([NII] 6585)
+0.2 0.0 −0.2
X (arcsec)
Hα+[NII] & [SII] − Narrow & Broad Cpt. Fit
[NII] 6585/Hα
10.0
1.0
0.1
F([NII])/F(Hα)
+0.2 0.0 −0.2
X (arcsec)
−2•10
6584 6638 6691 6745 6799 6852 6906
Wavelength (Angstroms)
−15
[NII]/Hα
X = −0.2
X = 0.0
X = +0.2
−1.01 −0.34 0.34 1.01
Y (arcsec)
Figure 3.1 Key to plots. Region (a): the HST acquisition image for each galaxy
observed is shown with the positions of the observed long slits overlaid. The relative
position angles of the galaxy major axes measured from the central isophotes (dashed
lines) and the arcsecond scale radio jets (dotted lines) are shown. These lines cross,
and a North-East indicator is drawn, at the location of the central pixel (see text).
Region (b): (i) the central portion of the reduced 2-D spectrum from the central
slit position is shown along with (ii) an image created from fitting a set of 5 Gaussian
lines to the same. Region (c): plots representing the two-dimensional distributions
of parameters measured by fitting a one Gaussian per emission line model to spectra
from the nuclear region. The dashed and dash-dot lines indicate the directions of the
minor and major axes respectively. The lines cross at the location of the central pixel.
We show: (i) radial velocity (filled circles represent velocities greater than the mean,
empty circles represent velocities less than the mean and the radius of each point [i,j]
is proportional to |vi,j − vmean|); (ii) velocity dispersion (the radius of the circle is
proportional to σi,j); (iii) integrated line flux (the area of each point is proportional
to Fi,j); and (iv) [N II]6585 / Hα ratio (The radius of each circle is proportional to
log(F([N II]6585)/F(Hα))). Region (d): single Gaussian per line fit and residuals
without (i) and with (ii) the additional free component described in the text for the
central spectrum of each galaxy. Region (e): plots of (i) radial velocity, (ii) velocity
dispersion, (iii) [N II] line flux and (iv) [N II]6585 / Hα ratio along each slit measured
by fitting a one Gaussian per line model to the emission line spectra. The vertical
dotted line indicates the Y position of the central row. The dash-dot line in the
velocity panel indicates the quoted recession velocity for the galaxy (see Table 2.1).
0.5"
121

Intensity (erg s −1 cm −2 Å −1 arcsec −2 )
v r (km s −1 )
8•10 −15
6•10 −15
4•10 −15
2•10 −15
4700
4600
4500
4400
4300
4200
4100
0
−2•10 −15
Reduced 2−D Spectrum
Single Gaussian per Line Fit
v r
X = −0.2
Y (arcsec)
Hα+[NII] & [SII] − Narrow Line Fit
0.91
0.41
−0.10
−0.61
σ gas
v r
+0.2 0.0 −0.2
X (arcsec)
6584 6638 6691 6745 6799 6852 6906
Wavelength (Angstroms)
X = 0.0
X = +0.2
−1.01 −0.34 0.34 1.01
Y (arcsec)
σ gas (km s −1 )
500
400
300
200
100
0
0.5"
X = −0.2
X = 0.0
X = +0.2
−1.01 −0.34 0.34 1.01
Y (arcsec)
Intensity (erg s −1 cm −2 Å −1 arcsec −2 )
F (10 −14 ergs s −1 cm −2 Hz −1 )
8•10 −15
6•10 −15
4•10 −15
2•10 −15
0.5
0.4
0.3
0.2
0.1
0.0
10
8
6
4
2
0
0.4
0.3
0.2
0.1
0
−2•10 −15
σ gas
+0.2 0.0 −0.2
X (arcsec)
[NII] 6585 Flux
X = −0.2
X = 0.0
X = +0.2
0.0
−0.1
−1.01 −0.34 0.34 1.01
Y (arcsec)
F([NII] 6585)
+0.2 0.0 −0.2
X (arcsec)
Hα+[NII] & [SII] − Narrow & Broad Cpt. Fit
[NII] 6585/Hα
10.0
1.0
0.1
F([NII])/F(Hα)
+0.2 0.0 −0.2
X (arcsec)
6584 6638 6691 6745 6799 6852 6906
Wavelength (Angstroms)
[NII]/Hα
X = −0.2
X = 0.0
X = +0.2
−1.01 −0.34 0.34 1.01
Y (arcsec)
Figure 3.2 Observation and fit data for NGC 193, see Figure 3.1 for description.
122

Intensity (erg s −1 cm −2 Å −1 arcsec −2 )
v r (km s −1 )
2.71•10 −14
2.12•10 −14
1.54•10 −14
9.58•10 −15
3.75•10 −15
−2.08•10 −15
5200
5100
5000
4900
4800
Reduced 2−D Spectrum
Single Gaussian per Line Fit
v r
X = −0.1
Y (arcsec)
0.46
0.20
-0.05
-0.30
Hα+[NII] & [SII] − Narrow Line Fit
σ gas
v r
+0.1 0.0 -0.1
X (arcsec)
6584 6638 6691 6745 6799 6852 6906
Wavelength (Angstroms)
X = 0.0
X = +0.1
−0.51 −0.17 0.17 0.51
Y (arcsec)
σ gas (km s −1 )
600
400
200
0
0.5"
X = −0.1
X = 0.0
X = +0.1
Intensity (erg s −1 cm −2 Å −1 arcsec −2 )
−0.51 −0.17 0.17 0.51
Y (arcsec)
F (10 −14 ergs s −1 cm −2 Hz −1 )
2.71•10 −14
2.12•10 −14
1.54•10 −14
9.58•10 −15
3.75•10 −15
−2.08•10 −15
5
4
3
2
1
0
80
60
40
20
0
−20
22.5
17.5
12.5
7.5
σ gas
+0.1 0.0 -0.1
X (arcsec)
[NII] 6585 Flux
X = −0.1
X = 0.0
X = +0.1
2.5
−2.5
−0.51 −0.17 0.17 0.51
Y (arcsec)
F([NII] 6585)
+0.1 0.0 -0.1
X (arcsec)
Hα+[NII] & [SII] − Narrow & Broad Cpt. Fit
[NII] 6585/Hα
10.0
1.0
0.1
F([NII])/F(Hα)
+0.1 0.0 -0.1
X (arcsec)
6584 6638 6691 6745 6799 6852 6906
Wavelength (Angstroms)
[NII]/Hα
X = −0.1
X = 0.0
X = +0.1
−0.51 −0.17 0.17 0.51
Y (arcsec)
Figure 3.3 Observation and fit data for NGC 315, see Figure 3.1 for description.
123

Intensity (erg s −1 cm −2 Å −1 arcsec −2 )
v r (km s −1 )
2.0•10 −14
1.5•10 −14
1.0•10 −14
5.0•10 −15
5400
5300
5200
5100
5000
4900
4800
4700
0
−5.0•10 −15
Reduced 2−D Spectrum
Single Gaussian per Line Fit
v r
X = −0.1
Y (arcsec)
0.46
0.20
-0.05
-0.30
Hα+[NII] & [SII] − Narrow Line Fit
σ gas
v r
+0.1 0.0 -0.1
X (arcsec)
6584 6638 6691 6745 6799 6852 6906
Wavelength (Angstroms)
X = 0.0
X = +0.1
−0.51 −0.17 0.17 0.51
Y (arcsec)
σ gas (km s −1 )
1000
800
600
400
200
0
0.5"
X = −0.1
X = 0.0
X = +0.1
−0.51 −0.17 0.17 0.51
Y (arcsec)
Intensity (erg s −1 cm −2 Å −1 arcsec −2 )
F (10 −14 ergs s −1 cm −2 Hz −1 )
2.0•10 −14
1.5•10 −14
1.0•10 −14
5.0•10 −15
9
7
5
3
1
−1
45
35
25
15
5
−5
8
6
4
2
0
−5.0•10 −15
σ gas
+0.1 0.0 -0.1
X (arcsec)
[NII] 6585 Flux
X = −0.1
X = 0.0
X = +0.1
0
−2
−0.51 −0.17 0.17 0.51
Y (arcsec)
F([NII] 6585)
+0.1 0.0 -0.1
X (arcsec)
Hα+[NII] & [SII] − Narrow & Broad Cpt. Fit
[NII] 6585/Hα
10.0
1.0
0.1
F([NII])/F(Hα)
+0.1 0.0 -0.1
X (arcsec)
6584 6638 6691 6745 6799 6852 6906
Wavelength (Angstroms)
[NII]/Hα
X = −0.1
X = 0.0
X = +0.1
−0.51 −0.17 0.17 0.51
Y (arcsec)
Figure 3.4 Observation and fit data for NGC 383, see Figure 3.1 for description.
124

Intensity (erg s −1 cm −2 Å −1 arcsec −2 )
v r (km s −1 )
2.5•10 −15
2.0•10 −15
1.5•10 −15
1.0•10 −15
5.0•10 −16
5700
5600
5500
5400
5300
5200
5100
5000
Reduced 2−D Spectrum
Single Gaussian per Line Fit
v r
X = −0.2
Y (arcsec)
0.91
0.41
-0.10
-0.61
Hα+[NII] & [SII] − Narrow Line Fit
σ gas
v r
+0.2 0.0 -0.2
X (arcsec)
0
6584 6638 6691 6745
Wavelength (Angstroms)
6799 6852 6906
X = 0.0
X = +0.2
−1.01 −0.34 0.34 1.01
Y (arcsec)
σ gas (km s −1 )
400
300
200
100
0
0.5"
X = −0.2
X = 0.0
X = +0.2
−1.01 −0.34 0.34 1.01
Y (arcsec)
Intensity (erg s −1 cm −2 Å −1 arcsec −2 )
F (10 −14 ergs s −1 cm −2 Hz −1 )
2.5•10 −15
2.0•10 −15
1.5•10 −15
1.0•10 −15
5.0•10 −16
0.8
0.6
0.4
0.2
0.0
−0.2
2.5
2.0
1.5
1.0
0.5
0.0
0.225
0.175
0.125
0.075
σ gas
+0.2 0.0 -0.2
X (arcsec)
[NII] 6585 Flux
X = −0.2
X = 0.0
X = +0.2
0.025
−0.025
−1.01 −0.34 0.34 1.01
Y (arcsec)
F([NII] 6585)
+0.2 0.0 -0.2
X (arcsec)
Hα+[NII] & [SII] − Narrow & Broad Cpt. Fit
[NII] 6585/Hα
10.0
1.0
0.1
F([NII])/F(Hα)
+0.2 0.0 -0.2
X (arcsec)
0
6584 6638 6691 6745
Wavelength (Angstroms)
6799 6852 6906
[NII]/Hα
X = −0.2
X = 0.0
X = +0.2
−1.01 −0.34 0.34 1.01
Y (arcsec)
Figure 3.5 Observation and fit data for NGC 541, see Figure 3.1 for description.
125

Intensity (erg s −1 cm −2 Å −1 arcsec −2 )
v r (km s −1 )
2.0•10 −15
1.5•10 −15
1.0•10 −15
5.0•10 −16
5800
5600
5400
5200
0
−5.0•10 −16
Reduced 2−D Spectrum
Single Gaussian per Line Fit
v r
X = −0.2
Y (arcsec)
0.91
0.41
-0.10
-0.61
Hα+[NII] & [SII] − Narrow Line Fit
σ gas
v r
+0.2 0.0 -0.2
X (arcsec)
6584 6638 6691 6745 6799 6852 6906
Wavelength (Angstroms)
X = 0.0
X = +0.2
−1.01 −0.34 0.34 1.01
Y (arcsec)
σ gas (km s −1 )
500
400
300
200
100
0
0.5"
X = −0.2
X = 0.0
X = +0.2
−1.01 −0.34 0.34 1.01
Y (arcsec)
Intensity (erg s −1 cm −2 Å −1 arcsec −2 )
F (10 −14 ergs s −1 cm −2 Hz −1 )
2.0•10 −15
1.5•10 −15
1.0•10 −15
5.0•10 −16
0.25
0.20
0.15
0.10
0.05
0.00
2.25
1.75
1.25
0.75
0.25
−0.25
0.20
0.15
0.10
0.05
0
−5.0•10 −16
σ gas
+0.2 0.0 -0.2
X (arcsec)
[NII] 6585 Flux
X = −0.2
X = 0.0
X = +0.2
0.00
−0.05
−1.01 −0.34 0.34 1.01
Y (arcsec)
F([NII] 6585)
+0.2 0.0 -0.2
X (arcsec)
Hα+[NII] & [SII] − Narrow & Broad Cpt. Fit
[NII] 6585/Hα
10.0
1.0
0.1
F([NII])/F(Hα)
+0.2 0.0 -0.2
X (arcsec)
6584 6638 6691 6745 6799 6852 6906
Wavelength (Angstroms)
[NII]/Hα
X = −0.2
X = 0.0
X = +0.2
−1.01 −0.34 0.34 1.01
Y (arcsec)
Figure 3.6 Observation and fit data for NGC 741, see Figure 3.1 for description.
126

Intensity (erg s −1 cm −2 Å −1 arcsec −2 )
v r (km s −1 )
1.75•10 −14
1.25•10 −14
7.50•10 −15
2.50•10 −15
−2.50•10 −15
−7.50•10 −15
6600
6500
6400
6300
6200
6100
Reduced 2−D Spectrum
Single Gaussian per Line Fit
v r
X = −0.2
Y (arcsec)
0.91
0.41
-0.10
-0.61
Hα+[NII] & [SII] − Narrow Line Fit
σ gas
v r
+0.2 0.0 -0.2
X (arcsec)
6584 6638 6691 6745 6799 6852 6906
Wavelength (Angstroms)
X = 0.0
X = +0.2
−1.01 −0.34 0.34 1.01
Y (arcsec)
σ gas (km s −1 )
800
600
400
200
0
0.5"
X = −0.2
X = 0.0
X = +0.2
Intensity (erg s −1 cm −2 Å −1 arcsec −2 )
−1.01 −0.34 0.34 1.01
Y (arcsec)
F (10 −14 ergs s −1 cm −2 Hz −1 )
1.75•10 −14
1.25•10 −14
7.50•10 −15
2.50•10 −15
−2.50•10 −15
−7.50•10 −15
2.25
1.75
1.25
0.75
0.25
−0.25
40
30
20
10
0
−10
0.9
0.7
0.5
0.3
σ gas
+0.2 0.0 -0.2
X (arcsec)
[NII] 6585 Flux
X = −0.2
X = 0.0
X = +0.2
0.1
−0.1
−1.01 −0.34 0.34 1.01
Y (arcsec)
F([NII] 6585)
+0.2 0.0 -0.2
X (arcsec)
Hα+[NII] & [SII] − Narrow & Broad Cpt. Fit
[NII] 6585/Hα
10.0
1.0
0.1
F([NII])/F(Hα)
+0.2 0.0 -0.2
X (arcsec)
6584 6638 6691 6745 6799 6852 6906
Wavelength (Angstroms)
[NII]/Hα
X = −0.2
X = 0.0
X = +0.2
−1.01 −0.34 0.34 1.01
Y (arcsec)
Figure 3.7 Observation and fit data for UGC 184, see Figure 3.1 for description.
127

Intensity (erg s −1 cm −2 Å −1 arcsec −2 )
v r (km s −1 )
9•10 −15
7•10 −15
5•10 −15
3•10 −15
1•10 −15
−1•10 −15
6000
5900
5800
5700
5600
5500
5400
5300
Reduced 2−D Spectrum
Single Gaussian per Line Fit
v r
X = −0.2
Y (arcsec)
0.91
0.41
-0.10
-0.61
Hα+[NII] & [SII] − Narrow Line Fit
σ gas
v r
+0.2 0.0 -0.2
X (arcsec)
6584 6638 6691 6745 6799 6852 6906
Wavelength (Angstroms)
X = 0.0
X = +0.2
−1.01 −0.34 0.34 1.01
Y (arcsec)
σ gas (km s −1 )
300
200
100
0
0.5"
X = −0.2
X = 0.0
X = +0.2
−1.01 −0.34 0.34 1.01
Y (arcsec)
Intensity (erg s −1 cm −2 Å −1 arcsec −2 )
F (10 −14 ergs s −1 cm −2 Hz −1 )
9•10 −15
7•10 −15
5•10 −15
3•10 −15
1•10 −15
−1•10 −15
0.5
0.4
0.3
0.2
0.1
0.0
10
8
6
4
2
0
0.45
0.35
0.25
0.15
σ gas
+0.2 0.0 -0.2
X (arcsec)
[NII] 6585 Flux
X = −0.2
X = 0.0
X = +0.2
0.05
−0.05
−1.01 −0.34 0.34 1.01
Y (arcsec)
F([NII] 6585)
+0.2 0.0 -0.2
X (arcsec)
Hα+[NII] & [SII] − Narrow & Broad Cpt. Fit
[NII] 6585/Hα
10.0
1.0
0.1
F([NII])/F(Hα)
+0.2 0.0 -0.2
X (arcsec)
6584 6638 6691 6745 6799 6852 6906
Wavelength (Angstroms)
[NII]/Hα
X = −0.2
X = 0.0
X = +0.2
−1.01 −0.34 0.34 1.01
Y (arcsec)
Figure 3.8 Observation and fit data for NGC 2329, see Figure 3.1 for description.
128

Intensity (erg s −1 cm −2 Å −1 arcsec −2 )
v r (km s −1 )
5•10 −15
4•10 −15
3•10 −15
2•10 −15
1•10 −15
7000
6900
6800
6700
6600
Reduced 2−D Spectrum
Single Gaussian per Line Fit
v r
X = −0.2
Y (arcsec)
0.91
0.41
-0.10
-0.61
Hα+[NII] & [SII] − Narrow Line Fit
σ gas
v r
+0.2 0.0 -0.2
X (arcsec)
0
6584 6638 6691 6745
Wavelength (Angstroms)
6799 6852 6906
X = 0.0
X = +0.2
−1.01 −0.34 0.34 1.01
Y (arcsec)
σ gas (km s −1 )
500
400
300
200
100
0
0.5"
X = −0.2
X = 0.0
X = +0.2
−1.01 −0.34 0.34 1.01
Y (arcsec)
Intensity (erg s −1 cm −2 Å −1 arcsec −2 )
F (10 −14 ergs s −1 cm −2 Hz −1 )
5•10 −15
4•10 −15
3•10 −15
2•10 −15
1•10 −15
0.25
0.20
0.15
0.10
0.05
0.00
10
8
6
4
2
0
0.5
0.4
0.3
0.2
σ gas
+0.2 0.0 -0.2
X (arcsec)
[NII] 6585 Flux
X = −0.2
X = 0.0
X = +0.2
0.1
0.0
−1.01 −0.34 0.34 1.01
Y (arcsec)
F([NII] 6585)
+0.2 0.0 -0.2
X (arcsec)
Hα+[NII] & [SII] − Narrow & Broad Cpt. Fit
[NII] 6585/Hα
10.0
1.0
0.1
F([NII])/F(Hα)
+0.2 0.0 -0.2
X (arcsec)
0
6584 6638 6691 6745
Wavelength (Angstroms)
6799 6852 6906
[NII]/Hα
X = −0.2
X = 0.0
X = +0.2
−1.01 −0.34 0.34 1.01
Y (arcsec)
Figure 3.9 Observation and fit data for NGC 2892, see Figure 3.1 for description.
129

Intensity (erg s −1 cm −2 Å −1 arcsec −2 )
v r (km s −1 )
1.0•10 −15
8.0•10 −16
6.0•10 −16
4.0•10 −16
2.0•10 −16
3600
3400
3200
3000
2800
Reduced 2−D Spectrum
Single Gaussian per Line Fit
v r
X = −0.2
Y (arcsec)
0.91
0.41
-0.10
-0.61
Hα+[NII] & [SII] − Narrow Line Fit
σ gas
v r
+0.2 0.0 -0.2
X (arcsec)
0
6584 6638 6691 6745
Wavelength (Angstroms)
6799 6852 6906
X = 0.0
X = +0.2
−1.01 −0.34 0.34 1.01
Y (arcsec)
σ gas (km s −1 )
250
200
150
100
50
0
0.5"
X = −0.2
X = 0.0
X = +0.2
−1.01 −0.34 0.34 1.01
Y (arcsec)
Intensity (erg s −1 cm −2 Å −1 arcsec −2 )
F (10 −14 ergs s −1 cm −2 Hz −1 )
1.0•10 −15
8.0•10 −16
6.0•10 −16
4.0•10 −16
2.0•10 −16
0.4
0.3
0.2
0.1
0.0
−0.1
0.5
0.4
0.3
0.2
0.1
0.0
0.175
0.125
0.075
0.025
σ gas
+0.2 0.0 -0.2
X (arcsec)
[NII] 6585 Flux
X = −0.2
X = 0.0
X = +0.2
−0.025
−0.075
−1.01 −0.34 0.34 1.01
Y (arcsec)
F([NII] 6585)
+0.2 0.0 -0.2
X (arcsec)
Hα+[NII] & [SII] − Narrow & Broad Cpt. Fit
[NII] 6585/Hα
10.0
1.0
0.1
F([NII])/F(Hα)
+0.2 0.0 -0.2
X (arcsec)
0
6584 6638 6691 6745
Wavelength (Angstroms)
6799 6852 6906
[NII]/Hα
X = −0.2
X = 0.0
X = +0.2
−1.01 −0.34 0.34 1.01
Y (arcsec)
Figure 3.10 Observation and fit data for NGC 3801, see Figure 3.1 for description.
130

Intensity (erg s −1 cm −2 Å −1 arcsec −2 )
v r (km s −1 )
2.0•10 −14
1.5•10 −14
1.0•10 −14
5.0•10 −15
6550
6500
6450
6400
6350
0
−5.0•10 −15
Reduced 2−D Spectrum
Single Gaussian per Line Fit
v r
X = −0.2
Y (arcsec)
0.91
0.41
-0.10
-0.61
Hα+[NII] & [SII] − Narrow Line Fit
σ gas
v r
+0.2 0.0 -0.2
X (arcsec)
6584 6638 6691 6745 6799 6852 6906
Wavelength (Angstroms)
X = 0.0
X = +0.2
−1.01 −0.34 0.34 1.01
Y (arcsec)
σ gas (km s −1 )
400
300
200
100
0
0.5"
X = −0.2
X = 0.0
X = +0.2
−1.01 −0.34 0.34 1.01
Y (arcsec)
Intensity (erg s −1 cm −2 Å −1 arcsec −2 )
F (10 −14 ergs s −1 cm −2 Hz −1 )
2.0•10 −14
1.5•10 −14
1.0•10 −14
5.0•10 −15
1.75
1.25
0.75
0.25
−0.25
−0.75
22.5
17.5
12.5
7.5
2.5
−2.5
0.8
0.6
0.4
0.2
0
−5.0•10 −15
σ gas
+0.2 0.0 -0.2
X (arcsec)
[NII] 6585 Flux
X = −0.2
X = 0.0
X = +0.2
0.0
−0.2
−1.01 −0.34 0.34 1.01
Y (arcsec)
F([NII] 6585)
+0.2 0.0 -0.2
X (arcsec)
Hα+[NII] & [SII] − Narrow & Broad Cpt. Fit
[NII] 6585/Hα
10.0
1.0
0.1
F([NII])/F(Hα)
+0.2 0.0 -0.2
X (arcsec)
6584 6638 6691 6745 6799 6852 6906
Wavelength (Angstroms)
[NII]/Hα
X = −0.2
X = 0.0
X = +0.2
−1.01 −0.34 0.34 1.01
Y (arcsec)
Figure 3.11 Observation and fit data for NGC 3862, see Figure 3.1 for description.
131

Intensity (erg s −1 cm −2 Å −1 arcsec −2 )
v r (km s −1 )
6•10 −15
5•10 −15
4•10 −15
3•10 −15
2•10 −15
1•10 −15
7000
6900
6800
6700
Reduced 2−D Spectrum
Single Gaussian per Line Fit
v r
X = 0.0
6600
−1.01 −0.34 0.34 1.01
Y (arcsec)
Y (arcsec)
0.91
0.41
-0.10
-0.61
Hα+[NII] & [SII] − Narrow Line Fit
σ gas (km s −1 )
600
400
200
σ gas
v r
+0.2 0.0 -0.2
X (arcsec)
0
6628 6687 6747 6806
Wavelength (Å)
6865 6925 6984
0.5"
X = 0.0
0
−1.01 −0.34 0.34 1.01
Y (arcsec)
Intensity (erg s −1 cm −2 Å −1 arcsec −2 )
F (10 −14 ergs s −1 cm −2 Hz −1 )
6•10 −15
5•10 −15
4•10 −15
3•10 −15
2•10 −15
1•10 −15
9
7
5
3
σ gas
+0.2 0.0 -0.2
X (arcsec)
[NII] 6585 Flux
X = 0.0
1
−1
−1.01 −0.34 0.34 1.01
Y (arcsec)
F([NII] 6585)
+0.2 0.0 -0.2
X (arcsec)
Hα+[NII] & [SII] − Narrow & Broad Cpt. Fit
[NII] 6585/Hα
10.0
1.0
F([NII])/F(Hα)
+0.2 0.0 -0.2
X (arcsec)
0
6628 6687 6747 6806
Wavelength (Angstroms)
6865 6925 6984
[NII]/Hα
X = 0.0
0.1
−1.01 −0.34 0.34 1.01
Y (arcsec)
Figure 3.12 Observation and fit data for UGC 7115, see Figure 3.1 for description.
132

Intensity (erg s −1 cm −2 Å −1 arcsec −2 )
v r (km s −1 )
2.0•10 −14
1.5•10 −14
1.0•10 −14
5.0•10 −15
2400
2300
2200
2100
2000
0
−5.0•10 −15
Reduced 2−D Spectrum
Single Gaussian per Line Fit
v r
X = −0.1
Y (arcsec)
0.46
0.20
-0.05
-0.30
Hα+[NII] & [SII] − Narrow Line Fit
σ gas
v r
+0.1 0.0 -0.1
X (arcsec)
6503 6557 6610 6664 6718 6772 6825
Wavelength (Angstroms)
X = 0.0
X = +0.1
−0.51 −0.17 0.17 0.51
Y (arcsec)
σ gas (km s −1 )
500
400
300
200
100
0
0.5"
X = −0.1
X = 0.0
X = +0.1
−0.51 −0.17 0.17 0.51
Y (arcsec)
Intensity (erg s −1 cm −2 Å −1 arcsec −2 )
2.0•10 −14
1.5•10 −14
1.0•10 −14
5.0•10 −15
F (10 −14 ergs s −1 cm −2 Hz −1 )
45
35
25
15
5
−5
5
4
3
2
1
0
2.5
2.0
1.5
1.0
0
−5.0•10 −15
σ gas
+0.1 0.0 -0.1
X (arcsec)
[NII] 6585 Flux
X = −0.1
X = 0.0
X = +0.1
0.5
0.0
−0.51 −0.17 0.17 0.51
Y (arcsec)
F([NII] 6585)
+0.1 0.0 -0.1
X (arcsec)
Hα+[NII] & [SII] − Narrow & Broad Cpt. Fit
[NII] 6585/Hα
10.0
1.0
0.1
F([NII])/F(Hα)
+0.1 0.0 -0.1
X (arcsec)
6503 6557 6610 6664 6718 6772 6825
Wavelength (Angstroms)
[NII]/Hα
X = −0.1
X = 0.0
X = +0.1
−0.51 −0.17 0.17 0.51
Y (arcsec)
Figure 3.13 Observation and fit data for NGC 4261, see Figure 3.1 for description.
133

Intensity (erg s −1 cm −2 Å −1 arcsec −2 )
v r (km s −1 )
1.0•10 −14
8.0•10 −15
6.0•10 −15
4.0•10 −15
2.0•10 −15
5000
4800
4600
4400
Reduced 2−D Spectrum
Single Gaussian per Line Fit
v r
X = −0.2
Y (arcsec)
0.91
0.41
-0.10
-0.61
Hα+[NII] & [SII] − Narrow Line Fit
σ gas
v r
+0.2 0.0 -0.2
X (arcsec)
0
6584 6638 6691 6745
Wavelength (Angstroms)
6799 6852 6906
X = 0.0
X = +0.2
−1.01 −0.34 0.34 1.01
Y (arcsec)
σ gas (km s −1 )
300
200
100
0
0.5"
X = −0.2
X = 0.0
X = +0.2
−1.01 −0.34 0.34 1.01
Y (arcsec)
Intensity (erg s −1 cm −2 Å −1 arcsec −2 )
1.75
1.25
0.75
0.25
−0.25
−0.75
F (10 −14 ergs s −1 cm −2 Hz −1 )
1.0•10 −14
8.0•10 −15
6.0•10 −15
4.0•10 −15
2.0•10 −15
9
7
5
3
1
−1
0.9
0.7
0.5
0.3
σ gas
+0.2 0.0 -0.2
X (arcsec)
[NII] 6585 Flux
X = −0.2
X = 0.0
X = +0.2
0.1
−0.1
−1.01 −0.34 0.34 1.01
Y (arcsec)
F([NII] 6585)
+0.2 0.0 -0.2
X (arcsec)
Hα+[NII] & [SII] − Narrow & Broad Cpt. Fit
[NII] 6585/Hα
10.0
1.0
0.1
F([NII])/F(Hα)
+0.2 0.0 -0.2
X (arcsec)
0
6584 6638 6691 6745
Wavelength (Angstroms)
6799 6852 6906
[NII]/Hα
X = −0.2
X = 0.0
X = +0.2
−1.01 −0.34 0.34 1.01
Y (arcsec)
Figure 3.14 Observation and fit data for NGC 4335, see Figure 3.1 for description.
134

Intensity (erg s −1 cm −2 Å −1 arcsec −2 )
v r (km s −1 )
1.75•10 −14
1.25•10 −14
7.50•10 −15
2.50•10 −15
−2.50•10 −15
−7.50•10 −15
1400
1200
1000
800
Reduced 2−D Spectrum
Single Gaussian per Line Fit
v r
X = −0.2
Y (arcsec)
0.46
0.20
-0.05
-0.30
Hα+[NII] & [SII] − Narrow Line Fit
σ gas
v r
+0.2 0.0 -0.2
X (arcsec)
6470 6531 6592 6652 6713 6774 6835
Wavelength (Angstroms)
X = 0.0
X = +0.2
−0.51 −0.17 0.17 0.51
Y (arcsec)
σ gas (km s −1 )
1000
800
600
400
200
0
0.5"
X = −0.2
X = 0.0
X = +0.2
Intensity (erg s −1 cm −2 Å −1 arcsec −2 )
−0.51 −0.17 0.17 0.51
Y (arcsec)
F (10 −14 ergs s −1 cm −2 Hz −1 )
1.75•10 −14
1.25•10 −14
7.50•10 −15
2.50•10 −15
−2.50•10 −15
−7.50•10 −15
4.5
3.5
2.5
1.5
0.5
−0.5
40
30
20
10
0
−10
2.0
1.5
1.0
0.5
σ gas
+0.2 0.0 -0.2
X (arcsec)
[NII] 6585 Flux
X = −0.2
X = 0.0
X = +0.2
0.0
−0.5
−0.51 −0.17 0.17 0.51
Y (arcsec)
F([NII] 6585)
+0.2 0.0 -0.2
X (arcsec)
Hα+[NII] & [SII] − Narrow & Broad Cpt. Fit
[NII] 6585/Hα
10.0
1.0
0.1
F([NII])/F(Hα)
+0.2 0.0 -0.2
X (arcsec)
6470 6531 6592 6652 6713 6774 6835
Wavelength (Angstroms)
[NII]/Hα
X = −0.2
X = 0.0
X = +0.2
−0.51 −0.17 0.17 0.51
Y (arcsec)
Figure 3.15 Observation and fit data for NGC 4374, see Figure 3.1 for description.
135

Intensity (erg s −1 cm −2 Å −1 arcsec −2 )
v r (km s −1 )
4.5•10 −14
3.5•10 −14
2.5•10 −14
1.5•10 −14
5.0•10 −15
−5.0•10 −15
2000
1800
1600
1400
1200
1000
800
Reduced 2−D Spectrum
Single Gaussian per Line Fit
v r
X = −0.2
Y (arcsec)
0.46
0.20
-0.05
-0.30
Hα+[NII] & [SII] − Narrow Line Fit
σ gas
v r
+0.2 0.0 -0.2
X (arcsec)
6470 6531 6592 6652 6713 6774 6835
Wavelength (Angstroms)
X = 0.0
X = +0.2
−0.51 −0.17 0.17 0.51
Y (arcsec)
σ gas (km s −1 )
1000
800
600
400
200
0
0.5"
X = −0.2
X = 0.0
X = +0.2
−0.51 −0.17 0.17 0.51
Y (arcsec)
Intensity (erg s −1 cm −2 Å −1 arcsec −2 )
F (10 −14 ergs s −1 cm −2 Hz −1 )
4.5•10 −14
3.5•10 −14
2.5•10 −14
1.5•10 −14
5.0•10 −15
−5.0•10 −15
25
20
15
10
5
0
80
60
40
20
0
−20
17.5
12.5
7.5
2.5
σ gas
+0.2 0.0 -0.2
X (arcsec)
[NII] 6585 Flux
X = −0.2
X = 0.0
X = +0.2
−2.5
−7.5
−0.51 −0.17 0.17 0.51
Y (arcsec)
F([NII] 6585)
+0.2 0.0 -0.2
X (arcsec)
Hα+[NII] & [SII] − Narrow & Broad Cpt. Fit
[NII] 6585/Hα
10.0
1.0
0.1
F([NII])/F(Hα)
+0.2 0.0 -0.2
X (arcsec)
6470 6531 6592 6652 6713 6774 6835
Wavelength (Angstroms)
[NII]/Hα
X = −0.2
X = 0.0
X = +0.2
−0.51 −0.17 0.17 0.51
Y (arcsec)
Figure 3.16 Observation and fit data for NGC 4486, see Figure 3.1 for description.
136

Intensity (erg s −1 cm −2 Å −1 arcsec −2 )
v r (km s −1 )
2.71•10 −15
2.12•10 −15
1.54•10 −15
9.58•10 −16
3.75•10 −16
−2.08•10 −16
5000
4900
4800
4700
4600
Reduced 2−D Spectrum
Single Gaussian per Line Fit
v r
X = −0.2
Y (arcsec)
0.91
0.41
-0.10
-0.61
Hα+[NII] & [SII] − Narrow Line Fit
σ gas
v r
+0.2 0.0 -0.2
X (arcsec)
6584 6638 6691 6745 6799 6852 6906
Wavelength (Angstroms)
X = 0.0
X = +0.2
−1.01 −0.34 0.34 1.01
Y (arcsec)
σ gas (km s −1 )
250
200
150
100
50
0
0.5"
X = −0.2
X = 0.0
X = +0.2
Intensity (erg s −1 cm −2 Å −1 arcsec −2 )
−1.01 −0.34 0.34 1.01
Y (arcsec)
F (10 −14 ergs s −1 cm −2 Hz −1 )
2.71•10 −15
2.12•10 −15
1.54•10 −15
9.58•10 −16
3.75•10 −16
−2.08•10 −16
0.25
0.20
0.15
0.10
0.05
0.00
2.0
1.5
1.0
0.5
0.0
−0.5
0.25
0.20
0.15
0.10
σ gas
+0.2 0.0 -0.2
X (arcsec)
[NII] 6585 Flux
X = −0.2
X = 0.0
X = +0.2
0.05
0.00
−1.01 −0.34 0.34 1.01
Y (arcsec)
F([NII] 6585)
+0.2 0.0 -0.2
X (arcsec)
Hα+[NII] & [SII] − Narrow & Broad Cpt. Fit
[NII] 6585/Hα
10.0
1.0
0.1
F([NII])/F(Hα)
+0.2 0.0 -0.2
X (arcsec)
6584 6638 6691 6745 6799 6852 6906
Wavelength (Angstroms)
[NII]/Hα
X = −0.2
X = 0.0
X = +0.2
−1.01 −0.34 0.34 1.01
Y (arcsec)
Figure 3.17 Observation and fit data for NGC 5127, see Figure 3.1 for description.
137

Intensity (erg s −1 cm −2 Å −1 arcsec −2 )
v r (km s −1 )
5•10 −15
4•10 −15
3•10 −15
2•10 −15
1•10 −15
5500
5400
5300
5200
5100
5000
4900
Reduced 2−D Spectrum
Single Gaussian per Line Fit
v r
X = −0.2
Y (arcsec)
0.91
0.41
-0.10
-0.61
Hα+[NII] & [SII] − Narrow Line Fit
σ gas
v r
+0.2 0.0 -0.2
X (arcsec)
0
6584 6638 6691 6745
Wavelength (Angstroms)
6799 6852 6906
X = 0.0
X = +0.2
−1.01 −0.34 0.34 1.01
Y (arcsec)
σ gas (km s −1 )
300
200
100
0
0.5"
X = −0.2
X = 0.0
X = +0.2
−1.01 −0.34 0.34 1.01
Y (arcsec)
Intensity (erg s −1 cm −2 Å −1 arcsec −2 )
F (10 −14 ergs s −1 cm −2 Hz −1 )
5•10 −15
4•10 −15
3•10 −15
2•10 −15
1•10 −15
2.0
1.5
1.0
0.5
0.0
−0.5
4.5
3.5
2.5
1.5
0.5
−0.5
1.75
1.25
0.75
0.25
σ gas
+0.2 0.0 -0.2
X (arcsec)
[NII] 6585 Flux
X = −0.2
X = 0.0
X = +0.2
−0.25
−0.75
−1.01 −0.34 0.34 1.01
Y (arcsec)
F([NII] 6585)
+0.2 0.0 -0.2
X (arcsec)
Hα+[NII] & [SII] − Narrow & Broad Cpt. Fit
[NII] 6585/Hα
10.0
1.0
0.1
F([NII])/F(Hα)
+0.2 0.0 -0.2
X (arcsec)
0
6584 6638 6691 6745
Wavelength (Angstroms)
6799 6852 6906
[NII]/Hα
X = −0.2
X = 0.0
X = +0.2
−1.01 −0.34 0.34 1.01
Y (arcsec)
Figure 3.18 Observation and fit data for NGC 5141, see Figure 3.1 for description.
138

Intensity (erg s −1 cm −2 Å −1 arcsec −2 )
v r (km s −1 )
5•10 −15
4•10 −15
3•10 −15
2•10 −15
1•10 −15
6500
6000
5500
5000
4500
Reduced 2−D Spectrum
Single Gaussian per Line Fit
v r
X = −0.2
Y (arcsec)
0.91
0.41
-0.10
-0.61
Hα+[NII] & [SII] − Narrow Line Fit
σ gas
v r
+0.2 0.0 -0.2
X (arcsec)
0
6584 6638 6691 6745
Wavelength (Angstroms)
6799 6852 6906
X = 0.0
X = +0.2
−1.01 −0.34 0.34 1.01
Y (arcsec)
σ gas (km s −1 )
400
300
200
100
0
0.5"
X = −0.2
X = 0.0
X = +0.2
−1.01 −0.34 0.34 1.01
Y (arcsec)
Intensity (erg s −1 cm −2 Å −1 arcsec −2 )
F (10 −14 ergs s −1 cm −2 Hz −1 )
5•10 −15
4•10 −15
3•10 −15
2•10 −15
1•10 −15
2.25
1.75
1.25
0.75
0.25
−0.25
2.5
2.0
1.5
1.0
0.5
0.0
0.4
0.3
0.2
0.1
σ gas
+0.2 0.0 -0.2
X (arcsec)
[NII] 6585 Flux
X = −0.2
X = 0.0
X = +0.2
0.0
−0.1
−1.01 −0.34 0.34 1.01
Y (arcsec)
F([NII] 6585)
+0.2 0.0 -0.2
X (arcsec)
Hα+[NII] & [SII] − Narrow & Broad Cpt. Fit
[NII] 6585/Hα
10.0
1.0
0.1
F([NII])/F(Hα)
+0.2 0.0 -0.2
X (arcsec)
0
6584 6638 6691 6745
Wavelength (Angstroms)
6799 6852 6906
[NII]/Hα
X = −0.2
X = 0.0
X = +0.2
−1.01 −0.34 0.34 1.01
Y (arcsec)
Figure 3.19 Observation and fit data for NGC 5490, see Figure 3.1 for description.
139

Intensity (erg s −1 cm −2 Å −1 arcsec −2 )
v r (km s −1 )
7•10 −15
5•10 −15
3•10 −15
1•10 −15
−1•10 −15
−3•10 −15
4800
4600
4400
4200
4000
3800
Reduced 2−D Spectrum
Single Gaussian per Line Fit
v r
X = −0.1
Y (arcsec)
0.46
0.20
-0.05
-0.30
Hα+[NII] & [SII] − Narrow Line Fit
σ gas
v r
+0.1 0.0 -0.1
X (arcsec)
6584 6638 6691 6745 6799 6852 6906
Wavelength (Angstroms)
X = 0.0
X = +0.1
−0.51 −0.17 0.17 0.51
Y (arcsec)
σ gas (km s −1 )
500
400
300
200
100
0
0.5"
X = −0.1
X = 0.0
X = +0.1
−0.51 −0.17 0.17 0.51
Y (arcsec)
Intensity (erg s −1 cm −2 Å −1 arcsec −2 )
F (10 −14 ergs s −1 cm −2 Hz −1 )
7•10 −15
5•10 −15
3•10 −15
1•10 −15
−1•10 −15
−3•10 −15
9
7
5
3
1
−1
9
7
5
3
1
−1
2.0
1.5
1.0
0.5
σ gas
+0.1 0.0 -0.1
X (arcsec)
[NII] 6585 Flux
X = −0.1
X = 0.0
X = +0.1
0.0
−0.5
−0.51 −0.17 0.17 0.51
Y (arcsec)
F([NII] 6585)
+0.1 0.0 -0.1
X (arcsec)
Hα+[NII] & [SII] − Narrow & Broad Cpt. Fit
[NII] 6585/Hα
10.0
1.0
0.1
F([NII])/F(Hα)
+0.1 0.0 -0.1
X (arcsec)
6584 6638 6691 6745 6799 6852 6906
Wavelength (Angstroms)
[NII]/Hα
X = −0.1
X = 0.0
X = +0.1
−0.51 −0.17 0.17 0.51
Y (arcsec)
Figure 3.20 Observation and fit data for NGC 7052, see Figure 3.1 for description.
140

Intensity (erg s −1 cm −2 Å −1 arcsec −2 )
v r (km s −1 )
8•10 −15
6•10 −15
4•10 −15
2•10 −15
5300
5200
5100
5000
4900
4800
0
−2•10 −15
Reduced 2−D Spectrum
Single Gaussian per Line Fit
v r
X = −0.1
Y (arcsec)
0.46
0.20
-0.05
-0.30
Hα+[NII] & [SII] − Narrow Line Fit
σ gas
v r
+0.1 0.0 -0.1
X (arcsec)
6584 6638 6691 6745 6799 6852 6906
Wavelength (Angstroms)
X = 0.0
X = +0.1
−0.51 −0.17 0.17 0.51
Y (arcsec)
σ gas (km s −1 )
600
400
200
0
0.5"
X = −0.1
X = 0.0
X = +0.1
−0.51 −0.17 0.17 0.51
Y (arcsec)
Intensity (erg s −1 cm −2 Å −1 arcsec −2 )
F (10 −14 ergs s −1 cm −2 Hz −1 )
8•10 −15
6•10 −15
4•10 −15
2•10 −15
2.5
2.0
1.5
1.0
0.5
0.0
22.5
17.5
12.5
7.5
2.5
−2.5
4.5
3.5
2.5
1.5
0
−2•10 −15
σ gas
+0.1 0.0 -0.1
X (arcsec)
[NII] 6585 Flux
X = −0.1
X = 0.0
X = +0.1
0.5
−0.5
−0.51 −0.17 0.17 0.51
Y (arcsec)
F([NII] 6585)
+0.1 0.0 -0.1
X (arcsec)
Hα+[NII] & [SII] − Narrow & Broad Cpt. Fit
[NII] 6585/Hα
10.0
1.0
0.1
F([NII])/F(Hα)
+0.1 0.0 -0.1
X (arcsec)
6584 6638 6691 6745 6799 6852 6906
Wavelength (Angstroms)
[NII]/Hα
X = −0.1
X = 0.0
X = +0.1
−0.51 −0.17 0.17 0.51
Y (arcsec)
Figure 3.21 Observation and fit data for UGC 12064, see Figure 3.1 for description.
141

Intensity (erg s −1 cm −2 Å −1 arcsec −2 )
v r (km s −1 )
8•10 −15
6•10 −15
4•10 −15
2•10 −15
3800
3600
3400
3200
0
−2•10 −15
Reduced 2−D Spectrum
Single Gaussian per Line Fit
v r
X = −0.2
Y (arcsec)
0.91
0.41
-0.10
-0.61
Hα+[NII] & [SII] − Narrow Line Fit
σ gas
v r
+0.2 0.0 -0.2
X (arcsec)
6584 6638 6691 6745 6799 6852 6906
Wavelength (Angstroms)
X = 0.0
X = +0.2
−1.01 −0.34 0.34 1.01
Y (arcsec)
σ gas (km s −1 )
400
300
200
100
0
0.5"
X = −0.2
X = 0.0
X = +0.2
−1.01 −0.34 0.34 1.01
Y (arcsec)
Intensity (erg s −1 cm −2 Å −1 arcsec −2 )
F (10 −14 ergs s −1 cm −2 Hz −1 )
8•10 −15
6•10 −15
4•10 −15
2•10 −15
0.8
0.6
0.4
0.2
0.0
−0.2
9
7
5
3
1
−1
0.9
0.7
0.5
0.3
0
−2•10 −15
σ gas
+0.2 0.0 -0.2
X (arcsec)
[NII] 6585 Flux
X = −0.2
X = 0.0
X = +0.2
0.1
−0.1
−1.01 −0.34 0.34 1.01
Y (arcsec)
F([NII] 6585)
+0.2 0.0 -0.2
X (arcsec)
Hα+[NII] & [SII] − Narrow & Broad Cpt. Fit
[NII] 6585/Hα
10.0
1.0
0.1
F([NII])/F(Hα)
+0.2 0.0 -0.2
X (arcsec)
6584 6638 6691 6745 6799 6852 6906
Wavelength (Angstroms)
[NII]/Hα
X = −0.2
X = 0.0
X = +0.2
−1.01 −0.34 0.34 1.01
Y (arcsec)
Figure 3.22 Observation and fit data for NGC 7626, see Figure 3.1 for description.
142

Difference in mean velocity on each side of nucleus (km s -1 )
1000
800
600
400
200
0 100 200 300 400 500
Mean gas velocity dispersion (km s -1 0
)
Figure 3.23 Difference in mean velocity within 100 pc of each side of the nucleus
(∆100pc, see text) as a function of the mean gas velocity dispersion within 100 pc
of the nucleus (σ100pc). The different kinematic classes and dust morphologies are
indicated. Filled symbols represent rotators: with dust disks (•), with dust lanes
(�) or with irregular dust (�); Empty symbols represent non-rotators: with dust
disks (◦), with dust lanes (�) or with no-dust or irregular dust (△). The solid line
is the 1:1 ratio between ∆100pc and σ100pc, indicating regions where organized motions
(above the line) or random motions (below the line) dominate.
143

Difference in mean velocity on each side of nucleus (km s -1 )
1000
800
600
400
200
0
0.0 0.2 0.4 0.6 0.8 1.0
Axis Ratio (b/a or width:length)
Figure 3.24 Difference in mean velocity within 100 pc of each side of the nucleus
(∆100pc, see text) as a function of dust disk axis ratio (b/a) or dust lane width : length
ratio, which is an indicator of inclination. The different kinematic classes and dust
morphologies are indicated. Filled symbols represent rotators: with dust disks (•),
with dust lanes (�) or with irregular dust (�); Empty symbols represent non-rotators:
with dust disks (◦), with dust lanes (�) or with no-dust or irregular dust (△). The
solid lines are loci for disks with the same intrinsic ∆100pc (990, 680 and 360 km s −1 )
viewed at inclinations projected assuming b/a = sin i (i.e. a circular disk).
144

Mean velocity dispersion (km s -1 )
500
400
300
200
100
0
0.0 0.2 0.4 0.6 0.8 1.0
Axis Ratio (b/a or width:length)
Figure 3.25 Mean gas velocity dispersion within 100 pc of the nucleus (σ100pc) as a
function of dust disk axis ratio (b/a) or dust lane width : length ratio, which is an
indicator of inclination. The different kinematic classes and dust morphologies are
indicated. Filled symbols represent rotators: with dust disks (•), with dust lanes
(�) or with irregular dust (�); Empty symbols represent non-rotators: with dust disks
(◦), with dust lanes (�) or with no-dust or irregular dust (△).
145

[N II] Flux
10 -12
10 -13
10 -14
10 -15
10 -15
10 -14
Hα Flux
10 -13
146
10 -12
Figure 3.26 [N II] against Hα fluxes for the UGC FR-I sample members. Formal errors
in the fluxes are shown. The shading of the symbols indicates the score assigned to
the broad component in each case (see text). A score of 3 (most confident) is shown
by black symbols, through to white symbols for a score of zero (no confidence in a
broad line). It is possible to see a trend with flux from less to more confidence in
broad-line detection.

Chapter 4
Modeling gas in gravitational
potentials
4.1 Introduction
Spectroscopic observations from the Hubble Space Telescope have made it possible
to attempt to measure the black hole masses in the centers of nearby galaxies using
stellar and gas kinematics (see Chapter 1). The black hole masses correlate somewhat
with the host luminosity, and more tightly with the inner velocity dispersion of the
stars (‘inner’ refers to inside the effective radius (Chapter 2), but still on much larger
scales than the region we describe as ‘central’ or ‘nuclear’ through this thesis). In
Chapter 3 we presented spectroscopic observations of the emission line gas in the
nuclear regions of our sample of 21 nearby radio-galaxies (Chapter 2). Here, we may
try to learn more about those data by comparing our observational results to models
147

for the gravitational potential from the stars and prospective nuclear black holes in
each galaxy.
In this chapter we present the techniques used to create model velocity profiles
for each set of observations including the stars, and black holes with masses of 0,
1 × 10 8 M⊙ and 9 × 10 8 M⊙. We go on to discuss the models for each galaxy and
compare the predicted kinematic signatures including the presence of supermassive
black holes to the observed gas velocity profiles presented in Chapter 3.
An important drawback of the approach of measuring black hole masses by using
gas kinematics is that the gas dynamics may be affected by many non-gravitational
sources and the gravitational motions may not be settled into a coplanar thin disk.
We describe any such motions as ‘unsettled’. In §4.4.3 we will discuss some non-
gravitational sources of kinetic energy in the gas and the consequences of unsettled
motions for the determination of black hole masses. We do not produce model fits for
each galaxy because, as we will see, a large proportion of the gas motion can not be
described by simple circular-thin-disk rotation, rendering such fits difficult constrain
and impossible to interpret meaningfully.
148

4.2 Thin disk models with and without a black
hole
We have created model velocity profiles assuming that the emission line gas that we
observe originates from a thin rotating circular disk in each nucleus. This assumption
matches our findings that the gas can be explained by a rotating system as we showed
in Chapter 3; however, the large velocity dispersions that we measure indicate that
the assumption that the disk is thin may not be very reliable. Yet for the purposes of
modeling this assumption is necessary: to enable first steps to be made and to give
us some handle on explanations of the nuclear gas dynamics.
We use modeling techniques very similar to those described by van der Marel &
van den Bosch (1998) and Verdoes Kleijn et al. (2002b) to generate velocity profiles
along the observed slits for gas sitting in the gravitational potential generated by the
stellar population of the galaxy and including (i) no black hole, (ii) a 1 × 10 8 M⊙
black hole and (iii) a 9×10 8 M⊙ black hole, and taking into account the instrumental
PSF. These values of black hole mass are in the range typically conjectured for the
nuclei of galaxies of this size, and we would not expect to resolve black holes of less
than ∼ 1 ×10 8 M⊙ at the distances of the majority of the galaxies in our sample. We
assume that the galaxy is at a distance D = v/H0, where v is the mean recessional
149

velocity as given earlier in Table 2.1.
4.2.1 WFPC2 imaging: stars and dust
Each galaxy was observed during HST program GO-6673 using the Wide Field and
Planetary Camera - 2 (WFPC2) instrument (described in, e.g. Trauger, 1994; Biretta,
1996) on the Hubble Space Telescope. Observations and reduction are described by
Verdoes Kleijn et al. (1999) (and also in Appendix A of Verdoes Kleijn et al., 2002a,
for UGC 7115 and UGC 12064). Observations were obtained using wide band filters
approximating the V (F555W or F547M) and I (F814W or F791W) bands, along with
a narrow band image obtained using a linear ramp filter.
Verdoes Kleijn et al. (1999) fitted an elliptical contour to the outline of the dust
disk in each case to find the position angles of the dust disks, which were listed
earlier in Table 3.3. We assume that the gas and dust disks are coincident (this is
consistent with the observations of the dust and the narrow band Hα+ [N II]), and
that they coincide with the major axis of the galaxy and define the major plane. This
final assumption seems reasonable based on the position angles for the majority of
galaxies, however there are some cases where this may not be a fair assumption to
make about the disk as we see large differences in the dust and galaxy position angles
(e.g. NGC 3801, NGC 4374, NGC 5490 and UGC 7115). Inclinations for the dust
150

gas disks were computed by making a circular thin disk assumption and deriving
the inclination angle from the observed axis ratio of the dust. For the galaxies with
dust lanes, inclinations were set at 80 ◦ (we do not observe disks below about 70 ◦ ,
which we interpret of the lower limit of the range of inclinations in systems where we
see lanes). The measured axis ratios and derived inclinations are given in Table 4.1,
along with dust masses.
4.2.2 Flux distributions
To model the observed gas kinematics we first need a description of the intrinsic
emission line flux distribution, for which we make use of the flux profiles obtained
from the Gaussian fits to our STIS spectroscopic results that we presented in Chapter
3, Tables 3.5 to 3.25. We model the face on flux profile as a double exponential,
151
F(R) = F1e −R/R1 + F2e −R/R2 , (4.1)
deriving the parameters assuming an infinitesimally thin disk, inclined at the angle
given in Table 4.1. We iterate a fit of the double exponential to the flux data, taking
into account the flux errors and convolution with the STIS PSF, aperture size and
pixel size.
The STIS PSF was represented by a combination of five Gaussians which represent

the PSF as
PSF(r) =
5�
γi
i=1 2πσ2 i
152
e −1
� �2 r
2 σi . (4.2)
The parameters γi, and σi were obtained by fitting the STIS PSF using the Tiny
Tim software (Krist & Hook, 1999) and are listed in Table 4.2. Differences between
the actual PSF and the analytical fit cause differences in the modeled kinematics
that are smaller than the errors in the data. We tested this by repeating all modeling
using a single Gaussian component to represent the PSF (see Section 4.2.6).
4.2.3 Stellar luminosity densities and mass distributions
For the purposes of the dynamical modeling we use a three-dimensional parameteri-
zation of the stellar luminosity density (j). We assume that j is oblate and axisym-
metric, i.e. there are isoluminosity spheroids with constant flattening q as a function
of radius, and that j can be parameterized as
j(R, z) = j0(m/a) α [1 + (m/a) 2 ] β , (4.3)
m 2 ≡ R 2 + (z/q) 2
(4.4)
Where R and z are cylindrical coordinates from the major plane of the galaxy. α, β,
a and j0 are free parameters. When viewed at an inclination angle i, the projected

intensity contours are aligned concentric ellipses with an axial ratio
153
q ′ ≡ cos 2 i + q 2 sin 2 i. (4.5)
Values of q ′ , measured from the ellipticity of the isophotes in the WFPC2 images,
are also listed in Table 4.1. Though the values of q ′ , and of the position angle of the
major axis of the isophotes varies over the region in which we are interested (Verdoes
Kleijn et al., 1999), we do not expect this to have a significant impact on the results
we derive (see Verdoes Kleijn et al., 2002b, and Section 4.2.6 below).
We determined the mean stellar flux profiles in the direction along the semi-
minor axis with least dust obscuration, in the reddest image observed by WFPC2
(to minimize the effects of both dust and emission lines) for each galaxy. We then
iteratively fit the model parameters to obtain the best fitting values for the parameters
α, β, a and j0, these are shown in Table 4.3.
We assume that the stellar mass density ρ(R, z) follows the luminosity density
distribution j(R, z) through a constant mass to light ratio (Υ) towards the center of
the galaxy. No conclusive data exist about how Υ may change towards the center,
though we observe changes in (V −I) (Verdoes Kleijn et al., 1999), much of this may
be attributed to dust rather than to changes in the stellar population. The fit is not
incredibly sensitive to this parameter until some distance from the nucleus where the

errors on the observed data preclude us for making any strong statements about the
fit in any case. Abnormally high values of Υ would be required to change the modeled
velocity profiles in the central regions, and we find this scenario somewhat unlikely.
Magorrian et al. (1998) give the relation shown in Equation 4.6 below as their
best fit to the V band mass-to-light ratio (ΥVgal ) for an early type galaxy with a given
absolute magnitude (MVgal ). We use the standard relation based on Equation 2.45
of Binney & Merrifield (1998) to convert the mass-to-light ratio from the V to the I
band (Equation 4.7).
154
ΥVgal = 10−1.11+0.072(MV ⊙ −MV gal )
, (4.6)
ΥIgal = ΥVgal100.4[(V −I) −(V −I)gal] ⊙
(4.7)
We take values of (V −I)⊙ = 0.71; MV ⊙ = 4.77. Input data and calculated values
of these parameters are shown in Table 4.4. We choose to use ΥIgal
as the I-band
stellar isophotes reduce the effects of dust on our results. For galaxies where we do
not have all of the necessary observational data to determine Υ we use a typical value
for early type galaxies of ΥIgal = 3.5. (The mean value for our sample galaxies where
we can find Υ is ΥIgal = 4.1, slightly higher but compatible with this value).

4.2.4 Dynamical models
As discussed above we assume that the gas is organized into an infinitesimally thin,
settled, rotating disk which is located in the major (equatorial) plane of the galaxy,
with a circularly symmetric flux distribution, F(R), as given in Section 4.2.2. The
inclinations of the dust and gas are again assumed to be identical and were determined
as discussed earlier; the major axis was assumed to lie along the major axis of the
galaxy, as the model requires a coplanar system.
For each galaxy we generate three models where we compute the circular velocity
Vc(R) from the combined gravitational potential of the stars with a black hole with
mass M• = 0, 1 × 10 8 M⊙, and 9 × 10 8 M⊙. The line of sight velocity profile of the
gas at position (x, y) on the sky is a Gaussian with
where
155
Mean = Vc(R) sin(ix/R), and (4.8)
Sigma = σgas(R), (4.9)
R = [x 2 + (y/ cosi) 2 ] 1/2
(4.10)
is the radius in the disk. We assume an isotropic model for the velocity dispersion,

with contributions from thermal and non-thermal motion:
156
σ 2 gas = σ2 th + σ2 tur , (4.11)
σ 2 tur(R) = σt0 + σt1e −R/R1 . (4.12)
We label the non-thermal motion as ‘turbulent’ but this is merely a label and
does not imply a source of the non-thermal motions. This functional form is used
only so that we may provide a fit to the observed dispersion, and is not based on
any underlying physical mechanism. The temperature of the gas is not important.
For T ∼ 10 4 K, σth ∼ 10 km s −1 which is always negligible in comparison to σtur.
The intrinsic line width is the dominant source of line broadening in the data, so
we can fix values for the line widths from the above parameterization alone; models
with different black hole masses and hence different amounts of rotational broadening
will still have about the same final line widths because the intrinsic line width is
significantly larger than the rotational broadening at most locations, and the different
sources of broadening effectively add in quadrature (see Barth et al., 2001).
The predicted velocity profile for any given observation is obtained through a flux
weighted convolution of the intrinsic velocity profile with the PSF of the observation
and the size of the aperture (van der Marel & van den Bosch, 1998). Again the PSF is
represented by a sum of five Gaussians (see above, and Table 4.2). The convolutions

are described in Appendix A of van der Marel (1997) and were performed using Gauss-
Legendre integration. A Gaussian is then fitted to each observed velocity profile. In
this way we produce three model data sets (with three different black hole masses)
that we may directly compare to the observed velocity data from Chapter 3.
Some weaknesses exist in the modeling methodology we have adopted, particu-
larly in the manner in which the flux profile across the slit is accounted for. These are
discussed more fully by van der Marel & van den Bosch (1998) and Verdoes Kleijn
et al. (2002b), and some improvements that may be made are discussed (and imple-
mented) by Barth et al. (2001). However, these factors are small compared to the
smoothness of the observed velocity profiles, so we need not concern ourselves with
these details in our discussions here. Because of the unsettled nature of much of the
observed velocity profiles we feel that it would be inappropriate to attempt to find
‘best fitting’ models, when we do not understand the majority of the motions in the
gas.
4.2.5 Locating the zero point velocities
In order to compare the observed velocity field to the model predictions we must
also account for the recessional velocity of the galaxy in the observations. The mean
recessional velocity of the galaxy may vary somewhat from the mean value from
157

various sources as quoted in Table 2.1. The sense of the rotation along the major
axis is also a free parameter at this point (whether the velocities go from positive to
negative, or negative to positive across the nucleus). For the majority of our sample
stellar dynamics are not available, and if they were it is not necessarily clear that the
gas closest to the nucleus must as a matter of course be rotating in the same direction
as the stars.
To fit both of these variables, we found the minimum in the signal-to-noise
weighted residuals between the observations and all three of the models, for both
senses of the velocity. In Figures 4.1 to 4.18 we plot these values for various devi-
ations of the recessional velocities from the quoted means and clear minima can be
seen, which we take to be a reliable way of determining the recession velocity. In
Table 4.5 the offset velocities (from the values in Table 2.1) are listed, along with an
indication of the sense of the direction of the rotation.
4.2.6 Sensitivity to parameters
The fit of the disk flux profile F(R) is the most sensitive to numerical noise and
leaves noticeable effects (‘numerical ringing’) in the output velocity profiles when
not properly modeled. We found it necessary to work in double precision for all
calculations at this stage in order to produce numerically stable results. We ran
158

models integrating using 150 by 150 Gauss-Legendre quadrature (GL) points (see
Press et al., 1992), we found that increasing the number of grid points beyond this
limit had no effect on the result - indicating to us that it is numerically stable. Again,
150 by 150 GL points were used to compute the velocity profiles, and found this to
be numerically stable also (even with lower values in this case).
We tested the effect of changing the STIS PSF by repeating the models using a
single Gaussian (γ1 = 1.00, σ1 = 0.0327) to represent the PSF instead of the sum
of five Gaussians. In Figure 4.19 we over-plot the results for the M• = 1 × 10 8 M⊙
model for NGC 193 with each PSF, to illustrate that the differences are insignificant
compared to the random variations in the observed velocity profile. This is the case
for all galaxies other than M84 and M87 which are much closer to us and so the PSF
becomes an important factor in these models.
Maciejewski & Binney (2001) explain many important difficulties that may be
encountered when modeling spectra of galaxies obtained through a ‘wide’ slit. In
this context wide may be judged by the steepness of the central velocity profile and
the size of the instrumental PSF. They found that the struggle between real velocity
differences within an object and offsets in velocity that arise because light is entering
the slit from different positions and at different angles can cause the intensity of
159

light on the detector to have more than one peak, leading to potentially misleading
phenomena in the velocity profiles. The effects become more pronounced if the slit is
not well aligned with a kinematic axis.
Features due to the effects that Maciejewski & Binney (2001) describe are clearly
present in the closest examples that we observed: M84 and M87. In M87 two obser-
vations were made offset by ∼ 0.1 pixels, which produced very different features in
the spectral rows closest to the nucleus (Figure 4.20). This highlights two problems:
(i) that it is essential to know the location of the center of the galaxy, on smaller
scales than the size of the spectroscopic slit, and (ii) fine details in flux weighting
the observed velocities through the PSF may make large differences to the modeled
velocity profiles - especially in nearby cases.
We tested the effects of varying the mass to light ratio (Υ), axis ratio (q ′ ) and
inclination angle (i) for two representative galaxies: NGC 193 (Figure 4.21) and
NGC 4335 (Figure 4.22). It is clear from those figures that the sensitivity to these
parameters is quite low, particularly in the central region where we expect the models
to best match the gas velocity profiles. Outside of the central region more variation
is apparent, but this is generally smaller than the point-to-point variations in the
velocity profile, so would not influence any conclusions drawn from these data and
160

models. Pronounced differences can be produced by differences in the angle of the
slits compared to the kinematic major axis of the gas. This may pose problems in
morphologically complex systems where we have no way of a priori determining the
kinematic axes.
4.3 Descriptions of individual galaxies
For each galaxy we compare the three models we obtained for 0, 1 × 10 8 M⊙ and
9 × 10 8 M⊙ black holes to the observed velocities in all three slits. We do not model
UGC 7115 (where we only have one spectroscopic slit, and relatively low signal to
noise), nor NGC 3801 (where we are clearly not on the nucleus and not aligned with
the kinematic axis). We present the results in Figures 4.23 to 4.41 and describe each
galaxy in turn below.
NGC 193: This S0 galaxy has a complex dust morphology with two distinct dust
systems clearly visible. The STIS slits were aligned parallel to the galaxy major axis,
which is also almost perpendicular to the radio jets. The weighted mean observation
- model residuals are plotted in Figure 4.1 and gives a minimum at an offset of
47 km s −1 , equivalent to a galaxy recessional velocity of 4390 km s −1 . The model
velocity profiles for these observations are shown in Figure 4.23, two plots are shown,
161

as an alternative fit by eye provides a more satisfactory description of the very central
kinematics. In the observed velocity profile a central velocity gradient is observed
which seems as if it may correspond to gas rotating in the potential generated by
a 1 × 10 8 M⊙ < M• < 9 × 10 8 M⊙ black hole. Further from the nucleus the gas
appears to have a flat velocity profile, possibly indicating that the rotation of this gas
is not along this axis. Two dimensional mapping of the velocity field would make it
possible to determine if this gas was in a kinematic system related to the secondary
dust component. There is a possible sign of a jet-disk interaction in the velocity field
of this galaxy which is described in §4.43 below.
NGC 315: This elliptical galaxy has a nuclear dust disk. The STIS slits were
aligned parallel to the galaxy major axis, which is almost coincident with the dust
disk axis. The weighted mean observation - model residuals are plotted in Figure 4.2
and gives a minimum at an offset of −137 km s −1 , equivalent to a galaxy recessional
velocity of 4956 km s −1 . The model velocity profiles for these observations are shown
in Figure 4.24. It is not clear that the modeled velocity profiles match any of the
observed kinematics in the nuclear region.
162

NGC 383: This S0 galaxy has a nuclear dust disk. The STIS slits were aligned
parallel to the galaxy major axis, 6 ◦ from the dust disk axis. The weighted mean
observation - model residuals are plotted in Figure 4.3 and gives a minimum at an
offset of 120 km s −1 , equivalent to a galaxy recessional velocity of 5010 km s −1 . The
model velocity profiles for these observations are shown in Figure 4.25. In the ob-
served velocity profile a central velocity gradient is observed which seems as if it may
correspond to gas rotating in the potential generated by a M• > 9 × 10 8 M⊙ black
hole, though the situation is very unclear, a second plot is shown which represents
more closely the profile in the very central few spectra, but provides a less good fit
in the outer parts.
NGC 541: This cD S0 galaxy has a nuclear dust disk. The STIS slits were aligned
to a mean of the position angles of the central isophotes measured from the WFPC2
images, which vary considerably. The dust disk is almost round so no dust axis can
be defined. The weighted mean observation - model residuals are plotted in Figure
4.4 and gives a minimum at an offset of 70 km s −1 , equivalent to a galaxy recessional
velocity of 5428 km s −1 . The model velocity profiles for these observations are shown
in Figure 4.26. It is not clear that the modeled velocity profiles match any of the
observed kinematics in the nuclear region.
163

NGC 741: This E0 galaxy has no apparent nuclear dust. The STIS slits were
aligned approximately parallel to the galaxy major axis. The weighted mean obser-
vation - model residuals are plotted in Figure 4.5 and gives a minimum at an offset
of 30 km s −1 , equivalent to a galaxy recessional velocity of 5295 km s −1 . The model
velocity profiles for these observations are shown in Figure 4.27. It is not clear that
the modeled velocity profiles match any of the observed kinematics in the nuclear
region.
UGC 1841: This elliptical galaxy has a nuclear dust disk. The STIS slits were
aligned parallel to the galaxy major axis. The dust disk is almost round, so no dust
axis can be defined. The weighted mean observation - model residuals are plotted
in Figure 4.6 and gives a minimum at an offset of 0 km s −1 , equivalent to a galaxy
recessional velocity of 6360 km s −1 . The model velocity profiles for these observations
are shown in Figure 4.28. It is not clear that the modeled velocity profiles match any
of the observed kinematics in the nuclear region.
NGC 2329: This S0 galaxy has a nuclear dust disk. The STIS slits were aligned
parallel to the galaxy major axis, which is 3 ◦ from the dust disk axis. The weighted
mean observation - model residuals are plotted in Figure 4.7 and gives a minimum
164

at an offset of 80 km s −1 , equivalent to a galaxy recessional velocity of 5805 km s −1 .
The model velocity profiles for these observations are shown in Figure 4.29. It is not
clear that the modeled velocity profiles match any of the observed kinematics in the
nuclear region. A dip in the velocity is observed in one side slit at the position closest
to the nucleus, and there is some sign of a peak in the other side slit profile. This
may support an inflow or outflow model for the disk.
NGC 2892: This elliptical galaxy has no apparent nuclear dust. The STIS slits
were aligned approximately parallel to the galaxy major axis. The weighted mean
observation - model residuals are plotted in Figure 4.8 and gives a minimum at an
offset of 37 km s −1 , equivalent to a galaxy recessional velocity of 6847 km s −1 . The
model velocity profiles for these observations are shown in Figure 4.30. It is not clear
that the modeled velocity profiles match any of the observed kinematics in the nuclear
region.
NGC 3862: This elliptical galaxy has a nuclear dust disk. The STIS slits were
aligned approximately perpendicular to the radio jets. The dust disk is almost round,
so no dust axis can be defined. The weighted mean observation - model residuals are
plotted in Figure 4.9 and gives a minimum at an offset of 160 km s −1 , equivalent to
165

a galaxy recessional velocity of 6490 km s −1 . The model velocity profiles for these
observations are shown in Figure 4.31. It is not clear that the modeled velocity profiles
match any of the observed kinematics in the nuclear region.
NGC 4261: This E2-3 galaxy has a nuclear dust disk. The STIS slits were aligned
parallel to the galaxy major axis, 5 ◦ from the dust disk axis. Due to a pointing error,
the center of the galaxy was not positioned well during the observations and fell closest
to one of the side slits. We are unable to constrain where the center fell precisely,
however we show the model velocity profiles for the observations in that side slit alone
in Figure 4.32. In the observed velocity profile a central velocity gradient is observed
which seems as if it may correspond to gas rotating in the potential generated by a
∼ 1 × 10 8 M⊙ black hole. We take this to be a lower limit on the mass as the galaxy
nucleus may be beyond the observed slit positions.
NGC 4335: This elliptical galaxy has a nuclear dust disk. The STIS slits were
aligned parallel to the galaxy major axis, 11 ◦ from the dust disk axis. The weighted
mean observation - model residuals are plotted in Figure 4.10 and gives a minimum
at an offset of 50 km s −1 , equivalent to a galaxy recessional velocity of 4723 km s −1 .
The model velocity profiles for these observations are shown in Figure 4.33. The
166

gas velocities are very well settled into a smooth rotation curve, however no nuclear
black hole is necessary to explain the observed kinematics. There is a possible sign
of a jet-disk interaction in the velocity field of this galaxy which is described in §4.43
below.
M84: This E1 galaxy has nuclear dust lane. The STIS slits were aligned approx-
imately perpendicular to the radio jets, 25 ◦ from the dust lane axis. The weighted
mean observation - model residuals are plotted in Figure 4.11 and gives a minimum
at an offset of −83 km s −1 , equivalent to a galaxy recessional velocity of 1072 km s −1 .
The model velocity profiles for these observations are shown in Figure 4.34. In the
observed velocity profile a central velocity gradient is observed which seems as if it
may correspond to gas rotating in the potential generated by a M• > 9×10 8 M⊙ black
hole. The proximity of this galaxy highlights many of the problems in interpreting
spectra from nearby sources where the steep flux profile becomes more resolved and
issues relating to the PSF and precise positioning of the slits (which is not known)
become important (see also Maciejewski & Binney, 2001).
NGC 4486: This elliptical galaxy has an irregular nuclear dust morphology. The
STIS slits were aligned to trace morphological features in the emission line gas. The
167

weighted mean observation - model residuals are plotted in Figure 4.12 and gives
a minimum at an offset of 63 km s −1 , equivalent to a galaxy recessional velocity
of 1218 km s −1 . The model velocity profiles for these observations are shown in
Figure 4.35. In the observed velocity profile a central velocity gradient is observed
which seems as if it may correspond to gas rotating in the potential generated by
a M• > 9 × 10 8 M⊙ black hole. The proximity of this galaxy highlights many of
the problems in interpreting spectra from nearby sources where the steep flux profile
becomes more resolved and issues relating to the PSF and precise positioning of the
slits (which is not known) become important (see also Maciejewski & Binney, 2001).
NGC 5127: This elliptical peculiar galaxy has a nuclear dust lane. The STIS slits
were aligned parallel to the galaxy major axis, 20 ◦ from the dust axis. The weighted
mean observation - model residuals are plotted in Figure 4.13 and gives a minimum
at an offset of 7 km s −1 , equivalent to a galaxy recessional velocity of 4837 km s −1 .
The model velocity profiles for these observations are shown in Figure 4.36. In the
observed velocity profile a central velocity gradient is observed which seems as if it
may correspond to gas rotating in the potential generated by a 1 × 10 8 M⊙ < M• <
9 × 10 8 M⊙ black hole.
168

NGC 5141: This S0 galaxy has a nuclear dust lane. The STIS slits were aligned
parallel to the galaxy major axis, 16 ◦ from the dust axis. The weighted mean obser-
vation - model residuals are plotted in Figure 4.14 and gives a minimum at an offset
of −50 km s −1 , equivalent to a galaxy recessional velocity of 5253 km s −1 . The model
velocity profiles for these observations are shown in Figure 4.37. The gas velocities
are very well settled into a smooth rotation curve, however no nuclear black hole is
necessary to explain the observed kinematics.
NGC 5490: This elliptical galaxy has a nuclear dust lane. The STIS slits were
aligned parallel to the galaxy major axis, 43 ◦ from the dust disk axis. The weighted
mean observation - model residuals are plotted in Figure 4.15 and gives a minimum
at an offset of −93 km s −1 , equivalent to a galaxy recessional velocity of 5697 km s −1 .
The model velocity profiles for these observations are shown in Figure 4.38. It is not
clear that the modeled velocity profiles match any of the observed kinematics in the
nuclear region. The fact that the dust disk and galaxy major axis are not coincident
by a sizeable angle also means that it is not clear what plane the gas will lie in, images
of the emission line disks (Verdoes Kleijn et al., 1999) do not make this any clearer.
169

NGC 7052: This elliptical galaxy has a nuclear dust disk. The STIS slits were
aligned parallel to the galaxy major axis, 1 ◦ from the dust disk axis. The weighted
mean observation - model residuals are plotted in Figure 4.16 and gives a minimum
at an offset of 280 km s −1 , equivalent to a galaxy recessional velocity of 4435 km s −1 .
The model velocity profiles for these observations are shown in Figure 4.39. Two
plots are shown as the velocity offset in this case was dominated by a large jump (∼
1000 km s −1 ) in the observed profile, the second plot shows an offset that best matches
the very central region. In the observed velocity profile a central velocity gradient
is observed which seems as if it may correspond to gas rotating in the potential
generated by a 1 × 10 8 M⊙ < M• < 9 × 10 8 M⊙ black hole. The nature of the second
velocity system is unknown, and generates far greater consequences for the velocity
than the potential nuclear black hole.
UGC 12064: This S0 galaxy has a nuclear dust disk. The STIS slits were aligned
parallel to the dust disk major axis. The weighted mean observation - model residuals
are plotted in Figure 4.17 and gives a minimum at an offset of −83 km s −1 , equivalent
to a galaxy recessional velocity of 5040 km s −1 . The model velocity profiles for these
observations are shown in Figure 4.40. It is not clear that the modeled velocity
profiles match any of the observed kinematics in the nuclear region, though they may
170

e compatible with a ∼ 9 × 10 8 M⊙. The very steep slope in the negative offset
slit may indicate that the position of the dynamical center is not coincident by the
center of the galaxy’s flux distribution (e.g. obscuration by nuclear dust). There is
a possible sign of a jet-disk interaction in the velocity field of this galaxy which is
described in §4.43 below.
NGC 7626: This elliptical peculiar galaxy has a nuclear dust lane. The STIS
slits were aligned parallel to the galaxy major axis, 4 ◦ from the dust disk axis. The
weighted mean observation - model residuals are plotted in Figure 4.18 and gives
a minimum at an offset of −47 km s −1 , equivalent to a galaxy recessional velocity
of 3448 km s −1 . The model velocity profiles for these observations are shown in
Figure 4.41. In the observed velocity profile a central velocity gradient is observed
which seems as if it may correspond to gas rotating in the potential generated by a
1 × 10 8 M⊙ < M• < 9 × 10 8 M⊙ black hole. Away from the nucleus a clear twist in
the velocities can be seen, suggesting the gas moves into a distinct second system at
larger radii. There is a possible sign of a jet-disk interaction in the velocity field of
this galaxy which is described in §4.43 below.
171

4.4 Discussion
In this section we will first discuss the central kinematics of each galaxy and compare
the black hole signatures that we observe to the predictions of the M − σ relation.
Next we will discuss the settling of gas into a thin disks in ellipticals and finally talk
about some sources of unsettled motions in this family of galaxies.
4.4.1 Description of the central kinematics
In some of the cases described above it is possible to attribute some of the observed
motion in the gas to the presence of a supermassive black hole. Table 4.6 summa-
rizes the galaxies status regarding possible black hole signatures, as described in the
previous section.
In 6 of the 19 galaxies the modeled velocity profile gives no clear results as the
non-rotational motions in the gas are too great. For 4 of the 13 remaining galaxies
we observe a signature compatible with a black hole in the range 1 × 10 8 M⊙ <
M• < 9 × 10 8 M⊙, for 5 we observe kinematic signatures that are compatible with
M• ∼ > 9 × 108 M⊙. NGC 4261 has a profile compatible with an ∼ 1 × 10 8 M⊙ black
hole, though these observations may not have been across the nucleus. Compatibility
with these kinematic signatures does not necessarily imply that we can state black
172

hole masses for these galaxies. The scale of the random motions in these galaxies is
so great that we have no reason to believe that the gas in the center is only affected
by the smooth gravitational potential of the stars and central black hole. More likely
is that these profiles are indicating the presence of a supermassive black hole on these
mass scales, but that the actual mass may vary considerably from any attempt to
best fit the nuclear slope.
The three remaining galaxies are of some interest: in NGC 4335 and NGC 5141 the
gas is the more settled into a smooth rotation curve than is the case for the majority
of the galaxies (other than the very nearby M84 and M87), however in both of these
cases we find that no black hole is necessary to explain the observed kinematics.
In NGC 2329 the central slope of the rotation curve is very shallow compared even
to the ‘no black hole’ model. This suggests that either the gas in this galaxy is in a
different plane to the one that we were expecting or that there is significant inflow
through the disk which is not supported by rotation in the gravitational potential.
If this is the case, then this type of motion could also be influential in other nuclei,
particularly as we know that in these radio galaxies, the central engine is being actively
fueled and generating jets. Possibly NGC 4335 and NGC 5141 also hint at this; their
slopes are also slightly too shallow (but within the errors in all of the parameters
173

used) for the zero black hole mass model. However we anticipate that a black hole is
present in these galaxies meaning the observed slope should be steeper if the disk is
stable. If flow is taking place then it may be possible to detect the signature across
the minor axis, and indeed in Figure 4.29 (for NGC 2329) it is possible to see positive
and negative velocity features in the side slit positions.
In Table 4.6 we also list the black hole masses predicted by the relationship fit
by Merritt & Ferrarese (2001). Though the kinematics will not allow us to fit exact
models for the black hole mass, we can see that the ranges derived from the kine-
matic signatures in the central regions lead to black hole masses that are generally
compatible with the M• − σc relation. In Figure 4.46 we plot our results on top
of the reliable black hole estimates and M• − σc relation as presented in Chapter
1. Though the agreement is generally good (for galaxies where we give the range of
masses 1×10 8 M⊙ < M• < 9×10 8 M⊙ and where M• ∼ > 9×108 M⊙ in particular), the
galaxies with an upper limit around 1 × 10 8 M⊙ lie somewhat below their predicted
values.
4.4.2 Settling of the gas into a thin disk
In Steiman-Cameron & Durisen (1986) the authors present a summary of results
relating to the settling of gas disks in elliptical galaxies. Through analytical and
174

numerical approaches they made the following conclusions: (i) Settling is a local
process, depending primarily on the local properties of the potential and the gas disk;
(ii) minimum settling times are on the order of two to three disk precession times
which is equivalent to ten to a few tens of rotation periods; (iii) that the actively
settling region is narrow, with a radial width of about 30% of its outer radius; and
(iv) radial inflow is enhanced during the active settling period.
This means that in our observations of gas disks in ellipticals we need not expect
all of the gas to be settled, even if some portions of it are, and it may not be easy to
identify which portions of the gas are settled and which are not without detailed 2D
kinematics. We might expect to see signs of inflow in the actively settling regions,
which means as the gas settles it may appear to be unstable in the gravitational
potential. This is possibly what we observe in NGC 2329.
Steiman-Cameron & Durisen (1988) describe disks which settle through differen-
tial precession and dissipation, picturing the disk as a cloud fluid, where cloud-cloud
interactions play an important role in the dissipation. In Chapter 5 we will see that
this model is compatible with some of the kinematic parameters of the gas. They
found that gravitational and Coriolis forces will twist disks that are not in the major
plane of the gravitation potential – compatible with observations discussed in the
175

next section.
Inflow is important in allowing fuel to reach the central engine and processes that
take place as the disk settles may be important in allowing that inflow to occur -
particularly turbulent viscosity in the disk or dynamical friction between clumps of
gas (for example Wada, 2004; Shlosman et al., 1990).
4.4.3 Drivers of unsettled motion
There are several sources from which we might expect energy to get deposited into the
gas and drive motions out of the settled major plane. Amongst these are interactions
with the Jets, twists and warps in the disks and activity resulting from starbursts
and mergers.
Interactions with jets: In four of the sample galaxies we have located instances
where a disturbance occurs in the gas at the location corresponding to the point
where the position angle of the radio jet crosses the side slit positions. With the
signal-to-noise of the data that we have available this may be merely a coincidence
(and the statistics are indeed very poor). However, we present these few examples
here as possible hints that we may be able to track down at least one source of
non-gravitational disturbance.
176

In the positive offset slit of NGC 4335 a step in the velocity profile of ∼ 150 km
s −1 occurs at the position that the jet would cross the disk, this is shown in Figure
4.42. We show an image of the nuclear region of this galaxy with the direction of the
jet indicated in Figure 2.13.
In the negative offset slit of NGC 7626 a velocity deviation of ∼ 300 km s −1 and a
velocity dispersion deviation of ∼ 100 km s −1 occur at the jet location (Figure 4.43).
We show an image of the nuclear region of this galaxy with the direction of the jet
indicated in Figure 2.21.
In NGC 193, effects are seen in both side slits at the jet locations: on the negative
offset side a velocity dispersion peak of ∼ 100 km s −1 is visible and in the positive
slit a velocity dispersion peak of ∼ 70 km s −1 is accompanied by a small peak in the
observed emission line flux (Figure 4.44). We show an image of the nuclear region of
this galaxy with the direction of the jet indicated in Figure 2.1.
Finally, in the positive offset slit of UGC 12064 (Figure 4.45) a velocity deviation
of ∼ 200 km s −1 can be seen at the jet location. We show an image of the nuclear
region of this galaxy with the direction of the jet indicated in Figure 2.20.
177

Non-circular morphologies: Twists and warps in the gas disk may lead to shifts
in the plane and sense of the rotation, and may drive non-gravitational motions in the
gas. The clearest evidence for a twist can be seen in the observations for NGC 7626
(Figure 4.41) where the gas velocities appear to ‘turn over’ to a component rotating in
a very different direction. Hints of similar profiles are seen in NGC 315, NGC 2892 and
NGC 4261. As we saw above forming twists and warps may be a natural consequence
of the disk not lying in the major plane of the galaxy.
In NGC 193, NGC 541, UGC 1841, NGC 5490 and NGC 7052, it is likely that
some of the observed features in the observed velocity profiles are due to the presence
of multiple (possibly disconnected) kinematic systems in the nuclei of these galaxies.
Non-gravitational energy sources: Other sources of unsettled motions in the
gas include activity from starbursts and mergers. It is extremely difficult to identify
the consequences of these types of activity as they can be very irregularly dispersed
through the galaxy and then mixed on dynamical timescales. However, if the settling
time in the gas disk is long they may have long lived consequences for the motions in
the gas.
178

4.5 Conclusions
In this chapter we presented thin disk model velocity profiles of gas sitting in the
stellar potential, and that potential including a 1 × 10 8 M⊙ and a 9 × 10 8 M⊙ black
hole in our sample of 21 galaxies, apart from UGC 7115 (for which we have insufficient
reliable data, from only one observational slit) and NGC 3801 (where it is quite clear
we are not observing the nucleus, which is highly dust obscured).
In 6 of the 19 galaxies the modeled velocity profile gives no clear results as the
non-rotational motions in the gas are too great. For 4 of the 13 remaining galaxies
we observe a signature compatible with a black hole in the range 1 × 10 8 M⊙ <
M• < 9 × 10 8 M⊙, for 5 we observe kinematic signatures that are compatible with
M• ∼ > 9 × 108 M⊙. NGC 4261 has a profile compatible with an ∼ 1 × 10 8 M⊙ black
hole, though this result is highly unreliable due to observational problems.
Compatibility with these kinematic signatures does not necessarily imply that we
can state black hole masses for these galaxies. The scale of the random motions in
these galaxies is so great that we have no reason to believe that the gas in the center
is only affected by the smooth gravitational potential of the stars and central black
hole. More likely is that these profiles are indicating the presence of a supermassive
179

lack hole on these mass scales, but that the actual mass may vary considerably from
any attempt to best fit the nuclear slope.
The three remaining galaxies are of some interest, in NGC 4335 and NGC 5141 the
gas is the more settled into a smooth rotation curve than is the case for the majority
of the galaxies (other than the very nearby M84 and M87), however in both of these
cases we find that no black hole is necessary to explain the observed kinematics. In
NGC 2329 the central slope of the rotation curve is very shallow compared even to
the M• = 0 model. This suggests that either the gas in this galaxy is in a different
plane to the one that we were expecting or that there is significant inflow through
the disk which is not supported by rotation in the gravitational potential.
The M• −σc relation appears to be compatible with the observations that we have
made here, other than for those three cases above. We are not satisfied, however, that
we are able to put good limits on any of the black hole masses as various effects in
the gas reduces our ability to understand the kinematics of the central regions. The
gas may not be settled into a stable disk in the major plane of the galaxy, and the
settling process may lead to inflow. In several nuclei we observe signs of kinematic
twists and warps and it is hard to accurately account for the consequences. Similar
phenomena may go undetected in other nuclei. In four nuclei we observe (at very
180

low statistical significance) possible signs of interactions with the jet, which would
add further confusion to the dynamical situation in the gas. Finally, events in the
evolution of the galaxy, such as mergers and episodes of star formation, could add
motion to the gas that is unrelated to the galaxy’s potential.
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Table 4.1. Disk inclinations and dust masses.
Galaxy i q ′ Mdust
( ◦ ) (10 4 M⊙)
(1) (2) (3) (4)
NGC 193 70.0 0.95 13
NGC 315 77.0 0.79 3
NGC 383 40.0 0.89 48
NGC 541 24.0 0.99 1
NGC 741 60.0 1.00 0
UGC 1841 11.0 1.00 1
NGC 2329 47.0 0.89 5
NGC 2892 60.0 0.92 0
NGC 3862 8.0 1.0 2
NGC 4261 63.0 0.79 1
NGC 4335 66.0 0.81 58
NGC 4374 80.0 0.82 1
NGC 4486 60.0 0.91 < 1
NGC 5127 80.0 0.91 6
NGC 5141 80.0 0.73 3
NGC 5490 80.0 0.87 < 1
NGC 7052 73.0 0.71 5
UGC 12064 57.0 1.00 · · ·
NGC 7626 80.0 0.86 < 1
Note. — Col. (1): Galaxy Name; Col. (2): Inclination
angle (i) derived from the axis ratio of the dust disk, galaxies
with dust lanes were set at an inclination of 80 ◦ , shown
in italic; Col. (3): The dust mass assuming a screen of dust
half-way in the galaxy
References. — Measurements of these parameters is described
in Verdoes Kleijn et al. (1999) (and Verdoes Kleijn
et al., 2002a, for UGC 12064).
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Table 4.2. STIS PSF Parameters.
Gaussian γi σi
(1) (2) (3)
1 0.674510 0.026922
2 -0.606168 0.045302
3 0.798732 0.066942
4 0.084999 0.272356
5 0.047927 0.860743
Note. — Tiny Tim (Krist &
Hook, 1999) parameters to represent
the STIS Point Spread Function
(see text).
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Table 4.3. Luminosity density fit parameters.
Galaxy α β a j0
(arcsec)
(1) (2) (3) (4) (5)
NGC 193 0.23 1.36 1.87 5.45
NGC 315 0.44 22.29 18.3 1.27
NGC 383 0.38 0.92 1.06 10.5
NGC 541 1.14 5.57 8.95 0.35
NGC 741 0.63 1.23 2.47 3.02
UGC 1841 0.94 2.37 5.12 0.59
NGC 2329 1.70 0.17 5.38 0.22
NGC 2892 0.65 1.05 1.34 4.78
NGC 3862 1.42 1.31 7.18 0.17
NGC 4261 0.00 1.13 2.29 17.9
NGC 4335 0.00 1.13 0.19 445.
M84 0.87 -1.05 9.24 6.49
NGC 4486 1.63 0.00 2.55 6.58
NGC 5127 0.00 1.51 1.30 8.69
NGC 5141 0.62 1.00 0.85 21.57
NGC 5490 0.00 1.16 0.44 85.86
NGC 7052 0.00 1.58 2.27 8.04
UGC 12064 1.13 1.76 7.78 0.17
NGC 7626 0.55 0.80 0.52 70.0
Note. — Col. (1): Galaxy Name; Col. (2-
5): Best fit parameters describing the stellar
luminosity distribution j through a relationship
of the form j(R, z) = j0(m/a) α [1 + (m/a) 2 ] β
(see text).
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Table 4.4. Mass to light ratio (Υ) estimates for sample galaxies.
Galaxy MB (B − V ) (V − I) ΥV ΥI
(1) (2) (3) (4) (5) (6)
NGC 193 -20.73 1.02 6.30
NGC 315 -22.35 1.08 8.32
NGC 383 -22.02 1.02 1.87 7.80 2.68
NGC 541 -21.46 0.85 1.24 6.91 4.24
NGC 741 -22.50 1.06 1.38 8.51 4.59
UGC 1841 -21.68 0.82 7.14
NGC 2329 -21.75 0.90 1.29 7.32 4.29
NGC 2892 -20.92
NGC 3801 -20.65 0.84 1.50 6.04 2.92
NGC 3862 -21.48 0.92 2.00 7.02 2.13
UGC 7115 -20.87 1.00 6.43
NGC 4261 -21.32 0.95 1.23 6.87 4.26
NGC 4335 -20.69 0.95 6.19
NGC 4374 -20.87 0.93 1.09 6.35 4.47
NGC 4486 -22.01 0.93 1.27 7.67 4.58
NGC 5127 -20.91 0.97 6.44
NGC 5141 -20.75 0.92 1.13 6.22 4.22
NGC 5490 -21.39 0.94 0.95 6.94 5.56
NGC 7052 -21.02 0.97 6.56
UGC 12064 -20.61 0.98 6.14
NGC 7626 -21.56 1.06 1.12 7.28 4.99
Note. — Col. (1): Galaxy name; Col. (2) The blue
band magnitude from the LEDA database (http://wwwobs.univ-lyon1.fr/hypercat).;
Col. (3) The B-V color from
LEDA; Col. (4) the V-I color from LEDA; Cols. (5-6)
The V band and I band mass to light ratios respectively,
calculated as described in the text.
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Table 4.5. Best fitting velocity offsets.
Galaxy δv Sense vr
(km s −1 ) (km s −1 )
(1) (2) (3) (4)
NGC 193 47 − 4390
NGC 315 -137 − 4956
NGC 383 120 − 5010
NGC 541 -70 + 5428
NGC 741 30 + 5295
UGC 1841 0 + 6360
NGC 2329 80 + 5805
NGC 2892 37 − 6847
NGC 3862 160 + 6490
NGC 4335 50 + 4723
NGC 4374 -83 + 1072
NGC 4486 63 + 1218
NGC 5127 7 + 4837
NGC 5141 -50 + 5253
NGC 5490 -93 − 5697
NGC 7052 280 + 4435
UGC 12064 -83 − 5040
NGC 7626 -47 + 3448
Note. — Col. (1): Galaxy name; Col.
(2): The offset velocity from the mean value
quoted in Table 2.1; Col. (3): The sense of
the rotation, + indicates the velocity profile
runs from positive to negative velocities
along the slit, - runs from negative to positive;
Col. (4): The recession velocity of the
galaxy corrected with the offsets in Col. (2).
186

Table 4.6. Black hole signatures in the central kinematics.
Galaxy M•/10 8 M⊙ MMF01/10 8 M⊙
(1) (2) (3)
NGC 193 1 < M• < 9 · · ·
NGC 315 Unclear 14.6
NGC 383 M• > 9? 9.24
NGC 541 Unclear 2.03
NGC 741 Unclear 5.24
UGC 1841 Unclear 18.6
NGC 2329 M• < 1 Inflow? 4.92
NGC 2892 Unclear · · ·
NGC 3862 Unclear 4.66
NGC 4261 M• ∼ 1* 7.75
NGC 4335 M• < 1 3.9
M84 M• > 9 7.30
NGC 4486 M• > 9 22.5
NGC 5127 1 < M• < 9 1.11
NGC 5141 M• < 1 · · ·
NGC 5490 Unclear 9.07
NGC 7052 1 < M• < 9 3.62
UGC 12064 M• ∼ 9 1.80
NGC 7626 1 < M• < 9 2.72
Note. — Col. (1): Galaxy Name; Col. (2):
Black hole mass range that would generate a kinematic
signature compatible with the observations
in the central part of the observed velocity profile.
(see text); Col. (3): The black hole mass
predicted by the M• − σc relationship of Merritt
& Ferrarese (2001)
187

weighted
500
400
300
200
100
= 47. km s -1
-400 -200 0 200 400
Velocity offset (km s -1 0
)
Figure 4.1 Data-Model weighted mean residuals with varying velocity offsets for
NGC 193. The dark lines represent the models with the velocity field running from
negative to positive velocities (which produces the minimum result in this case),
the light lines show the values with the sense of the model velocities reversed. The
three lines in each set represent the weighted-mean residuals between the data and
the M• = 0 (solid lines), M• = 1 × 10 8 M⊙ (dashed lines), and M• = 9 × 10 8 M⊙
(dash-dot lines) models.
188

weighted
600
500
400
300
200
100
= -137. km s -1
-400 -200 0 200 400
Velocity offset (km s -1 0
)
Figure 4.2 Data-Model weighted mean residuals with varying velocity offsets for
NGC 315. The dark lines represent the models with the velocity field running from
negative to positive velocities (which produces the minimum result in this case),
the light lines show the values with the sense of the model velocities reversed. The
three lines in each set represent the weighted-mean residuals between the data and
the M• = 0 (solid lines), M• = 1 × 10 8 M⊙ (dashed lines), and M• = 9 × 10 8 M⊙
(dash-dot lines) models.
189

weighted
600
500
400
300
200
100
= 120. km s -1
-400 -200 0 200 400
Velocity offset (km s -1 0
)
Figure 4.3 Data-Model weighted mean residuals with varying velocity offsets for
NGC 383. The dark lines represent the models with the velocity field running from
positive to negative velocities (which produces the minimum result in this case),
the light lines show the values with the sense of the model velocities reversed. The
three lines in each set represent the weighted-mean residuals between the data and
the M• = 0 (solid lines), M• = 1 × 10 8 M⊙ (dashed lines), and M• = 9 × 10 8 M⊙
(dash-dot lines) models.
190

weighted
600
500
400
300
200
100
= -70. km s -1
-400 -200 0 200 400
Velocity offset (km s -1 0
)
Figure 4.4 Data-Model weighted mean residuals with varying velocity offsets for
NGC 541. The dark lines represent the models with the velocity field running from
positive to negative velocities (which produces the minimum result in this case),
the light lines show the values with the sense of the model velocities reversed. The
three lines in each set represent the weighted-mean residuals between the data and
the M• = 0 (solid lines), M• = 1 × 10 8 M⊙ (dashed lines), and M• = 9 × 10 8 M⊙
(dash-dot lines) models.
191

weighted
500
400
300
200
100
= 30. km s -1
-400 -200 0 200 400
Velocity offset (km s -1 0
)
Figure 4.5 Data-Model weighted mean residuals with varying velocity offsets for
NGC 741. The dark lines represent the models with the velocity field running from
positive to negative velocities (which produces the minimum result in this case),
the light lines show the values with the sense of the model velocities reversed. The
three lines in each set represent the weighted-mean residuals between the data and
the M• = 0 (solid lines), M• = 1 × 10 8 M⊙ (dashed lines), and M• = 9 × 10 8 M⊙
(dash-dot lines) models.
192

weighted
500
400
300
200
100
= 0. km s -1
-400 -200 0 200 400
Velocity offset (km s -1 0
)
Figure 4.6 Data-Model weighted mean residuals with varying velocity offsets for
UGC 1841. The dark lines represent the models with the velocity field running
from positive to negative velocities (which produces the minimum result in this case),
the light lines show the values with the sense of the model velocities reversed. The
three lines in each set represent the weighted-mean residuals between the data and
the M• = 0 (solid lines), M• = 1 × 10 8 M⊙ (dashed lines), and M• = 9 × 10 8 M⊙
(dash-dot lines) models.
193

weighted
500
400
300
200
100
= 80. km s -1
-400 -200 0 200 400
Velocity offset (km s -1 0
)
Figure 4.7 Data-Model weighted mean residuals with varying velocity offsets for
NGC 2329. The dark lines represent the models with the velocity field running
from positive to negative velocities (which produces the minimum result in this case),
the light lines show the values with the sense of the model velocities reversed. The
three lines in each set represent the weighted-mean residuals between the data and
the M• = 0 (solid lines), M• = 1 × 10 8 M⊙ (dashed lines), and M• = 9 × 10 8 M⊙
(dash-dot lines) models.
194

weighted
500
400
300
200
100
= 37. km s -1
-400 -200 0 200 400
Velocity offset (km s -1 0
)
Figure 4.8 Data-Model weighted mean residuals with varying velocity offsets for
NGC 2892. The dark lines represent the models with the velocity field running
from negative to positive velocities (which produces the minimum result in this case),
the light lines show the values with the sense of the model velocities reversed. The
three lines in each set represent the weighted-mean residuals between the data and
the M• = 0 (solid lines), M• = 1 × 10 8 M⊙ (dashed lines), and M• = 9 × 10 8 M⊙
(dash-dot lines) models.
195

weighted
600
500
400
300
200
100
= 160. km s -1
-400 -200 0 200 400
Velocity offset (km s -1 0
)
Figure 4.9 Data-Model weighted mean residuals with varying velocity offsets for
NGC 3862. The dark lines represent the models with the velocity field running
from positive to negative velocities (which produces the minimum result in this case),
the light lines show the values with the sense of the model velocities reversed. The
three lines in each set represent the weighted-mean residuals between the data and
the M• = 0 (solid lines), M• = 1 × 10 8 M⊙ (dashed lines), and M• = 9 × 10 8 M⊙
(dash-dot lines) models.
196

weighted
500
400
300
200
100
= 50. km s -1
-400 -200 0 200 400
Velocity offset (km s -1 0
)
Figure 4.10 Data-Model weighted mean residuals with varying velocity offsets for
NGC 4335. The dark lines represent the models with the velocity field running from
positive to negative velocities (which produces the minimum result in this case),
the light lines show the values with the sense of the model velocities reversed. The
three lines in each set represent the weighted-mean residuals between the data and
the M• = 0 (solid lines), M• = 1 × 10 8 M⊙ (dashed lines), and M• = 9 × 10 8 M⊙
(dash-dot lines) models.
197

weighted
500
400
300
200
100
= -83. km s -1
-400 -200 0 200 400
Velocity offset (km s -1 0
)
Figure 4.11 Data-Model weighted mean residuals with varying velocity offsets for M84.
The dark lines represent the models with the velocity field running from positive to
negative velocities (which produces the minimum result in this case), the light lines
show the values with the sense of the model velocities reversed. The three lines in
each set represent the weighted-mean residuals between the data and the M• = 0
(solid lines), M• = 1 × 10 8 M⊙ (dashed lines), and M• = 9 × 10 8 M⊙ (dash-dot lines)
models.
198

weighted
600
500
400
300
200
100
= 63. km s -1
-400 -200 0 200 400
Velocity offset (km s -1 0
)
Figure 4.12 Data-Model weighted mean residuals with varying velocity offsets for
NGC 4486. The dark lines represent the models with the velocity field running from
positive to negative velocities (which produces the minimum result in this case),
the light lines show the values with the sense of the model velocities reversed. The
three lines in each set represent the weighted-mean residuals between the data and
the M• = 0 (solid lines), M• = 1 × 10 8 M⊙ (dashed lines), and M• = 9 × 10 8 M⊙
(dash-dot lines) models.
199

weighted
500
400
300
200
100
= 7. km s -1
-400 -200 0 200 400
Velocity offset (km s -1 0
)
Figure 4.13 Data-Model weighted mean residuals with varying velocity offsets for
NGC 5127. The dark lines represent the models with the velocity field running from
positive to negative velocities (which produces the minimum result in this case),
the light lines show the values with the sense of the model velocities reversed. The
three lines in each set represent the weighted-mean residuals between the data and
the M• = 0 (solid lines), M• = 1 × 10 8 M⊙ (dashed lines), and M• = 9 × 10 8 M⊙
(dash-dot lines) models.
200

weighted
500
400
300
200
100
= -50. km s -1
-400 -200 0 200 400
Velocity offset (km s -1 0
)
Figure 4.14 Data-Model weighted mean residuals with varying velocity offsets for
NGC 5141. The dark lines represent the models with the velocity field running from
positive to negative velocities (which produces the minimum result in this case),
the light lines show the values with the sense of the model velocities reversed. The
three lines in each set represent the weighted-mean residuals between the data and
the M• = 0 (solid lines), M• = 1 × 10 8 M⊙ (dashed lines), and M• = 9 × 10 8 M⊙
(dash-dot lines) models.
201

weighted
500
400
300
200
100
= -93. km s -1
-400 -200 0 200 400
Velocity offset (km s -1 0
)
Figure 4.15 Data-Model weighted mean residuals with varying velocity offsets for
NGC 5490. The dark lines represent the models with the velocity field running from
negative to positive velocities (which produces the minimum result in this case),
the light lines show the values with the sense of the model velocities reversed. The
three lines in each set represent the weighted-mean residuals between the data and
the M• = 0 (solid lines), M• = 1 × 10 8 M⊙ (dashed lines), and M• = 9 × 10 8 M⊙
(dash-dot lines) models.
202

weighted
800
600
400
200
= 280. km s -1
-400 -200 0 200 400
Velocity offset (km s -1 0
)
Figure 4.16 Data-Model weighted mean residuals with varying velocity offsets for
NGC 7052. The dark lines represent the models with the velocity field running from
positive to negative velocities (which produces the minimum result in this case),
the light lines show the values with the sense of the model velocities reversed. The
three lines in each set represent the weighted-mean residuals between the data and
the M• = 0 (solid lines), M• = 1 × 10 8 M⊙ (dashed lines), and M• = 9 × 10 8 M⊙
(dash-dot lines) models.
203

weighted
500
400
300
200
100
= -83. km s -1
-400 -200 0 200 400
Velocity offset (km s -1 0
)
Figure 4.17 Data-Model weighted mean residuals with varying velocity offsets for
UGC 12064. The dark lines represent the models with the velocity field running
from negative to positive velocities (which produces the minimum result in this case),
the light lines show the values with the sense of the model velocities reversed. The
three lines in each set represent the weighted-mean residuals between the data and
the M• = 0 (solid lines), M• = 1 × 10 8 M⊙ (dashed lines), and M• = 9 × 10 8 M⊙
(dash-dot lines) models.
204

weighted
500
400
300
200
100
= -47. km s -1
-400 -200 0 200 400
Velocity offset (km s -1 0
)
Figure 4.18 Data-Model weighted mean residuals with varying velocity offsets for
NGC 7626. The dark lines represent the models with the velocity field running from
positive to negative velocities (which produces the minimum result in this case),
the light lines show the values with the sense of the model velocities reversed. The
three lines in each set represent the weighted-mean residuals between the data and
the M• = 0 (solid lines), M• = 1 × 10 8 M⊙ (dashed lines), and M• = 9 × 10 8 M⊙
(dash-dot lines) models.
205

Gas Radial Velocity (km s -1 )
100
0
-100
-200
-300
NGC193 Central Slit (Varying PSF)
-1.0 -0.5 0.0 0.5 1.0
Position along slit (arcsec)
Figure 4.19 The 1×10 8 M⊙ model for NGC 193 repeated using 1 Gaussian (solid line)
and 5 Gaussians (dotted line) to represent the PSF (see text). Observed data points
and formal errors are also shown. NGC 193 is at a distance typical of the UGC FR-I
sample members.
206

Gas Radial Velocity (km s -1 )
400
300
200
100
0
-100
-200
-0.4 -0.2 0.0 0.2 0.4
Position along slit (arcsec)
-0.4 -0.2 0.0 0.2 0.4
Position along slit (arcsec)
Figure 4.20 Observed velocity profiles in the central slit position of NGC 4486 (M87)
during two different visits. Measured from the flux and velocity dispersion profiles
the observations were separated by approximately 0.1 pixels. Large differences in the
measured velocities in the very central pixels are readily apparent.
Gas Radial Velocity (km s -1 )
400
300
200
100
0
-100
-200
207

Gas Radial Velocity (km s -1 )
Gas Radial Velocity (km s -1 )
Gas Radial Velocity (km s -1 )
100
0
-100
-200
-300
100
-100
-200
-300
NGC193 Central Slit (Varying M/L)
-1.0 -0.5 0.0 0.5 1.0
Position along slit (arcsec)
0
100
NGC193 Central Slit (Varying q’)
-1.0 -0.5 0.0 0.5 1.0
Position along slit (arcsec)
0
-100
-200
-300
NGC193 Central Slit (Varying i)
-1.0 -0.5 0.0 0.5 1.0
Position along slit (arcsec)
Figure 4.21 Varying Υ (top), q ′ (middle) and i (bottom) in models of the velocity
profile of NGC 193. Models with M• = 1 × 10 8 M⊙ are shown in each case. Top:
shows data plus models with Υ = 2, 4, and 6; Middle: shows data plus models with
q ′ = 0.95, 0.85, and 0.75; Bottom: shows data plus models with i = 65 ◦ , 75 ◦ , and
85 ◦ . Definitions of the parameters are given in the text.
208

Gas Radial Velocity (km s -1 )
Gas Radial Velocity (km s -1 )
Gas Radial Velocity (km s -1 )
200
0
-200
300
200
100
-100
-200
NGC4335 Central Slit (Varying M/L)
-1.0 -0.5 0.0 0.5 1.0
Position along slit (arcsec)
0
NGC4335 Central Slit (Varying q’)
-300
-1.0 -0.5 0.0 0.5 1.0
Position along slit (arcsec)
300
200
100
0
-100
-200
NGC4335 Central Slit (Varying i)
-1.0 -0.5 0.0 0.5 1.0
Position along slit (arcsec)
Figure 4.22 Varying Υ (top), q ′ (middle) and i (bottom) in models of the velocity
profile of NGC 4335. Models with M• = 1 × 10 8 M⊙ are shown in each case. Top:
shows data plus models with Υ = 2, 4, and 6; Middle: shows data plus models with
q ′ = 0.95, 0.85, and 0.75; Bottom: shows data plus models with i = 65 ◦ , 75 ◦ , and
85 ◦ . Definitions of the parameters are given in the text.
209

Gas Radial Velocity (km s -1 )
Gas Radial Velocity (km s -1 )
Gas Radial Velocity (km s -1 )
200
100
0
-100
-200
-300
200
100
0
-100
-200
-300
200
100
0
-100
-200
-300
NGC193 Central Slit: ∆v = 47 km s -1
-1.0 -0.5 0.0 0.5 1.0
Position along slit (arcsec)
-ve offset slit position
-1.0 -0.5 0.0 0.5 1.0
Position along slit (arcsec)
+ve offset slit position
-1.0 -0.5 0.0 0.5 1.0
Position along slit (arcsec)
Gas Radial Velocity (km s -1 )
Gas Radial Velocity (km s -1 )
200
100
0
-100
-200
-300
200
100
0
-100
-200
-300
NGC193 Central Slit: ∆v = 90 km s -1
-1.0 -0.5 0.0 0.5 1.0
Position along slit (arcsec)
-ve offset slit position
-1.0 -0.5 0.0 0.5 1.0
Position along slit (arcsec)
+ve offset slit position
-1.0 -0.5 0.0 0.5 1.0
Position along slit (arcsec)
Figure 4.23 The observed velocity profiles of NGC 193 for each of the three observed
slit positions: (left) offset by the velocity and slope calculated in §4.2.5 and (right)
with a velocity offset of 90 km s −1 , and the velocity field running from positive to
negative, which provides a more meaningful fit (judged by the author). The velocities
are shown shaded according to the relative signal-to-noise of each spectrum, formal
errors from the fit are also indicated (see Chapter 3). The three solid lines show
model velocity profiles for no black hole, a 1 × 10 8 M⊙ black hole and a 9 × 10 8 M⊙
(the steeper lines from models with the greatest black hole mass). See text for details
of the models. The dashed vertical lines give a rough approximation of the sphere of
influence of a black hole based on the mass estimate from the M• − σ relation and
the size of the random motions observed.
Gas Radial Velocity (km s -1 )
200
100
0
-100
-200
-300
210

Gas Radial Velocity (km s -1 )
Gas Radial Velocity (km s -1 )
Gas Radial Velocity (km s -1 )
400
300
200
100
0
-100
-200
400
300
200
100
0
-100
-200
400
300
200
100
0
-100
-200
NGC315 Central Slit: ∆v = -137 km s -1
-0.4 -0.2 0.0 0.2 0.4
Position along slit (arcsec)
-ve offset slit position
-0.4 -0.2 0.0 0.2 0.4
Position along slit (arcsec)
+ve offset slit position
-0.4 -0.2 0.0 0.2 0.4
Position along slit (arcsec)
Figure 4.24 The observed velocity profiles of NGC 315 for each of the three observed
slit positions. The velocities are shown shaded according to the relative signal-tonoise
of each spectrum, formal errors from the fit are also indicated (see Chapter 3).
The three solid lines show model velocity profiles for no black hole, a 1 × 10 8 M⊙
black hole and a 9 × 10 8 M⊙ (the steeper lines from models with the greatest black
hole mass). See text for details of the models. The dashed vertical lines give a rough
approximation of the radius of influence of a black hole based on the mass estimate
from the M• − σ relation and the size of the random motions observed.
211

Gas Radial Velocity (km s -1 )
Gas Radial Velocity (km s -1 )
Gas Radial Velocity (km s -1 )
200
0
-200
-400
-600
200
0
-200
-400
-600
200
0
-200
-400
-600
NGC383 Central Slit: ∆v = 120 km s -1
-0.4 -0.2 0.0 0.2 0.4
Position along slit (arcsec)
-ve offset slit position
-0.4 -0.2 0.0 0.2 0.4
Position along slit (arcsec)
+ve offset slit position
-0.4 -0.2 0.0 0.2 0.4
Position along slit (arcsec)
Gas Radial Velocity (km s -1 )
Gas Radial Velocity (km s -1 )
200
0
-200
-400
-600
200
0
-200
-400
-600
NGC383 Central Slit: ∆v = 220 km s -1
-0.4 -0.2 0.0 0.2 0.4
Position along slit (arcsec)
-ve offset slit position
-0.4 -0.2 0.0 0.2 0.4
Position along slit (arcsec)
+ve offset slit position
-0.4 -0.2 0.0 0.2 0.4
Position along slit (arcsec)
Figure 4.25 The observed velocity profiles of NGC 383 for each of the three observed
slit positions: (left) offset by the velocity and slope calculated in §4.2.5 and (right)
with a velocity offset of 220 km s −1 , which provides a more meaningful fit (judged
by the author), extra power in the velocity field in the side slit position may result
from the nucleus lying off center across the width of the central slit. The velocities
are shown shaded according to the relative signal-to-noise of each spectrum, formal
errors from the fit are also indicated (see Chapter 3). The three solid lines show
model velocity profiles for no black hole, a 1 × 10 8 M⊙ black hole and a 9 × 10 8 M⊙
(the steeper lines from models with the greatest black hole mass). See text for details
of the models. The dashed vertical lines give a rough approximation of the radius of
influence of a black hole based on the mass estimate from the M• − σ relation and
the size of the random motions observed.
Gas Radial Velocity (km s -1 )
200
0
-200
-400
-600
212

Gas Radial Velocity (km s -1 )
Gas Radial Velocity (km s -1 )
Gas Radial Velocity (km s -1 )
400
300
200
100
0
-100
-200
-300
400
300
200
100
0
-100
-200
-300
400
300
200
100
0
-100
-200
-300
NGC541 Central Slit: ∆v = -70 km s -1
-1.0 -0.5 0.0 0.5 1.0
Position along slit (arcsec)
-ve offset slit position
-1.0 -0.5 0.0 0.5 1.0
Position along slit (arcsec)
+ve offset slit position
-1.0 -0.5 0.0 0.5 1.0
Position along slit (arcsec)
Figure 4.26 The observed velocity profiles of NGC 541 for each of the three observed
slit positions. The velocities are shown shaded according to the relative signal-tonoise
of each spectrum, formal errors from the fit are also indicated (see Chapter 3).
The three solid lines show model velocity profiles for no black hole, a 1 × 10 8 M⊙
black hole and a 9 × 10 8 M⊙ (the steeper lines from models with the greatest black
hole mass). See text for details of the models. The dashed vertical lines give a rough
approximation of the radius of influence of a black hole based on the mass estimate
from the M• − σ relation and the size of the random motions observed.
213

Gas Radial Velocity (km s -1 )
Gas Radial Velocity (km s -1 )
Gas Radial Velocity (km s -1 )
600
400
200
0
-200
600
400
200
0
-200
600
400
200
0
-200
NGC741 Central Slit: ∆v = 30 km s -1
-1.0 -0.5 0.0 0.5 1.0
Position along slit (arcsec)
-ve offset slit position
-1.0 -0.5 0.0 0.5 1.0
Position along slit (arcsec)
+ve offset slit position
-1.0 -0.5 0.0 0.5 1.0
Position along slit (arcsec)
Figure 4.27 The observed velocity profiles of NGC 741 for each of the three observed
slit positions. The velocities are shown shaded according to the relative signal-tonoise
of each spectrum, formal errors from the fit are also indicated (see Chapter 3).
The three solid lines show model velocity profiles for no black hole, a 1 × 10 8 M⊙
black hole and a 9 × 10 8 M⊙ (the steeper lines from models with the greatest black
hole mass). See text for details of the models. The dashed vertical lines give a rough
approximation of the radius of influence of a black hole based on the mass estimate
from the M• − σ relation and the size of the random motions observed.
214

Gas Radial Velocity (km s -1 )
Gas Radial Velocity (km s -1 )
Gas Radial Velocity (km s -1 )
300
200
100
0
-100
-200
300
200
100
0
-100
-200
300
200
100
0
-100
-200
UGC01841 Central Slit: ∆v = 0 km s -1
-1.0 -0.5 0.0 0.5 1.0
Position along slit (arcsec)
-ve offset slit position
-1.0 -0.5 0.0 0.5 1.0
Position along slit (arcsec)
+ve offset slit position
-1.0 -0.5 0.0 0.5 1.0
Position along slit (arcsec)
Figure 4.28 The observed velocity profiles of UGC 1841 for each of the three observed
slit positions. The velocities are shown shaded according to the relative signal-tonoise
of each spectrum, formal errors from the fit are also indicated (see Chapter 3).
The three solid lines show model velocity profiles for no black hole, a 1 × 10 8 M⊙
black hole and a 9 × 10 8 M⊙ (the steeper lines from models with the greatest black
hole mass). See text for details of the models. The dashed vertical lines give a rough
approximation of the radius of influence of a black hole based on the mass estimate
from the M• − σ relation and the size of the random motions observed.
215

Gas Radial Velocity (km s -1 )
Gas Radial Velocity (km s -1 )
Gas Radial Velocity (km s -1 )
400
300
200
100
0
-100
-200
400
300
200
100
0
-100
-200
400
300
200
100
0
-100
-200
NGC2329 Central Slit: ∆v = 80 km s -1
-1.0 -0.5 0.0 0.5 1.0
Position along slit (arcsec)
-ve offset slit position
-1.0 -0.5 0.0 0.5 1.0
Position along slit (arcsec)
+ve offset slit position
-1.0 -0.5 0.0 0.5 1.0
Position along slit (arcsec)
Figure 4.29 The observed velocity profiles of NGC 2329 for each of the three observed
slit positions. The velocities are shown shaded according to the relative signal-tonoise
of each spectrum, formal errors from the fit are also indicated (see Chapter 3).
The three solid lines show model velocity profiles for no black hole, a 1 × 10 8 M⊙
black hole and a 9 × 10 8 M⊙ (the steeper lines from models with the greatest black
hole mass). See text for details of the models. The dashed vertical lines give a rough
approximation of the radius of influence of a black hole based on the mass estimate
from the M• − σ relation and the size of the random motions observed.
216

Gas Radial Velocity (km s -1 )
Gas Radial Velocity (km s -1 )
Gas Radial Velocity (km s -1 )
400
200
0
-200
-400
400
200
0
-200
-400
400
200
0
-200
-400
NGC2892 Central Slit: ∆v = 37 km s -1
-1.0 -0.5 0.0 0.5 1.0
Position along slit (arcsec)
-ve offset slit position
-1.0 -0.5 0.0 0.5 1.0
Position along slit (arcsec)
+ve offset slit position
-1.0 -0.5 0.0 0.5 1.0
Position along slit (arcsec)
Figure 4.30 The observed velocity profiles of NGC 2892 for each of the three observed
slit positions. The velocities are shown shaded according to the relative signal-tonoise
of each spectrum, formal errors from the fit are also indicated (see Chapter 3).
The three solid lines show model velocity profiles for no black hole, a 1 × 10 8 M⊙
black hole and a 9 × 10 8 M⊙ (the steeper lines from models with the greatest black
hole mass). See text for details of the models. The dashed vertical lines give a rough
approximation of the radius of influence of a black hole based on the mass estimate
from the M• − σ relation and the size of the random motions observed.
217

Gas Radial Velocity (km s -1 )
Gas Radial Velocity (km s -1 )
Gas Radial Velocity (km s -1 )
200
100
0
-100
-200
-300
-400
200
100
0
-100
-200
-300
-400
200
100
0
-100
-200
-300
-400
NGC3862 Central Slit: ∆v = 160 km s -1
-1.0 -0.5 0.0 0.5 1.0
Position along slit (arcsec)
-ve offset slit position
-1.0 -0.5 0.0 0.5 1.0
Position along slit (arcsec)
+ve offset slit position
-1.0 -0.5 0.0 0.5 1.0
Position along slit (arcsec)
Figure 4.31 The observed velocity profiles of NGC 3862 for each of the three observed
slit positions. The velocities are shown shaded according to the relative signal-tonoise
of each spectrum, formal errors from the fit are also indicated (see Chapter 3).
The three solid lines show model velocity profiles for no black hole, a 1 × 10 8 M⊙
black hole and a 9 × 10 8 M⊙ (the steeper lines from models with the greatest black
hole mass). See text for details of the models. The dashed vertical lines give a rough
approximation of the radius of influence of a black hole based on the mass estimate
from the M• − σ relation and the size of the random motions observed.
218

Gas Radial Velocity (km s -1 )
300
200
100
0
-100
-200
-300
NGC4261 Central Slit: ∆v = 0 km s -1
-0.4 -0.2 0.0 0.2 0.4 0.6
Position along slit (arcsec)
Figure 4.32 The observed velocity profiles of NGC 4261 for the positive offset slit
position – which lies closest to the nucleus (though it may not include the kinematic
center of the galaxy). The velocities are shown shaded according to the relative signalto-noise
of each spectrum, formal errors from the fit are also indicated (see Chapter
3). The three solid lines show model velocity profiles for no black hole, a 1 × 10 8 M⊙
black hole and a 9 × 10 8 M⊙ (the steeper lines from models with the greatest black
hole mass). See text for details of the models. The dashed vertical lines give a rough
approximation of the radius of influence of a black hole based on the mass estimate
from the M• − σ relation and the size of the random motions observed.
219

Gas Radial Velocity (km s -1 )
Gas Radial Velocity (km s -1 )
Gas Radial Velocity (km s -1 )
300
200
100
0
-100
-200
-300
300
200
100
0
-100
-200
-300
300
200
100
0
-100
-200
-300
NGC4335 Central Slit: ∆v = 50 km s -1
-1.0 -0.5 0.0 0.5 1.0
Position along slit (arcsec)
-ve offset slit position
-1.0 -0.5 0.0 0.5 1.0
Position along slit (arcsec)
+ve offset slit position
-1.0 -0.5 0.0 0.5 1.0
Position along slit (arcsec)
Figure 4.33 The observed velocity profiles of NGC 4335 for each of the three observed
slit positions. The velocities are shown shaded according to the relative signal-tonoise
of each spectrum, formal errors from the fit are also indicated (see Chapter 3).
The three solid lines show model velocity profiles for no black hole, a 1 × 10 8 M⊙
black hole and a 9 × 10 8 M⊙ (the steeper lines from models with the greatest black
hole mass). See text for details of the models. The dashed vertical lines give a rough
approximation of the radius of influence of a black hole based on the mass estimate
from the M• − σ relation and the size of the random motions observed.
220

Gas Radial Velocity (km s -1 )
Gas Radial Velocity (km s -1 )
Gas Radial Velocity (km s -1 )
200
0
-200
200
0
-200
200
0
-200
M84 Central Slit: ∆v = -83 km s -1
-0.4 -0.2 0.0 0.2 0.4
Position along slit (arcsec)
-ve offset slit position
-0.4 -0.2 0.0 0.2 0.4
Position along slit (arcsec)
+ve offset slit position
-0.4 -0.2 0.0 0.2 0.4
Position along slit (arcsec)
Figure 4.34 The observed velocity profiles of M84 for each of the three observed slit
positions. The velocities are shown shaded according to the relative signal-to-noise
of each spectrum, formal errors from the fit are also indicated (see Chapter 3). The
three solid lines show model velocity profiles for no black hole, a 1 × 10 8 M⊙ black
hole and a 9 × 10 8 M⊙ (the steeper lines from models with the greatest black hole
mass). See text for details of the models. The dashed vertical lines give a rough
approximation of the radius of influence of a black hole based on the mass estimate
from the M• − σ relation and the size of the random motions observed.
221

Gas Radial Velocity (km s -1 )
Gas Radial Velocity (km s -1 )
Gas Radial Velocity (km s -1 )
600
400
200
0
-200
-400
600
400
200
0
-200
-400
600
400
200
0
-200
-400
NGC4486 Central Slit: ∆v = 63 km s -1
-0.4 -0.2 0.0 0.2 0.4
Position along slit (arcsec)
-ve offset slit position
-0.4 -0.2 0.0 0.2 0.4
Position along slit (arcsec)
+ve offset slit position
-0.4 -0.2 0.0 0.2 0.4
Position along slit (arcsec)
Figure 4.35 The observed velocity profiles of NGC 4486 for each of the three observed
slit positions. The velocities are shown shaded according to the relative signal-tonoise
of each spectrum, formal errors from the fit are also indicated (see Chapter 3).
The three solid lines show model velocity profiles for no black hole, a 1 × 10 8 M⊙
black hole and a 9 × 10 8 M⊙ (the steeper lines from models with the greatest black
hole mass). See text for details of the models. The dashed vertical lines give a rough
approximation of the radius of influence of a black hole based on the mass estimate
from the M• − σ relation and the size of the random motions observed.
222

Gas Radial Velocity (km s -1 )
Gas Radial Velocity (km s -1 )
Gas Radial Velocity (km s -1 )
200
0
-200
-400
200
0
-200
-400
200
0
-200
-400
NGC5127 Central Slit: ∆v = 7 km s -1
-1.0 -0.5 0.0 0.5 1.0
Position along slit (arcsec)
-ve offset slit position
-1.0 -0.5 0.0 0.5 1.0
Position along slit (arcsec)
+ve offset slit position
-1.0 -0.5 0.0 0.5 1.0
Position along slit (arcsec)
Figure 4.36 The observed velocity profiles of NGC 5127 for each of the three observed
slit positions. The velocities are shown shaded according to the relative signal-tonoise
of each spectrum, formal errors from the fit are also indicated (see Chapter 3).
The three solid lines show model velocity profiles for no black hole, a 1 × 10 8 M⊙
black hole and a 9 × 10 8 M⊙ (the steeper lines from models with the greatest black
hole mass). See text for details of the models. The dashed vertical lines give a rough
approximation of the radius of influence of a black hole based on the mass estimate
from the M• − σ relation and the size of the random motions observed.
223

Gas Radial Velocity (km s -1 )
Gas Radial Velocity (km s -1 )
Gas Radial Velocity (km s -1 )
600
400
200
0
-200
600
400
200
0
-200
600
400
200
0
-200
NGC5141 Central Slit: ∆v = -50 km s -1
-1.0 -0.5 0.0 0.5 1.0
Position along slit (arcsec)
-ve offset slit position
-1.0 -0.5 0.0 0.5 1.0
Position along slit (arcsec)
+ve offset slit position
-1.0 -0.5 0.0 0.5 1.0
Position along slit (arcsec)
Figure 4.37 The observed velocity profiles of NGC 5141 for each of the three observed
slit positions. The velocities are shown shaded according to the relative signal-tonoise
of each spectrum, formal errors from the fit are also indicated (see Chapter 3).
The three solid lines show model velocity profiles for no black hole, a 1 × 10 8 M⊙
black hole and a 9 × 10 8 M⊙ (the steeper lines from models with the greatest black
hole mass). See text for details of the models. The dashed vertical lines give a rough
approximation of the radius of influence of a black hole based on the mass estimate
from the M• − σ relation and the size of the random motions observed.
224

Gas Radial Velocity (km s -1 )
Gas Radial Velocity (km s -1 )
Gas Radial Velocity (km s -1 )
400
200
0
-200
-400
400
200
0
-200
-400
400
200
0
-200
-400
NGC5490 Central Slit: ∆v = -93 km s -1
-1.0 -0.5 0.0 0.5 1.0
Position along slit (arcsec)
-ve offset slit position
-1.0 -0.5 0.0 0.5 1.0
Position along slit (arcsec)
+ve offset slit position
-1.0 -0.5 0.0 0.5 1.0
Position along slit (arcsec)
Figure 4.38 The observed velocity profiles of NGC 5490 for each of the three observed
slit positions. The velocities are shown shaded according to the relative signal-tonoise
of each spectrum, formal errors from the fit are also indicated (see Chapter 3).
The three solid lines show model velocity profiles for no black hole, a 1 × 10 8 M⊙
black hole and a 9 × 10 8 M⊙ (the steeper lines from models with the greatest black
hole mass). See text for details of the models. The dashed vertical lines give a rough
approximation of the radius of influence of a black hole based on the mass estimate
from the M• − σ relation and the size of the random motions observed.
225

Gas Radial Velocity (km s -1 )
Gas Radial Velocity (km s -1 )
Gas Radial Velocity (km s -1 )
400
200
0
-200
-400
-600
-800
400
200
0
-200
-400
-600
-800
400
200
0
-200
-400
-600
-800
NGC7052 Central Slit: ∆v = 280 km s -1
-0.4 -0.2 0.0 0.2 0.4
Position along slit (arcsec)
-ve offset slit position
-0.4 -0.2 0.0 0.2 0.4
Position along slit (arcsec)
+ve offset slit position
-0.4 -0.2 0.0 0.2 0.4
Position along slit (arcsec)
Gas Radial Velocity (km s -1 )
Gas Radial Velocity (km s -1 )
200
0
-200
-400
-600
-800
-1000
200
0
-200
-400
-600
-800
-1000
NGC7052 Central Slit: ∆v = 550 km s -1
-0.4 -0.2 0.0 0.2 0.4 0.6
Position along slit (arcsec)
-ve offset slit position
-0.4 -0.2 0.0 0.2 0.4 0.6
Position along slit (arcsec)
+ve offset slit position
-0.4 -0.2 0.0 0.2 0.4 0.6
Position along slit (arcsec)
Figure 4.39 The observed velocity profiles of NGC 7052 for each of the three observed
slit positions: (left) offset by the velocity and slope calculated in §4.2.5 and (right)
with a velocity offset of 550 km s −1 , and the velocity field running from negative
to positive, which provides a more meaningful fit to the nuclear region (judged by
the author), the velocity fit in §4.2.5 was strongly influenced by the large velocity
feature at ∼ 0. ′′ 15 from the nucleus. The velocities are shown shaded according to the
relative signal-to-noise of each spectrum, formal errors from the fit are also indicated
(see Chapter 3). The three solid lines show model velocity profiles for no black hole,
a 1 × 10 8 M⊙ black hole and a 9 × 10 8 M⊙ (the steeper lines from models with the
greatest black hole mass). See text for details of the models. The dashed vertical lines
give a rough approximation of the radius of influence of a black hole based on the
mass estimate from the M• −σ relation and the size of the random motions observed.
Gas Radial Velocity (km s -1 )
200
0
-200
-400
-600
-800
-1000
226

Gas Radial Velocity (km s -1 )
Gas Radial Velocity (km s -1 )
Gas Radial Velocity (km s -1 )
300
200
100
0
-100
-200
-300
300
200
100
0
-100
-200
-300
300
200
100
0
-100
-200
-300
UGC12064 Central Slit: ∆v = -83 km s -1
-0.4 -0.2 0.0 0.2 0.4 0.6
Position along slit (arcsec)
-ve offset slit position
-0.4 -0.2 0.0 0.2 0.4 0.6
Position along slit (arcsec)
+ve offset slit position
-0.4 -0.2 0.0 0.2 0.4 0.6
Position along slit (arcsec)
Figure 4.40 The observed velocity profiles of UGC 12064 for each of the three observed
slit positions. The velocities are shown shaded according to the relative signal-to-noise
of each spectrum, formal errors from the fit are also indicated (see Chapter 3). The
three solid lines show model velocity profiles for no black hole, a 1 × 10 8 M⊙ black
hole and a 9 × 10 8 M⊙ (the steeper lines from models with the greatest black hole
mass). See text for details of the models. The dashed vertical lines give a rough
approximation of the radius of influence of a black hole based on the mass estimate
from the M• − σ relation and the size of the random motions observed.
227

Gas Radial Velocity (km s -1 )
Gas Radial Velocity (km s -1 )
Gas Radial Velocity (km s -1 )
400
200
0
-200
-400
400
200
0
-200
-400
400
200
0
-200
-400
NGC7626 Central Slit: ∆v = -47 km s -1
-1.0 -0.5 0.0 0.5 1.0
Position along slit (arcsec)
-ve offset slit position
-1.0 -0.5 0.0 0.5 1.0
Position along slit (arcsec)
+ve offset slit position
-1.0 -0.5 0.0 0.5 1.0
Position along slit (arcsec)
Figure 4.41 The observed velocity profiles of NGC 7626 for each of the three observed
slit positions. The velocities are shown shaded according to the relative signal-tonoise
of each spectrum, formal errors from the fit are also indicated (see Chapter 3).
The three solid lines show model velocity profiles for no black hole, a 1 × 10 8 M⊙
black hole and a 9 × 10 8 M⊙ (the steeper lines from models with the greatest black
hole mass). See text for details of the models. The dashed vertical lines give a rough
approximation of the radius of influence of a black hole based on the mass estimate
from the M• − σ relation and the size of the random motions observed.
228

v r (km s −1 )
5000
4800
4600
4400
v r
X = -0.2
X = 0.0
X = +0.2
-1.01 -0.34 0.34 1.01
Y (arcsec)
σ gas (km s −1 )
300
200
100
0
σ gas
X = -0.2
X = 0.0
X = +0.2
-1.01 -0.34 0.34 1.01
Y (arcsec)
F (10 −14 ergs s −1 cm −2 Hz −1 )
1.75
1.25
0.75
0.25
-0.25
-0.75
-1
9
7
5
3
1
0.9
0.7
0.5
0.3
0.1
[NII] 6585 Flux
X = -0.2
X = 0.0
X = +0.2
-0.1
-1.01 -0.34 0.34 1.01
Y (arcsec)
[NII] 6585/Hα
10.0
1.0
0.1
[NII]/Hα
229
X = -0.2
X = 0.0
X = +0.2
-1.01 -0.34 0.34 1.01
Y (arcsec)
Figure 4.42 NGC 4335: velocity, velocity dispersion, flux and flux ratio data (see
Figure 3.1, panel (c) for details). The vertical dash-dot lines in the side slit positions
indicate the projected position of the radio jet.

v r (km s −1 )
3800
3600
3400
3200
v r
X = -0.2
X = 0.0
X = +0.2
-1.01 -0.34 0.34 1.01
Y (arcsec)
σ gas (km s −1 )
400
300
200
100
0
σ gas
X = -0.2
X = 0.0
X = +0.2
-1.01 -0.34 0.34 1.01
Y (arcsec)
F (10 −14 ergs s −1 cm −2 Hz −1 )
0.8
0.6
0.4
0.2
0.0
-0.2
-1
9
7
5
3
1
0.9
0.7
0.5
0.3
0.1
[NII] 6585 Flux
X = -0.2
X = 0.0
X = +0.2
-0.1
-1.01 -0.34 0.34 1.01
Y (arcsec)
[NII] 6585/Hα
10.0
1.0
0.1
[NII]/Hα
230
X = -0.2
X = 0.0
X = +0.2
-1.01 -0.34 0.34 1.01
Y (arcsec)
Figure 4.43 NGC 7626: velocity, velocity dispersion, flux and flux ratio data (see
Figure 3.1, panel (c) for details). The vertical dash-dot lines in the side slit positions
indicate the projected position of the radio jet.

v r (km s −1 )
4700
4600
4500
4400
4300
4200
4100
v r
X = -0.2
X = 0.0
X = +0.2
-1.01 -0.34 0.34 1.01
Y (arcsec)
σ gas (km s −1 )
500
400
300
200
100
0
σ gas
X = -0.2
X = 0.0
X = +0.2
-1.01 -0.34 0.34 1.01
Y (arcsec)
F (10 −14 ergs s −1 cm −2 Hz −1 )
0.5
0.4
0.3
0.2
0.1
0.0
10
8
6
4
2
0
0.4
0.3
0.2
0.1
0.0
[NII] 6585 Flux
X = -0.2
X = 0.0
X = +0.2
-0.1
-1.01 -0.34 0.34 1.01
Y (arcsec)
[NII] 6585/Hα
10.0
1.0
0.1
[NII]/Hα
231
X = -0.2
X = 0.0
X = +0.2
-1.01 -0.34 0.34 1.01
Y (arcsec)
Figure 4.44 NGC 193: velocity, velocity dispersion, flux and flux ratio data (see Figure
3.1, panel (c) for details). The vertical dash-dot lines in the side slit positions indicate
the projected position of the radio jet.

v r (km s −1 )
5300
5200
5100
5000
4900
4800
v r
X = -0.1
X = 0.0
X = +0.1
-0.51 -0.17 0.17 0.51
Y (arcsec)
σ gas (km s −1 )
600
400
200
0
σ gas
X = -0.1
X = 0.0
X = +0.1
-0.51 -0.17 0.17 0.51
Y (arcsec)
F (10 −14 ergs s −1 cm −2 Hz −1 )
2.5
2.0
1.5
1.0
0.5
0.0
22.5
17.5
12.5
7.5
2.5
-2.5
4.5
3.5
2.5
1.5
0.5
[NII] 6585 Flux
X = -0.1
X = 0.0
X = +0.1
-0.5
-0.51 -0.17 0.17 0.51
Y (arcsec)
[NII] 6585/Hα
10.0
1.0
0.1
[NII]/Hα
232
X = -0.1
X = 0.0
X = +0.1
-0.51 -0.17 0.17 0.51
Y (arcsec)
Figure 4.45 UGC 12064: velocity, velocity dispersion, flux and flux ratio data (see
Figure 3.1, panel (c) for details). The vertical dash-dot lines in the side slit positions
indicate the projected position of the radio jet.

M BH (M Sun)
10 10
10 9
10 8
10 7
10 6
60 70 80 90100 200 300 400
σ c (km s -1 )
Figure 4.46 Measured black hole masses (MBH) as a function of central stellar velocity
dispersion (σc) for reliable determinations summarized by Tremaine et al. (2002). The
line indicates the fit M• = 1.3 ×10 8 M⊙(σc/200) 4.72 . (*) indicates masses determined
from stellar dynamical modeling; (◦) indicates masses determined from gas kinematics;
and (△) indicates masses determined from MASER kinematics. Potential black
holes estimated from the central gas kinematic signatures in the UGC FR-I galaxies
(see text) are indicated in bold (see Table 4.6). (×) indicates published black hole
mass measurements for the UGC FR-I galaxies (see Chapter 2).
233

Chapter 5
Nuclear gas kinematics and central
engines
5.1 Introduction
Given the discoveries by Kormendy & Richstone (1995) of a connection between black
hole mass and host galaxy luminosity, and the tighter correlations between the black
hole mass and host kinematics (Gebhardt et al., 2000a; Ferrarese & Merritt, 2000) it
is of interest to investigate how the global properties of the emission line gas relate
to the properties of the host galaxy and central engine in the hopes of uncovering
connections between these systems.
In §3.5 we introduced two parameters to estimate the kinematic properties of
the central 100 pc of each galaxy, along the central slit (Equations 3.4 and 3.5).
234

We showed that the mean dispersions are consistent with being drawn from a single
population (a probability of P = .93 from a Kolmogorov-Smirnov test) and the ∆100pc
is consistent with rotation (i.e. the mean velocities are higher on one side of the nucleus
than the other along the major axis) for all cases other than where the dust disks
are very face on or the central dust morphologies are very complex. We suggested
that this evidence shows that these systems, whether we do or do not see signs of
rotation, represent the same type of kinematic systems, with observational effects
such as inclination and dust properties limiting our ability to detect the rotation in
those systems where we do not. We concluded that a model of a rotating gas disk
with significant random motions is compatible with all of the observations.
In this chapter we will progress from our earlier work to produce parameters that
improve the reliability of our description of the kinematic state of the gas in each
nucleus. We discuss the kinematics of systems that we are viewing from different
inclinations to identify global trends. We then go on to investigate correlations be-
tween these parameters and what they can tell us about the kinematic state of the
gas, before going on to compare the gas and stellar kinematics.
In §5.3 we discuss some properties most closely related to the central engines in
each nucleus: we discuss the broad lines that we identified in Chapter 3 in more depth,
235

and search for correlations with other properties of the central engine that might
indicate a connection between M• (the black hole mass) and/or ˙ M, the accretion
rate (or at least the central engine fueling rate) in the nucleus. We also extend
the earlier work of Verdoes Kleijn et al. (2002a), correlating fluxes in the nucleus of
each galaxy, out to the X-ray regime. Finally we will discuss connections between
kinematic parameters and the properties of the central engines.
5.2 Global kinematic parameterizations
In order to more reliably parameterize the kinematics in the nucleus of each galaxy,
we now define three weighted-mean parameters: (i) the difference in the weighted
mean gas velocity within 100 pc on each side of the nucleus:
�⎛
�
�
∆100 = �⎝
�
�
� vj
j
236
/
dvj
�
⎞ �
1 � vk ⎠ − /
dvj dvk
�
�
1
dvk
� �
����
; (5.1)
j
(ii) the mean velocity dispersion of the gas within 100 pc of the nucleus:
σ100 = �
i
σi
dσi
� �
i
k
1
dσi
k
� −1
; (5.2)
and (iii) an estimator of the point-to-point variations in the gas velocity profile

within 100 pc of the nucleus:
�
N−1 � �
�
�
�
i=2
ɛ100 =
� vi−1
dvi−1
+ vi+1
� �
1
/ +
dvi+1 dvi−1
1
�
dvi+1
N−1
�
i=2
1
dvi
These parameters are defined over the region such that
�
�
�
− vi�
�
· 1
dvi
237
. (5.3)
|xi| ≤ 100pc, (5.4)
−100pc ≤ xj < 0pc, and (5.5)
0pc < xk ≤ 100pc. (5.6)
vj are the gas velocities and σj are the gas velocity dispersions measured in each
spectrum j; dvj and dσj are their respective formal errors. All of the parameters
were measured along the central slit position only (and in the negative offset slit only
for NGC 4261, which appears to be closer to the nucleus of that galaxy). We give
the values of these parameters for each galaxy in Table 5.1. We do not include the
galaxies NGC 741 or NGC 5490 in the discussions in this chapter as both of these
galaxies have very low signal to noise out to 100 pc so provide very unreliable data.
In the following discussions where we describe ‘no-correlation’ we have tested that
the probability of a linear correlation P ≪ .0001 from a χ 2 test of the best fitting
straight line.

5.2.1 Effects of inclination
We use the dust disk axis ratio (b/a) or dust lane width : length ratio as an indicator
of the inclination of the nuclear gas and dust. In Figures 5.1, 5.2 and 5.3 we plot
∆100, σ100 and ɛ100 respectively against this dust axis ratio parameter. This leads
naturally to the most edge on systems being plotted at the left (where the galaxies
with dust lanes are found) to face on systems at the right (which include face on
disks where we are unable to pick up the rotation profile). The fact that systems
with dust lanes and dust disks form a continuum in all of these parameters suggests
that the lanes observed may be the edges of highly inclined dust disks rather than
being physically distinct types of systems. Verdoes Kleijn et al. (1999) found that dust
lanes and disks may represent distinct physical systems, primarily based on increased
irregular structure observed in lane systems and misalignments with the major axes.
It is possible that if the dust is indeed in two distinct morphological types, that the
gas forms into a kinematically similar system in either case. In the light of evidence
relating to the settling of the gas perpendicular to the disk presented below, it is
also possible that the observed irregularities in dust lane systems originate from less
settled motions out of the plane of the disk.
238
In Figure 5.1 it is possible to see a decreasing upper envelope to the value of ∆100

as face on disks are approached; the observed velocity difference is smaller, which is
as we would expect. The face on disks do not, however, sit at a value of ∆100 = 0,
indicating that there may be motions perpendicular to the plane of the disk across
the nuclei of these galaxies (for example precession of the disk), which may indicate
they are not settled into the major plane of the galaxy. However, we cannot rule
out the possibility that they are simply amongst the fastest rotators in the sample
– the small number statistics do not present strong constraints. Lines are indicated
where we approximately project the ‘intrinsic’ ∆int through inclination using the
relationship:
�
�
�
�
∆obs ≈ ∆int sin i ≈ ∆int × 1 −
239
� �2 b
, (5.7)
a
Two outliers are labeled in the figure: NGC 383 and UGC 7115 which, despite
being fairly face on, have large values of ∆100. In the case of NGC 383 it seems
that the observed rotation is compatible with the fastest rotating sample members
that are viewed edge on. Those fastest edge-on galaxies are NGC 4486 and M84,
which are both nearby so that ∆100 includes a great deal more of the resolved central
velocities, which makes comparisons with other galaxies less meaningful, and thus
leaves NGC 383 as an outlier. The large values of ∆100 may be an indicator that the
gas in these two galaxies is indeed rotating very fast, that there are gas systems present
that are very poorly described by the thin disk model, or that the dust distribution

is not a good indicator of the gas distribution for these galaxies.
In Figure 5.2 we show the weighted mean velocity dispersion (σ100) as a function
of the axis ratio. Here it is clear that there is no relationship between this parameter
and the inclination. We interpret this to mean that the velocity dispersion is fairly
evenly distributed three-dimensionally, so is not just a consequence of observing the
organized motions from different angles, but is an intrinsic property of the gas within
the disks. The slight rise seen from the lowest to highest dust ratios is likely a
consequence of the σ100 parameter picking up more of the organized motion, but this
is a small effect. As mentioned in §4.2.4, gas at T ∼ 10 4 K would have a thermal
velocity dispersion of σth ∼ 10 km s −1 , which is well below the minimum observed
dispersion in any of the galaxies, indicating that non-thermal random motions are
present (and important) in all of the gas disks.
We again highlight the galaxy NGC 383, which also sits high in the velocity
dispersion distribution. The fact that this galaxy is high in both parameters may
indicate that the gas is in a state far from being satisfactorily represented by a settled
thin disk.
We show the point-to-point variations in the gas velocity profile, as parameterized
by ɛ100 in Figure 5.3. Here we observe that, for the most part, ɛ100 is not a function of
240

the inclination of the dust disk. Other than two outliers that we indicate (NGC 7052
and UGC 7115), it seems that the mean point-to-point variations sit between ∼
20 km s −1 (comparable to the expected velocity errors in the data, see Chapter 3)
and ∼ 80 km s −1 , other than in face on systems. In the face on systems it seems
that we may pick up motions perpendicular to the plane of the disk. These motions
could indicate that while the disk is settling into a preferred plane in the gravitational
potential of the galaxy, that the motions perpendicular to that plane have not yet
settled out into a smooth disk, and that the settling time for these motions may be
long compared to other dynamical time-scales in the disk.
The outlier NGC 7052 has a very high value of ɛ100 due to the very large (∼
1000 km s −1 ) break in the velocity profile along the central slit in this galaxy (see
Figures 4.39 and 3.20). This is not a true point-to-point variation, but may be due
to a second dynamical system in the gas; this parameter is taking on a very different
meaning for this galaxy, so the data point is not representative. In UGC 7115, the fact
that both ɛ100 and ∆100 are high could indicate that there are considerable motions
in the gas in this galaxy out of the plane of the disk. Unfortunately as only one slit
position was observed for this galaxy (see Chapter 3), we have no two-dimensional
information about the kinematics, which we would need in order to interpret these
motions further.
241

Comparisons of the form σ 2 /v 2 are typically used as indicators of the energy divi-
sion between random and systematic motions and in Figure 5.4 we show σ100 2 /∆ 2 100.
We notice that the dust lane systems all lie near the bottom of the distribution –
compatible with the idea that here we are picking up the motions from edge on disks
– and that the irregular systems sit near the top of the distribution – compatible with
the suggestion that galaxies with less regular nuclear morphologies would be prone to
have greater random motions. The profile shows an upward slope as we move from
edge on to face on systems and we are able to see less of the organized motion. The
three outlying galaxies from earlier discussions are again highlighted, though none
are outliers here. This is interesting for NGC 383 as it confirms that though the
organized and random motions are both large, the partition of energy is not unusual.
5.2.2 Correlations between kinematic parameters
Figure 5.5 shows σ100 as a function of ∆100. We can pick out no apparent relation-
ship between the two. We made a division at ∆100 = 180 km s −1 into low-∆100 and
high-∆100 systems. The low-∆100 systems have a mean σ100 = 233 ± 98 km s −1 and
the high-∆100 systems have a mean σ100 = 232 ± 85 km s −1 . The two groups have a
probability of P = .61 (from a Kolmogorov-Smirnov statistic) of being drawn from
the same population, i.e. there is no distinction in velocity dispersion in systems
242

where we observe smaller and larger organized motions. This result does not signif-
icantly change if we exclude the two outlying results from above, highlighted again
here. Though the distribution now looks tighter for the high-∆100 systems, the two
distributions are still not significantly different.
We also note that in all of the systems where ∆100 dominates over σ100 that we
observe rotation, and that all of the dust lane (i.e. the most edge on) systems lie
in this regime. These systems are the ones where the a larger portion of the gas
kinetic energy is in organized rotational motion in the disk and likely more strongly
gravitationally bound, rather than below the line where a larger fraction of the kinetic
energy is in random motions, and the gas may not be so well gravitationally bound.
In §5.2.1, we noted that the face on systems appear to have higher ɛ100 than do
the edge on systems, and commented that this could be due to dissipations organizing
the motion in the preferred plane only, with motions in other directions taking longer
to settle into the disk. This result is supported by an apparent upper envelope to the
value of ɛ100 as a function of ∆100 that we show in Figure 5.6. We must here ignore the
two outliers NGC 7052 and UGC 7115, which we feel confident in doing for reasons
described above. The descending upper limit on the value of ɛ100 indicates that in
the systems where we observe more of the rotational motion, we are able to see less
243

‘disorganized’ point-to-point motions. Again, the systems where we do not observe
rotation (empty symbols) tend to lie towards the top of the envelope and include
the face on disks. NGC 383, highlighted earlier, does not lie outside expectations -
indicating it is settling just as the other disks are but with considerably higher energy.
From Figure 5.7 we can appreciate that the values of ɛ100 are consistently lower
than the values of σ100 though these two parameters show no particular relationship
beyond that. This indicates to us that the small scale 3D random motions, as seen
in the velocity dispersion, are a more significant kinematic factor in the disks than
larger scale point-to-point motions. This would be compatible with a picture where
the gas is made up of turbulent cells, where the cells are settling into a disk and losing
their random bulk motions to rotation, while maintaining at least a large portion of
their intrinsic turbulence. Numerical simulations of the gas in the nuclei of galaxies
suggest that clumpy turbulent structures may be a common feature of systems where
active fueling of the central engine is taking place (see e.g. Wada, 2004, for a recent
review).
5.2.3 Relationships to the stellar kinematics
We described the central stellar velocity dispersion σc in Chapter 2, and values of that
parameter were given in Table 2.3. We remind the reader here that σc is measured
244

on scales of 1/8 the Effective radius of each galaxy, which is larger than the nuclear
regions we discuss in this dissertation. Correlations between σc and M• may be valid
for radio galaxies (§4.4.1) other than for a few examples; in the following discussions
we will use σc as an approximate proxy for M•.
In Figure 5.8 we see no relationship whatsoever between the value of ∆100 and the
central stellar velocity dispersion, nor is the correlation improved if we investigate one
particular dust-morphology group at a time. ∆100 is not a good tracer of the central
potential (it is, of course, subject to effects of the inclination at the very least).
Figure 5.9 shows that the velocity dispersion of the gas is closely related to the
velocity dispersion of the stars. This probably implies that the stellar velocity dis-
persion drives the gas velocity dispersion to some extent, and may be an important
factor in why the velocity dispersion of the gas remains high, and does not settle into
a cold thin disk. In a similar data set to our own for 54 spiral galaxies 1 where the
stellar velocity dispersions are lower, the emission line gas dispersions are also low (D.
Axon, Private Communication), indicating that some factors driving this relationship
may apply between morphological types. Straight line fits are shown including all the
data and also with the four identified high outliers excluded. The fits have reduced-
1 The spiral sample is described by Hughes et al. (2003), ∼ 65% of the galaxies show some kind
of activity.
245

χ 2 parameters = 0.25 and 0.81 respectively, indicating a good fit in the latter case.
NGC 383 and UGC 7115 have already been identified as somewhat unusual, so it may
be reasonable to exclude them once more.
In Figure 5.10 we see again that the point-to-point variations in the motion are
smaller than the velocity dispersions, and again the motion is not correlated with σc.
This indicates to us that these point-to-point motions are not driven by the large-scale
gravitational potential of the galaxy and black hole, nor by the random motions of
the stars in this region (as σc is measured on large scales it includes any comparable
point-to-point motions if such motions exist).
We show the parameter σ100 2 /∆ 2 100 once more, now as a function of σc, in Figure
5.11. Again no correlation exists between this pair of parameters, though this tells
us that the velocity dispersion of the stars, though driving the velocity dispersion of
the gas, does not have strong consequences for the division of kinetic energy in the
gas over the rotational motion in the gravitational potential.
5.3 The central engines
In this section we discuss the broad components that we found improved the fit to the
very central spectra in §3.3.2 further, as we anticipate that these broad components
246

may have some connections with the central engines. We next discuss correlations
between the nuclear fluxes across many different wave-bands, and then correlations
between properties of the host galaxies and central engines.
5.3.1 Are the Broad Lines physical?
In Chapter 3 (§3.3.2) we showed that fits to the very central spectra improved with
the inclusion of a broad component which we attributed to either a physical broad
line region or an artifact of fitting to an asymmetrical line shape (§3.5.3). It is likely
that both of these factors do indeed play a role.
Whittle (1985) found relationships between narrow-line widths and shapes (of
[O III]) and the radio properties of the galaxies. If modifications to the velocity pro-
file of the narrow lines in the nuclear regions can occur (e.g. from jet interactions and
outflows) then this may indeed modify the line profiles so that a broad component
would improve the fit. Deeper observations of the sample nuclei are necessary before
we can perform multi-Gaussian fits, such as those described in §3.5.4, which would
enable us to better disentangle light from broad emission line regions to modifica-
tions of the narrow line shapes, though the results in that section suggest models
with a combination of asymmetric profiles and a broad component provide the best
representation of the central spectra.
247

Barth et al. (1999) found polarized Hα broad line emission in the nucleus of
NGC 315, and fit a profile of FWHM 3200 km s −1 in polarized light. This gives
σBL ∼ 1400 km s −1 which is certainly compatible with our earlier measurement of
1790 km s −1 where the errors were likely to be large. They also made observations
of NGC 4261, but were unable to readily separate a broad component; this matches
our findings shown in Table 3.27 that the broad line in NGC 4261 was a less strong
detection than the one in NGC 315.
Barth, et al.’s findings suggests that at least some of the broad emission we see
originates in physical broad-line regions. The broad emission comes from systems
closest to the central engine, as expected from the AGN unified model paradigm
(Urry & Padovani, 1995). The two primary sources to drive the broad line width are
therefore the gravitational potential in the central region (which is dominated by M•
in this regime) and the activity of the central engine (which is dominated by ˙ M). We
will revisit this issue later.
For the 11 galaxies where we were able to detect a broad component we measured
the kinematic properties of the Broad and Narrow lines, these were presented in
Table 3.28. Cross-correlating the velocity dispersions of these lines with the central
stellar velocity dispersion (σc) we find that neither the narrow nor broad component
248

is well correlated with σc (correlation coefficients .49 and .46 respectively). Though
we described above how the velocity dispersion on scales of 100 pc was driven by the
velocity dispersion of the stars, it seems that this driver is not the dominant factor
in the nuclear region.
As we may use σc as an approximate proxy for M• the poor correlation above in-
dicates that the gas does not show signs of originating in an isotropic gravitationally-
driven source in the nuclear region. If the broad line originated from a disk in the
central region then it might be expected that a correlation between σc and σBL/ sin i
may exit, but these two parameters correlate with a similar cross-correlation coeffi-
cient of .48, though we can not rule out the possibility that the nuclear disk is at a
very different inclination to the outer regions.
5.3.2 Correlation of nuclear fluxes
Verdoes Kleijn et al. (2002a) present correlations between the nuclear fluxes in the
radio and optical regimes for each galaxy, we presented those nuclear fluxes in Table
2.2, along with newly determined X-ray fluxes. In Table 5.2 we show that the X-ray
flux also correlates well with the other nuclear fluxes. We show the flux parameters
plotted against each other in Figure 5.12. Though we have only five X-ray data points
at this stage so the statistical significance is still low, it is a strong hint that, as one
249

might expect, the X-ray flux originates from the same physical processes in (or close
to) the central engine or jet bases as the other nuclear fluxes. We explain the tighter
correlation between X-ray and radio fluxes in that these two parameters are the least
likely to be contaminated by stellar light.
In Figure 5.13 we show the Spectral Energy Distributions (SEDS) for the 5 sample
galaxies where we have data at each wavelength, which do show fairly similar shapes
as implied by the above correlations. In Figure 5.14 we show data for the nucleus of
M87 (from Perlman et al., 2001) along with a set of emission mechanisms illustrative of
the type that may be present in the central engine (di Matteo et al., 2000) and would
produce correlations between the nuclear fluxes (e.g. various synchrotron models from
jets, and Advection Dominated Accretion Flows with dominant outflows or dominant
disks). Our data represent the outline shape of these models well, and more detailed
analysis and modeling may yield information about the relative contributions of jets
and disks in the nuclear light.
5.3.3 Correlations between host galaxy and central engine
In Table 5.3 we show the cross-correlation coefficients between Broad and Narrow
line widths and the X-ray and VLBA luminosities in the nucleus. The correlations
between the X-ray and Radio fluxes and σBL suggest that the Broad Line width may
250

e primarily driven by the central engine, and so ˙ M may be the more important
factor rather than M•. This is supported by the poor correlation between σc and σBL
discussed above. Some component of the broad line may be driven by the central
mass, but it certainly seems here that the more important factor may be the energy
released by processes in the central engine.
That there is no relationship between σBL and σc or the emission fluxes from the
nucleus and σc suggests that there is no connection of the form
˙M
M•
251
= f, (5.8)
(where again we use σc as a proxy for black hole mass, M•), which would be the
case if the central engine was being fueled at some particular fraction of the Eddington
luminosity in FR-I galaxies. In a sample of radio loud and radio quiet quasars and
radio galaxies, Dunlop et al. (2003) found that the maximum and minimum limits
of the emission may be set by the black hole mass, but that the emission was not
at a particular fraction of the Eddington luminosity. This also implies that while
the velocity dispersion of the stars drives the velocity dispersion of the gas, it is not
directly related to the present day fueling rate of the central engine by that gas.
Modeling of the broad line could provide further hints towards the connections
between galaxy and central engine, but deeper observations would be required to get

a good handle on the properties of the broad lines in our sample nuclei.
5.4 Conclusions
In this chapter we characterized the kinematics of the nuclear regions through three
parameters, measured within 100 pc of the nucleus, along the central slit position
observed: σ100, the weighted mean gas velocity dispersion; ∆100, the difference in
weighted mean velocity on each side of the nucleus; and ɛ100, an estimator of the
weighted mean point-to-point variations in the velocity profile.
We showed that the point-to-point variations in the velocity profiles are largest
perpendicular to the preferred plane of rotation in the nuclei, indicating that these
motions originate from velocity components that are not yet settled into a thin disk
configuration. We found that the velocity dispersion is distributed fairly evenly in
all orientations, so likely originates from intrinsically isotropic random motions. We
found that there may be bulk motions of the entire disk, as the difference in mean
velocities on each side of the nucleus does not vanish (and remains larger than the
size of the typical errors) even in face on systems.
Investigating relationships between these kinematic parameters we confirmed that
we can observe greater point-to-point variations in systems where we observe less
252

organized rotation. This supports the picture described above, and the view that
dispersive effects are less efficient perpendicular to the plane of the disk, so settling
may be slow, which supports the picture we developed for the nuclei of these galaxies
in Chapter 4.
Comparing to the central stellar velocity dispersion, as discussed in Chapters 1
and 2, we found that the stellar velocity dispersion and the gas velocity dispersions
are closely related, implying that the stellar dispersion drives some of the random
motions in the gas. This has possible implications for fueling of the black hole, and
connections between the stellar velocity dispersion and central engine.
We presented some evidence that the broad components used in earlier fits (Chap-
ter 3) may originate from physical broad-line regions in the galaxy. We also showed
that newly obtained X-ray fluxes are correlated with other fluxes in the nuclear re-
gions, extending the correlations found by Verdoes Kleijn et al. (2002a) to a new
wavelength regime. Finally we found correlations between the broad line width and
the VLBA and X-ray luminosities indicating that the activity of the central engine
may be responsible for driving a large component of the dispersion in this gas, rather
than it being due to gravitational motion around the black hole. As we cannot con-
firm that the M• − σc relation applies to all radio galaxies, we can not determine if
253

the activity in the central engine is also related to the black hole mass, however such
a relationship does not appear to exist. More detailed observations and modeling of
the broad line may shed some light on this issue in future.
254

Table 5.1. Weighted mean kinematic parameters.
Galaxy ∆100 σ100 ɛ100
(km s −1 ) (km s −1 ) (km s −1 )
(1) (2) (3) (4)
NGC 193 158 228 100
NGC 315 141 333 73
NGC 383 235 399 60
NGC 541 135 182 127
UGC 1841 87 392 137
NGC 2329 56 149 32
NGC 2892 96 370 56
NGC 3801 52 157 27
NGC 3862 82 182 90
UGC 7115 291 287 192
NGC 4261 143 224 28
NGC 4335 214 166 18
M84 381 229 45
NGC 4486 438 313 33
NGC 5127 124 105 31
NGC 5141 152 145 31
NGC 7052 242 178 194
UGC 12064 86 327 69
NGC 7626 331 190 65
Mean 181 240 74
StDev 112 92 54
Note. — Col. (1): Galaxy Name; Cols. (2-4):
Weighted mean kinematic parameters within
100 pc of the brightest point in the nucleus of
each galaxy. See text for definitions.
255

Table 5.2. Correlation of X-ray flux with other nuclear flux parameters.
Parameter X-raysoft X-rayhard
Inuc .74 .12
Vnuc .94 .50
VLBApeak .99 .76
VLApeak .95 .89
Note. — Cross-correlation coefficients
are shown between each parameter
pair. See Chapter 2, Table
2.2 and discussion for a description
and listing of all of the parameters
used.
256

Table 5.3. Correlations between kinematic parameters and nuclear fluxes.
σNL σBL VLBApeak X-raysoft X-rayhard
σNL 1.00 .39 .31 -.38 -.42
σBL 1.00 .70 .69 .86
VLBApeak 1.00 .99 .76
X-raysoft 1.00 .75
X-rayhard
1.00
Note. — Cross-correlation coefficients between nuclear narrow
(σNL) and broad (σBL) line velocity dispersions and nuclear
flux parameters (see Chapter 2, fluxes were then corrected
for distance)
257

∆ 100 (km s -1 )
500
400
300
200
100
NGC383
UGC7115
0
0.0 0.2 0.4 0.6 0.8 1.0
Dust axis ratio (b/a or width/length)
Figure 5.1 Difference in weighted mean velocity within 100 pc on each side of the
nucleus (∆100, see text) along the central slit of each galaxy as a function of dust disk
axis ratio (b/a) or dust lane width : length ratio, which is an indicator of inclination.
The solid lines indicate intrinsic values of ∆100 approximately projected for varying
inclinations with ∆int = 100, 250 and 400 km s −1 . The different kinematic classes and
dust morphologies (see Chapter 3) are indicated. Filled symbols represent rotators:
with dust disks (•), with dust lanes (�) or with irregular dust (�); Empty symbols
represent non-rotators: with dust disks (◦), with dust lanes (�) or with no-dust or
irregular dust (△).
258

σ100 (km s -1 −−−
)
500
400
300
200
100
NGC383
0
0.0 0.2 0.4 0.6 0.8 1.0
Dust axis ratio (b/a or width/length)
Figure 5.2 Weighted mean gas velocity dispersion (σ100) along the central slit of each
galaxy as a function of dust disk axis ratio (b/a) or dust lane width : length ratio,
which is an indicator of inclination. The different kinematic classes and dust morphologies
(see Chapter 3) are indicated. Filled symbols represent rotators: with dust
disks (•), with dust lanes (�) or with irregular dust (�); Empty symbols represent
non-rotators: with dust disks (◦), with dust lanes (�) or with no-dust or irregular
dust (△).
259

ε 100 (km s -1 )
250
200
150
100
50
NGC7052 UGC7115
0
0.0 0.2 0.4 0.6 0.8 1.0
Dust axis ratio (b/a or width/length)
Figure 5.3 Weighted mean point-to-point variations in gas velocity (ɛ100) along the
central slit as a function of dust disk axis ratio (b/a) or dust lane width : length ratio,
which is an indicator of inclination. The different kinematic classes and dust morphologies
(see Chapter 3) are indicated. Filled symbols represent rotators: with dust
disks (•), with dust lanes (�) or with irregular dust (�); Empty symbols represent
non-rotators: with dust disks (◦), with dust lanes (�) or with no-dust or irregular
dust (△).
260

−−− 2 2
σ100 / ∆100
100.00
10.00
1.00
0.10
NGC7052
NGC383
UGC7115
0.01
0.0 0.2 0.4 0.6 0.8 1.0
Dust axis ratio (b/a or width/length)
Figure 5.4 σ100 2 /∆2 100 as a function of dust disk axis ratio (b/a) or dust lane width :
length ratio, which is an indicator of inclination. The different kinematic classes and
dust morphologies (see Chapter 3) are indicated. Filled symbols represent rotators:
with dust disks (•), with dust lanes (�) or with irregular dust (�); Empty symbols
represent non-rotators: with dust disks (◦), with dust lanes (�) or with no-dust or
irregular dust (△).
261

σ100 (km s -1 −−−
)
500
400
300
200
100
NGC383
UGC7115
0 100 200 300 400 500
∆100 (km s -1 0
)
Figure 5.5 σ100 as a function of ∆100 for the sample nuclei (see text for definitions).
The solid line indicates a 1:1 ratio of the two parameters. The different kinematic
classes and dust morphologies (see Chapter 3) are indicated. Filled symbols represent
rotators: with dust disks (•), with dust lanes (�) or with irregular dust (�); Empty
symbols represent non-rotators: with dust disks (◦), with dust lanes (�) or with
no-dust or irregular dust (△).
262

ε 100 (km s -1 )
250
200
150
100
50
NGC7052
NGC383
UGC7115
0 100 200 300 400 500
∆100 (km s -1 0
)
Figure 5.6 ɛ100 as a function of ∆100 for the sample nuclei (see text for definitions).
The solid line indicates a 1:1 ratio of the two parameters. The different kinematic
classes and dust morphologies (see Chapter 3) are indicated. Filled symbols represent
rotators: with dust disks (•), with dust lanes (�) or with irregular dust (�); Empty
symbols represent non-rotators: with dust disks (◦), with dust lanes (�) or with
no-dust or irregular dust (△).
263

ε 100 (km s -1 )
250
200
150
100
50
NGC7052 UGC7115
NGC383
0 100 200 300
σ100 (km s
400 500
-1 0
−−−
)
Figure 5.7 ɛ100 as a function of σ100 for the sample nuclei (see text for definitions).
The solid line indicates a 1:1 ratio of the two parameters. The different kinematic
classes and dust morphologies (see Chapter 3) are indicated. Filled symbols represent
rotators: with dust disks (•), with dust lanes (�) or with irregular dust (�); Empty
symbols represent non-rotators: with dust disks (◦), with dust lanes (�) or with
no-dust or irregular dust (△).
264

∆ 100 (km s -1 )
500
400
300
200
100
0 100 200 300 400 500
Stellar velocity dispersion: σc (km s -1 0
)
Figure 5.8 ∆100 (see text) for each nucleus as a function of the central stellar velocity
dispersion (σc, see Chapter 2). The solid line indicates a 1:1 ratio of the two parameters.
The different kinematic classes and dust morphologies (see Chapter 3) are
indicated. Filled symbols represent rotators: with dust disks (•), with dust lanes
(�) or with irregular dust (�); Empty symbols represent non-rotators: with dust disks
(◦), with dust lanes (�) or with no-dust or irregular dust (△).
265

σ100 (km s -1 −−−
)
500
400
300
200
100
UGC7115
NGC383
UGC12064
UGC1841
0 100 200 300 400 500
Stellar velocity dispersion: σc (km s -1 0
)
Figure 5.9 σ100 (see text) for each nucleus as a function of the central stellar velocity
dispersion (σc, see Chapter 2). The solid line indicates a 1:1 ratio of the two parameters.
The dash-dot and dotted lines are straight line fits with all of the data
included, and excluding the four labeled points, respectively. The different kinematic
classes and dust morphologies (see Chapter 3) are indicated. Filled symbols represent
rotators: with dust disks (•), with dust lanes (�) or with irregular dust (�); Empty
symbols represent non-rotators: with dust disks (◦), with dust lanes (�) or with
no-dust or irregular dust (△).
266

ε 100 (km s -1 )
250
200
150
100
50
UGC7115
NGC7052
0 100 200 300 400 500
Stellar velocity dispersion: σc (km s -1 0
)
Figure 5.10 ɛ100 (see text) for each nucleus as a function of the central stellar velocity
dispersion (σc, see Chapter 2). The solid line indicates a 1:1 ratio of the two parameters.
The different kinematic classes and dust morphologies (see Chapter 3) are
indicated. Filled symbols represent rotators: with dust disks (•), with dust lanes
(�) or with irregular dust (�); Empty symbols represent non-rotators: with dust disks
(◦), with dust lanes (�) or with no-dust or irregular dust (△).
267

−−− 2 2
σ100 / ∆100
100.00
10.00
1.00
0.10
0 100 200 300 400 500
Stellar velocity dispersion: σc (km s -1 0.01
)
Figure 5.11 σ1002 /∆2 100 (see text) for each nucleus as a function of the central stellar
velocity dispersion (σc, see Chapter 2). The different kinematic classes and dust morphologies
(see Chapter 3) are indicated. Filled symbols represent rotators: with dust
disks (•), with dust lanes (�) or with irregular dust (�); Empty symbols represent
non-rotators: with dust disks (◦), with dust lanes (�) or with no-dust or irregular
dust (△).
268

V-Band
I-Band
VLA Peak
VLBA Peak
10 -16
10 -17
10 -18
10 -16
10 -17
1000
100
10 -14
10 -14
10
1000
100
10 -14
10
10 -14
10 -13
Soft X-Ray
10 -13
Soft X-Ray
10 -13
Soft X-Ray
10 -13
Soft X-Ray
10 -12
10 -12
10 -12
10 -12
V-Band
I-Band
VLA Peak
VLBA Peak
10 -16
10 -17
10 -18
10 -16
10 -17
1000
100
10 -14
10 -14
10
10 -14
10 -14
10 -13
Hard X-Ray
10 -13
Hard X-Ray
10 -13
Hard X-Ray
10 -13
Hard X-Ray
Figure 5.12 Pairs of nuclear flux parameters are shown, plotted against the Soft (left
panels) and Hard (right panels) X-ray fluxes. From top to bottom we show V -Band,
I-Band, VLA Peak flux and VLBA Peak flux (flux parameters are given in Table 2.2).
The dash-dot line shows the best fitting power law relationship. The cross-correlation
coefficients between the parameters shown are listed in Table 5.2.
1000
100
10
10 -12
10 -12
10 -12
10 -12
269

log Luminosity (erg s -1 )
44
42
40
38
36
8 10 12 14 16 18
log Frequency (Hz)
Figure 5.13 Nuclear Spectral Energy Distributions for 5 of the UGC FR-I sample
galaxies for which data exists. We include 1.6 GHz VLBA, HST/WFPC2 V and I
band and Chandra X-ray data points. (◦ - NGC 315; � - NGC 383; � - UGC 1841;
• - NGC 4261; △ - M84)
270

42
41
40
39
38
M87 nuclear SED
37
8 10 12 14 16 18
Figure 5.14 M87 Nuclear SED: Data from Perlman et al. (2001). The dotted
and short-dashed lines are Kardashev-Pacholczyk and Continuous Injection synchrotron
fits to the spectrum respectively. The long-dashed and dot-dashed lines are
ADAF+Outflow and ADAF+Disk models respectively (Quataert & Narayan, 2001;
di Matteo et al., 2000), with thanks to Tiziana Di Matteo. The ADAF models are
templates for illustration and are not fits to the data.
271

Chapter 6
Conclusions
We begin by summarizing the results presented through this dissertation, placing
those conclusions in the context of the questions asked in the introduction. We then
go on to discuss future directions in this field.
6.1 Summary
In the introduction we posed four specific questions relating to the work undertaken
in this thesis:
• What is the nature of the spectra observed from the nuclei of nearby radio
galaxies?
• What can be said about the masses of the black holes in these radio galaxies
272

ased on the gas kinematics?
• How is the gas organized in the central regions?
• What connections can be found between the central engines and that gas?
Here we summarize the conclusions we came to through this dissertation in the
context of those questions.
What is the nature of the spectra observed from the nuclei of nearby
radio galaxies? In Chapter 3, we presented medium resolution spectra obtained
using STIS on board the HST for the 21 galaxies in the UGC FR-I sample (Chapter
2), using three parallel adjacent spectroscopic slit positions to map the gas kinematics.
We find that the gas in all of the nuclei is compatible with a single kinematic
description: a rotating gas disk, where random motions are always important. We
see patterns reminiscent of rotation in 67% of the nuclei, in the remainder of the
galaxies the non-detection is accounted for by either face on morphologies or complex
central morphologies (Chapter 3).
We find that the inclusion of an additional broad component improves the fit to
the spectrum in 62% of the galaxies, in the vicinity of the Hα + [N II] complex. The
273

detection of the broad component is flux limited. The broad components have a mean
velocity dispersion of 1349 ±345km s −1 and, assuming an origin in Hα are redshifted
by an average of 486 ± 443km s −1 (Chapter 3). The broad components could be
a consequence of non-Gaussian line profiles with wings or from physical broad line
regions (Chapter 5).
What can be said about the masses of the black holes in these radio galaxies
based on the gas kinematics? In Chapter 4, we compared the observed profiles
to model profiles from thin gas disks in gravitational potentials including no black
hole, and 1 × 10 8 M⊙ and 9 × 10 8 M⊙ black holes.
In 6 of 19 galaxies for which we produced thin disk models we could not identify
any of the observed kinematics with the models. For 3 of the remaining 13 galaxies
we observed a signature compatible with a black hole in the range 1×10 8 M⊙ < M• <
9 ×10 8 M⊙, for 5 we observe kinematic signatures compatible with M• ∼ > 9 ×108 M⊙.
NGC 4261 has a profile compatible with a ∼ 1×10 8 M⊙ black hole, though this result
is highly unreliable due to observational problems. These masses are compatible with
the predictions of the M• − σc relationship of Merritt & Ferrarese (2001), however
we do not consider them to be reliable mass determinations as we find unsettled
motions in the gas play a very significant role in the observed kinematics. The three
274

emaining galaxies may be of particular interest: NGC 4335 and NGC 5141 have the
most settled observed velocity profiles out to 100 pc, however in both of these cases
we find that no black hole is necessary to fit the observed kinematics; in NGC 2329
the central slope is very shallow compared to all rotating thin disk models, suggesting
that inflow could be important (Chapter 4).
How is the gas organized in the central regions? In Chapter 5, we used
weighted mean parameters within 100 pc of the center of each nucleus to describe the
kinematic state of the gas.
We showed that the point-to-point variations in the velocity profiles are largest
perpendicular to the preferred plane of rotation in the nuclei, indicating that these
motions originate from velocity components that have not settled into a thin disk
configuration. We found that the velocity dispersion is distributed fairly evenly in all
orientations, so likely originates from intrinsically isotropic random motions. Even
in face on systems we observe differences in the mean velocities on either side of the
nucleus, indicating we may be observing bulk motions of the disk. From this set of
evidence we conclude that the gas disks are not intrinsically settled and are probably
not well settled into the major plane of the galaxy potential (Chapter 5).
275

What connections can be found between the central engines and that gas?
We showed that the nuclear fluxes are well correlated from radio to x-ray wavelengths,
suggesting a common source for the emission in the central engine, either from the
accretion disk or from the jet bases. These fluxes appear to correlate with the broad
line velocity dispersion, though with fairly small number statistics (Chapter 5).
We found that the mean gas velocity dispersion within 100 pc of the nucleus is
closely related to the mean stellar velocity dispersion, implying that the stellar dis-
persion drives the random motions in the gas (or that both sets of motion, though
measured on very different scales, are governed by a common factor). This has possi-
ble implications for the fueling and growth of the black hole, and connections between
the stellar velocity dispersion and central engine (Chapter 5).
6.2 Future directions
We have convincingly found that the gas disks in the nuclei of nearby radio galaxies
are not well settled, and are not necessarily lying in the major planes of the galactic
potentials. These unsettled motions have important implications for mass models
based on gas dynamics in galaxies.
276
The M• − σc relation is now becoming a common estimator of black hole masses

in nearby galaxies, and is being used to calibrate other indicators of black hole mass
(such as the use of particular emission line widths), which may be applied more
distantly in the universe. 25% of the ‘good’ black hole determinations available to
date (Tremaine et al., 2002) are based on gas dynamics, so understanding the gas
systems in the nuclei of galaxies is key in ensuring that the M• − σc relation is built
on strong foundations so that it can reliably be applied with the level of assurance
that appears to be becoming common practice.
Progress in explaining the motions that we observe can be made by mapping the
spectra over a larger area of the nuclei, either through the use of multiple spectro-
scopic slit positions, or by using more recently developed integral field spectrographs
which can produce three-dimensional (x,y,λ) maps of large areas simultaneously. The
instruments of choice at the time of writing are STIS on HST for long slit spectra
(Brown et al., 2002), or SAURON on the William Herschell Telescope and OASIS on
the Canada-France-Hawaii Telescope for integral field spectroscopy.
This field is already somewhat saturated with large data sets (particularly from
STIS on HST), of which the analysis has proven somewhat treacherous. Before con-
tinuing to gather increasingly large data sets it is important to address what we could
hope to learn. Many of the existing data were gathered along the same lines as the
277

strategy used to obtain the data discussed in this thesis (Chapter 3) by placing adja-
cent parallel slits on each nucleus, in order to seek the kinematic signatures of nuclear
black holes.
The multiple-slit approach with STIS has several drawbacks that have become
clear from studying these data. (i) The slit width selection has no happy medium:
With 0. ′′ 1 slits, the HST acquisition seems unable to reliably place the nucleus in the
center of the central slit; the flux profile can be highly asymmetrical across the central
slit, and very uneven in the side slits. With 0. ′′ 2 slits (or larger) the spatial resolution
in the direction across the slit is comparatively poor, which becomes an issue when the
slits are not precisely aligned with the kinematic axes (e.g. Maciejewski, 2004). (ii)
the position angle of the kinematic axes is not a priori known; choices are made based
on the nuclear morphologies of the stars, gas and dust however we have found that
the gas may not be kinematically settled in the planes that we expect, and may not be
settled in a single preferred kinematic coordinate system. (iii) The flux distributions
are not mapped with sufficient detail in comparison to the spatial resolution of the
spectra, so the distribution of light as it enters the slits is not well known, and the
placement of the slits compared to the global flux distribution is not sufficiently well
known. (Barth et al., 2001, found that representing the nuclear emission flux better
than by using a sum of Gaussians they were able to reproduce a good deal more
278

of the features observed in the velocity profiles. Knowing the flux distributions at
higher spatial resolutions than the spectra are obtained at will yield models with far
stronger constraining power).
Integral field data may suffer from related problems, in that we would also expect
the exact placement of the flux, on sub-pixel scales where it is steep, to have conse-
quences in the observed kinematics and the relationship between dispersion axes and
kinematic axes will also be important, though now on a pixel-by-pixel level rather
than along the length of the slit.
Observed velocity profiles are convolved with all of the factors described above,
and the ‘raw kinematic data’ from observations is therefore likely to be somewhat
misleading about the true velocity profiles in the gas. Models are forced to have
an almost backwards approach to deconvolving these factors, by instead making con-
volved predictions based on the chosen input models. This means that the underlying
velocity profile is never seen, which necessarily makes the choice of model somewhat
hard (worse still, at this point, the state-of-the-art generally relies on a thin, circular
disk model settled in the major plane of the galaxy).
The galaxies for which thin gas disk modeling is considered to provide reliable
estimates of the black hole mass tend to be those few individual members of samples
279

where the gas appears to be in a smooth, well ordered velocity profile. Considering
that we have found unsettled motions to play such a significant role in many nuclei,
we should probably question the safety of these assumptions. We may very well be
missing a lot of the unsettled motions in these galaxies, for example inflow or outflow
could produce effects resembling (or canceling out) rotation and, at a minimum, the
consequences of flow in model velocity profiles should be investigated.
The two galaxies in our own sample for which the gas appears to be well settled,
NGC 4335 and NGC 5141, appear to require ‘no black hole’ to explain the central
kinematics (no black hole here implies a M• < 1 × 10 8 M⊙). However, these galaxies
are not particularly unusual in their other properties, so how they would contrive to
have a smaller than usual black hole, yet still have nuclear and large scale properties
(e.g. the production of radio jets, typical velocity dispersions, etc...) comparable to
other radio galaxies is somewhat questionable. I feel that it is somewhat more likely
that the black hole is of a more typical size, and that we do not observe the full
kinematic signature as it is softened by the effects of flow in the gas. This conceivably
hints that if regular flow can be set up then other motions can be dissipated more
quickly resulting in velocity profiles that appear smother, though hydrodynamical
models would be required to test that possibility.
280

From the work presented in this dissertation it is clear that one should not gen-
erally expect the gas to be settled, or to be in a thin disk. Furthermore it seems
unreasonable to expect the gas to be coplanar with the major plane of the galaxy
potential (and possibly even with the plane of the dust, if the gas and dust are not
necessarily well coupled). Moreover, we observe warps, twists and other less expli-
cable unsettled motions in the gas, suggesting that any representation by a single
kinematic system may not be appropriate. In those cases where we do not directly
observe this type of feature, it is always possible that these characteristics occur non
the less, but possibly on smaller scales than can be observed or in planes for which
we do not gather kinematical data. (we of course only ever have a 1 dimensional
kinematic view of these three dimensional systems).
Gathering data sets that improve the spatial coverage of the nuclear kinematics
will help identify kinematic patterns in the gas and trace them on larger scales, so
that we may be able to understand how they fit into the galaxy’s structure. If we
understand the consequences of the physical systems driving features in the kinemat-
ics of samples of galaxies, then we should be able to estimate how they effect the
constraining power of models that we develop to represent the situation in individual
nuclei (and hence the limits that we can place on the determination of the black
hole masses). It is unlikely no matter how sophisticated observational and modeling
281

techniques become that strict limits will be able to be placed on black hole masses of
individual galaxies, but we can certainly do a better job of understanding the limita-
tions involved, and understand the dynamics of the nuclear regions far better, which
likely has implications for the connections between central engines and their host
galaxies. It is here that increasing the body of available data (in particular improved
spatial coverage) will have value.
Future comparisons between the stellar and gas kinematics should also produce
interesting results relating to the connections between the various kinematic systems
in an active galaxy. We showed in Chapter 5 that the stellar and gas velocity dis-
persions seem related, and tracing this relationship on larger scales, and combining
models of stars and gas sitting in the same potential, could teach us how these sys-
tems are connected. This is of interest first because it seems reasonable to assume
that the gas provides a good avenue for the stellar kinematics and the central engine
to develop connections (such as the M• − σc relation); and second as a calibration
check between those galaxies where the black hole mass is determined from stellar
dynamics and where the black hole mass is determined through gas dynamics. At the
time of writing, there is not a single example for which the black hole mass has been
reliably determined by both methods.
282

Comparing samples of active and quiescent galaxies, or samples where the level of
activity is different (e.g. between FR-I and FR-II galaxies) could help to explain how
some galaxies are active and others are not. The gas and dust is the most obvious
source of readily available fuel for the central engine, and how the fueling differs in
active and quiescent galaxies with apparently similar nuclear morphologies is of great
interest in understanding the activity in galaxies. Currently it seems that models are
not sophisticated enough to pick up differences between active and quiescent systems
– as mentioned previously detailed models are restricted to those galaxies where the
velocity profile appears smoothest, so we may miss all of the features that differentiate
the level of fueling that occurs, which may be quite subtle effects. It is also possible
that the effects that lead to fueling may always be too modest to detect above the
scale of unsettled motions, but that is also of interest in terms of the triggering of
activity in galaxies and the evolution of activity throughout cosmic evolution.
These thoughts are no doubt an incomplete representation of what will happen
as this field progresses, and many more issues in this field will be addresses over the
coming years. New instrumentation, particularly telescopes able to work at higher
spatial resolutions and integral field spectrographs, will provide rich new information
for the exploration and understanding of the nuclear regions of radio galaxies, both
nearby and further afield.
283

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