Gas Disks and Supermassive Black Holes in Nearby Radio Galaxies

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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
Page 1 and 2: Gas Disks and Supermassive Black Ho
Page 3 and 4: Abstract Gas Disks and Supermassive
Page 5 and 6: Contents 1 Introduction 1 1.1 Radio
Page 7 and 8: 4.2.3 Stellar luminosity densities
Page 9 and 10: List of Tables 1.1 Properties of va
Page 11 and 12: 5.1 Weighted mean kinematic paramet
Page 13 and 14: 2.12 Optical continuum image of the
Page 15: 4.14 Data-Model residuals with vary
Page 19 and 20: Chapter 1 Introduction The relation
Page 21 and 22: 1.1 Radio galaxies A radio galaxy c
Page 23 and 24: This thesis focuses on a sample of
Page 25 and 26: et al., 2000; Tomita et al., 2000;
Page 27 and 28: larger than the generally expected
Page 29 and 30: most reliable is, of course, by the
Page 31 and 32: galaxies were obtained with the Fai
Page 33 and 34: • What connections can be found b
Page 35 and 36: Table 1.2. Reliable black hole mass
Page 37 and 38: Figure 1.2 An example of a FR-I (le
Page 39 and 40: Figure 1.4 From Martel et al. (2000
Page 41 and 42: Figure 1.6 The famous cartoon by Ph
Page 43 and 44: M BH (M Sun) 10 10 10 9 10 8 10 7 1
Page 45 and 46: dish flux density measurements at 1
Page 47 and 48: 2.2.1 Radio properties Radio observ
Page 49 and 50: scribed by Verdoes Kleijn et al. (1
Page 51 and 52: Table 2.2. Multiwavelength Fluxes o
Page 53 and 54: 0.5" Figure 2.1 Optical continuum i
Page 63 and 64: 0.5" Figure 2.11 Optical continuum
Page 65 and 66: 0.5" Figure 2.13 Optical continuum
Page 67 and 68:
0.5" Figure 2.15 Optical continuum
Page 69 and 70:
Page 71 and 72:
Page 73 and 74:
Page 75 and 76:
Chapter 3 STIS spectroscopy of the
Page 77 and 78:
spectra in a future paper. We inclu
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3.2.1 Data Reduction We used the st
Page 81 and 82:
λvac − λair λair = 6.4328 × 1
Page 83 and 84:
line flux of the Hα line and colum
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3.3.3 Quantifying error sources The
Page 87 and 88:
and velocity dispersions (dominated
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slits were aligned to a mean of the
Page 91 and 92:
windows. The central kinematic and
Page 93 and 94:
(slit one) than the central positio
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(see key in Figure 3.1 for an expla
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the gas exhibits a regular rotation
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show the relationship between the t
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3.5.2 Flux ratios and ionization In
Page 103 and 104:
them to the samples of LINERS by Ho
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lines. 5. Flux-unconstrained Broad
Page 107 and 108:
Table 3.1. HST-STIS G750M observing
Page 109 and 110:
Table 3.3. Position angles of vario
Page 111 and 112:
Table 3.5. NGC 193: Measured Parame
Page 113 and 114:
Page 115 and 116:
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Table 3.11. NGC 2329: Measured Para
Page 119 and 120:
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Table 3.15. UGC 7115: Measured Para
Page 123 and 124:
Page 125 and 126:
Page 127 and 128:
Page 129 and 130:
Page 131 and 132:
Page 133 and 134:
Table 3.27. Presence of a Nuclear B
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Table 3.29. Fits to the central pix
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Table 3.31. Comparison of broad lin
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(a) (b) (i) (ii) (c) (i) (ii) (iii)
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Intensity (erg s −1 cm −2 Å
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Page 145 and 146:
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Page 149 and 150:
Page 151 and 152:
Page 153 and 154:
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Page 157 and 158:
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Difference in mean velocity on each
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Mean velocity dispersion (km s -1 )
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Chapter 4 Modeling gas in gravitati
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4.2 Thin disk models with and witho
Page 169 and 170:
gas disks were computed by making a
Page 171 and 172:
intensity contours are aligned conc
Page 173 and 174:
4.2.4 Dynamical models As discussed
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are described in Appendix A of van
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models integrating using 150 by 150
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models. Pronounced differences can
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NGC 383: This S0 galaxy has a nucle
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at an offset of 80 km s −1 , equi
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gas velocities are very well settle
Page 187 and 188:
NGC 5141: This S0 galaxy has a nucl
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e compatible with a ∼ 9 × 10 8 M
Page 191 and 192:
hole masses for these galaxies. The
Page 193 and 194:
numerical approaches they made the
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In the positive offset slit of NGC
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4.5 Conclusions In this chapter we
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low statistical significance) possi
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Table 4.2. STIS PSF Parameters. Gau
Page 203 and 204:
Table 4.4. Mass to light ratio (Υ)
Page 205 and 206:
Table 4.6. Black hole signatures in
Page 207 and 208:
weighted 600 500 400 300 200 100 =
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weighted 600 500 400 300 200 100 =
Page 211 and 212:
weighted 500 400 300 200 100 = 0. k
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weighted 500 400 300 200 100 = 37.
Page 215 and 216:
weighted 500 400 300 200 100 = 50.
Page 217 and 218:
weighted 600 500 400 300 200 100 =
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weighted 500 400 300 200 100 = -50.
Page 221 and 222:
weighted 800 600 400 200 = 280. km
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weighted 500 400 300 200 100 = -47.
Page 225 and 226:
Gas Radial Velocity (km s -1 ) 400
Page 227 and 228:
Gas Radial Velocity (km s -1 ) Gas
Page 229 and 230:
Page 231 and 232:
Page 233 and 234:
Page 235 and 236:
Page 237 and 238:
Gas Radial Velocity (km s -1 ) 300
Page 239 and 240:
Page 241 and 242:
Page 243 and 244:
Page 245 and 246:
Page 247 and 248:
v r (km s −1 ) 5000 4800 4600 440
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v r (km s −1 ) 4700 4600 4500 440
Page 251 and 252:
M BH (M Sun) 10 10 10 9 10 8 10 7 1
Page 253 and 254:
We showed that the mean dispersions
Page 255 and 256:
within 100 pc of the nucleus: � N
Page 257 and 258:
as face on disks are approached; th
Page 259 and 260:
the inclination of the dust disk. O
Page 261 and 262:
where we observe smaller and larger
Page 263 and 264:
on scales of 1/8 the Effective radi
Page 265 and 266:
may have some connections with the
Page 267 and 268:
is well correlated with σc (correl
Page 269 and 270:
e primarily driven by the central e
Page 271 and 272:
organized rotation. This supports t
Page 273 and 274:
Table 5.1. Weighted mean kinematic
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Table 5.3. Correlations between kin
Page 277 and 278:
σ100 (km s -1 −−− ) 500 400
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−−− 2 2 σ100 / ∆100 100.00
Page 281 and 282:
ε 100 (km s -1 ) 250 200 150 100 5
Page 283 and 284:
∆ 100 (km s -1 ) 500 400 300 200
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ε 100 (km s -1 ) 250 200 150 100 5
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V-Band I-Band VLA Peak VLBA Peak 10
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42 41 40 39 38 M87 nuclear SED 37 8
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ased on the gas kinematics? • How
Page 293 and 294:
emaining galaxies may be of particu
Page 295 and 296:
in nearby galaxies, and is being us
Page 297 and 298:
of the features observed in the vel
Page 299 and 300:
From the work presented in this dis
Page 301 and 302:
Comparing samples of active and qui
Page 303 and 304:
Bower, G. A., Green, R. F., Danks,
Page 305 and 306:
Herrnstein, J. R., Moran, J. M., Gr
Page 307 and 308:
Quataert, E., & Narayan, R. 2001, A
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Gas Disks and Supermassive Black Holes in Nearby Radio Galaxies

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