Gas Disks and Supermassive Black Holes in Nearby Radio Galaxies

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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
Page 1 and 2: Gas Disks and Supermassive Black Ho
Page 3 and 4: Abstract Gas Disks and Supermassive
Page 5: Contents 1 Introduction 1 1.1 Radio
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 and 16: 4.14 Data-Model residuals with vary
Page 17 and 18: Acknowledgments First I would like,
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 55 and 56: 0.5" Figure 2.3 Optical continuum i
Page 57 and 58:
0.5" Figure 2.5 Optical continuum i
Page 59 and 60:
Page 61 and 62:
Page 63 and 64:
0.5" Figure 2.11 Optical continuum
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Chapter 3 STIS spectroscopy of the
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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
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line flux of the Hα line and colum
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3.3.3 Quantifying error sources The
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and velocity dispersions (dominated
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slits were aligned to a mean of the
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windows. The central kinematic and
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(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
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them to the samples of LINERS by Ho
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lines. 5. Flux-unconstrained Broad
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Table 3.1. HST-STIS G750M observing
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Table 3.3. Position angles of vario
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Table 3.5. NGC 193: Measured Parame
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Table 3.11. NGC 2329: Measured Para
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Table 3.15. UGC 7115: Measured Para
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Page 129 and 130:
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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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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
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gas disks were computed by making a
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intensity contours are aligned conc
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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
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NGC 5141: This S0 galaxy has a nucl
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e compatible with a ∼ 9 × 10 8 M
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hole masses for these galaxies. The
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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
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Table 4.4. Mass to light ratio (Υ)
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Table 4.6. Black hole signatures in
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weighted 600 500 400 300 200 100 =
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weighted 600 500 400 300 200 100 =
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weighted 500 400 300 200 100 = 0. k
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weighted 500 400 300 200 100 = 37.
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weighted 500 400 300 200 100 = 50.
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weighted 600 500 400 300 200 100 =
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weighted 500 400 300 200 100 = -50.
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weighted 800 600 400 200 = 280. km
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weighted 500 400 300 200 100 = -47.
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Gas Radial Velocity (km s -1 ) 400
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Gas Radial Velocity (km s -1 ) Gas
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Gas Radial Velocity (km s -1 ) 300
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v r (km s −1 ) 5000 4800 4600 440
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v r (km s −1 ) 4700 4600 4500 440
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M BH (M Sun) 10 10 10 9 10 8 10 7 1
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We showed that the mean dispersions
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within 100 pc of the nucleus: � N
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as face on disks are approached; th
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the inclination of the dust disk. O
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where we observe smaller and larger
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on scales of 1/8 the Effective radi
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may have some connections with the
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is well correlated with σc (correl
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e primarily driven by the central e
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organized rotation. This supports t
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Table 5.1. Weighted mean kinematic
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Table 5.3. Correlations between kin
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σ100 (km s -1 −−− ) 500 400
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−−− 2 2 σ100 / ∆100 100.00
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ε 100 (km s -1 ) 250 200 150 100 5
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∆ 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
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emaining galaxies may be of particu
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in nearby galaxies, and is being us
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of the features observed in the vel
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From the work presented in this dis
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Comparing samples of active and qui
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Bower, G. A., Green, R. F., Danks,
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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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