Gas Disks and Supermassive Black Holes in Nearby Radio Galaxies

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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
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Gas Disks and Supermassive Black Ho
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Abstract Gas Disks and Supermassive
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Contents 1 Introduction 1 1.1 Radio
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4.2.3 Stellar luminosity densities
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List of Tables 1.1 Properties of va
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5.1 Weighted mean kinematic paramet
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2.12 Optical continuum image of the
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4.14 Data-Model residuals with vary
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Acknowledgments First I would like,
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Chapter 1 Introduction The relation
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1.1 Radio galaxies A radio galaxy c
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This thesis focuses on a sample of
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et al., 2000; Tomita et al., 2000;
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larger than the generally expected
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most reliable is, of course, by the
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galaxies were obtained with the Fai
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• What connections can be found b
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Table 1.2. Reliable black hole mass
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Figure 1.2 An example of a FR-I (le
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Figure 1.4 From Martel et al. (2000
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Figure 1.6 The famous cartoon by Ph
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M BH (M Sun) 10 10 10 9 10 8 10 7 1
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dish flux density measurements at 1
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2.2.1 Radio properties Radio observ
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scribed by Verdoes Kleijn et al. (1
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Table 2.2. Multiwavelength Fluxes o
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0.5" Figure 2.1 Optical continuum i
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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
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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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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
Page 183 and 184: at an offset of 80 km s −1 , equi
Page 185 and 186: gas velocities are very well settle
Page 187 and 188: NGC 5141: This S0 galaxy has a nucl
Page 189 and 190: 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
Page 195 and 196: In the positive offset slit of NGC
Page 197 and 198: 4.5 Conclusions In this chapter we
Page 199 and 200: low statistical significance) possi
Page 201 and 202: 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 =
Page 211 and 212: weighted 500 400 300 200 100 = 0. k
Page 213 and 214: weighted 500 400 300 200 100 = 37.
Page 215 and 216: weighted 500 400 300 200 100 = 50.
Page 219 and 220: weighted 500 400 300 200 100 = -50.
Page 221 and 222: weighted 800 600 400 200 = 280. km
Page 223 and 224: 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 233: Gas Radial Velocity (km s -1 ) Gas
Page 237 and 238: Gas Radial Velocity (km s -1 ) 300
Page 247 and 248: v r (km s −1 ) 5000 4800 4600 440
Page 249 and 250: 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
Page 275 and 276: Table 5.3. Correlations between kin
Page 277 and 278: σ100 (km s -1 −−− ) 500 400
Page 279 and 280: −−− 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
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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
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Quataert, E., & Narayan, R. 2001, A
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Gas Disks and Supermassive Black Holes in Nearby Radio Galaxies

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