Gas Disks and Supermassive Black Holes in Nearby Radio Galaxies

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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
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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
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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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Page 233 and 234: 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: ∆ 100 (km s -1 ) 500 400 300 200
Page 287 and 288: V-Band I-Band VLA Peak VLBA Peak 10
Page 289 and 290: 42 41 40 39 38 M87 nuclear SED 37 8
Page 291 and 292: 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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