Gas Disks and Supermassive Black Holes in Nearby Radio Galaxies

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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
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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
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 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: as face on disks are approached; th
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
Page 285 and 286: ε 100 (km s -1 ) 250 200 150 100 5
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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