Gas Disks and Supermassive Black Holes in Nearby Radio Galaxies

More documents

Recommendations

Info

Lobe Jet Core Optical galaxy Jet Lobe Figure 1.1 A cartoon view of a radio galaxy showing the core, jets and lobes as observed at radio wavelengths, a typical size scale for the elliptical host galaxy observed at visible wavelengths is also indicated. 18
Figure 1.2 An example of a FR-I (left) and a FR-II (right) radio galaxy, observed at 20 cm wavelengths by Owen & Ledlow (1997). The FR-I is characterized by bright jets, closest to the nucleus, while the FR-II has bright radio lobes. 19
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 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: Table 1.2. Reliable black hole mass
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 75 and 76: Chapter 3 STIS spectroscopy of the
Page 77 and 78: spectra in a future paper. We inclu
Page 79 and 80: 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
Page 85 and 86: 3.3.3 Quantifying error sources The
Page 87 and 88:
and velocity dispersions (dominated
Page 89 and 90:
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
Page 95 and 96:
(see key in Figure 3.1 for an expla
Page 97 and 98:
the gas exhibits a regular rotation
Page 99 and 100:
show the relationship between the t
Page 101 and 102:
3.5.2 Flux ratios and ionization In
Page 103 and 104:
them to the samples of LINERS by Ho
Page 105 and 106:
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:
Page 117 and 118:
Table 3.11. NGC 2329: Measured Para
Page 119 and 120:
Page 121 and 122:
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
Page 135 and 136:
Table 3.29. Fits to the central pix
Page 137 and 138:
Table 3.31. Comparison of broad lin
Page 139 and 140:
(a) (b) (i) (ii) (c) (i) (ii) (iii)
Page 141 and 142:
Intensity (erg s −1 cm −2 Å
Page 143 and 144:
Page 145 and 146:
Page 147 and 148:
Page 149 and 150:
Page 151 and 152:
Page 153 and 154:
Page 155 and 156:
Page 157 and 158:
Page 159 and 160:
Page 161 and 162:
Difference in mean velocity on each
Page 163 and 164:
Mean velocity dispersion (km s -1 )
Page 165 and 166:
Chapter 4 Modeling gas in gravitati
Page 167 and 168:
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
Page 175 and 176:
are described in Appendix A of van
Page 177 and 178:
models integrating using 150 by 150
Page 179 and 180:
models. Pronounced differences can
Page 181 and 182:
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 209 and 210:
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 217 and 218:
weighted 600 500 400 300 200 100 =
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 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
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
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
show all

Gas Disks and Supermassive Black Holes in Nearby Radio Galaxies

Create successful ePaper yourself

Delete template?

Save as template?