Gas Disks and Supermassive Black Holes in Nearby Radio Galaxies

More documents

Recommendations

Info

[N II] Flux 10 -12 10 -13 10 -14 10 -15 10 -15 10 -14 Hα Flux 10 -13 146 10 -12 Figure 3.26 [N II] against Hα fluxes for the UGC FR-I sample members. Formal errors in the fluxes are shown. The shading of the symbols indicates the score assigned to the broad component in each case (see text). A score of 3 (most confident) is shown by black symbols, through to white symbols for a score of zero (no confidence in a broad line). It is possible to see a trend with flux from less to more confidence in broad-line detection.
Chapter 4 Modeling gas in gravitational potentials 4.1 Introduction Spectroscopic observations from the Hubble Space Telescope have made it possible to attempt to measure the black hole masses in the centers of nearby galaxies using stellar and gas kinematics (see Chapter 1). The black hole masses correlate somewhat with the host luminosity, and more tightly with the inner velocity dispersion of the stars (‘inner’ refers to inside the effective radius (Chapter 2), but still on much larger scales than the region we describe as ‘central’ or ‘nuclear’ through this thesis). In Chapter 3 we presented spectroscopic observations of the emission line gas in the nuclear regions of our sample of 21 nearby radio-galaxies (Chapter 2). Here, we may try to learn more about those data by comparing our observational results to models 147
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 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:
Page 57 and 58:
Page 59 and 60:
Page 61 and 62:
Page 63 and 64:
0.5" Figure 2.11 Optical continuum
Page 65 and 66:
Page 67 and 68:
Page 69 and 70:
Page 71 and 72:
Page 73 and 74:
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: Table 3.7. NGC 383: Measured Parame
Page 115 and 116: Table 3.9. NGC 741: Measured Parame
Page 117 and 118: Table 3.11. NGC 2329: Measured Para
Page 121 and 122: Table 3.15. UGC 7115: Measured Para
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 161 and 162: Difference in mean velocity on each
Page 163: Mean velocity dispersion (km s -1 )
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

You also want an ePaper? Increase the reach of your titles

Delete template?

Save as template?