Gas Disks and Supermassive Black Holes in Nearby Radio Galaxies

More documents

Recommendations

Info

Intensity (erg s −1 cm −2 Å −1 arcsec −2 ) v r (km s −1 ) 8•10 −15 6•10 −15 4•10 −15 2•10 −15 3800 3600 3400 3200 0 −2•10 −15 Reduced 2−D Spectrum Single Gaussian per Line Fit v r X = −0.2 Y (arcsec) 0.91 0.41 -0.10 -0.61 Hα+[NII] & [SII] − Narrow Line Fit σ gas v r +0.2 0.0 -0.2 X (arcsec) 6584 6638 6691 6745 6799 6852 6906 Wavelength (Angstroms) X = 0.0 X = +0.2 −1.01 −0.34 0.34 1.01 Y (arcsec) σ gas (km s −1 ) 400 300 200 100 0 0.5" X = −0.2 X = 0.0 X = +0.2 −1.01 −0.34 0.34 1.01 Y (arcsec) Intensity (erg s −1 cm −2 Å −1 arcsec −2 ) F (10 −14 ergs s −1 cm −2 Hz −1 ) 8•10 −15 6•10 −15 4•10 −15 2•10 −15 0.8 0.6 0.4 0.2 0.0 −0.2 9 7 5 3 1 −1 0.9 0.7 0.5 0.3 0 −2•10 −15 σ gas +0.2 0.0 -0.2 X (arcsec) [NII] 6585 Flux X = −0.2 X = 0.0 X = +0.2 0.1 −0.1 −1.01 −0.34 0.34 1.01 Y (arcsec) F([NII] 6585) +0.2 0.0 -0.2 X (arcsec) Hα+[NII] & [SII] − Narrow & Broad Cpt. Fit [NII] 6585/Hα 10.0 1.0 0.1 F([NII])/F(Hα) +0.2 0.0 -0.2 X (arcsec) 6584 6638 6691 6745 6799 6852 6906 Wavelength (Angstroms) [NII]/Hα X = −0.2 X = 0.0 X = +0.2 −1.01 −0.34 0.34 1.01 Y (arcsec) Figure 3.22 Observation and fit data for NGC 7626, see Figure 3.1 for description. 142
Difference in mean velocity on each side of nucleus (km s -1 ) 1000 800 600 400 200 0 100 200 300 400 500 Mean gas velocity dispersion (km s -1 0 ) Figure 3.23 Difference in mean velocity within 100 pc of each side of the nucleus (∆100pc, see text) as a function of the mean gas velocity dispersion within 100 pc of the nucleus (σ100pc). The different kinematic classes and dust morphologies 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 (△). The solid line is the 1:1 ratio between ∆100pc and σ100pc, indicating regions where organized motions (above the line) or random motions (below the line) dominate. 143
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 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 159: Intensity (erg s −1 cm −2 Å
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

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

Delete template?

Save as template?