Gas Disks and Supermassive Black Holes in Nearby Radio Galaxies

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5.2.1 Effects of inclination We use the dust disk axis ratio (b/a) or dust lane width : length ratio as an indicator of the inclination of the nuclear gas and dust. In Figures 5.1, 5.2 and 5.3 we plot ∆100, σ100 and ɛ100 respectively against this dust axis ratio parameter. This leads naturally to the most edge on systems being plotted at the left (where the galaxies with dust lanes are found) to face on systems at the right (which include face on disks where we are unable to pick up the rotation profile). The fact that systems with dust lanes and dust disks form a continuum in all of these parameters suggests that the lanes observed may be the edges of highly inclined dust disks rather than being physically distinct types of systems. Verdoes Kleijn et al. (1999) found that dust lanes and disks may represent distinct physical systems, primarily based on increased irregular structure observed in lane systems and misalignments with the major axes. It is possible that if the dust is indeed in two distinct morphological types, that the gas forms into a kinematically similar system in either case. In the light of evidence relating to the settling of the gas perpendicular to the disk presented below, it is also possible that the observed irregularities in dust lane systems originate from less settled motions out of the plane of the disk. 238 In Figure 5.1 it is possible to see a decreasing upper envelope to the value of ∆100
as face on disks are approached; the observed velocity difference is smaller, which is as we would expect. The face on disks do not, however, sit at a value of ∆100 = 0, indicating that there may be motions perpendicular to the plane of the disk across the nuclei of these galaxies (for example precession of the disk), which may indicate they are not settled into the major plane of the galaxy. However, we cannot rule out the possibility that they are simply amongst the fastest rotators in the sample – the small number statistics do not present strong constraints. Lines are indicated where we approximately project the ‘intrinsic’ ∆int through inclination using the relationship: � � � � ∆obs ≈ ∆int sin i ≈ ∆int × 1 − 239 � �2 b , (5.7) a Two outliers are labeled in the figure: NGC 383 and UGC 7115 which, despite being fairly face on, have large values of ∆100. In the case of NGC 383 it seems that the observed rotation is compatible with the fastest rotating sample members that are viewed edge on. Those fastest edge-on galaxies are NGC 4486 and M84, which are both nearby so that ∆100 includes a great deal more of the resolved central velocities, which makes comparisons with other galaxies less meaningful, and thus leaves NGC 383 as an outlier. The large values of ∆100 may be an indicator that the gas in these two galaxies is indeed rotating very fast, that there are gas systems present that are very poorly described by the thin disk model, or that the dust distribution
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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)
Page 205 and 206: 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: within 100 pc of the nucleus: � N
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
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Quataert, E., & Narayan, R. 2001, A
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Gas Disks and Supermassive Black Holes in Nearby Radio Galaxies

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