Gas Disks and Supermassive Black Holes in Nearby Radio Galaxies

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Table 4.3. Luminosity density fit parameters. Galaxy α β a j0 (arcsec) (1) (2) (3) (4) (5) NGC 193 0.23 1.36 1.87 5.45 NGC 315 0.44 22.29 18.3 1.27 NGC 383 0.38 0.92 1.06 10.5 NGC 541 1.14 5.57 8.95 0.35 NGC 741 0.63 1.23 2.47 3.02 UGC 1841 0.94 2.37 5.12 0.59 NGC 2329 1.70 0.17 5.38 0.22 NGC 2892 0.65 1.05 1.34 4.78 NGC 3862 1.42 1.31 7.18 0.17 NGC 4261 0.00 1.13 2.29 17.9 NGC 4335 0.00 1.13 0.19 445. M84 0.87 -1.05 9.24 6.49 NGC 4486 1.63 0.00 2.55 6.58 NGC 5127 0.00 1.51 1.30 8.69 NGC 5141 0.62 1.00 0.85 21.57 NGC 5490 0.00 1.16 0.44 85.86 NGC 7052 0.00 1.58 2.27 8.04 UGC 12064 1.13 1.76 7.78 0.17 NGC 7626 0.55 0.80 0.52 70.0 Note. — Col. (1): Galaxy Name; Col. (2- 5): Best fit parameters describing the stellar luminosity distribution j through a relationship of the form j(R, z) = j0(m/a) α [1 + (m/a) 2 ] β (see text). 184
Table 4.4. Mass to light ratio (Υ) estimates for sample galaxies. Galaxy MB (B − V ) (V − I) ΥV ΥI (1) (2) (3) (4) (5) (6) NGC 193 -20.73 1.02 6.30 NGC 315 -22.35 1.08 8.32 NGC 383 -22.02 1.02 1.87 7.80 2.68 NGC 541 -21.46 0.85 1.24 6.91 4.24 NGC 741 -22.50 1.06 1.38 8.51 4.59 UGC 1841 -21.68 0.82 7.14 NGC 2329 -21.75 0.90 1.29 7.32 4.29 NGC 2892 -20.92 NGC 3801 -20.65 0.84 1.50 6.04 2.92 NGC 3862 -21.48 0.92 2.00 7.02 2.13 UGC 7115 -20.87 1.00 6.43 NGC 4261 -21.32 0.95 1.23 6.87 4.26 NGC 4335 -20.69 0.95 6.19 NGC 4374 -20.87 0.93 1.09 6.35 4.47 NGC 4486 -22.01 0.93 1.27 7.67 4.58 NGC 5127 -20.91 0.97 6.44 NGC 5141 -20.75 0.92 1.13 6.22 4.22 NGC 5490 -21.39 0.94 0.95 6.94 5.56 NGC 7052 -21.02 0.97 6.56 UGC 12064 -20.61 0.98 6.14 NGC 7626 -21.56 1.06 1.12 7.28 4.99 Note. — Col. (1): Galaxy name; Col. (2) The blue band magnitude from the LEDA database (http://wwwobs.univ-lyon1.fr/hypercat).; Col. (3) The B-V color from LEDA; Col. (4) the V-I color from LEDA; Cols. (5-6) The V band and I band mass to light ratios respectively, calculated as described in the text. 185
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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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Page 151 and 152: Intensity (erg s −1 cm −2 Å
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: Table 4.2. STIS PSF Parameters. Gau
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
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We showed that the mean dispersions
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within 100 pc of the nucleus: � N
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as face on disks are approached; th
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the inclination of the dust disk. O
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where we observe smaller and larger
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on scales of 1/8 the Effective radi
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may have some connections with the
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is well correlated with σc (correl
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e primarily driven by the central e
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organized rotation. This supports t
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Table 5.1. Weighted mean kinematic
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Table 5.3. Correlations between kin
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σ100 (km s -1 −−− ) 500 400
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−−− 2 2 σ100 / ∆100 100.00
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ε 100 (km s -1 ) 250 200 150 100 5
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∆ 100 (km s -1 ) 500 400 300 200
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ε 100 (km s -1 ) 250 200 150 100 5
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V-Band I-Band VLA Peak VLBA Peak 10
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42 41 40 39 38 M87 nuclear SED 37 8
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ased on the gas kinematics? • How
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emaining galaxies may be of particu
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in nearby galaxies, and is being us
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of the features observed in the vel
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From the work presented in this dis
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Comparing samples of active and qui
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Bower, G. A., Green, R. F., Danks,
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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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