Gas Disks and Supermassive Black Holes in Nearby Radio Galaxies

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Table 2.3. Stellar velocity dispersions and estimated black hole masses. Galaxy σmeas Ref. rap re σc M• MF01 M•Meas. Ref. (km s −1 ) (arcsec) (arcsec) (km s −1 ) (10 8 M⊙) (10 8 M⊙) NGC 193 · · · · · · · · · 25.90 · · · · · · · · · · · · NGC 315 357 (1) 1.48 62.78 334 14.6 · · · · · · NGC 383 311 (1) 1.48 22.65 303 9.24 · · · · · · NGC 541 225 (1) 1.48 21.34 220 2.03 · · · · · · NGC 741 284 (1) 1.48 47.01 269 5.24 · · · · · · UGC 1841 382 (10) Re · · · 352 18.6 · · · · · · NGC 2329 274 (1) 1.48 26.81 265 4.92 · · · · · · NGC 2892 · · · · · · · · · 33.51 · · · · · · · · · · · · NGC 3801 225 (2) Re? · · · 207 1.53 · · · · · · NGC 3862 263 (1) 1.48 12.87 264 4.66 · · · · · · UGC 7115 198 (3) 3.39 13.63 204 1.41 · · · · · · NGC 4261 306 (1) 1.48 38.25 292 7.75 5.4 (5) NGC 4335 282 (9) 2Re · · · 252 3.9 ≤ 1.0 (9) NGC 4374 304 (1) 1.48 43.87 288 7.30 4.3 (6) NGC 4486 383 (1) 4.50 113.87 366 22.5 35.7 (7) NGC 5127 198 (3) 3.39 48.12 194 1.11 · · · · · · NGC 5141 · · · · · · · · · 15.13 · · · · · · · · · · · · NGC 5490 305 (1) 1.48 15.39 302 9.07 · · · · · · NGC 7052 270 (4) ∼ Re · · · 248 3.62 3.7 (8) UGC 12064 233 (10) Re · · · 214 1.80 · · · · · · NGC 7626 244 (1) 1.48 34.16 234 2.72 · · · · · · Note. — Measured stellar velocity dispersions are shown, with the source reference indicated. These have then been adapted to yield σc based on measurements of re from our WFPC2 data (see text). The relation of Merritt & Ferrarese (2001) was then used to yield estimates of the black hole masses. References. — (1) Davies et al. (1987); (2) Di Nella et al. (1995); (3) Tonry & Davis (1981); (4) Wagner et al. (1988); (5) Ferrarese et al. (1996); (6) Maciejewski & Binney (2001); (7) Macchetto et al. (1997); (8) van der Marel & van den Bosch (1998); (9) Verdoes Kleijn et al. (2002b); (10) Balcells et al. (1995); (11) van der Marel & van den Bosch (1998). 34
0.5" Figure 2.1 Optical continuum image of the nuclear region of NGC 193. The position of the spectroscopic slits used in the observing program described in Chapter 3 are indicated. The dashed line indicates the galaxy major axis position angle, the dotted line indicates the direction of the radio jet. A north-east indicator is shown. 35
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: Table 2.2. Multiwavelength Fluxes o
Page 55 and 56: 0.5" Figure 2.3 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
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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)
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Table 4.6. Black hole signatures in
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weighted 600 500 400 300 200 100 =
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weighted 600 500 400 300 200 100 =
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weighted 500 400 300 200 100 = 0. k
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weighted 500 400 300 200 100 = 37.
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weighted 500 400 300 200 100 = 50.
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weighted 600 500 400 300 200 100 =
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weighted 500 400 300 200 100 = -50.
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weighted 800 600 400 200 = 280. km
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weighted 500 400 300 200 100 = -47.
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Gas Radial Velocity (km s -1 ) 400
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Gas Radial Velocity (km s -1 ) Gas
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Gas Radial Velocity (km s -1 ) 300
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v r (km s −1 ) 5000 4800 4600 440
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v r (km s −1 ) 4700 4600 4500 440
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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
Page 307 and 308:
Quataert, E., & Narayan, R. 2001, A
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Gas Disks and Supermassive Black Holes in Nearby Radio Galaxies

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