Gas Disks and Supermassive Black Holes in Nearby Radio Galaxies

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Table 3.4. Spectral Lines in the region of Hα. Ion Ref. Transition λair λvac (˚A) (˚A) (1) (2) (3) (4) (5) [N II] (a) 3 P1 − 1 D2 6548.05 6549.86 Hα (b) 6562.80 6564.61 [N II] (a) 3 P2 − 1 D2 6583.39 6585.21 [S II] (a) 4 S3/2 − 2 D5/2 6716.44 6718.29 [S II] (a) 4 S3/2 − 2 D3/2 6730.81 6732.67 Note. — Col. (1): Ion responsible for the line; Col. (2): Wavelength reference; Col. (3): Transition configuration terms; Col. (4): Air wavelength; Col. (5): Vacuum wavelength. Note that the value for Hα is computed from the intensity weighted mean of fine structure lines at λair = 6562.7247 and λair = 6562.8516 with relative intensities of 120 and 180 respectively. References. — (a) Wallerstein, et al. (2001); (b) Reader & Corliss (1998) 92
Table 3.5. NGC 193: Measured Parameters. Row Y-Offset vr σgas F(Hα/10 −16 ) F([NII]6585) F([SII]total) R 2 ( ′′ ) (km s −1 ) (km s −1 ) (erg s −1 cm −2 Hz −1 ) F(Hα) F(Hα) Slit 1: X-Offset -0.2 ′′ 2 -0.9128 4334 ± 30 135 ± 30 6.6 ± 2.9 1.7 ± 0.9 1.2 ± 0.7 3.79 3 -0.8114 4270 ± 30 121 ± 32 6.9 ± 3.3 1.5 ± 1.0 0.2 ± 0.3 3.17 4 -0.7099 4323 ± 22 124 ± 23 10.6 ± 4.0 1.5 ± 0.7 0.1 ± 0.2 3.90 5 -0.6085 4390 ± 7 40 ± 7 7.8 ± 2.3 1.4 ± 0.6 0.1 ± 0.2 3.23 6 -0.5071 4602 ± 42 233 ± 41 12.9 ± 4.5 0.0 ± 0.3 1.8 ± 0.8 2.83 7 -0.4057 4371 ± 10 67 ± 10 7.4 ± 2.3 1.5 ± 0.6 1.2 ± 0.5 3.67 8 -0.3043 4402 ± 9 48 ± 9 6.2 ± 2.2 1.1 ± 0.5 0.9 ± 0.5 3.46 9 -0.2028 4369 ± 23 210 ± 18 24.7 ± 4.4 1.2 ± 0.3 1.3 ± 0.3 3.28 10 -0.1014 4344 ± 9 132 ± 9 12.5 ± 2.8 2.9 ± 0.7 3.0 ± 0.7 3.49 11 0.0000 4336 ± 7 121 ± 7 18.3 ± 2.8 2.8 ± 0.5 2.2 ± 0.4 3.66 12 0.1014 4340 ± 8 128 ± 8 18.6 ± 2.9 2.7 ± 0.5 1.6 ± 0.3 3.50 13 0.2028 4374 ± 6 85 ± 6 18.0 ± 2.7 1.8 ± 0.3 1.1 ± 0.2 3.11 14 0.3043 4343 ± 7 86 ± 7 19.2 ± 3.1 1.3 ± 0.3 1.0 ± 0.2 2.77 15 0.4057 4298 ± 14 97 ± 14 8.0 ± 2.6 2.6 ± 1.0 0.2 ± 0.3 2.52 16 0.5071 4309 ± 10 64 ± 10 8.0 ± 2.3 1.5 ± 0.6 1.0 ± 0.4 3.05 17 0.6085 4303 ± 8 66 ± 8 9.9 ± 2.3 1.7 ± 0.5 0.9 ± 0.3 2.96 18 0.7099 4317 ± 6 47 ± 6 13.3 ± 2.7 0.5 ± 0.2 0.6 ± 0.2 2.95 19 0.8114 4331 ± 8 45 ± 7 10.8 ± 2.9 0.6 ± 0.3 0.2 ± 0.1 3.50 20 0.9128 4390 ± 31 169 ± 29 5.7 ± 3.1 3.2 ± 1.9 1.6 ± 1.1 3.42 Slit 0: X-Offset 0.0 ′′ 1 -1.0142 4425 ± 41 164 ± 38 7.2 ± 4.0 2.5 ± 1.6 0.4 ± 0.5 2.62 4 -0.7099 4336 ± 10 75 ± 10 10.5 ± 3.1 1.9 ± 0.7 0.8 ± 0.4 2.41 5 -0.6085 4353 ± 10 96 ± 10 13.4 ± 3.1 1.9 ± 0.5 1.4 ± 0.4 2.58 6 -0.5071 4345 ± 18 163 ± 17 22.8 ± 4.5 1.2 ± 0.3 1.0 ± 0.3 2.81 7 -0.4057 4391 ± 22 178 ± 18 22.4 ± 4.7 1.0 ± 0.3 1.7 ± 0.4 2.86 8 -0.3043 4331 ± 39 223 ± 31 17.3 ± 4.9 1.4 ± 0.5 1.6 ± 0.6 2.78 9 -0.2028 4551 ± 15 274 ± 12 54.9 ± 6.3 2.3 ± 0.3 2.1 ± 0.3 2.61 10 -0.1014 4560 ± 10 444 ± 9 205.9 ± 13.8 3.2 ± 0.2 2.0 ± 0.2 3.16 11 0.0000 4481 ± 7 437 ± 6 316.4 ± 16.3 3.5 ± 0.2 1.8 ± 0.1 3.89 12 0.1014 4308 ± 5 178 ± 4 74.1 ± 5.0 2.5 ± 0.2 1.6 ± 0.1 2.87 13 0.2028 4339 ± 10 135 ± 9 16.0 ± 3.4 2.2 ± 0.6 3.4 ± 0.8 2.33 14 0.3043 4323 ± 12 109 ± 11 10.1 ± 3.0 2.1 ± 0.8 3.5 ± 1.2 2.67 15 0.4057 4336 ± 9 51 ± 8 11.2 ± 3.0 0.9 ± 0.4 0.3 ± 0.2 2.50 16 0.5071 4288 ± 26 159 ± 25 17.0 ± 4.4 1.0 ± 0.4 0.9 ± 0.4 2.88 17 0.6085 4314 ± 25 137 ± 24 7.9 ± 3.3 2.4 ± 1.2 1.9 ± 1.0 2.97 18 0.7099 4331 ± 15 80 ± 16 11.4 ± 3.6 1.0 ± 0.5 0.3 ± 0.2 2.90 20 0.9128 4110 ± 28 158 ± 24 11.4 ± 3.5 0.1 ± 0.3 2.3 ± 0.9 2.96 21 1.0142 4483 ± 39 200 ± 33 8.7 ± 3.8 3.0 ± 1.5 0.7 ± 0.6 2.86 Slit 2: X-Offset +0.2 ′′ 1 -1.0142 4366 ± 10 75 ± 9 11.1 ± 2.7 1.4 ± 0.4 0.4 ± 0.2 3.19 2 -0.9128 4380 ± 10 80 ± 10 8.5 ± 2.4 1.8 ± 0.6 1.1 ± 0.4 3.07 7 -0.4057 4450 ± 13 101 ± 13 4.6 ± 2.5 3.5 ± 2.0 3.7 ± 2.1 2.81 8 -0.3043 4466 ± 9 84 ± 9 4.2 ± 2.2 4.2 ± 2.3 5.0 ± 2.7 2.91 9 -0.2028 4449 ± 11 91 ± 11 6.7 ± 2.4 2.1 ± 0.9 3.0 ± 1.2 2.83 10 -0.1014 4453 ± 7 84 ± 7 9.6 ± 2.6 3.3 ± 1.0 1.8 ± 0.6 2.91 11 0.0000 4433 ± 7 87 ± 7 9.3 ± 2.6 3.8 ± 1.2 2.4 ± 0.7 2.78 12 0.1014 4385 ± 7 77 ± 7 10.8 ± 2.5 2.5 ± 0.7 1.4 ± 0.4 2.67 13 0.2028 4386 ± 14 131 ± 15 5.2 ± 2.7 6.5 ± 3.5 1.9 ± 1.1 2.56 14 0.3043 4411 ± 8 61 ± 8 8.3 ± 2.3 1.7 ± 0.6 1.3 ± 0.5 2.61 15 0.4057 4421 ± 20 107 ± 19 10.6 ± 3.5 1.1 ± 0.5 0.9 ± 0.4 2.66 16 0.5071 4342 ± 22 83 ± 23 6.1 ± 2.8 1.1 ± 0.7 1.1 ± 0.7 2.77 17 0.6085 4413 ± 44 114 ± 44 3.7 ± 2.8 2.2 ± 2.0 0.4 ± 0.7 2.96 21 1.0142 4112 ± 35 130 ± 34 5.6 ± 2.8 0.1 ± 0.4 2.0 ± 1.2 3.34 93
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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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Page 59 and 60: 0.5" Figure 2.7 Optical continuum i
Page 61 and 62: 0.5" Figure 2.9 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
Page 107 and 108: Table 3.1. HST-STIS G750M observing
Page 109: Table 3.3. Position angles of vario
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
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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
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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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