Gas Disks and Supermassive Black Holes in Nearby Radio Galaxies

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Table 3.10. UGC 01841: 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 ′′ 1 -1.0142 6626 ± 13 87 ± 13 10.6 ± 2.6 1.0 ± 0.3 0.4 ± 0.2 4.21 2 -0.9128 6276 ± 27 172 ± 25 5.5 ± 2.4 3.5 ± 1.7 1.3 ± 0.9 4.16 5 -0.6085 6444 ± 7 60 ± 7 13.1 ± 2.6 0.8 ± 0.2 0.3 ± 0.2 4.90 6 -0.5071 6258 ± 47 289 ± 35 22.2 ± 4.6 1.0 ± 0.3 1.1 ± 0.3 4.45 7 -0.4057 6416 ± 9 115 ± 9 6.9 ± 2.1 4.6 ± 1.5 1.5 ± 0.6 4.76 8 -0.3043 6411 ± 7 137 ± 7 9.3 ± 2.2 5.8 ± 1.5 2.9 ± 0.8 4.34 9 -0.2028 6379 ± 13 234 ± 10 48.3 ± 4.0 1.5 ± 0.2 0.5 ± 0.1 3.53 10 -0.1014 6155 ± 29 574 ± 25 28.0 ± 11.2 7.2 ± 2.9 3.0 ± 1.3 4.58 11 0.0000 6228 ± 10 316 ± 8 85.7 ± 5.9 2.5 ± 0.2 1.0 ± 0.1 4.20 12 0.1014 6305 ± 8 212 ± 7 38.8 ± 3.5 2.5 ± 0.3 1.1 ± 0.2 4.32 13 0.2028 6088 ± 47 426 ± 47 12.8 ± 5.8 4.4 ± 2.1 0.6 ± 0.6 4.56 14 0.3043 6369 ± 36 155 ± 32 4.1 ± 2.4 3.2 ± 2.0 0.3 ± 0.9 4.48 15 0.4057 6458 ± 24 95 ± 23 3.4 ± 2.0 1.7 ± 1.2 2.3 ± 1.7 5.04 16 0.5071 6725 ± 19 57 ± 19 5.2 ± 2.4 0.4 ± 0.3 0.4 ± 0.4 3.89 17 0.6085 6433 ± 32 125 ± 32 3.2 ± 2.0 2.7 ± 2.0 0.9 ± 1.1 5.27 19 0.8114 6617 ± 20 84 ± 20 9.2 ± 3.8 0.4 ± 0.3 0.1 ± 0.3 3.96 20 0.9128 6320 ± 22 112 ± 21 4.8 ± 1.9 2.3 ± 1.1 1.1 ± 0.7 4.76 Slit 0: X-Offset 0.0 ′′ 3 -0.8114 6350 ± 12 68 ± 11 4.0 ± 2.2 3.9 ± 2.4 0.4 ± 0.7 3.40 4 -0.7099 6339 ± 23 125 ± 23 14.1 ± 4.2 1.1 ± 0.4 0.5 ± 0.3 2.62 6 -0.5071 6276 ± 21 169 ± 19 9.2 ± 3.6 4.4 ± 1.9 1.1 ± 0.7 2.43 7 -0.4057 6371 ± 15 163 ± 14 16.3 ± 3.8 3.0 ± 0.8 0.1 ± 0.3 3.18 8 -0.3043 6428 ± 10 164 ± 10 22.8 ± 3.9 3.2 ± 0.6 0.9 ± 0.3 3.83 9 -0.2028 6329 ± 10 278 ± 8 110.7 ± 7.2 1.9 ± 0.2 1.1 ± 0.1 3.44 10 -0.1014 6337 ± 7 596 ± 6 215.6 ± 26.7 9.1 ± 1.1 3.2 ± 0.4 4.16 11 0.0000 6305 ± 5 592 ± 4 1001.2 ± 37.8 3.0 ± 0.1 1.1 ± 0.1 4.79 13 0.2028 6322 ± 26 260 ± 21 26.3 ± 5.2 2.2 ± 0.5 0.3 ± 0.2 3.46 14 0.3043 6126 ± 27 176 ± 26 5.2 ± 3.3 5.2 ± 3.5 2.8 ± 2.1 2.94 15 0.4057 6451 ± 31 105 ± 31 5.1 ± 3.0 1.6 ± 1.1 1.6 ± 1.2 3.10 17 0.6085 6407 ± 36 104 ± 33 10.6 ± 4.8 0.2 ± 0.2 0.5 ± 0.4 3.84 Slit 2: X-Offset +0.2 ′′ 1 -1.0142 6449 ± 35 172 ± 33 7.7 ± 3.1 2.0 ± 1.0 0.7 ± 0.6 4.02 3 -0.8114 6303 ± 12 109 ± 12 4.6 ± 2.1 4.8 ± 2.3 3.8 ± 1.9 3.60 6 -0.5071 6394 ± 10 85 ± 10 12.3 ± 2.7 1.5 ± 0.4 0.9 ± 0.3 3.62 7 -0.4057 6393 ± 5 72 ± 4 7.1 ± 1.9 5.2 ± 1.5 1.3 ± 0.5 3.12 8 -0.3043 6412 ± 5 111 ± 5 17.2 ± 2.6 3.9 ± 0.6 0.9 ± 0.3 3.54 9 -0.2028 6388 ± 5 120 ± 5 25.7 ± 3.1 2.4 ± 0.3 1.6 ± 0.3 4.25 10 -0.1014 6390 ± 6 166 ± 6 42.1 ± 3.7 2.2 ± 0.2 1.5 ± 0.2 3.76 11 0.0000 6363 ± 6 150 ± 6 46.0 ± 3.8 1.5 ± 0.2 1.1 ± 0.1 3.04 12 0.1014 6415 ± 10 165 ± 9 21.3 ± 3.4 2.8 ± 0.5 1.1 ± 0.3 4.05 14 0.3043 6328 ± 20 123 ± 20 7.3 ± 2.6 2.4 ± 1.0 0.5 ± 0.6 4.44 17 0.6085 6204 ± 14 79 ± 14 6.7 ± 2.3 1.8 ± 0.8 0.1 ± 0.5 3.44 18 0.7099 6450 ± 44 268 ± 39 7.3 ± 3.6 3.6 ± 1.9 1.0 ± 0.9 3.65 20 0.9128 6391 ± 27 120 ± 27 7.7 ± 2.9 0.0 ± 0.2 1.9 ± 1.0 3.41 21 1.0142 6118 ± 7 45 ± 7 9.7 ± 2.3 0.4 ± 0.2 0.5 ± 0.3 3.95 98
Table 3.11. NGC 2329: 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 6017 ± 7 52 ± 7 13.0 ± 2.6 0.4 ± 0.1 0.3 ± 0.2 3.27 3 -0.8114 5709 ± 49 164 ± 48 4.6 ± 2.7 1.7 ± 1.2 1.7 ± 1.4 2.73 4 -0.7099 5752 ± 52 284 ± 40 28.8 ± 5.7 0.4 ± 0.2 0.2 ± 0.2 3.24 5 -0.6085 5973 ± 10 67 ± 11 8.9 ± 2.3 1.2 ± 0.4 0.5 ± 0.3 3.19 6 -0.5071 5989 ± 13 59 ± 12 8.8 ± 3.1 0.5 ± 0.3 0.8 ± 0.4 2.98 7 -0.4057 5493 ± 26 112 ± 26 7.4 ± 2.7 1.2 ± 0.6 0.6 ± 0.5 3.33 8 -0.3043 5816 ± 39 223 ± 30 12.7 ± 3.8 2.1 ± 0.7 0.2 ± 0.4 3.04 9 -0.2028 5810 ± 20 154 ± 20 9.5 ± 3.2 3.3 ± 1.3 0.2 ± 0.5 2.53 10 -0.1014 5763 ± 13 133 ± 13 16.6 ± 3.6 2.3 ± 0.6 0.7 ± 0.4 2.67 11 0.0000 5747 ± 13 150 ± 12 16.0 ± 3.2 3.4 ± 0.8 0.5 ± 0.4 2.51 12 0.1014 5775 ± 19 201 ± 16 25.0 ± 4.0 1.8 ± 0.4 0.1 ± 0.2 2.94 13 0.2028 5855 ± 26 170 ± 22 9.4 ± 3.0 2.7 ± 1.0 0.9 ± 0.6 2.90 14 0.3043 5678 ± 8 29 ± 7 2.8 ± 1.2 1.6 ± 0.9 1.0 ± 0.9 3.03 18 0.7099 5748 ± 32 137 ± 31 6.4 ± 2.6 1.6 ± 0.8 0.6 ± 0.7 3.22 Slit 0: X-Offset 0.0 ′′ 1 -1.0142 5898 ± 23 74 ± 23 3.7 ± 2.6 2.2 ± 1.8 2.0 ± 2.0 1.93 5 -0.6085 6063 ± 10 38 ± 11 5.3 ± 2.5 1.2 ± 0.8 0.4 ± 0.6 2.34 6 -0.5071 5877 ± 28 129 ± 28 11.8 ± 4.2 0.1 ± 0.3 1.9 ± 0.9 2.50 7 -0.4057 5943 ± 12 79 ± 11 11.8 ± 3.3 1.8 ± 0.7 1.1 ± 0.5 2.20 9 -0.2028 5819 ± 9 104 ± 9 20.5 ± 4.3 2.6 ± 0.6 1.7 ± 0.5 2.17 10 -0.1014 5795 ± 5 268 ± 5 96.0 ± 9.6 6.6 ± 0.7 2.2 ± 0.3 3.19 11 0.0000 5789 ± 4 301 ± 4 348.6 ± 13.8 3.0 ± 0.1 1.1 ± 0.1 3.82 12 0.1014 5735 ± 2 61 ± 2 30.4 ± 4.1 3.7 ± 0.6 0.1 ± 0.2 4.66 14 0.3043 5627 ± 16 76 ± 16 13.3 ± 4.5 0.7 ± 0.4 0.3 ± 0.4 2.64 20 0.9128 5782 ± 45 146 ± 43 12.2 ± 5.1 0.6 ± 0.4 0.2 ± 0.5 2.23 21 1.0142 5770 ± 38 111 ± 37 4.1 ± 3.0 2.5 ± 2.1 0.6 ± 1.4 2.25 Slit 2: X-Offset +0.2 ′′ 1 -1.0142 5643 ± 37 154 ± 35 8.9 ± 3.4 1.4 ± 0.7 0.5 ± 0.6 2.15 2 -0.9128 5560 ± 7 32 ± 10 6.7 ± 2.9 0.4 ± 0.3 0.4 ± 0.4 2.48 8 -0.3043 5905 ± 5 53 ± 5 21.3 ± 3.3 0.5 ± 0.1 0.7 ± 0.2 2.64 9 -0.2028 5830 ± 21 195 ± 20 11.6 ± 3.8 3.9 ± 1.4 1.2 ± 0.7 2.69 10 -0.1014 5875 ± 9 119 ± 9 25.0 ± 3.8 1.9 ± 0.4 0.1 ± 0.2 2.94 11 0.0000 5844 ± 10 123 ± 10 24.2 ± 4.0 1.8 ± 0.4 1.0 ± 0.3 2.44 12 0.1014 5839 ± 6 82 ± 6 20.7 ± 3.3 1.8 ± 0.4 0.6 ± 0.2 2.66 13 0.2028 5742 ± 12 77 ± 12 12.5 ± 3.1 1.1 ± 0.4 0.5 ± 0.3 2.25 14 0.3043 5700 ± 8 45 ± 8 10.9 ± 2.9 0.7 ± 0.3 0.2 ± 0.3 2.58 15 0.4057 5631 ± 10 39 ± 9 6.5 ± 2.4 0.5 ± 0.3 0.3 ± 0.4 2.59 17 0.6085 5774 ± 30 157 ± 29 4.8 ± 2.8 4.0 ± 2.5 0.5 ± 1.1 2.71 19 0.8114 5841 ± 20 60 ± 20 5.3 ± 2.7 0.6 ± 0.5 0.9 ± 0.8 2.43 20 0.9128 5742 ± 13 59 ± 13 5.4 ± 2.2 1.6 ± 0.8 0.5 ± 0.7 2.61 99
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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
Page 65 and 66: 0.5" Figure 2.13 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 and 110: Table 3.3. Position angles of vario
Page 111 and 112: Table 3.5. NGC 193: Measured Parame
Page 113 and 114: Table 3.7. NGC 383: Measured Parame
Page 115: Table 3.9. NGC 741: Measured Parame
Page 119 and 120: Table 3.13. NGC 3801: 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 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
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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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