Gas Disks and Supermassive Black Holes in Nearby Radio Galaxies

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Table 3.22. NGC 5490: 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 ′′ 3 -0.8114 5164 ± 33 76 ± 33 5.8 ± 3.5 0.5 ± 0.5 0.3 ± 0.6 2.42 5 -0.6085 5104 ± 7 33 ± 10 9.8 ± 4.1 0.1 ± 0.2 0.6 ± 0.4 2.05 10 -0.1014 5008 ± 16 162 ± 15 16.1 ± 4.4 3.4 ± 1.0 0.8 ± 0.5 2.02 11 0.0000 4999 ± 10 205 ± 9 41.3 ± 5.4 3.3 ± 0.5 0.8 ± 0.2 2.29 12 0.1014 5154 ± 11 261 ± 9 79.9 ± 7.0 2.6 ± 0.3 1.0 ± 0.2 2.29 13 0.2028 5220 ± 9 160 ± 8 29.9 ± 4.4 3.6 ± 0.6 1.5 ± 0.3 1.94 14 0.3043 5204 ± 18 145 ± 18 24.3 ± 5.3 1.3 ± 0.4 0.8 ± 0.3 2.00 16 0.5071 5213 ± 17 63 ± 17 7.9 ± 3.3 1.0 ± 0.6 0.5 ± 0.5 2.07 19 0.8114 5154 ± 17 77 ± 16 11.0 ± 3.4 0.9 ± 0.4 0.2 ± 0.3 2.45 20 0.9128 5002 ± 48 192 ± 39 7.4 ± 3.6 2.4 ± 1.4 1.0 ± 0.9 2.51 Slit 0: X-Offset 0.0 ′′ 2 -0.9128 5214 ± 10 34 ± 9 7.0 ± 3.6 0.0 ± 0.2 1.0 ± 0.7 2.21 3 -0.8114 5073 ± 8 39 ± 8 11.4 ± 3.4 0.1 ± 0.2 0.2 ± 0.2 2.37 6 -0.5071 5317 ± 9 38 ± 9 10.6 ± 3.6 0.2 ± 0.2 0.5 ± 0.4 2.20 7 -0.4057 5537 ± 28 115 ± 28 22.9 ± 8.2 0.3 ± 0.2 0.2 ± 0.3 1.79 10 -0.1014 4701 ± 11 280 ± 9 74.4 ± 7.4 3.4 ± 0.4 1.3 ± 0.2 2.24 13 0.2028 5058 ± 16 199 ± 14 40.2 ± 6.6 2.3 ± 0.5 0.7 ± 0.3 2.18 18 0.7099 5491 ± 26 60 ± 25 7.4 ± 4.3 0.2 ± 0.4 0.2 ± 0.5 1.93 21 1.0142 5350 ± 37 131 ± 36 7.7 ± 3.7 1.7 ± 1.1 0.3 ± 0.7 2.43 Slit 2: X-Offset +0.2 ′′ 1 -1.0142 5222 ± 13 41 ± 13 6.1 ± 2.7 0.1 ± 0.2 0.1 ± 0.4 2.81 4 -0.7099 5506 ± 8 30 ± 7 −3.1 ± 1.7 1.1 ± 0.8 3.0 ± 2.0 2.38 13 0.2028 5083 ± 6 77 ± 6 15.3 ± 3.0 3.0 ± 0.7 0.4 ± 0.3 1.67 16 0.5071 5228 ± 36 131 ± 36 8.8 ± 4.0 1.5 ± 0.9 0.2 ± 0.6 1.91 110
Table 3.23. NGC 7052: 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 -0.1 ′′ 2 -0.4564 4310 ± 26 153 ± 23 35.8 ± 10.0 1.9 ± 0.7 0.3 ± 0.3 2.33 5 -0.3043 4466 ± 26 186 ± 24 28.5 ± 9.9 3.3 ± 1.3 0.6 ± 0.5 1.94 6 -0.2535 4527 ± 24 179 ± 22 25.7 ± 9.8 4.0 ± 1.7 0.7 ± 0.5 2.75 7 -0.2028 4461 ± 26 241 ± 22 50.7 ± 12.0 2.9 ± 0.8 1.0 ± 0.4 2.97 8 -0.1521 4481 ± 27 281 ± 21 86.0 ± 15.0 2.3 ± 0.5 1.6 ± 0.4 2.15 9 -0.1014 4487 ± 15 285 ± 12 167.2 ± 17.1 2.4 ± 0.3 1.1 ± 0.2 2.62 10 -0.0507 4463 ± 15 413 ± 14 289.4 ± 29.2 3.0 ± 0.3 1.1 ± 0.2 2.31 11 0.0000 4541 ± 17 456 ± 16 354.7 ± 35.1 2.7 ± 0.3 0.8 ± 0.1 2.94 12 0.0507 4722 ± 24 387 ± 22 148.1 ± 24.7 2.8 ± 0.5 0.9 ± 0.2 2.95 16 0.2535 4173 ± 7 37 ± 6 29.4 ± 7.9 0.4 ± 0.2 0.1 ± 0.2 2.29 18 0.3550 4130 ± 14 59 ± 13 20.7 ± 8.5 0.1 ± 0.3 1.2 ± 0.6 3.04 19 0.4057 4210 ± 15 54 ± 15 20.2 ± 7.7 0.0 ± 0.2 0.5 ± 0.5 2.56 Slit 0: X-Offset 0.0 ′′ 1 -0.5071 4434 ± 8 66 ± 7 87.2 ± 15.5 0.5 ± 0.1 0.4 ± 0.2 1.76 4 -0.3550 4606 ± 21 130 ± 20 37.3 ± 13.6 1.6 ± 0.7 1.8 ± 0.8 1.65 7 -0.2028 4511 ± 22 175 ± 19 59.6 ± 15.7 2.0 ± 0.6 1.6 ± 0.5 2.02 8 -0.1521 4558 ± 19 232 ± 18 48.1 ± 17.2 5.6 ± 2.1 1.5 ± 0.7 1.46 9 -0.1014 4665 ± 14 265 ± 13 110.1 ± 20.7 4.1 ± 0.8 2.3 ± 0.5 1.54 10 -0.0507 4677 ± 10 268 ± 8 244.8 ± 24.5 3.1 ± 0.3 1.3 ± 0.2 2.09 11 0.0000 4772 ± 11 303 ± 9 285.5 ± 29.5 3.1 ± 0.4 0.5 ± 0.1 1.97 12 0.0507 4832 ± 17 346 ± 16 153.1 ± 28.8 4.1 ± 0.8 1.6 ± 0.4 1.91 14 0.1521 3887 ± 25 65 ± 24 21.6 ± 11.3 0.4 ± 0.4 0.4 ± 0.5 1.64 Slit 2: X-Offset +0.1 ′′ 1 -0.5071 4468 ± 9 84 ± 9 87.2 ± 14.6 0.5 ± 0.1 0.0 ± 0.1 1.91 2 -0.4564 4479 ± 15 99 ± 15 62.3 ± 13.8 0.4 ± 0.2 0.5 ± 0.2 1.73 3 -0.4057 4561 ± 13 75 ± 13 47.9 ± 12.4 0.7 ± 0.3 0.3 ± 0.2 1.82 4 -0.3550 4572 ± 18 114 ± 17 51.7 ± 13.3 1.3 ± 0.4 0.3 ± 0.2 2.24 5 -0.3043 4576 ± 20 105 ± 19 53.3 ± 14.5 0.6 ± 0.3 0.4 ± 0.2 1.99 6 -0.2535 4582 ± 13 79 ± 13 41.2 ± 10.9 0.9 ± 0.4 0.7 ± 0.3 1.82 7 -0.2028 4536 ± 21 127 ± 21 71.6 ± 16.4 0.2 ± 0.2 0.1 ± 0.2 1.87 8 -0.1521 4641 ± 9 69 ± 9 55.7 ± 11.1 1.0 ± 0.3 0.2 ± 0.2 2.06 9 -0.1014 4667 ± 11 126 ± 11 73.4 ± 12.1 1.8 ± 0.4 0.8 ± 0.2 1.91 10 -0.0507 4670 ± 7 109 ± 7 68.4 ± 10.4 2.3 ± 0.4 1.6 ± 0.3 1.73 11 0.0000 4678 ± 9 137 ± 9 65.2 ± 11.1 2.6 ± 0.5 2.1 ± 0.4 2.11 13 0.1014 4726 ± 13 87 ± 12 14.5 ± 7.5 5.8 ± 3.2 0.9 ± 0.8 1.62 14 0.1521 4759 ± 33 125 ± 33 32.5 ± 13.3 1.1 ± 0.6 0.2 ± 0.3 1.50 16 0.2535 4738 ± 32 132 ± 32 20.8 ± 10.5 1.7 ± 1.1 1.8 ± 1.2 2.30 20 0.4564 3941 ± 15 73 ± 15 11.0 ± 5.9 2.9 ± 1.8 2.6 ± 1.6 1.96 111
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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
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 117 and 118: Table 3.11. NGC 2329: Measured Para
Page 121 and 122: Table 3.15. UGC 7115: Measured Para
Page 127: Table 3.21. NGC 5141: 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
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
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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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