Gas Disks and Supermassive Black Holes in Nearby Radio Galaxies

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Table 3.28. Fits to the central pixel for each galaxy, including broad lines. Kinematics. Galaxy Row vr(NL) vr(BL) σgas(NL) σgas(BL) R 2 (km s −1 ) (km s −1 ) (km s −1 ) (km s −1 ) (1) (2) (3) (4) (5) (6) (7) NGC 193 11 4417 ± 7 5128 ± 36 277 ± 6 967 ± 21 3.15 NGC 315 11 4830 ± 9 5738 ± 55 406 ± 9 1790 ± 67 2.06 NGC 383 11 5278 ± 54 5568 ± 29 669 ± 39 1367 ± 79 2.25 UGC 1841 11 6409 ± 8 6585 ± 20 436 ± 7 1254 ± 35 3.11 NGC 4261 † 11 2056 ± 9 2703 ± 68 366 ± 12 1079 ± 55 1.69 NGC 4335 11 4618 ± 3 4893 ± 37 188 ± 4 1299 ± 51 1.93 NGC 4486 11 1417 ± 14 1408 ± 28 534 ± 12 1479 ± 42 6.01 NGC 5141 11 5229 ± 3 5356 ± 86 121 ± 4 1223 ± 96 2.01 NGC 5490 11 4733 ± 16 5621 ± 61 377 ± 22 1336 ± 56 1.94 UGC 12064 11 5195 ± 16 5417 ± 90 423 ± 19 1321 ± 168 1.49 NGC 7626 11 3432 ± 7 4083 ± 76 287 ± 10 1126 ± 73 2.29 Note. — †For NGC 4261 slit 1 (offset -0.1 arcsec) was used; Col. (1): NGC/UGC Number; Col. (2): Central pixel row number referenced from the earlier data tables for each galaxy; Col. (3): The line of sight velocities of the narrow line components; Col. (4): The line of sight velocities of the broad components (where present); Col. (5): The line of sight velocity dispersions of the narrow line components; Col. (6): The line of sight velocity dispersions of the broad components (where present); Col. (7): The reduced χ 2 value of the fit. The parameters were measured by fitting a models with 5 narrow lines, fixed to each other in velocity and velocity dispersion and one free broad component, except as noted above. Errors quoted are the formal errors on the various parameters from the fit. 116
Table 3.29. Fits to the central pixel for each galaxy, including broad lines. Fluxes. Galaxy F(HαNarrow) F([N II]6585) F([S II]total) F(Broad Line) F([S II]6733) (ergs −1 cm −2 Hz −1 ) F(HαNarrow) F(HαNarrow) F(HαNarrow) F([S II]6718) (1) (2) (3) (4) (5) (6) NGC 193 1.33 ± 0.23 4.21 ± 0.77 3.86 ± 0.71 7.60 ± 1.46 1.18 ± 0.07 NGC 315 9.28 ± 0.77 4.72 ± 0.42 1.81 ± 0.21 4.40 ± 0.51 1.80 ± 0.14 NGC 383 27.72 ± 3.65 0.33 ± 0.18 0.56 ± 0.63 2.14 ± 0.50 0.11 ± 0.12 UGC 1841 7.71 ± 0.46 2.41 ± 0.16 1.39 ± 0.11 2.57 ± 0.28 1.09 ± 0.06 NGC 4261 4.36 ± 1.53 6.76 ± 2.42 3.37 ± 1.23 7.22 ± 2.93 1.55 ± 0.15 NGC 4335 1.33 ± 0.13 4.46 ± 0.44 2.63 ± 0.32 7.54 ± 0.87 1.04 ± 0.08 NGC 4486 44.96 ± 1.53 0.43 ± 0.04 0.59 ± 0.60 1.37 ± 0.11 0.03 ± 0.03 NGC 5141 0.91 ± 0.07 2.95 ± 0.25 1.38 ± 0.22 3.11 ± 0.45 0.97 ± 0.14 NGC 5490 0.25 ± 0.20 14.34 ± 11.64 9.12 ± 7.56 40.54 ± 32.95 1.94 ± 0.38 UGC 12064 0.48 ± 1.14 30.72 ± 72.97 11.16 ± 26.60 32.31 ± 77.41 0.58 ± 0.12 NGC 7626 1.48 ± 0.24 3.80 ± 0.66 1.98 ± 0.38 4.00 ± 1.01 0.95 ± 0.09 Note. — Col. (1): NGC/UGC Number; Col. (2): Hα narrow line flux; Col. (3): Ratio of the broad line flux to the Hα narrow line flux; Col. (4) Ratio of the [N II]6585 narrow line flux to the Hα Narrow line flux; Col. (5) Ratio of the total [S II] flux to the Hα Narrow line flux; Col. (6) Ratio of the [S II]6733 narrow line to the [S II]6718 narrow line. The parameters were measured by fitting a models with 5 narrow lines, fixed to each other in velocity and velocity dispersion and one free broad component, except as noted above. Errors quoted are the formal errors on the various parameters from the fit. 117
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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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Page 85 and 86: 3.3.3 Quantifying error sources The
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Page 89 and 90: slits were aligned to a mean of the
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Page 93 and 94: (slit one) than the central positio
Page 95 and 96: (see key in Figure 3.1 for an expla
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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 133: Table 3.27. Presence of a Nuclear B
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
Page 179 and 180: models. Pronounced differences can
Page 181 and 182: NGC 383: This S0 galaxy has a nucle
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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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