Gas Disks and Supermassive Black Holes in Nearby Radio Galaxies

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Table 3.26. Effect of making various fit parameters free. Fit description vHα v[NII] σHα σ[NII] F([N II]6585) R 2 (km s −1 ) (km s −1 ) (km s −1 ) (km s −1 ) F([N II]6549) (1) (2) (3) (4) (5) (6) (7) 114 initial parameters 4620 ± 4 249 ± 3 3.0 3.21 vHα free 4616 ± 9 4620 ± 3 249 ± 3 3.0 3.22 σHα free 4619 ± 3 228 ± 9 256 ± 4 3.0 3.21 vHα + σHα free 4618 ± 9 4619 ± 4 228 ± 9 256 ± 4 3.0 3.22 [N II] ratio free 4622 ± 3 248 ± 3 2.32 ± 0.09 3.04 Note. — The measurements shown were made using the central spectral row in the central slit observed for NGC 4335. Col. (1): Parameters made free, Initially a set of lines with one velocity and one velocity dispersion was used, with the ratio of the two [N II] lines fixed to 3.0. The two [S II] lines are fixed in velocity and width to the [N II] lines in every case; Col. (2-3): The radial velocities of the Hα and [N II] lines; Col. (3-4): The velocity dispersions of the Hα and [N II] lines; Col. (5): The ratio of the [N II]6585 and [N II]6549 lines; Col. (6): The reduced χ 2 value of the resulting fit.
Table 3.27. Presence of a Nuclear Broad Line. Galaxy ∆|residual| R 2 N − R 2 A By eye Score Broad Cpt. (%) R 2 N (1) (2) (3) (4) (5) (6) NGC 193 9.6 0.19 � 3 Yes NGC 315 25.0 0.46 � 3 Yes NGC 383 8.7 0.16 ◦ 2 Yes NGC 541 4.6 0.12 � 1 No NGC 741 1.9 0.01 ◦ 0 No UGC 1841 14.7 0.35 � 3 Yes NGC 2329 9.4 0.32 ◦ 2 * NGC 2892 2.8 0.09 ◦ 0 No NGC 3801 0.1 0.01 ◦ 0 No NGC 3862 8.0 0.22 ◦ 2 * UGC 7115 2.6 0.09 ◦ 0 No NGC 4261 7.8 0.22 � 3 Yes NGC 4335 8.0 0.40 � 3 Yes NGC 4374 2.4 0.12 ◦ 0 No NGC 4486 3.4 0.15 � 2 Yes NGC 5127 -1.5 -0.01 ◦ 0 No NGC 5141 3.7 0.16 � 2 Yes NGC 5490 5.2 0.23 � 3 Yes NGC 7052 4.9 0.04 � 1 No UGC 12064 6.7 0.11 � 2 Yes NGC 7626 2.5 0.13 � 2 Yes Note. — Col. (1): NGC/UGC Identification; Col. (2): Difference in the mean of the absolute values of the residuals from the fits including and excluding the additional component; Col. (3): Relative change in reduced χ 2 value between fits with the narrow lines alone (N) and with the additional component (A); Col. (4): Could an improvement in the fit be judged by eye?; Col. (5): Additional component ‘score’, one point available from each of columns 2 to 6, see text for criteria; Col. (6) Is an additional broad component useful in the fit based on these results? An asterisk (*) indicates the component appears to represent a non-flat continuum. 115
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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
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
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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 131: Table 3.25. NGC 7626: Measured Para
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
Page 179 and 180: models. Pronounced differences can
Page 181 and 182: 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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