Gas Disks and Supermassive Black Holes in Nearby Radio Galaxies

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various sources as quoted in Table 2.1. The sense of the rotation along the major axis is also a free parameter at this point (whether the velocities go from positive to negative, or negative to positive across the nucleus). For the majority of our sample stellar dynamics are not available, and if they were it is not necessarily clear that the gas closest to the nucleus must as a matter of course be rotating in the same direction as the stars. To fit both of these variables, we found the minimum in the signal-to-noise weighted residuals between the observations and all three of the models, for both senses of the velocity. In Figures 4.1 to 4.18 we plot these values for various devi- ations of the recessional velocities from the quoted means and clear minima can be seen, which we take to be a reliable way of determining the recession velocity. In Table 4.5 the offset velocities (from the values in Table 2.1) are listed, along with an indication of the sense of the direction of the rotation. 4.2.6 Sensitivity to parameters The fit of the disk flux profile F(R) is the most sensitive to numerical noise and leaves noticeable effects (‘numerical ringing’) in the output velocity profiles when not properly modeled. We found it necessary to work in double precision for all calculations at this stage in order to produce numerically stable results. We ran 158
models integrating using 150 by 150 Gauss-Legendre quadrature (GL) points (see Press et al., 1992), we found that increasing the number of grid points beyond this limit had no effect on the result - indicating to us that it is numerically stable. Again, 150 by 150 GL points were used to compute the velocity profiles, and found this to be numerically stable also (even with lower values in this case). We tested the effect of changing the STIS PSF by repeating the models using a single Gaussian (γ1 = 1.00, σ1 = 0.0327) to represent the PSF instead of the sum of five Gaussians. In Figure 4.19 we over-plot the results for the M• = 1 × 10 8 M⊙ model for NGC 193 with each PSF, to illustrate that the differences are insignificant compared to the random variations in the observed velocity profile. This is the case for all galaxies other than M84 and M87 which are much closer to us and so the PSF becomes an important factor in these models. Maciejewski & Binney (2001) explain many important difficulties that may be encountered when modeling spectra of galaxies obtained through a ‘wide’ slit. In this context wide may be judged by the steepness of the central velocity profile and the size of the instrumental PSF. They found that the struggle between real velocity differences within an object and offsets in velocity that arise because light is entering the slit from different positions and at different angles can cause the intensity of 159
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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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line flux of the Hα line and colum
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3.3.3 Quantifying error sources The
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and velocity dispersions (dominated
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slits were aligned to a mean of the
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windows. The central kinematic and
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(slit one) than the central positio
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(see key in Figure 3.1 for an expla
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the gas exhibits a regular rotation
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show the relationship between the t
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3.5.2 Flux ratios and ionization In
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them to the samples of LINERS by Ho
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lines. 5. Flux-unconstrained Broad
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Table 3.1. HST-STIS G750M observing
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Table 3.3. Position angles of vario
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Table 3.5. NGC 193: Measured Parame
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Table 3.11. NGC 2329: Measured Para
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Table 3.15. UGC 7115: Measured Para
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Page 125 and 126: Table 3.19. NGC 4486: 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: are described in Appendix A of van
Page 179 and 180: models. Pronounced differences can
Page 181 and 182: NGC 383: This S0 galaxy has a nucle
Page 183 and 184: at an offset of 80 km s −1 , equi
Page 185 and 186: gas velocities are very well settle
Page 187 and 188: NGC 5141: This S0 galaxy has a nucl
Page 189 and 190: e compatible with a ∼ 9 × 10 8 M
Page 191 and 192: hole masses for these galaxies. The
Page 193 and 194: numerical approaches they made the
Page 195 and 196: In the positive offset slit of NGC
Page 197 and 198: 4.5 Conclusions In this chapter we
Page 199 and 200: low statistical significance) possi
Page 201 and 202: Table 4.2. STIS PSF Parameters. Gau
Page 203 and 204: Table 4.4. Mass to light ratio (Υ)
Page 205 and 206: Table 4.6. Black hole signatures in
Page 207 and 208: weighted 600 500 400 300 200 100 =
Page 211 and 212: weighted 500 400 300 200 100 = 0. k
Page 213 and 214: weighted 500 400 300 200 100 = 37.
Page 215 and 216: weighted 500 400 300 200 100 = 50.
Page 219 and 220: weighted 500 400 300 200 100 = -50.
Page 221 and 222: weighted 800 600 400 200 = 280. km
Page 223 and 224: weighted 500 400 300 200 100 = -47.
Page 225 and 226: 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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