Gas Disks and Supermassive Black Holes in Nearby Radio Galaxies

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strategy used to obtain the data discussed in this thesis (Chapter 3) by placing adja- cent parallel slits on each nucleus, in order to seek the kinematic signatures of nuclear black holes. The multiple-slit approach with STIS has several drawbacks that have become clear from studying these data. (i) The slit width selection has no happy medium: With 0. ′′ 1 slits, the HST acquisition seems unable to reliably place the nucleus in the center of the central slit; the flux profile can be highly asymmetrical across the central slit, and very uneven in the side slits. With 0. ′′ 2 slits (or larger) the spatial resolution in the direction across the slit is comparatively poor, which becomes an issue when the slits are not precisely aligned with the kinematic axes (e.g. Maciejewski, 2004). (ii) the position angle of the kinematic axes is not a priori known; choices are made based on the nuclear morphologies of the stars, gas and dust however we have found that the gas may not be kinematically settled in the planes that we expect, and may not be settled in a single preferred kinematic coordinate system. (iii) The flux distributions are not mapped with sufficient detail in comparison to the spatial resolution of the spectra, so the distribution of light as it enters the slits is not well known, and the placement of the slits compared to the global flux distribution is not sufficiently well known. (Barth et al., 2001, found that representing the nuclear emission flux better than by using a sum of Gaussians they were able to reproduce a good deal more 278
of the features observed in the velocity profiles. Knowing the flux distributions at higher spatial resolutions than the spectra are obtained at will yield models with far stronger constraining power). Integral field data may suffer from related problems, in that we would also expect the exact placement of the flux, on sub-pixel scales where it is steep, to have conse- quences in the observed kinematics and the relationship between dispersion axes and kinematic axes will also be important, though now on a pixel-by-pixel level rather than along the length of the slit. Observed velocity profiles are convolved with all of the factors described above, and the ‘raw kinematic data’ from observations is therefore likely to be somewhat misleading about the true velocity profiles in the gas. Models are forced to have an almost backwards approach to deconvolving these factors, by instead making convolved predictions based on the chosen input models. This means that the underlying velocity profile is never seen, which necessarily makes the choice of model somewhat hard (worse still, at this point, the state-of-the-art generally relies on a thin, circular disk model settled in the major plane of the galaxy). The galaxies for which thin gas disk modeling is considered to provide reliable estimates of the black hole mass tend to be those few individual members of samples 279
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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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Table 3.27. Presence of a Nuclear B
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Table 3.29. Fits to the central pix
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Table 3.31. Comparison of broad lin
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(a) (b) (i) (ii) (c) (i) (ii) (iii)
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Intensity (erg s −1 cm −2 Å
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Difference in mean velocity on each
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Mean velocity dispersion (km s -1 )
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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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Page 245 and 246: Gas Radial Velocity (km s -1 ) Gas
Page 247 and 248: v r (km s −1 ) 5000 4800 4600 440
Page 249 and 250: v r (km s −1 ) 4700 4600 4500 440
Page 251 and 252: M BH (M Sun) 10 10 10 9 10 8 10 7 1
Page 253 and 254: We showed that the mean dispersions
Page 255 and 256: within 100 pc of the nucleus: � N
Page 257 and 258: as face on disks are approached; th
Page 259 and 260: the inclination of the dust disk. O
Page 261 and 262: where we observe smaller and larger
Page 263 and 264: on scales of 1/8 the Effective radi
Page 265 and 266: may have some connections with the
Page 267 and 268: is well correlated with σc (correl
Page 269 and 270: e primarily driven by the central e
Page 271 and 272: organized rotation. This supports t
Page 273 and 274: Table 5.1. Weighted mean kinematic
Page 275 and 276: Table 5.3. Correlations between kin
Page 277 and 278: σ100 (km s -1 −−− ) 500 400
Page 279 and 280: −−− 2 2 σ100 / ∆100 100.00
Page 281 and 282: ε 100 (km s -1 ) 250 200 150 100 5
Page 283 and 284: ∆ 100 (km s -1 ) 500 400 300 200
Page 285 and 286: ε 100 (km s -1 ) 250 200 150 100 5
Page 287 and 288: V-Band I-Band VLA Peak VLBA Peak 10
Page 289 and 290: 42 41 40 39 38 M87 nuclear SED 37 8
Page 291 and 292: ased on the gas kinematics? • How
Page 293 and 294: emaining galaxies may be of particu
Page 295: in nearby galaxies, and is being us
Page 299 and 300: From the work presented in this dis
Page 301 and 302: Comparing samples of active and qui
Page 303 and 304: Bower, G. A., Green, R. F., Danks,
Page 305 and 306: Herrnstein, J. R., Moran, J. M., Gr
Page 307 and 308: Quataert, E., & Narayan, R. 2001, A
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Gas Disks and Supermassive Black Holes in Nearby Radio Galaxies

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