Gas Disks and Supermassive Black Holes in Nearby Radio Galaxies

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4.4 Discussion In this section we will first discuss the central kinematics of each galaxy and compare the black hole signatures that we observe to the predictions of the M − σ relation. Next we will discuss the settling of gas into a thin disks in ellipticals and finally talk about some sources of unsettled motions in this family of galaxies. 4.4.1 Description of the central kinematics In some of the cases described above it is possible to attribute some of the observed motion in the gas to the presence of a supermassive black hole. Table 4.6 summa- rizes the galaxies status regarding possible black hole signatures, as described in the previous section. In 6 of the 19 galaxies the modeled velocity profile gives no clear results as the non-rotational motions in the gas are too great. For 4 of the 13 remaining galaxies we observe a signature compatible with a black hole in the range 1 × 10 8 M⊙ < M• < 9 × 10 8 M⊙, for 5 we observe kinematic signatures that are compatible with M• ∼ > 9 × 108 M⊙. NGC 4261 has a profile compatible with an ∼ 1 × 10 8 M⊙ black hole, though these observations may not have been across the nucleus. Compatibility with these kinematic signatures does not necessarily imply that we can state black 172
hole masses for these galaxies. The scale of the random motions in these galaxies is so great that we have no reason to believe that the gas in the center is only affected by the smooth gravitational potential of the stars and central black hole. More likely is that these profiles are indicating the presence of a supermassive black hole on these mass scales, but that the actual mass may vary considerably from any attempt to best fit the nuclear slope. The three remaining galaxies are of some interest: in NGC 4335 and NGC 5141 the gas is the more settled into a smooth rotation curve than is the case for the majority of the galaxies (other than the very nearby M84 and M87), however in both of these cases we find that no black hole is necessary to explain the observed kinematics. In NGC 2329 the central slope of the rotation curve is very shallow compared even to the ‘no black hole’ model. This suggests that either the gas in this galaxy is in a different plane to the one that we were expecting or that there is significant inflow through the disk which is not supported by rotation in the gravitational potential. If this is the case, then this type of motion could also be influential in other nuclei, particularly as we know that in these radio galaxies, the central engine is being actively fueled and generating jets. Possibly NGC 4335 and NGC 5141 also hint at this; their slopes are also slightly too shallow (but within the errors in all of the parameters 173
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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
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
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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
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: e compatible with a ∼ 9 × 10 8 M
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
Page 227 and 228: Gas Radial Velocity (km s -1 ) Gas
Page 237 and 238: Gas Radial Velocity (km s -1 ) 300
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Gas Radial Velocity (km s -1 ) Gas
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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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