Gas Disks and Supermassive Black Holes in Nearby Radio Galaxies

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apparent presence of fuel, these galaxies fail to produce radio jets or any significant nuclear activity. Unified schemes (see above) suggest that the ionized gas disk not intersect the photo-ionization cone of the central engine, which would require that the disks be shock ionized (Doptia et al., 1997). An investigation of the ionization structure of the disk, and any variations, can therefore reveal properties important to understanding and confirming the position of FR-I galaxies in such schemes. The nature of the gas disks is differentiated between the different types of AGN with key parameters being the gas mass, the black hole mass and the star formation rate. Different AGN can be plotted as a function of these parameters as represented in Figure 1.5. Radio Galaxies have large black hole masses, low star formation rates and relatively low gas masses so would fall into the same region of this plot as occupied by the quasars (QSOs). Different fueling mechanism may operate to bring the fuel into the center depending on these parameters (see Wada, 2004, for a recent review). Asymmetries in galaxy potentials can induce dynamical resonances that perturb the gas dynamics in the central regions. Hydrodynamical simulations (e.g., Ma- ciejewski, 2004) show that these resonances, and the resulting perturbations in the gas motions, can be governed primarily by the central black hole and on scales much 8
larger than the generally expected sphere of influence (see Equation 1.1 below). These results may imply that the central black hole is able to have kinematic influences far into the gas disk, and may even be able to regulate flow (and hence the fueling of the central engine) though these mechanisms. The nuclear gas and dust may be perturbed by sources unrelated to the gravita- tional potential of the galaxy, for example interactions with jets, starburst activity and galactic mergers, each of which could have considerable consequences for the kinematics of the gas, and the organization of structures in the central regions of these galaxies. Solórzano-Iñarrea et al. (2001) suggest that the emission line gas may be affected by jet induced shocks even in sources where the radio emission structures are much larger in extent than the regions of emission line gas (as is the case for the radio galaxies described in this thesis). It would take a certain amount of misalignment between jet and disk for such interactions to be possible, and such large misalignments between disks and jets may be observed in some radio galaxies (Schmitt et al., 2002; Verdoes Kleijn & de Zeeuw, 2004). Starbursts and AGN go hand in hand in many galactic nuclei (Beckman, 2001) and episodes of star burst activity could induce shocks into the gas disks, having a 9
Page 1 and 2: Gas Disks and Supermassive Black Ho
Page 3 and 4: Abstract Gas Disks and Supermassive
Page 5 and 6: Contents 1 Introduction 1 1.1 Radio
Page 7 and 8: 4.2.3 Stellar luminosity densities
Page 9 and 10: List of Tables 1.1 Properties of va
Page 11 and 12: 5.1 Weighted mean kinematic paramet
Page 13 and 14: 2.12 Optical continuum image of the
Page 15 and 16: 4.14 Data-Model residuals with vary
Page 17 and 18: Acknowledgments First I would like,
Page 19 and 20: Chapter 1 Introduction The relation
Page 21 and 22: 1.1 Radio galaxies A radio galaxy c
Page 23 and 24: This thesis focuses on a sample of
Page 25: et al., 2000; Tomita et al., 2000;
Page 29 and 30: most reliable is, of course, by the
Page 31 and 32: galaxies were obtained with the Fai
Page 33 and 34: • What connections can be found b
Page 35 and 36: Table 1.2. Reliable black hole mass
Page 37 and 38: Figure 1.2 An example of a FR-I (le
Page 39 and 40: Figure 1.4 From Martel et al. (2000
Page 41 and 42: Figure 1.6 The famous cartoon by Ph
Page 43 and 44: M BH (M Sun) 10 10 10 9 10 8 10 7 1
Page 45 and 46: dish flux density measurements at 1
Page 47 and 48: 2.2.1 Radio properties Radio observ
Page 49 and 50: scribed by Verdoes Kleijn et al. (1
Page 51 and 52: Table 2.2. Multiwavelength Fluxes o
Page 53 and 54: 0.5" Figure 2.1 Optical continuum i
Page 63 and 64: 0.5" Figure 2.11 Optical continuum
Page 75 and 76: Chapter 3 STIS spectroscopy of the
Page 77 and 78:
spectra in a future paper. We inclu
Page 79 and 80:
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
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3.3.3 Quantifying error sources The
Page 87 and 88:
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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Page 115 and 116:
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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:
Page 127 and 128:
Page 129 and 130:
Page 131 and 132:
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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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Page 157 and 158:
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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
Page 193 and 194:
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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Page 237 and 238:
Gas Radial Velocity (km s -1 ) 300
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Page 243 and 244:
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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,
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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