Gas Disks and Supermassive Black Holes in Nearby Radio Galaxies

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The ‘cartoon view’ of a typical radio galaxy structure contains a bright core from which emanate two jets of radio emitting material which terminate in two large radio lobes. (Figure 1.1 shows such a cartoon view). Two classes of radio galaxy were defined by Fanaroff & Riley (1974) based on the morphology of the radio emission. Fanaroff-Riley Class I galaxies (FR-Is) are brightest at the inner jets, with emission that becomes gradually fainter out into the radio lobes, while in the more powerful FR-II galaxies, hot spots at the outer edges of the radio lobes dominate the emission. Owen & Ledlow (1997) present observations of many radio galaxies, illustrating of course that there are many inadequacies in such a simplified viewpoint; in Figure 1.2 we present examples of a typical FR-I and FR-II galaxy from their sample. Radio galaxies belong to the class of galaxies that have Active Galactic Nuclei (AGN) which are characterized by large energy outputs from very small regions in their cores. Commonly, the ‘Unified Scheme’ (Urry & Padovani, 1995) is used to explain different properties of the different types of AGN and the connections between them, principally by observing the model from varying orientations. A representation of an AGN according to the unified scheme is shown in Figure 1.3. Various types of AGN and their properties are listed in Table 1.1. The type of AGN and host galaxy are also linked, radio galaxies being almost exclusively found in early-type (elliptical or S0) galaxies. 4
This thesis focuses on a sample of nearby radio galaxies (see Chapter 2). The sample is complete out to redshifts of 7000 km s −1 (100 Mpc) in the northern hemi- sphere, and contains only FR-I galaxies, as no FR-IIs are found in this volume (there is only one FR-II within 7000 km s −1 , Centaurus A, which is in the southern sky at a declination of ∼ −43 ◦ ). Radio galaxies and BL-Lacs provide a high energy contrast to Seyfert galaxies and LINERs (Low Ionization Narrow line Emission Region galaxies), and may be close cousins of the Quasars observed at higher redshifts. Both FR-I and FR-II galaxies have jets that are well collimated on all scales, though FR-Is tend to be more prone to having twisted and ‘blobby’ jets while FR-IIs tend to have straighter more uniform jets (see Bridle, 1984). The accepted paradigm is that the jets start out at relativistic velocities in both FR-Is and FR-IIs, but that in FR-Is the jets then decelerate on scales less than ∼ 1 kpc. (Bridle & Perley, 1984, provide a review of the phenomenology of extragalactic jets). The most elegant demonstration that flow may actually takes place along the jets is presented by Biretta et al. (1999), who while monitoring the jet of M87 over four years were able to trace the motion of blobs of emission, providing compelling evidence that some type of flow does occur along the jets. Baum et al. (1995) describe various differences in the populations of FR-I and FR- 5
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: 1.1 Radio galaxies A radio galaxy c
Page 25 and 26: et al., 2000; Tomita et al., 2000;
Page 27 and 28: larger than the generally expected
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
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0.5" Figure 2.21 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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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
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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