Gas Disks and Supermassive Black Holes in Nearby Radio Galaxies

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kinematics seem either irregular or organized in some manner that does not represent regular rotation. We do not include NGC 741 in discussions of kinematics as very few points were well fit during our analysis. We classify 67% (N = 14/21) of the UGC FR-I galaxies as rotators. 73% of galaxies with dust disks (N = 8/11), 100% of galaxies with dust lanes (N = 5/5) and 50% of galaxies with complex dust or no dust (N = 2/4) are rotators. We have made use of the mean velocity dispersion σ100pc = 1 N 80 � σi : xi ≤ 100pc, (3.4) and the difference in mean velocities on each side of the nucleus � �� ⎛ � 1 � ∆100pc = � � vi : −100pc ≤ xi < 0 − ⎝ � N1 i 1 ⎞� � � � vj : 0 < xj ≤ 100pc⎠� � N2 j � i (3.5) within 100 pc of the brightest pixel as illustrative of the global kinematic parameters along the central slit 2 . These parameters are shown in Table 3.30 for each galaxy, along with the mean properties for each class of galaxy. In Figure 3.23 we 2 For NGC 4261 we used the offset slit closest to the nucleus as explained above.
show the relationship between the two parameters for each galaxy. It is clear that the non-rotators lie at the bottom of the ∆100pc distribution, so it is conceivable that irregular motions conceal any remaining signs of rotation in these cases. We note that we detect rotation in all cases where the disk is ∼ > 25 ◦ from face on, other than those cases where the dust morphology is highly irregular. The only exception is NGC 5490 where the signal to noise was particularly poor. In Figure 3.24 we show the values of ∆100pc plotted as a function of dust disk axis ratio, or dust lane width to length ratio; if the dust were all in circular disks this would be an indicator of disk inclination. We included lines showing an indication of the projection of several values of ∆100pc at different disk inclinations through the relation � � � � ∆obs ≈ ∆int.sini ≈ ∆int × 1 − 81 � �2 b , (3.6) a Where ∆obs is the observed ∆100pc parameter at a given inclination, ∆int is the presumed intrinsic rotation of the disk and b/a is the axis (or width:length) ratio. This is not a rigorously valid means of projecting these values, but it serves our purposes of illustration here.
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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
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
Page 85 and 86: 3.3.3 Quantifying error sources The
Page 87 and 88: and velocity dispersions (dominated
Page 89 and 90: slits were aligned to a mean of the
Page 91 and 92: windows. The central kinematic and
Page 93 and 94: (slit one) than the central positio
Page 95 and 96: (see key in Figure 3.1 for an expla
Page 97: the gas exhibits a regular rotation
Page 101 and 102: 3.5.2 Flux ratios and ionization In
Page 103 and 104: them to the samples of LINERS by Ho
Page 105 and 106: lines. 5. Flux-unconstrained Broad
Page 107 and 108: Table 3.1. HST-STIS G750M observing
Page 109 and 110: Table 3.3. Position angles of vario
Page 111 and 112: Table 3.5. NGC 193: Measured Parame
Page 117 and 118: Table 3.11. NGC 2329: Measured Para
Page 121 and 122: Table 3.15. UGC 7115: 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
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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
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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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