Gas Disks and Supermassive Black Holes in Nearby Radio Galaxies

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Table 3.2. HST/STIS Instrumental properties for the configurations used. Grating Aperture Slit Width Binning Wavelength Covered λ Scale Spatial Scale ( ′′ ) (˚A ... ˚A) (˚A/ pixel) ( ′′ / pixel) (1) (2) (3) (4) (5) (6) (7) G750M 52x0.1 0.1 2 × 1 6482 ... 7054 1.108 0.05 G750M 52x0.2 0.2 2 × 2 6482 ... 7054 1.108 0.1 G750M 52x0.2 (M84) 0.2 1 × 1 6295 ... 6867 0.554 0.05 G750M 52x0.2 (M87) 0.2 1 × 1 6295 ... 6867 0.554 0.05 Note. — Col. (1): HST/STIS Grating Used; Col. (2): HST/STIS Aperture Used; Col. (3): The slit width of the chosen aperture; Col. (4): The degree of on chip binning used given as binaxis1× binaxis2 (wavelength by spatial binning); Col. (5): The minimum and maximum wavelengths on the CCD chip at that central wavelength position; Col. (6) The wavelength scale per binned pixel; Col. (7) The spatial scale per binned pixel. Further details of HST/STIS configurations can be found in Kimble, et al. (1998). 90
Table 3.3. Position angles of various axes. Galaxy Major Axis Radio Axis Dust Axis STIS Slits Target ∆PA ( ◦ N ↩→ E) ( ◦ N ↩→ E) ( ◦ N ↩→ E) ( ◦ N ↩→ E) ( ◦ ) (1) (2) (3) (4) (5) (6) (7) NGC 193 58 104 0 57.9 � M.Ax. 0.1 NGC 315 39 130 40 -143.8 � M.Ax. 2.8 NGC 383 144 162 138 144.1 � M.Ax. 0.1 NGC 541 143 76 · · · -85.6 · · · · · · NGC 741 92 · · · · · · -107.4 � M.Ax. † 19.4 UGC 1841 91 50 · · · 90.0 � M.Ax. 1.0 NGC 2329 171 150 174 170.8 � M.Ax. 0.2 NGC 2892 164 52 · · · 142.0 � M.Ax. † 22.0 NGC 3801 121 121 24 121.1 � M.Ax. 0.1 NGC 3862 25 30 · · · 122.3 ⊥ Jet 2.3 UGC 7115 91 116 175 -174.4 ⊥ Jet † 20.4 NGC 4261 155 87 163 157.9 � M.Ax. 2.9 NGC 4335 156 82 158 -32.5 � M.Ax. 8.5 NGC 4374 128 1 79 104.0 ⊥ Jet 13.0 NGC 4486 128 112 · · · 164.7 · · · · · · NGC 5127 68 118 48 68.0 � M.Ax. 0.0 NGC 5141 65 12 88 71.9 � M.Ax. 6.9 NGC 5490 1 75 143 -173.9 � M.Ax. 5.1 NGC 7052 64 23 65 63.6 � M.Ax. 0.4 UGC 12064 39 11 171 170.6 � Dust 0.4 NGC 7626 171 44 167 170.8 � M.Ax. 0.2 Note. — Col. (1): NGC/UGC Name; Col. (2): Position angles of the major axes just outside the central dust distributions; Col. (3): Position angles of the radio jet axes on arcsecond scales or smaller; Col. (4): Position angles of the central dust distributions; Col. (5): Position angles of the STIS slits on the nucleus; Col. (6): The target orientation of the STIS slits (� M.Ax.: Parallel to the Major Axis; � Dust: Parallel to the Dust Axis; ⊥ Jet: Perpendicular to the radio jet; † Additional flexibility allowed to reduce scheduling constraints); Col. (7): Offset in degrees of the STIS slits from the target orientation. References. — Data for Columns 3 - 5 taken from Verdoes Kleijn, et al. (1999) 91
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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 2.3 Optical continuum i
Page 57 and 58: 0.5" Figure 2.5 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 and 98: the gas exhibits a regular rotation
Page 99 and 100: show the relationship between the t
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: Table 3.1. HST-STIS G750M observing
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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