Gas Disks and Supermassive Black Holes in Nearby Radio Galaxies

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Table 3.32. Model ID Description vr(NL) vr(BB) vr(BC) σgas(NL) σgas(BB) σgas(BC) R 2 (km s −1 ) (km s −1 ) (km s −1 ) (km s −1 ) (km s −1 ) (km s −1 ) (1) (2) (3) (4) (5) (6) (7) (8) (9) 1 Narrow lines only 4620 · · · · · · 249 · · · · · · 3.21 2 (1) + Extra Broad Component 4618 · · · 4893 188 · · · 1299 1.93 3 (2) + Constrained Broad Bases (i) 4616 = 4616 4767 139 354 1565 1.73 4 (2) + Constrained Broad Bases (ii) 4595 4724 4680 139 319 1417 1.60 5 (2) + Unconstrained Broad Bases 4616 = 4616 4764 128 319 1389 1.68 Note. — Col. (1) Model ID (see text); Col. (2): Brief description of the fit; Cols. (3-5): The radial velocities of the narrow line (NL), broad base (BB) and broad components (BC) respectively; Cols. (6-8): The velocity dispersions of the narrow line (NL), broad base (BB) and broad components (BC) respectively. Fits were performed on the central row of the central slit of the observations of NGC 4335; Col. (9): The reduced χ 2 value of the fit. Table 3.32 Kinematic parameters measured using various free-parameter sets. 120
(a) (b) (i) (ii) (c) (i) (ii) (iii) (iv) (d) (i) (ii) (e) (i) (ii) (iii) (iv) Intensity (erg s −1 cm −2 Å −1 arcsec −2 ) v r (km s −1 ) 8•10 −15 6•10 −15 4•10 −15 2•10 −15 4700 4600 4500 4400 4300 4200 4100 0 Reduced 2−D Spectrum Single Gaussian per Line Fit v r X = −0.2 Y (arcsec) Hα+[NII] & [SII] − Narrow Line Fit 0.91 0.41 −0.10 −0.61 σ gas v r +0.2 0.0 −0.2 X (arcsec) −2•10 6584 6638 6691 6745 6799 6852 6906 Wavelength (Angstroms) −15 X = 0.0 X = +0.2 −1.01 −0.34 0.34 1.01 Y (arcsec) σ gas (km s −1 ) 500 400 300 200 100 0 X = −0.2 X = 0.0 X = +0.2 −1.01 −0.34 0.34 1.01 Y (arcsec) Intensity (erg s −1 cm −2 Å −1 arcsec −2 ) F (10 −14 ergs s −1 cm −2 Hz −1 ) 8•10 −15 6•10 −15 4•10 −15 2•10 −15 0.5 0.4 0.3 0.2 0.1 0.0 10 8 6 4 2 0 0.4 0.3 0.2 0.1 0 σ gas +0.2 0.0 −0.2 X (arcsec) [NII] 6585 Flux X = −0.2 X = 0.0 X = +0.2 0.0 −0.1 −1.01 −0.34 0.34 1.01 Y (arcsec) F([NII] 6585) +0.2 0.0 −0.2 X (arcsec) Hα+[NII] & [SII] − Narrow & Broad Cpt. Fit [NII] 6585/Hα 10.0 1.0 0.1 F([NII])/F(Hα) +0.2 0.0 −0.2 X (arcsec) −2•10 6584 6638 6691 6745 6799 6852 6906 Wavelength (Angstroms) −15 [NII]/Hα X = −0.2 X = 0.0 X = +0.2 −1.01 −0.34 0.34 1.01 Y (arcsec) Figure 3.1 Key to plots. Region (a): the HST acquisition image for each galaxy observed is shown with the positions of the observed long slits overlaid. The relative position angles of the galaxy major axes measured from the central isophotes (dashed lines) and the arcsecond scale radio jets (dotted lines) are shown. These lines cross, and a North-East indicator is drawn, at the location of the central pixel (see text). Region (b): (i) the central portion of the reduced 2-D spectrum from the central slit position is shown along with (ii) an image created from fitting a set of 5 Gaussian lines to the same. Region (c): plots representing the two-dimensional distributions of parameters measured by fitting a one Gaussian per emission line model to spectra from the nuclear region. The dashed and dash-dot lines indicate the directions of the minor and major axes respectively. The lines cross at the location of the central pixel. We show: (i) radial velocity (filled circles represent velocities greater than the mean, empty circles represent velocities less than the mean and the radius of each point [i,j] is proportional to |vi,j − vmean|); (ii) velocity dispersion (the radius of the circle is proportional to σi,j); (iii) integrated line flux (the area of each point is proportional to Fi,j); and (iv) [N II]6585 / Hα ratio (The radius of each circle is proportional to log(F([N II]6585)/F(Hα))). Region (d): single Gaussian per line fit and residuals without (i) and with (ii) the additional free component described in the text for the central spectrum of each galaxy. Region (e): plots of (i) radial velocity, (ii) velocity dispersion, (iii) [N II] line flux and (iv) [N II]6585 / Hα ratio along each slit measured by fitting a one Gaussian per line model to the emission line spectra. The vertical dotted line indicates the Y position of the central row. The dash-dot line in the velocity panel indicates the quoted recession velocity for the galaxy (see Table 2.1). 0.5" 121
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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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Page 89 and 90: slits were aligned to a mean of the
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Page 93 and 94: (slit one) than the central positio
Page 95 and 96: (see key in Figure 3.1 for an expla
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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: Table 3.31. Comparison of broad lin
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Page 161 and 162: Difference in mean velocity on each
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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
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Page 187 and 188: 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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