Gas Disks and Supermassive Black Holes in Nearby Radio Galaxies

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Table 1.1. Properties of various classes of Active Galactic Nuclei. Type Broad Lines Narrow Lines Radio (1) (2) (3) (4) Radio-loud Quasars � � Loud Radio-quiet Quasars � � Weak Broad-line Radio Galaxies � � Loud Narrow-line Radio Galaxies × � Loud BL-Lacs × × Loud Seyfert-1 � � Weak Seyfert-2 × � Weak LINERS × � No Note. — Col. (1): Name of the type of AGN; Cols. (2-3): Are broad and narrow gas emission lines present?; Col. (4): Is the AGN radio loud? References. — Adapted from Table 1.2 of Krolik (1999) 16
Table 1.2. Reliable black hole mass measurements. Name Type M• Method σ∗ Reference (M ⊙ ) (km s −1 ) (1) (2) (3) (4) (5) (6) Milky Way SBbc 1.8 × 10 6 s, p 103 (1) M32 E2 2.5 × 10 6 s, 3I 75 (2) M31 Sb 4.5 × 10 7 s 160 (3),(4),(5) NGC 821 E4 3.7 × 10 7 s, 3I 209 (6),(7) NGC 1023 SB0 4.4 × 10 7 s, 3I 205 (8) NGC 1068 Sb 1.5 × 10 7 m 151 (9) NGC 2778 E2 1.4 × 10 7 s, 3I 175 (6),(7) NGC 2787 SB0 4.1 × 10 7 g 140 (10) NGC 3115 S0 1.0 × 10 9 s 230 (11) NGC 3245 S0 2.1 × 10 8 g 205 (12) NGC 3377 E5 1.0 × 10 8 s, 3I 145 (6),(13) NGC 3379 E1 1.0 × 10 8 s, 3I 206 (14) NGC 3384 S0 1.6 × 10 7 s, 3I 143 (6),(7) NGC 3608 E2 1.9 × 10 8 s, 3I 182 (6),(7) NGC 4258 Sbc 3.9 × 10 7 m, a 130 (15) NGC 4261 E2 5.2 × 10 8 g 315 (16) NGC 4291 E2 3.1 × 10 8 s, 3I 242 (6),(7) NGC 4342 S0 3.0 × 10 8 s, 3I 225 (17) NGC 4459 S0 7.0 × 10 7 g 186 (10) NGC 4473 E5 1.1 × 10 8 s, 3I 190 (6),(7) NGC 4486 E0 3.0 × 10 9 g 375 (18),(19) NGC 4564 E3 5.6 × 10 7 s, 3I 162 (6),(7) NGC 4596 SB0 7.8 × 10 7 g 152 (10) NGC 4649 E1 5.6 × 10 7 s, 3I 385 (6),(7) NGC 4697 E4 1.7 × 10 8 s, 3I 177 (6),(7) NGC 4742 E4 1.4 × 10 7 s, 3I 90 (20) NGC 5845 E3 2.4 × 10 8 s, 3I 234 (6) NGC 6251 E2 5.3 × 10 8 g 290 (21) NGC 7052 E4 3.3 × 10 8 g 266 (22) NGC 7457 S0 3.5 × 10 6 s, 3I 67 (6),(7) IC 1459 E3 2.5 × 10 9 s, 3I 340 (23) Note. — Data from Tremaine et al. (2002). Col. (1): Galaxy Name; Col. (2): Morphological Type; Col. (3): Determined black hole mass; Col. (4): Method used, g - gas dynamics, m - maser dynamics, s - stars, 3I - three integral modeling, a - maser accelerations, p - proper motions; Col. (5): Central stellar velocity dispersion; Col. (6): Reference for the Black Hole Mass References. — Black Hole Mass References: (1) Chakrabarty & Saha (2001); (2) Verolme et al. (2002); (3) Tremaine (1995); (4) Kormendy & Bender (1999); (5) Bacon et al. (2001); (6) Gebhardt et al. (2003); (7) Pinkney et al. (2003); (8) Bower et al. (2001); (9) Greenhill & Gwinn (1997); (10) Sarzi et al. (2001); (11) Kormendy et al. (1996); (12) Barth et al. (2001); (13) Kormendy et al. (1998); (14) Gebhardt et al. (2000b); (15) Herrnstein et al. (1999); (16) Ferrarese et al. (1996); (17) Cretton & van den Bosch (1999); (18) Harms et al. (1994); (19) Macchetto et al. (1997); (20) Kaiser, in preparation; (21) Ferrarese & Ford (1999); (22) van der Marel & van den Bosch (1998); (23) Cappellari et al. (2002). 17
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 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: • What connections can be found b
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
Page 85 and 86:
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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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
Page 203 and 204:
Table 4.4. Mass to light ratio (Υ)
Page 205 and 206:
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 235 and 236:
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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
Page 257 and 258:
as face on disks are approached; th
Page 259 and 260:
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
Page 293 and 294:
emaining galaxies may be of particu
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in nearby galaxies, and is being us
Page 297 and 298:
of the features observed in the vel
Page 299 and 300:
From the work presented in this dis
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Comparing samples of active and qui
Page 303 and 304:
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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