Gas Disks and Supermassive Black Holes in Nearby Radio Galaxies

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eminiscent of rotation in 67% of the nuclei, in the remainder the non-detection can be accounted for as the systems are either face on, have complex central morphologies (as judged from the nuclear dust distribution) or, in the case of NGC 5490, particularly poor signal to noise. We find that the inclusion of an additional fit component with unconstrained parameters improves our fit to the nuclear spectrum in 62% of the galaxies, where it fits in every case as a broad component in the vicinity of Hα and [N II]. The detection of the broad component is related to the line flux (and therefore the signal to noise). The broad components have a mean velocity dispersion of 1349±345 km s −1 and are redshifted from the narrow line components (assuming an origin in Hα) by 486 ± 443 km s −1 . The broad component could be a consequence of non-Gaussian line profiles with broad wings, which would be biased toward the brightest [N II] line (redwards of Hα). However, our more detailed analysis of line shape shows that it is very hard to reproduce this effect by including broad (even asymmetric) wings on each line, suggesting the broad component may indeed have a physical origin. The measured Hα to [N II] ratios for the narrow components in the central spectra are consistent with standard photo-ionization or shock-ionization models (for example, Doptia et al., 1997) other than two examples where the lines are highly blended and may be leading us to misleading fits in the very center. 88
Table 3.1. HST-STIS G750M observing log for this program. Galaxy Visit ID Aperture Offsets Exposure times Brightest Row ( ′′ ) (seconds) (1) (2) (3) (4) (5) (6) NGC 193 o5ee01 52x0.2 -0.20, 0.00, +0.20 1700, 1300, 1560 300 NGC 315 o5ee02 52x0.1 -0.10, 0.00, +0.10 1082, 1000, 1098 598 NGC 383 o5ee03 52x0.1 -0.10, 0.00, +0.10 1082, 1000, 1098 599 NGC 541 o5ee04 52x0.2 -0.20, 0.00, +0.20 1442, 1300, 1500 300 NGC 741 o5ee05 52x0.2 -0.20, 0.00, +0.20 1667, 1145, 1500 300 UGC 1841 o5ee06 52x0.2 -0.20, 0.00, +0.20 1870, 1300, 1560 300 NGC 2329 o5ee07 52x0.2 -0.20, 0.00, +0.20 1967, 1245, 1560 300 NGC 2892 o5ee09 52x0.2 -0.20, 0.00, +0.20 2037, 1300, 1560 299 NGC 3801 o5ee10 52x0.2 -0.20, 0.00, +0.20 1699, 1292, 1560 305 NGC 3862 o5ee11 52x0.2 -0.20, 0.00, +0.20 900, 731, 1066 300 UGC 7115 o5ee22 52x0.2 0.00 2058 299 NGC 4261 o5ee12 52x0.1 -0.10, 0.00, +0.10 994, 1000, 1000 601 NGC 4335 o5ee13 52x0.2 -0.20, 0.00, +0.20 2154, 1300, 1560 300 NGC 4374 o3wn01 52x0.2 -0.20, 0.00, +0.20 2245, 2600, 2600 600 NGC 4486 o67z01/2 52x0.2 -0.20, 0.00, +0.20 1708, 1380, 1708 601 NGC 5127 o5ee15 52x0.2 -0.20, 0.00, +0.20 1660, 1000, 1500 303 NGC 5141 o5ee16 52x0.2 -0.20, 0.00, +0.20 1968, 1300, 1560 300 NGC 5490 o5ee17 52x0.2 -0.20, 0.00, +0.20 1590, 1300, 1560 299 NGC 7052 o5ee18 52x0.1 -0.10, 0.00, +0.10 1747, 1300, 1500 600 UGC 12064 o5ee20 52x0.1 -0.10, 0.00, +0.10 1532, 1000, 1500 599 NGC 7626 o5ee19 52x0.2 -0.20, 0.00, +0.20 1905, 1263, 1560 300 Note. — Col. (1): NGC/UGC Number; Col. (2): Root name for the HST visit and data sets; Col. (3): HST/STIS aperture used; Col. (4): Slit positions with offsets perpendicular to the slit direction, given relative to the central slit position. UGC 7115 was observed in only one position. Further data not included here is available for NGC 4374 (M84) and NGC 4486 (M87); Col. (5): Exposure times in each offset position. For each position two observations were obtained separated by 0. ′′ 2028 along the direction of the slit, the combined exposure time is shown; Col. (6): Row number in the final x2d file of the brightest row. 89
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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
Page 55 and 56: 0.5" Figure 2.3 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: lines. 5. Flux-unconstrained Broad
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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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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