2005ApJ...618..618K


Query : 2005ApJ...618..618K

2005ApJ...618..618K - Astrophys. J., 618, 618-634 (2005/January-2)

Evidence for a geometrically thick self-gravitating accretion disk in NGC 3079.

KONDRATKO P.T., GREENHILL L.J. and MORAN J.M.

Abstract (from CDS):

We have mapped, for the first time, the full velocity extent of the water maser emission in NGC 3079. The largely north-south distribution of emission, aligned with a kiloparsec-scale molecular disk, and the segregation of blueshifted and redshifted emission on the sky are suggestive of a nearly edge-on molecular disk on parsec scales. Positions and line-of-sight velocities of blueshifted and redshifted maser emission are consistent with a central mass of ∼2x106 Menclosed within a radius of ∼0.4 pc. The corresponding mean mass density of 106.8 M/pc3 is suggestive of a central black hole, which is consistent with the detection of hard X-ray excess (20-100 keV) and an Fe Kα line from the nucleus. Because the rotation curve traced by the maser emission is flat, the mass of the parsec-scale disk is significant with respect to the central mass. Since the velocity dispersion of the maser features does not decrease with radius and constitutes a large fraction of the orbital velocity, the disk is probably thick and flared. The rotation curve and the physical conditions necessary to support maser emission imply a Toomre Q-parameter that is ≪1. Thus, the disk is most likely clumpy, and we argue that it is probably forming stars. Overall, the accretion disk in NGC 3079 stands in contrast to the compact, thin, warped, differentially rotating disk in the archetypal maser galaxy NGC 4258.

We have also mapped radio continuum emission in the vicinity of the disk and identify a new, time-variable, nonthermal component (E) that is not collinear with the previously imaged putative jet. Based on the large luminosity and the unusually steep spectrum (α←2.1), we exclude a radio supernova as the progenitor of E. However, because its spectrum is consistent with an aging electron energy distribution, E might be a rapidly cooling remnant, which may indicate that the jet axis wobbles. Alternatively, considering its location, the component might mark a shock in a wide-angle outflow that is interacting with a dense ambient medium. In this context, masers at high latitudes above the disk, mapped in this and previous studies, may be tracing an inward extension of the kiloparsec-scale bipolar wide-angle outflow previously observed along the galactic minor axis.


Abstract Copyright:

Journal keyword(s): Galaxies: Active - Galaxies: Individual: NGC Number: NGC 3079 - Galaxies: Seyfert - Galaxies: Starburst - ISM: Jets and Outflows - Masers

CDS comments: Fig.13: X-ray emission peak = CXOU J100157.9+554047

Simbad objects: 22

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Number of rows : 22
N Identifier Otype ICRS (J2000)
RA
ICRS (J2000)
DEC
Mag U Mag B Mag V Mag R Mag I Sp type #ref
1850 - 2022
#notes
1 NGC 253 SyG 00 47 33.134 -25 17 19.68   8.03   6.94 8.1 ~ 3148 2
2 M 77 GiP 02 42 40.7091669408 -00 00 47.859690204 9.70 9.61 8.87 10.1 9.9 ~ 4348 2
3 QSO J0854+2006 BLL 08 54 48.8749846272 +20 06 30.639583620   15.91 15.43 15.56   ~ 2181 1
4 ICRF J092703.0+390220 Sy1 09 27 03.0138528936 +39 02 20.850343332   17.17 17.00 16.486   ~ 961 1
5 M 82 IG 09 55 52.430 +69 40 46.93 9.61 9.30 8.41     ~ 5616 6
6 NGC 3079 Sy2 10 01 57.8789863992 +55 40 47.449758324 11.57 11.54 10.86     ~ 1320 3
7 CXOU J100157.9+554047 X 10 01 57.91 +55 40 47.7           ~ 1 0
8 8C 1150+812 QSO 11 53 12.4986308136 +80 58 29.152394328     18.5 18.54   ~ 227 1
9 M 106 Sy2 12 18 57.620 +47 18 13.39   9.14 8.41 8.11   ~ 2239 3
10 3C 273 BLL 12 29 06.6998257176 +02 03 08.597629980   13.05 14.830 14.11   ~ 5584 1
11 7C 1308+3236 BLL 13 10 28.6639899312 +32 20 43.774028664   15.61 15.24 17.91   ~ 803 1
12 3C 286 Sy1 13 31 08.2883506368 +30 30 32.960091564   17.51 17.25     ~ 4092 2
13 QSO B1404+286 BLL 14 07 00.3941769384 +28 27 14.692128372   16.13 15.35 10.29   ~ 729 2
14 NAME Circinus Galaxy Sy2 14 13 09.906 -65 20 20.47   10.89 9.84 10.6 10.0 ~ 1098 2
15 3C 345 QSO 16 42 58.8102993888 +39 48 37.002763188   16.81 16.59 16.84   ~ 1630 2
16 W 49n HII 19 10 13.2 +09 06 12           ~ 439 3
17 [IS88] D Rad ~ ~           ~ 3 1
18 [IS88] E Rad ~ ~           ~ 4 0
19 [IS88] C Rad ~ ~           ~ 7 0
20 [IS88] B Rad ~ ~           ~ 8 0
21 [IS88] A Rad ~ ~           ~ 8 0
22 [IS88] F Rad ~ ~           ~ 3 0

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2022.08.08-03:12:49

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