2009ApJ...696..448H


C.D.S. - SIMBAD4 rel 1.7 - 2021.05.15CEST21:57:49

2009ApJ...696..448H - Astrophys. J., 696, 448-470 (2009/May-1)

The role of molecular gas in obscuring Seyfert active galactic nuclei.

HICKS E.K.S., DAVIES R.I., MALKAN M.A., GENZEL R., TACCONI L.J., SANCHEZ F.M. and STERNBERG A.

Abstract (from CDS):

In a sample of local active galactic nuclei (AGNs) studied at a spatial resolution on the order of 10 pc, we show that the interstellar medium traced by the molecular hydrogen ν = 1-0 S(1) line at 2.1 µm forms a geometrically thick, clumpy disk. The kinematics of the molecular gas reveals general rotation, although an additional significant component of random bulk motion is required by the high local velocity dispersion. The size scale of the typical gas disk is found to have a radius of ∼30 pc with a comparable vertical height. Within this radius, the average gas mass is estimated to be ∼107 M based on a typical gas mass fraction of 10%, which suggests column densities of NH∼ 5x1023/cm2. Extinction of the stellar continuum within this same region suggests lower column densities of NH∼2x1022/cm2, indicating that the gas distribution on these scales is dominated by dense clumps. In half of the observed Seyfert galaxies, this lower column density is still great enough to obscure the AGN at optical/infrared wavelengths. We conclude, based on the spatial distribution, kinematics, and column densities that the molecular gas observed is spatially mixed with the nuclear stellar population and is likely to be associated with the outer extent of any smaller scale nuclear obscuring structure. Furthermore, we find that the velocity dispersion of the molecular gas is correlated with the star formation rate per unit area, suggesting a link between the two phenomena, and that the gas surface density follows known "Schmidt-Kennicutt" relations. The molecular/dusty structure on these scales may be dynamic since it is possible that the velocity dispersion of the gas, and hence the vertical disk height, is maintained by a short, massive inflow of material into the nuclear region and/or by intense, short-lived nuclear star formation.

Abstract Copyright:

Journal keyword(s): galaxies: active - galaxies: kinematics and dynamics - galaxies: nuclei - galaxies: Seyfert - infrared: galaxies

Simbad objects: 18

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Number of rows : 18

N Identifier Otype ICRS (J2000)
RA
ICRS (J2000)
DEC
Mag U Mag B Mag V Mag R Mag I Sp type #ref
1850 - 2021
#notes
1 M 77 GiP 02 42 40.771 -00 00 47.84 9.70 9.61 8.87 10.1 9.9 ~ 4204 2
2 NGC 1097 LIN 02 46 19.059 -30 16 29.68 10.46 9.97 9.48 8.72 9.8 ~ 1211 3
3 NGC 3227 GiP 10 23 30.57 +19 51 54.3   12.61 11.79     ~ 1573 2
4 NGC 3783 Sy1 11 39 01.7095761008 -37 44 19.008597647   12.46 13.43 11.33 12.1 ~ 1506 0
5 NGC 4015 IG 11 58 42.642 +25 02 12.35   14.2       ~ 59 0
6 NGC 4051 Sy1 12 03 09.6098828919 +44 31 52.693714606   11.08 12.92 9.94   ~ 2038 1
7 NGC 4151 Sy1 12 10 32.5771747733 +39 24 21.057727323   12.18 11.48     ~ 3450 2
8 M 100 AGN 12 22 54.9318850854 +15 49 20.294302163 10.04 10.05 9.35     ~ 1692 2
9 M 58 SyG 12 37 43.597 +11 49 05.12 10.80 10.48 9.66     ~ 993 2
10 M 64 SyG 12 56 43.696 +21 40 57.57   9.36 8.52     ~ 841 2
11 NAME Circinus Galaxy Sy2 14 13 09.906 -65 20 20.47   10.89 9.84 10.6 10.0 ~ 1042 2
12 NGC 6240 Sy2 16 52 58.861 +02 24 03.55   14.31 13.37     ~ 1518 2
13 NAME Galactic Center gam 17 45 39.60213 -29 00 22.0000           ~ 12183 0
14 NGC 6574 GiG 18 11 51.2462161679 +14 58 54.740459628   12.5       ~ 173 0
15 HH 99B HH 19 02 05.61 -36 54 35.0           ~ 19 0
16 NGC 6814 Sy1 19 42 40.5857305428 -10 19 25.102133898   15.33 14.21 11.7 11.3 ~ 737 0
17 NGC 6951 Sy2 20 37 14.1181441937 +66 06 20.078027288   11.64 10.65     ~ 504 2
18 NGC 7469 Sy1 23 03 15.674 +08 52 25.28 12.60 13.00 12.34     ~ 1926 3

    Equat.    Gal    SGal    Ecl

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