2015A&A...573A.116M


Query : 2015A&A...573A.116M

2015A&A...573A.116M - Astronomy and Astrophysics, volume 573A116-116 (2015/1-1)

Multimolecule ALMA observations toward the Seyfert 1 galaxy NGC 1097.

MARTIN S., KOHNO K., IZUMI T., KRIPS M., MEIER D.S., ALADRO R., MATSUSHITA S., TAKANO S., TURNER J.L., ESPADA D., NAKAJIMA T., TERASHIMA Y., FATHI K., HSIEH P.-Y., IMANISHI M., LUNDGREN A., NAKAI N., SCHINNERER E., SHETH K. and WIKLIND T.

Abstract (from CDS):

The nearby Sy 1 galaxy NGC 1097 represents an ideal laboratory for exploring the molecular chemistry in the surroundings of an active galactic nucleus (AGN). Exploring the distribution of different molecular species allows us to understand the physical processes affecting the interstellar medium both in the AGN vicinity and in the outer star forming molecular ring. We carried out 3 mm ALMA observations that include seven different molecular species, namely HCN, HCO+, CCH, CS, HNCO, SiO, HC3N, and SO, as well as the 13C isotopologues of the first two. Spectra were extracted from selected positions and all species were imaged over the central 2kpc (∼30") of the galaxy at a resolution of ∼2.2"x1.5" (150pcx100pc). HCO+ and CS appear to be slightly enhanced in the star forming ring. CCH shows the largest variations across NGC 1097 and is suggested to be a good tracer of both obscured and early stage star formation. HNCO, SiO, and HC3N are significantly enhanced in the inner circumnuclear disk surrounding the AGN. Differences in the molecular abundances are observed between the star forming ring and the inner circumnuclear disk. We conclude that the HCN/HCO+ and HCN/CS differences observed between AGN-dominated and starburst (SB) galaxies are not due to a HCN enhancement due to X-rays, but rather this enhancement is produced by shocked material at distances of 200pc from the AGN. Additionally, we claim that lower HCN/CS is a combination of a small underabundance of CS in AGNs, together with excitation effects, where a high density gas component (∼106cm–3) may be more prominent in SB galaxies. However, the most promising are the differences found among the dense gas tracers that, at our modest spatial resolution, seem to outline the physical structure of the molecular disk around the AGN. In this picture, HNCO probes the well-shielded gas in the disk, surrounding the dense material moderately exposed to the X-ray radiation traced by HC3N. Finally SiO might be the innermost molecule in the disk structure.

Abstract Copyright: ∼

Journal keyword(s): astrochemistry - ISM: abundances - ISM: molecules - galaxies: ISM

Simbad objects: 11

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Number of rows : 11
N Identifier Otype ICRS (J2000)
RA
ICRS (J2000)
DEC
Mag U Mag B Mag V Mag R Mag I Sp type #ref
1850 - 2026
#notes
1 NGC 253 SyG 00 47 33.134 -25 17 19.68   8.03   6.94 8.1 ~ 3588 2
2 M 77 Sy2 02 42 40.7091669408 -00 00 47.859690204 9.70 9.61 8.87 10.1 9.9 ~ 4897 2
3 NGC 1097 LIN 02 46 19.059 -30 16 29.68 10.46 9.97 9.48 8.72 9.8 ~ 1448 3
4 QSO B0332-403 BLL 03 34 13.65448823 -40 08 25.3979928 18.54 18.35 17.87 17.5   ~ 349 1
5 M 82 AGN 09 55 52.430 +69 40 46.93 9.61 9.30 8.41     ~ 6156 6
6 NGC 4355 Sy2 12 26 54.6206739120 -00 52 39.421212996   14.21 13.37     ~ 527 2
7 Z 294-4 Sy1 12 56 14.2341182928 +56 52 25.238373852   14.68 13.84     ~ 2096 3
8 M 51 Sy2 13 29 52.698 +47 11 42.93   9.26 8.36 8.40   ~ 4565 4
9 NGC 5690 GiG 14 37 41.0621949635 +02 17 27.095213875   13.10       ~ 182 1
10 NAME Galactic Center reg 17 45 39.60213 -29 00 22.0000           ~ 16269 0
11 QSO B1921-293 BLL 19 24 51.05595254 -29 14 30.1210248   18.71 18.21 15.07   ~ 918 1

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