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Multimolecule ALMA observations toward the Seyfert 1 galaxy NGC 1097
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2015 (English)In: Astronomy and Astrophysics, ISSN 0004-6361, E-ISSN 1432-0746, Vol. 573, A116Article in journal (Refereed) Published
Abstract [en]

Context. 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). Aims. 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. Methods. 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 C-13 isotopologues of the first two. Spectra were extracted from selected positions and all species were imaged over the central 2 kpc (similar to 30 '') of the galaxy at a resolution of similar to 2.2 '' x 1.5 '' (150 pc x 100 pc). Results. 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. Conclusions. 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 200 pc 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 (similar to 10(6) cm(-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.

Place, publisher, year, edition, pages
2015. Vol. 573, A116
Keyword [en]
astrochemistry, ISM: abundances, ISM: molecules, galaxies: ISM
National Category
Astronomy, Astrophysics and Cosmology
URN: urn:nbn:se:su:diva-116841ISI: 000350806000042OAI: diva2:809447


Available from: 2015-05-04 Created: 2015-04-29 Last updated: 2015-05-04Bibliographically approved

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Fathi, Kambiz
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Department of AstronomyThe Oskar Klein Centre for Cosmo Particle Physics (OKC)
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