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Article: Interferometric 12CO J = 2-1 image of the nuclear region of Seyfert 1 galaxy NGC 1097

TitleInterferometric 12CO J = 2-1 image of the nuclear region of Seyfert 1 galaxy NGC 1097
Authors
KeywordsGalaxies: Active
Galaxies: Individual (Ngc 1097)
Galaxies: Ism
Galaxies: Nuclei
Galaxies: Seyfert
Issue Date2008
PublisherInstitute of Physics Publishing Ltd. The Journal's web site is located at http://iopscience.iop.org/2041-8205
Citation
Astrophysical Journal Letters, 2008, v. 683 n. 1, p. 70-77 How to Cite?
AbstractWe have mapped the central region of the Seyfert 1 galaxy NGC 1097 in 12CO J = 2-1 with the Submillieter Array (SMA). The 12CO J = 2-1 map shows a central concentration and a surrounding ring coinciding, respectively, with the Seyfert nucleus and a starburst ring. The line intensity peaks at the nucleus, whereas in a previously published 12CO J = 1-0 map the intensity peaks at the starburst ring. The azimuthally averaged 12CO J = 1-0 intensity ratio R 21 of the ring is about unity, which is similar to those in nearby active star-forming galaxies, suggesting that most of the molecular gas in the ring is involved in fueling the starburst. The ratio of molecular gas to dynamical mass in the starburst ring shows a somewhat lower value than that found in nearby star-forming galaxies, suggesting that the high R 21 of unity may be caused by additional effects, such as shocks induced by gas infall along the bar. The molecular gas can last for about 1.2 × 10 8 yr without further replenishment, assuming a constant star formation rate. The central gas is rotating with the molecular ring in the same direction, while its velocity gradient is steeper than that of the ring, and similar to what usually observed in Seyfert 2 galaxies. To view the Seyfert nucleus without obscuration, the central gas can be a low-inclined disk or torus but not too low to be less massive than the mass of the host galaxy, or be a highly inclined thin disk or clumpy and thick torus, inner part of the galactic disk is also possible. The R 21 of ∼1.9 of the central gas is significantly higher than that of the ring, indicates that the activity of the Seyfert nucleus may significant influence the central gas. © 2008. The American Astronomical Society. All rights reserved.
Persistent Identifierhttp://hdl.handle.net/10722/175148
ISSN
2015 Impact Factor: 5.487
2015 SCImago Journal Rankings: 3.369
ISI Accession Number ID
References

 

DC FieldValueLanguage
dc.contributor.authorHsieh, PYen_US
dc.contributor.authorMatsushita, Sen_US
dc.contributor.authorLim, Jen_US
dc.contributor.authorKohno, Ken_US
dc.contributor.authorSawadaSatoh, Sen_US
dc.date.accessioned2012-11-26T08:49:25Z-
dc.date.available2012-11-26T08:49:25Z-
dc.date.issued2008en_US
dc.identifier.citationAstrophysical Journal Letters, 2008, v. 683 n. 1, p. 70-77en_US
dc.identifier.issn2041-8205en_US
dc.identifier.urihttp://hdl.handle.net/10722/175148-
dc.description.abstractWe have mapped the central region of the Seyfert 1 galaxy NGC 1097 in 12CO J = 2-1 with the Submillieter Array (SMA). The 12CO J = 2-1 map shows a central concentration and a surrounding ring coinciding, respectively, with the Seyfert nucleus and a starburst ring. The line intensity peaks at the nucleus, whereas in a previously published 12CO J = 1-0 map the intensity peaks at the starburst ring. The azimuthally averaged 12CO J = 1-0 intensity ratio R 21 of the ring is about unity, which is similar to those in nearby active star-forming galaxies, suggesting that most of the molecular gas in the ring is involved in fueling the starburst. The ratio of molecular gas to dynamical mass in the starburst ring shows a somewhat lower value than that found in nearby star-forming galaxies, suggesting that the high R 21 of unity may be caused by additional effects, such as shocks induced by gas infall along the bar. The molecular gas can last for about 1.2 × 10 8 yr without further replenishment, assuming a constant star formation rate. The central gas is rotating with the molecular ring in the same direction, while its velocity gradient is steeper than that of the ring, and similar to what usually observed in Seyfert 2 galaxies. To view the Seyfert nucleus without obscuration, the central gas can be a low-inclined disk or torus but not too low to be less massive than the mass of the host galaxy, or be a highly inclined thin disk or clumpy and thick torus, inner part of the galactic disk is also possible. The R 21 of ∼1.9 of the central gas is significantly higher than that of the ring, indicates that the activity of the Seyfert nucleus may significant influence the central gas. © 2008. The American Astronomical Society. All rights reserved.en_US
dc.languageengen_US
dc.publisherInstitute of Physics Publishing Ltd. The Journal's web site is located at http://iopscience.iop.org/2041-8205en_US
dc.relation.ispartofAstrophysical Journal Lettersen_US
dc.subjectGalaxies: Activeen_US
dc.subjectGalaxies: Individual (Ngc 1097)en_US
dc.subjectGalaxies: Ismen_US
dc.subjectGalaxies: Nucleien_US
dc.subjectGalaxies: Seyferten_US
dc.titleInterferometric 12CO J = 2-1 image of the nuclear region of Seyfert 1 galaxy NGC 1097en_US
dc.typeArticleen_US
dc.identifier.emailLim, J: jjlim@hku.hken_US
dc.identifier.authorityLim, J=rp00745en_US
dc.description.naturelink_to_subscribed_fulltexten_US
dc.identifier.doi10.1086/589804en_US
dc.identifier.scopuseid_2-s2.0-49549117335en_US
dc.relation.referenceshttp://www.scopus.com/mlt/select.url?eid=2-s2.0-49549117335&selection=ref&src=s&origin=recordpageen_US
dc.identifier.volume683en_US
dc.identifier.issue1en_US
dc.identifier.spage70en_US
dc.identifier.epage77en_US
dc.identifier.isiWOS:000258296100007-
dc.publisher.placeUnited Kingdomen_US
dc.identifier.scopusauthoridHsieh, PY=9841991200en_US
dc.identifier.scopusauthoridMatsushita, S=7201408992en_US
dc.identifier.scopusauthoridLim, J=7403453870en_US
dc.identifier.scopusauthoridKohno, K=7201467352en_US
dc.identifier.scopusauthoridSawadaSatoh, S=6603503908en_US

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