A STUDY OF HEATING AND COOLING OF THE ISM IN NGC 1097 WITH HERSCHEL-PACS AND SPITZER-IRS

被引：30

作者：

Beirao, P. ^{[1
]}

Armus, L. ^{[1
]}

Helou, G. ^{[2
]}

Appleton, P. N. ^{[3
]}

Smith, J. -D. T. ^{[4
]}

Croxall, K. V. ^{[4
]}

Murphy, E. J. ^{[5
]}

Dale, D. A. ^{[6
]}

Draine, B. T. ^{[7
]}

Wolfire, M. G. ^{[8
]}

Sandstrom, K. M. ^{[9
]}

Aniano, G. ^{[7
]}

Bolatto, A. D. ^{[8
]}

Groves, B. ^{[9
]}

Brandl, B. R. ^{[10
]}

Schinnerer, E. ^{[9
]}

Crocker, A. F. ^{[11
]}

Hinz, J. L. ^{[12
]}

Rix, H. -W. ^{[9
]}

Kennicutt, R. C. ^{[13
]}

Calzetti, D. ^{[11
]}

Gil de Paz, A. ^{[14
]}

Dumas, G. ^{[9
]}

Galametz, M. ^{[13
]}

Gordon, K. D. ^{[15
]}

Hao, C. -N. ^{[16
]}

Johnson, B. ^{[17
]}

Koda, J. ^{[18
]}

Krause, O. ^{[9
]}

van der Laan, T. ^{[9
]}

Leroy, A. K. ^{[19
]}

Li, Y. ^{[11
]}

Meidt, S. E. ^{[9
]}

Meyer, J. D. ^{[18
]}

Rahman, N. ^{[8
]}

Roussel, H. ^{[17
]}

Sauvage, M. ^{[17
]}

Srinivasan, S. ^{[17
]}

Vigroux, L. ^{[20
]}

Walter, F. ^{[9
]}

Warren, B. E. ^{[21
]}

机构：

[1] CALTECH, Spitzer Sci Ctr, Pasadena, CA 91125 USA

[2] CALTECH, Ctr Infrared Proc & Anal, Pasadena, CA 91125 USA

[3] CALTECH, NASA, Herschel Sci Ctr, Pasadena, CA 91125 USA

[4] Univ Toledo, Dept Phys & Astron, Toledo, OH 43606 USA

[5] Carnegie Observ, Pasadena, CA 91101 USA

[6] Univ Wyoming, Dept Phys & Astron, Laramie, WY 82071 USA

[7] Princeton Univ, Dept Astrophys Sci, Princeton, NJ 08544 USA

[8] Univ Maryland, Dept Astron, College Pk, MD 20742 USA

[9] Max Planck Inst Astron, D-69117 Heidelberg, Germany

[10] Leiden Univ, Leiden Observ, NL-2300 RA Leiden, Netherlands

[11] Univ Massachusetts, Dept Astron, Amherst, MA 01003 USA

[12] Univ Arizona, Steward Observ, Tucson, AZ 85721 USA

[13] Univ Cambridge, Inst Astron, Cambridge CB3 0HA, England

[14] Univ Complutense Madrid, Dept Astrofis, Fac Ciencias Fis, E-28040 Madrid, Spain

[15] Space Telescope Sci Inst, Baltimore, MD 21218 USA

[16] Tianjin Normal Univ, Tianjin Astrophys Ctr, Tianjin 300387, Peoples R China

[17] Univ Paris 06, Inst Astrophys Paris, UMR7095, CNRS, F-75014 Paris, France

[18] SUNY Stony Brook, Dept Phys & Astron, Stony Brook, NY 11794 USA

[19] Natl Radio Astron Observ, Charlottesville, VA 22903 USA

[20] CE Saclay, CEA, DSM, DAPNIA,Serv Astrophys,UMR, F-91191 Gif Sur Yvette, France

[21] Univ Western Australia, ICRAR, M468, Crawley, WA 6009, Australia

来源：

ASTROPHYSICAL JOURNAL | 2012年 / 751卷 / 02期

关键词：

galaxies: individual (NGC 1097); galaxies: ISM; galaxies: starburst; infrared: galaxies; FAR-INFRARED SPECTROSCOPY; NEARBY GALAXIES SURVEY; STAR-FORMING GALAXIES; INTERSTELLAR-MEDIUM; C-II; PHOTODISSOCIATION REGIONS; MOLECULAR-HYDROGEN; TRANSLUCENT CLOUDS; SEYFERT-GALAXIES; IRON PROJECT;

D O I：

10.1088/0004-637X/751/2/144

中图分类号：

P1 [天文学];

学科分类号：

0704 ;

摘要：

NGC 1097 is a nearby Seyfert 1 galaxy with a bright circumnuclear starburst ring, a strong large-scale bar, and an active nucleus. We present a detailed study of the spatial variation of the far-infrared (FIR) [CII]158 mu m and [OI]63 mu m lines and mid-infrared H-2 emission lines as tracers of gas cooling, and of the polycyclic aromatic hydrocarbon (PAH) bands as tracers of the photoelectric heating, using Herschel-PACS and Spitzer-IRS infrared spectral maps. We focus on the nucleus and the ring, and two star-forming regions (Enuc N and Enuc S). We estimated a photoelectric gas heating efficiency ([CII]158 mu m+[OI]63 mu m)/PAH in the ring about 50% lower than in Enuc N and S. The average 11.3/7.7 mu m PAH ratio is also lower in the ring, which may suggest a larger fraction of ionized PAHs, but no clear correlation with [CII]158 mu m/PAH(5.5-14 mu m) is found. PAHs in the ring are responsible for a factor of two more [CII]158 mu m and [OI]63 mu m emission per unit mass than PAHs in the Enuc S. spectral energy distribution (SED) modeling indicates that at most 25% of the FIR power in the ring and Enuc S can come from high-intensity photodissociation regions (PDRs), in which case G(0) similar to 10(2.3) and n(H) similar to 10(3.5) cm(-3) in the ring. For these values of G(0) and n(H), PDR models cannot reproduce the observed H-2 emission. Much of the H-2 emission in the starburst ring could come from warm regions in the diffuse interstellar medium that are heated by turbulent dissipation or shocks.

引用

页数：16

共 15 条

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