A STUDY OF HEATING AND COOLING OF THE ISM IN NGC 1097 WITH HERSCHEL-PACS AND SPITZER-IRS
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 sub(2) emission lines as tracers o...
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| Veröffentlicht in: | The Astrophysical journal 2012-06, Vol.751 (2), p.1-16 |
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| creator | BEIRAO, P ARMUS, L SANDSTROM, K. M ANIANO, G BOLATTO, A. D GROVES, B BRANDL, B. R SCHINNERER, E CROCKER, A. F HINZ, J. L RIX, H.-W KENNICUTT, R. C HELOU, G CALZETTI, D GIL DE PAZ, A DUMAS, G GALAMETZ, M GORDON, K. D HAO, C.-N JOHNSON, B KODA, J KRAUSE, O VAN DER LAAN, T APPLETON, P. N LEROY, A. K LI, Y MEIDT, S. E MEYER, J. D RAHMAN, N ROUSSEL, H SAUVAGE, M SRINIVASAN, S VIGROUX, L WALTER, F SMITH, J.-D. T WARREN, B. E CROXALL, K. V MURPHY, E. J DALE, D. A DRAINE, B. T WOLFIRE, M. G |
| description | 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 sub(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 +[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 sub(0) ~ 10 super(2.3) and n sub(H) ~ 10 super(3.5) cm super(-3) in the ring. For these values of G sub(0) and n sub(H), PDR models cannot reproduce the observed H sub(2) emission. Much of the H sub(2) emission in the starburst ring could come from warm regions in the diffuse interstellar medium that are heated by turbulent dissipation or shocks. |
| doi_str_mv | 10.1088/0004-637X/751/2/144 |
| format | Article |
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M ; ANIANO, G ; BOLATTO, A. D ; GROVES, B ; BRANDL, B. R ; SCHINNERER, E ; CROCKER, A. F ; HINZ, J. L ; RIX, H.-W ; KENNICUTT, R. C ; HELOU, G ; CALZETTI, D ; GIL DE PAZ, A ; DUMAS, G ; GALAMETZ, M ; GORDON, K. D ; HAO, C.-N ; JOHNSON, B ; KODA, J ; KRAUSE, O ; VAN DER LAAN, T ; APPLETON, P. N ; LEROY, A. K ; LI, Y ; MEIDT, S. E ; MEYER, J. D ; RAHMAN, N ; ROUSSEL, H ; SAUVAGE, M ; SRINIVASAN, S ; VIGROUX, L ; WALTER, F ; SMITH, J.-D. T ; WARREN, B. E ; CROXALL, K. V ; MURPHY, E. J ; DALE, D. A ; DRAINE, B. T ; WOLFIRE, M. G</creator><creatorcontrib>BEIRAO, P ; ARMUS, L ; SANDSTROM, K. M ; ANIANO, G ; BOLATTO, A. D ; GROVES, B ; BRANDL, B. R ; SCHINNERER, E ; CROCKER, A. F ; HINZ, J. L ; RIX, H.-W ; KENNICUTT, R. C ; HELOU, G ; CALZETTI, D ; GIL DE PAZ, A ; DUMAS, G ; GALAMETZ, M ; GORDON, K. D ; HAO, C.-N ; JOHNSON, B ; KODA, J ; KRAUSE, O ; VAN DER LAAN, T ; APPLETON, P. N ; LEROY, A. K ; LI, Y ; MEIDT, S. E ; MEYER, J. D ; RAHMAN, N ; ROUSSEL, H ; SAUVAGE, M ; SRINIVASAN, S ; VIGROUX, L ; WALTER, F ; SMITH, J.-D. T ; WARREN, B. E ; CROXALL, K. V ; MURPHY, E. J ; DALE, D. A ; DRAINE, B. T ; WOLFIRE, M. G</creatorcontrib><description>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 sub(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 +[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 sub(0) ~ 10 super(2.3) and n sub(H) ~ 10 super(3.5) cm super(-3) in the ring. For these values of G sub(0) and n sub(H), PDR models cannot reproduce the observed H sub(2) emission. Much of the H sub(2) emission in the starburst ring could come from warm regions in the diffuse interstellar medium that are heated by turbulent dissipation or shocks.</description><identifier>ISSN: 0004-637X</identifier><identifier>EISSN: 1538-4357</identifier><identifier>DOI: 10.1088/0004-637X/751/2/144</identifier><identifier>CODEN: ASJOAB</identifier><language>eng</language><publisher>Bristol: IOP</publisher><subject>ASTRONOMY ; ASTROPHYSICS ; ASTROPHYSICS, COSMOLOGY AND ASTRONOMY ; COMPUTERIZED SIMULATION ; Earth, ocean, space ; Emission ; EMISSION SPECTROSCOPY ; ENERGY SPECTRA ; Exact sciences and technology ; FAR INFRARED RADIATION ; GALAXIES ; GALAXY NUCLEI ; GAS COOLING ; Gas heating ; HEATING ; HYDROGEN ; Nuclei ; Photoelectricity ; PHOTOLYSIS ; PHOTON EMISSION ; Polyallylamine hydrochloride ; POLYCYCLIC AROMATIC HYDROCARBONS ; Sciences of the Universe ; Spectral energy distribution ; STARS ; Tracers</subject><ispartof>The Astrophysical journal, 2012-06, Vol.751 (2), p.1-16</ispartof><rights>2015 INIST-CNRS</rights><rights>Distributed under a Creative Commons Attribution 4.0 International License</rights><lds50>peer_reviewed</lds50><oa>free_for_read</oa><woscitedreferencessubscribed>false</woscitedreferencessubscribed><citedby>FETCH-LOGICAL-c337t-1efcbd3a0eeaebc384e07135fd95ffec410214a46009a3f257553ed066a69bbe3</citedby><cites>FETCH-LOGICAL-c337t-1efcbd3a0eeaebc384e07135fd95ffec410214a46009a3f257553ed066a69bbe3</cites><orcidid>0000-0002-3933-7677 ; 0000-0003-4793-7880 ; 0000-0002-0283-8689 ; 0000-0002-9768-0246</orcidid></display><links><openurl>$$Topenurl_article</openurl><openurlfulltext>$$Topenurlfull_article</openurlfulltext><thumbnail>$$Tsyndetics_thumb_exl</thumbnail><link.rule.ids>230,314,780,784,885,27924,27925</link.rule.ids><backlink>$$Uhttp://pascal-francis.inist.fr/vibad/index.php?action=getRecordDetail&idt=25968634$$DView record in Pascal Francis$$Hfree_for_read</backlink><backlink>$$Uhttps://hal.science/hal-03645828$$DView record in HAL$$Hfree_for_read</backlink><backlink>$$Uhttps://www.osti.gov/biblio/22037150$$D View this record in Osti.gov$$Hfree_for_read</backlink></links><search><creatorcontrib>BEIRAO, P</creatorcontrib><creatorcontrib>ARMUS, L</creatorcontrib><creatorcontrib>SANDSTROM, K. 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G</creatorcontrib><title>A STUDY OF HEATING AND COOLING OF THE ISM IN NGC 1097 WITH HERSCHEL-PACS AND SPITZER-IRS</title><title>The Astrophysical journal</title><description>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 sub(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 +[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 sub(0) ~ 10 super(2.3) and n sub(H) ~ 10 super(3.5) cm super(-3) in the ring. For these values of G sub(0) and n sub(H), PDR models cannot reproduce the observed H sub(2) emission. Much of the H sub(2) emission in the starburst ring could come from warm regions in the diffuse interstellar medium that are heated by turbulent dissipation or shocks.</description><subject>ASTRONOMY</subject><subject>ASTROPHYSICS</subject><subject>ASTROPHYSICS, COSMOLOGY AND ASTRONOMY</subject><subject>COMPUTERIZED SIMULATION</subject><subject>Earth, ocean, space</subject><subject>Emission</subject><subject>EMISSION SPECTROSCOPY</subject><subject>ENERGY SPECTRA</subject><subject>Exact sciences and technology</subject><subject>FAR INFRARED RADIATION</subject><subject>GALAXIES</subject><subject>GALAXY NUCLEI</subject><subject>GAS COOLING</subject><subject>Gas heating</subject><subject>HEATING</subject><subject>HYDROGEN</subject><subject>Nuclei</subject><subject>Photoelectricity</subject><subject>PHOTOLYSIS</subject><subject>PHOTON EMISSION</subject><subject>Polyallylamine hydrochloride</subject><subject>POLYCYCLIC AROMATIC HYDROCARBONS</subject><subject>Sciences of the Universe</subject><subject>Spectral energy distribution</subject><subject>STARS</subject><subject>Tracers</subject><issn>0004-637X</issn><issn>1538-4357</issn><fulltext>true</fulltext><rsrctype>article</rsrctype><creationdate>2012</creationdate><recordtype>article</recordtype><recordid>eNqNkV1r2zAUhsXYYFm3X7AbwRhsF270_XFpXDc2uEmJXdbtRiiKTD3cuLPcQv995abkeleSDs-rczgPAF8xOsdIqSVCiCWCytul5HhJlpixd2CBOVUJo1y-B4sT8RF8CuHv_CRaL8BtCuvm5uI33FzCIk-bcr2C6foCZptNNd9juSlyWNZXsFzD9SqDGGkJf5VNEfltnRV5lVynWf2aqq_L5k--Tcpt_Rl8aG0f_Je38wzcXOZNViTVZlVmaZU4SuWUYN-63Z5a5L31O0cV80hiytu95m3rHcOIYGaZQEhb2hIuOad-j4SwQu92np6Bb8d_hzB1Jrhu8u7ODYeDd5MhBFGJOYrUzyN1Z3vzMHb3dnw2g-1MkVZmriEqGFdEPeHI_jiyD-Pw79GHydx3wfm-twc_PAaDJVaa6riH_0ARZpowoSJKj6gbhxBG357GwMjMEs3sxMyKTJRoiIkSY-r7WwMbnO3b0R5cF05RwrVQgjL6AkD1kSI</recordid><startdate>20120601</startdate><enddate>20120601</enddate><creator>BEIRAO, P</creator><creator>ARMUS, L</creator><creator>SANDSTROM, K. 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G</creatorcontrib><collection>Pascal-Francis</collection><collection>CrossRef</collection><collection>Meteorological & Geoastrophysical Abstracts</collection><collection>Meteorological & Geoastrophysical Abstracts - Academic</collection><collection>Technology Research Database</collection><collection>Aerospace Database</collection><collection>Advanced Technologies Database with Aerospace</collection><collection>Hyper Article en Ligne (HAL)</collection><collection>OSTI.GOV</collection><jtitle>The Astrophysical journal</jtitle></facets><delivery><delcategory>Remote Search Resource</delcategory><fulltext>fulltext</fulltext></delivery><addata><au>BEIRAO, P</au><au>ARMUS, L</au><au>SANDSTROM, K. M</au><au>ANIANO, G</au><au>BOLATTO, A. D</au><au>GROVES, B</au><au>BRANDL, B. R</au><au>SCHINNERER, E</au><au>CROCKER, A. F</au><au>HINZ, J. L</au><au>RIX, H.-W</au><au>KENNICUTT, R. C</au><au>HELOU, G</au><au>CALZETTI, D</au><au>GIL DE PAZ, A</au><au>DUMAS, G</au><au>GALAMETZ, M</au><au>GORDON, K. D</au><au>HAO, C.-N</au><au>JOHNSON, B</au><au>KODA, J</au><au>KRAUSE, O</au><au>VAN DER LAAN, T</au><au>APPLETON, P. N</au><au>LEROY, A. K</au><au>LI, Y</au><au>MEIDT, S. E</au><au>MEYER, J. D</au><au>RAHMAN, N</au><au>ROUSSEL, H</au><au>SAUVAGE, M</au><au>SRINIVASAN, S</au><au>VIGROUX, L</au><au>WALTER, F</au><au>SMITH, J.-D. T</au><au>WARREN, B. E</au><au>CROXALL, K. V</au><au>MURPHY, E. J</au><au>DALE, D. A</au><au>DRAINE, B. T</au><au>WOLFIRE, M. G</au><format>journal</format><genre>article</genre><ristype>JOUR</ristype><atitle>A STUDY OF HEATING AND COOLING OF THE ISM IN NGC 1097 WITH HERSCHEL-PACS AND SPITZER-IRS</atitle><jtitle>The Astrophysical journal</jtitle><date>2012-06-01</date><risdate>2012</risdate><volume>751</volume><issue>2</issue><spage>1</spage><epage>16</epage><pages>1-16</pages><issn>0004-637X</issn><eissn>1538-4357</eissn><coden>ASJOAB</coden><abstract>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 sub(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 +[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 sub(0) ~ 10 super(2.3) and n sub(H) ~ 10 super(3.5) cm super(-3) in the ring. For these values of G sub(0) and n sub(H), PDR models cannot reproduce the observed H sub(2) emission. Much of the H sub(2) emission in the starburst ring could come from warm regions in the diffuse interstellar medium that are heated by turbulent dissipation or shocks.</abstract><cop>Bristol</cop><pub>IOP</pub><doi>10.1088/0004-637X/751/2/144</doi><tpages>16</tpages><orcidid>https://orcid.org/0000-0002-3933-7677</orcidid><orcidid>https://orcid.org/0000-0003-4793-7880</orcidid><orcidid>https://orcid.org/0000-0002-0283-8689</orcidid><orcidid>https://orcid.org/0000-0002-9768-0246</orcidid><oa>free_for_read</oa></addata></record> |
| fulltext | fulltext |
| identifier | ISSN: 0004-637X |
| ispartof | The Astrophysical journal, 2012-06, Vol.751 (2), p.1-16 |
| issn | 0004-637X 1538-4357 |
| language | eng |
| recordid | cdi_osti_scitechconnect_22037150 |
| source | Institute of Physics Open Access Journal Titles; Alma/SFX Local Collection; EZB Electronic Journals Library |
| subjects | ASTRONOMY ASTROPHYSICS ASTROPHYSICS, COSMOLOGY AND ASTRONOMY COMPUTERIZED SIMULATION Earth, ocean, space Emission EMISSION SPECTROSCOPY ENERGY SPECTRA Exact sciences and technology FAR INFRARED RADIATION GALAXIES GALAXY NUCLEI GAS COOLING Gas heating HEATING HYDROGEN Nuclei Photoelectricity PHOTOLYSIS PHOTON EMISSION Polyallylamine hydrochloride POLYCYCLIC AROMATIC HYDROCARBONS Sciences of the Universe Spectral energy distribution STARS Tracers |
| title | A STUDY OF HEATING AND COOLING OF THE ISM IN NGC 1097 WITH HERSCHEL-PACS AND SPITZER-IRS |
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