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The physical characteristics of the gas in the disk of Centaurus A using the Herschel Space Observatory

TJ Parkin, CD Wilson, MRP Schirm, Maarten Baes (UGent) , M Boquien, A Boselli, D Cormier, M Galametz, OL Karczewski, V Lebouteiller, et al.
(2014) ASTROPHYSICAL JOURNAL. 787(1).
Author
Organization
Abstract
We search for variations in the disk of Centaurus A of the emission from atomic fine structure lines using Herschel PACS and SPIRE spectroscopy. In particular, we observe the [C II](158 mu m), [N II](122 and 205 mu m), [O I](63 and 145 mu m), and [O III](88 mu m) lines, which all play an important role in cooling the gas in photo-ionized and photodissociation regions (PDRs). We determine that the ([C II]+[O I](63))/F-TIR line ratio, a proxy for the heating efficiency of the gas, shows no significant radial trend across the observed region, in contrast to observations of other nearby galaxies. We determine that 10%-20% of the observed [C II] emission originates in ionized gas. Comparison between our observations and a PDR model shows that the strength of the far-ultraviolet radiation field, G(0), varies between 10(1.75) and 10(2.75) and the hydrogen nucleus density varies between 10(2.75) and 10(3.75) cm(-3), with no significant radial trend in either property. In the context of the emission line properties of the grand-design spiral galaxy M51 and the elliptical galaxy NGC 4125, the gas in Cen A appears more characteristic of that in typical disk galaxies rather than elliptical galaxies.
Keywords
galaxies: ISM, galaxies: individual (Centaurus A), infrared: ISM, ISM: lines and bands, PHOTON-DOMINATED REGIONS, EARLY-TYPE GALAXIES, ULTRALUMINOUS INFRARED GALAXIES, STAR-FORMING GALAXIES, C-II, MOLECULAR GAS, MU-M, PHOTODISSOCIATION REGIONS, INTERSTELLAR-MEDIUM, NGC 5128

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MLA
Parkin, TJ, et al. “The Physical Characteristics of the Gas in the Disk of Centaurus A Using the Herschel Space Observatory.” ASTROPHYSICAL JOURNAL, vol. 787, no. 1, 2014, doi:10.1088/0004-637X/787/1/16.
APA
Parkin, T., Wilson, C., Schirm, M., Baes, M., Boquien, M., Boselli, A., … Spinoglio, L. (2014). The physical characteristics of the gas in the disk of Centaurus A using the Herschel Space Observatory. ASTROPHYSICAL JOURNAL, 787(1). https://doi.org/10.1088/0004-637X/787/1/16
Chicago author-date
Parkin, TJ, CD Wilson, MRP Schirm, Maarten Baes, M Boquien, A Boselli, D Cormier, et al. 2014. “The Physical Characteristics of the Gas in the Disk of Centaurus A Using the Herschel Space Observatory.” ASTROPHYSICAL JOURNAL 787 (1). https://doi.org/10.1088/0004-637X/787/1/16.
Chicago author-date (all authors)
Parkin, TJ, CD Wilson, MRP Schirm, Maarten Baes, M Boquien, A Boselli, D Cormier, M Galametz, OL Karczewski, V Lebouteiller, Ilse De Looze, SC Madden, H Roussel, MWL Smith, and L Spinoglio. 2014. “The Physical Characteristics of the Gas in the Disk of Centaurus A Using the Herschel Space Observatory.” ASTROPHYSICAL JOURNAL 787 (1). doi:10.1088/0004-637X/787/1/16.
Vancouver
1.
Parkin T, Wilson C, Schirm M, Baes M, Boquien M, Boselli A, et al. The physical characteristics of the gas in the disk of Centaurus A using the Herschel Space Observatory. ASTROPHYSICAL JOURNAL. 2014;787(1).
IEEE
[1]
T. Parkin et al., “The physical characteristics of the gas in the disk of Centaurus A using the Herschel Space Observatory,” ASTROPHYSICAL JOURNAL, vol. 787, no. 1, 2014.
@article{5921238,
  abstract     = {{We search for variations in the disk of Centaurus A of the emission from atomic fine structure lines using Herschel PACS and SPIRE spectroscopy. In particular, we observe the [C II](158 mu m), [N II](122 and 205 mu m), [O I](63 and 145 mu m), and [O III](88 mu m) lines, which all play an important role in cooling the gas in photo-ionized and photodissociation regions (PDRs). We determine that the ([C II]+[O I](63))/F-TIR line ratio, a proxy for the heating efficiency of the gas, shows no significant radial trend across the observed region, in contrast to observations of other nearby galaxies. We determine that 10%-20% of the observed [C II] emission originates in ionized gas. Comparison between our observations and a PDR model shows that the strength of the far-ultraviolet radiation field, G(0), varies between 10(1.75) and 10(2.75) and the hydrogen nucleus density varies between 10(2.75) and 10(3.75) cm(-3), with no significant radial trend in either property. In the context of the emission line properties of the grand-design spiral galaxy M51 and the elliptical galaxy NGC 4125, the gas in Cen A appears more characteristic of that in typical disk galaxies rather than elliptical galaxies.}},
  articleno    = {{16}},
  author       = {{Parkin, TJ and Wilson, CD and Schirm, MRP and Baes, Maarten and Boquien, M and Boselli, A and Cormier, D and Galametz, M and Karczewski, OL and Lebouteiller, V and De Looze, Ilse and Madden, SC and Roussel, H and Smith, MWL and Spinoglio, L}},
  issn         = {{0004-637X}},
  journal      = {{ASTROPHYSICAL JOURNAL}},
  keywords     = {{galaxies: ISM,galaxies: individual (Centaurus A),infrared: ISM,ISM: lines and bands,PHOTON-DOMINATED REGIONS,EARLY-TYPE GALAXIES,ULTRALUMINOUS INFRARED GALAXIES,STAR-FORMING GALAXIES,C-II,MOLECULAR GAS,MU-M,PHOTODISSOCIATION REGIONS,INTERSTELLAR-MEDIUM,NGC 5128}},
  language     = {{eng}},
  number       = {{1}},
  pages        = {{14}},
  title        = {{The physical characteristics of the gas in the disk of Centaurus A using the Herschel Space Observatory}},
  url          = {{http://doi.org/10.1088/0004-637X/787/1/16}},
  volume       = {{787}},
  year         = {{2014}},
}
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