Pineda, Jorge L., Fischer, Christian, Kapala, Maria, Stutzki, Juergen, Buchbender, Christof, Goldsmith, Paul F., Ziebart, Monika, Glover, Simon C. O., Klessen, Ralf S., Koda, Jin, Kramer, Carsten, Mookerjea, Bhaswati ORCID: 0000-0003-1766-6303, Sandstrom, Karin, Scoville, Nick and Smith, Rowan ORCID: 0000-0002-0820-1814 (2018). A SOFIA Survey of [C II] in the Galaxy M51. I. [C II] as a Tracer of Star Formation. Astrophys. J. Lett., 869 (2). BRISTOL: IOP PUBLISHING LTD. ISSN 2041-8213

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Abstract

We present a [C II] 158 mu m map of the entire M51 (including M51b) grand design spiral galaxy observed with the Far Infrared Field-Imaging Line Spectrometer (FIFI-LS) instrument on board the Stratospheric Observatory For Infrared Astronomy (SOFIA). We compare the [C II] emission with the total far-infrared (TIR) intensity and star formation rate (SFR) surface density maps (derived using Ha and 24 mu m emission) to study the relationship between [C II] and the star formation activity in a variety of environments within M51 on scales of 16 '' corresponding to similar to 660 pc. We find that [C II] and the SFR surface density are well correlated in the central, spiral arm, and inter-arm regions. The correlation is in good agreement with that found for a larger sample of nearby galaxies at kpc scales. We find that the SFR, and [C II] and TIR luminosities in M51, are dominated by the extended emission in M51's disk. The companion galaxy M51b, however, shows a deficit of [C II] emission compared with the TIR emission and SFR surface density, with [C II] emission detected only in the SW part of this galaxy. The [C II] deficit is associated with an enhanced dust temperature in this galaxy. We interpret the faint [C II] emission in M51b to be a result of suppressed star formation in this galaxy, while the bright mid-and far-infrared emission, which drive the TIR and SFR values, are powered by other mechanisms. A similar but less-pronounced effect is seen at the location of the black hole in M51's center. The observed [C II] deficit in M51b suggests that this galaxy is a valuable laboratory to study the origin of the apparent [C II] deficit observed in ultra-luminous galaxies.

Item Type: Journal Article
Creators:
CreatorsEmailORCIDORCID Put Code
Pineda, Jorge L.UNSPECIFIEDUNSPECIFIEDUNSPECIFIED
Fischer, ChristianUNSPECIFIEDUNSPECIFIEDUNSPECIFIED
Kapala, MariaUNSPECIFIEDUNSPECIFIEDUNSPECIFIED
Stutzki, JuergenUNSPECIFIEDUNSPECIFIEDUNSPECIFIED
Buchbender, ChristofUNSPECIFIEDUNSPECIFIEDUNSPECIFIED
Goldsmith, Paul F.UNSPECIFIEDUNSPECIFIEDUNSPECIFIED
Ziebart, MonikaUNSPECIFIEDUNSPECIFIEDUNSPECIFIED
Glover, Simon C. O.UNSPECIFIEDUNSPECIFIEDUNSPECIFIED
Klessen, Ralf S.UNSPECIFIEDUNSPECIFIEDUNSPECIFIED
Koda, JinUNSPECIFIEDUNSPECIFIEDUNSPECIFIED
Kramer, CarstenUNSPECIFIEDUNSPECIFIEDUNSPECIFIED
Mookerjea, BhaswatiUNSPECIFIEDorcid.org/0000-0003-1766-6303UNSPECIFIED
Sandstrom, KarinUNSPECIFIEDUNSPECIFIEDUNSPECIFIED
Scoville, NickUNSPECIFIEDUNSPECIFIEDUNSPECIFIED
Smith, RowanUNSPECIFIEDorcid.org/0000-0002-0820-1814UNSPECIFIED
URN: urn:nbn:de:hbz:38-161806
DOI: 10.3847/2041-8213/aaf1ad
Journal or Publication Title: Astrophys. J. Lett.
Volume: 869
Number: 2
Date: 2018
Publisher: IOP PUBLISHING LTD
Place of Publication: BRISTOL
ISSN: 2041-8213
Language: English
Faculty: Unspecified
Divisions: Unspecified
Subjects: no entry
Uncontrolled Keywords:
KeywordsLanguage
NEARBY GALAXIES; EMISSION; LINE; M83; AGNMultiple languages
Astronomy & AstrophysicsMultiple languages
Refereed: Yes
URI: http://kups.ub.uni-koeln.de/id/eprint/16180

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