Survey of lines in M 31: [CII] as SFR tracer at ~ 50 pc scales. Issue Volume 10:Issue S309(2014) (9th February 2015)

• Record Type: Journal Article
• Authors: Kapala, M. J.; Sandstrom, K.; Groves, B.
• Editors: Ziegler, Bodo L.; Combes, Françoise; Dannerbauer, Helmut; Verdugo, Miguel
• Is Part Of: Proceedings of the International Astronomical Union. Volume 10:Issue S309(2014)
• Page Start: 321
• Page End: 321
• Publication Date: 2015-02-09
• Subjects: Astronomy -- Congresses; Astronomy -- Periodicals; 520
• DOI: 10.1017/S1743921314010175
• Languages: English
• ISSNs: 1743-9213

Abstract

Abstract : The [CII] 158 μm line is typically the brightest far-IR emission line from star-forming galaxies. As such, this line is a possible tracer of star-formation, but to do so we need the relative contributions of different ISM phases. Using high physical resolution observations of the [CII] 158 μm line from Herschel PACS in five 3'×3' field in M 31 and optical IFU spectra from PPaK and ancillary IR data, we are able to spatially separate out the ISM phases Kapala . We find that a large fraction of [CII] emission in M 31 arises from diffuse gas (~20–90), with a sub-linear relation of [CII]–SFR at ~50 pc scales. However, on ~kpc scales, the observed empirical [CII]–SFR relation is in agreement with other extragalactic studies.