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Survey of lines in M 31: [CII] as SFR tracer at ~ 50 pc scales

Published online by Cambridge University Press:  09 February 2015

M. J. Kapala ,
K. Sandstrom  and
B. Groves
M. J. Kapala
Affiliation:
Max Planck Institut für Astronomie, Königstuhl 17, D-69117 Heidelberg, Germany email: [email protected]
K. Sandstrom
Affiliation:
Max Planck Institut für Astronomie, Königstuhl 17, D-69117 Heidelberg, Germany email: [email protected] Steward Observatory, Tucson, USA
B. Groves
Affiliation:
Max Planck Institut für Astronomie, Königstuhl 17, D-69117 Heidelberg, Germany email: [email protected]
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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.

Type
Contributed Papers
Information
Proceedings of the International Astronomical Union , Volume 10 , Issue S309: Galaxies in 3D across the Universe , July 2014 , pp. 321
Copyright
Copyright © International Astronomical Union 2015 

References

Kapala, M. J., et al., subm., ApJGoogle Scholar