%0 Generic %1 Mookerjea2011 %A Mookerjea, B. %A Kramer, C. %A Buchbender, C. %A Boquien, M. %A Verley, S. %A Relano, M. %A Quintana-Lacaci, G. %A Aalto, S. %A Braine, J. %A Calzetti, D. %A Combes, F. %A Garcia-Burillo, S. %A Gratier, P. %A Henkel, C. %A Israel, F. %A Lord, S. %A Nikola, T. %A Roellig, M. %A Stacey, G. %A Tabatabaei, F. S. %A van der Tak, F. %A van der Werf, P. %D 2011 %K CO [CII] cooling ism m33 %T The Herschel M33 extended survey (HerM33es): PACS spectroscopy of the star forming region BCLMP 302 %U http://arxiv.org/abs/1106.5464 %X Context: The emission line of CII at 158 micron is one of the strongest cooling lines of the interstellar medium (ISM) in galaxies. Aims: Disentangling the relative contributions of the different ISM phases to CII emission, is a major topic of the HerM33es program, a Herschel key project to study the ISM in the nearby spiral galaxy M33. Methods: Using PACS, we have mapped the emission of CII 158 micron, OI 63 micron, and other FIR lines in a 2'x2' region of the northern spiral arm of M33, centered on the HII region BCLMP302. At the peak of H-alpha emission, we have observed in addition a velocity resolved CII spectrum using HIFI. We use scatterplots to compare these data with PACS 160 micron continuum maps, and with maps of CO and HI data, at a common resolution of 12 arcsec or 50 pc. Maps of H-alpha and 24 micron emission observed with Spitzer are used to estimate the SFR. We have created maps of the CII and OI 63 micron emission and detected NII 122 micron and NIII 57 micron at individual positions. Results: The CII line observed with HIFI is significantly broader than that of CO, and slightly blue-shifted. In addition, there is little spatial correlation between CII observed with PACS and CO over the mapped region. There is even less spatial correlation between CII and the atomic gas traced by HI. Detailed comparison of the observed intensities towards the HII region with models of photo ionization and photon dominated regions, confirms that a significant fraction, 20--30%, of the observed CII emission stems from the ionized gas and not from the molecular cloud. The gas heating efficiency, using the ratio between CII and the TIR as a proxy, varies between 0.07 and 1.5%, with the largest variations found outside the HII region.

@misc{Mookerjea2011, abstract = { Context: The emission line of [CII] at 158 micron is one of the strongest cooling lines of the interstellar medium (ISM) in galaxies. Aims: Disentangling the relative contributions of the different ISM phases to [CII] emission, is a major topic of the HerM33es program, a Herschel key project to study the ISM in the nearby spiral galaxy M33. Methods: Using PACS, we have mapped the emission of [CII] 158 micron, [OI] 63 micron, and other FIR lines in a 2'x2' region of the northern spiral arm of M33, centered on the HII region BCLMP302. At the peak of H-alpha emission, we have observed in addition a velocity resolved [CII] spectrum using HIFI. We use scatterplots to compare these data with PACS 160 micron continuum maps, and with maps of CO and HI data, at a common resolution of 12 arcsec or 50 pc. Maps of H-alpha and 24 micron emission observed with Spitzer are used to estimate the SFR. We have created maps of the [CII] and [OI] 63 micron emission and detected [NII] 122 micron and NIII 57 micron at individual positions. Results: The [CII] line observed with HIFI is significantly broader than that of CO, and slightly blue-shifted. In addition, there is little spatial correlation between [CII] observed with PACS and CO over the mapped region. There is even less spatial correlation between [CII] and the atomic gas traced by HI. Detailed comparison of the observed intensities towards the HII region with models of photo ionization and photon dominated regions, confirms that a significant fraction, 20--30%, of the observed [CII] emission stems from the ionized gas and not from the molecular cloud. The gas heating efficiency, using the ratio between [CII] and the TIR as a proxy, varies between 0.07 and 1.5%, with the largest variations found outside the HII region. }, added-at = {2011-06-28T08:43:46.000+0200}, author = {Mookerjea, B. and Kramer, C. and Buchbender, C. and Boquien, M. and Verley, S. and Relano, M. and Quintana-Lacaci, G. and Aalto, S. and Braine, J. and Calzetti, D. and Combes, F. and Garcia-Burillo, S. and Gratier, P. and Henkel, C. and Israel, F. and Lord, S. and Nikola, T. and Roellig, M. and Stacey, G. and Tabatabaei, F. S. and van der Tak, F. and van der Werf, P.}, biburl = {https://www.bibsonomy.org/bibtex/2798b1356354f1d220da8bf8cf75da67b/miki}, description = {[1106.5464] The Herschel M33 extended survey (HerM33es): PACS spectroscopy of the star forming region BCLMP 302}, interhash = {ca5318753e0fb64b6d3d84668aa6ed50}, intrahash = {798b1356354f1d220da8bf8cf75da67b}, keywords = {CO [CII] cooling ism m33}, note = {cite arxiv:1106.5464Comment: Accepted for publication in A&A. 12 pages, 12 figures}, timestamp = {2011-06-28T08:43:46.000+0200}, title = {The Herschel M33 extended survey (HerM33es): PACS spectroscopy of the star forming region BCLMP 302}, url = {http://arxiv.org/abs/1106.5464}, year = 2011 }