%0 Generic %1 pabst2021158mumathrmm %A Pabst, C. H. M. %A Hacar, A. %A Goicoechea, J. R. %A Teyssier, D. %A Berné, O. %A Wolfire, M. G. %A Higgins, R. D. %A Chambers, E. T. %A Kabanovic, S. %A Güsten, R. %A Stutzki, J. %A Kramer, C. %A Tielens, A. G. G. M. %D 2021 %K library %T CII $158\,\mum$ line emission from Orion A. I. A template for extragalactic studies? %U http://arxiv.org/abs/2105.03735 %X The CII $158\,\mum$ fine-structure line is one of the dominant coolants of the neutral interstellar medium. It is hence one of the brightest far-infrared emission lines and can be observed not only in star-forming regions throughout the Galaxy, but also in the diffuse interstellar medium and in distant galaxies. CII line emission has been suggested to be a powerful tracer of star-formation. We aim to understand the origin of CII emission and its relation to other tracers of interstellar gas and dust. This includes a study of the heating efficiency of interstellar gas as traced by the CII line to test models of gas heating. We make use of a one-square-degree map of velocity-resolved CII line emission towards the Orion Nebula complex, including M43 and NGC 1977. The CII intensity is tightly correlated with PAH emission in the IRAC $8\,\mum$ band and far-infrared emission from warm dust. The correlation between CII and CO(2-1) is affected by the detailed geometry of the region. We find particularly low CII-over-FIR intensity ratios towards large columns of (warm and cold) dust, which suggest the interpretation of the "CII deficit" in terms of a "FIR excess". A slight decrease in the FIR line-over-continuum intensity ratio can be attributed to a decreased heating efficiency of the gas. We find that, at the mapped spatial scales, predictions of the star-formation rate from CII emission underestimate the star-formation rate calculated from YSO counts in the Orion Nebula complex by an order of magnitude. CII emission from the Orion Nebula complex arises dominantly in the cloud surfaces, many viewed in edge-on geometry. CII emission from extended faint cloud surfaces may contribute significantly to the total CII emission on galactic scales.

@misc{pabst2021158mumathrmm, abstract = {The [CII] $158\,\mu\mathrm{m}$ fine-structure line is one of the dominant coolants of the neutral interstellar medium. It is hence one of the brightest far-infrared emission lines and can be observed not only in star-forming regions throughout the Galaxy, but also in the diffuse interstellar medium and in distant galaxies. [CII] line emission has been suggested to be a powerful tracer of star-formation. We aim to understand the origin of [CII] emission and its relation to other tracers of interstellar gas and dust. This includes a study of the heating efficiency of interstellar gas as traced by the [CII] line to test models of gas heating. We make use of a one-square-degree map of velocity-resolved [CII] line emission towards the Orion Nebula complex, including M43 and NGC 1977. The [CII] intensity is tightly correlated with PAH emission in the IRAC $8\,\mu\mathrm{m}$ band and far-infrared emission from warm dust. The correlation between [CII] and CO(2-1) is affected by the detailed geometry of the region. We find particularly low [CII]-over-FIR intensity ratios towards large columns of (warm and cold) dust, which suggest the interpretation of the "[CII] deficit" in terms of a "FIR excess". A slight decrease in the FIR line-over-continuum intensity ratio can be attributed to a decreased heating efficiency of the gas. We find that, at the mapped spatial scales, predictions of the star-formation rate from [CII] emission underestimate the star-formation rate calculated from YSO counts in the Orion Nebula complex by an order of magnitude. [CII] emission from the Orion Nebula complex arises dominantly in the cloud surfaces, many viewed in edge-on geometry. [CII] emission from extended faint cloud surfaces may contribute significantly to the total [CII] emission on galactic scales.}, added-at = {2021-05-11T07:26:54.000+0200}, author = {Pabst, C. H. M. and Hacar, A. and Goicoechea, J. R. and Teyssier, D. and Berné, O. and Wolfire, M. G. and Higgins, R. D. and Chambers, E. T. and Kabanovic, S. and Güsten, R. and Stutzki, J. and Kramer, C. and Tielens, A. G. G. M.}, biburl = {https://www.bibsonomy.org/bibtex/2680cc7ebad67f0bd2e8777effe7b2902/gpkulkarni}, description = {[CII] $158\,\mu\mathrm{m}$ line emission from Orion A. I. A template for extragalactic studies?}, interhash = {c69e42369c6777c0d9f05bc1c7e58bb0}, intrahash = {680cc7ebad67f0bd2e8777effe7b2902}, keywords = {library}, note = {cite arxiv:2105.03735}, timestamp = {2021-05-11T07:26:54.000+0200}, title = {[CII] $158\,\mu\mathrm{m}$ line emission from Orion A. I. A template for extragalactic studies?}, url = {http://arxiv.org/abs/2105.03735}, year = 2021 }