2013
DOI: 10.1051/0004-6361/201322129
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Gas-phase CO depletion and N2H+abundances in starless cores

Abstract: Context. In the dense and cold interiors of starless molecular cloud cores, a number of chemical processes allow for the formation of complex molecules and the deposition of ice layers on dust grains. Dust density and temperature maps of starless cores derived from Herschel continuum observations constrain the physical structure of the cloud cores better than ever before. We use these to model the temporal chemical evolution of starless cores. Aims. We derive molecular abundance profiles for a sample of starle… Show more

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Cited by 46 publications
(100 citation statements)
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“…For instance, temperatures based on such observations are around the (for a dense core) surprisingly high value of ∼25 K. At temperatures below this, which are commonly encountered in dense cores, the CO gas will be depleted because of freeze-out of the molecules onto the surfaces of the accompanying grains. In contrast, N 2 H + molecules remain in the gas phase down to much lower temperatures (Lippok et al 2013, and references therein).…”
Section: Discussionmentioning
confidence: 99%
See 1 more Smart Citation
“…For instance, temperatures based on such observations are around the (for a dense core) surprisingly high value of ∼25 K. At temperatures below this, which are commonly encountered in dense cores, the CO gas will be depleted because of freeze-out of the molecules onto the surfaces of the accompanying grains. In contrast, N 2 H + molecules remain in the gas phase down to much lower temperatures (Lippok et al 2013, and references therein).…”
Section: Discussionmentioning
confidence: 99%
“…However, at temperatures below about 25 K, the abundance of the dominant gas tracer, CO and its isotopologues, could also become highly diminished by freeze-out (e.g., Lippok et al 2013, and references therein). One might therefore select spectral lines of a molecule that is seen in regions where CO is thought to be depleted.…”
Section: Introductionmentioning
confidence: 99%
“…Previous papers in this series made such data available for the giant molecular clouds near W51 and W3 (Bieging et al 2010;Bieging & Peters 2011); and for the intermediate mass Serpens cloud (Burleigh et al 2013). Observations of Bok globules are shown in Stutz et al (2009) and Lippok et al (2013). We have also given summary results for GMCs associated with the H ii regions Sh 254-258 ) and M17 (Povich et al 2009).…”
Section: Introductionmentioning
confidence: 98%
“…Previous papers reported on the giant molecular clouds (GMCs) associated with H II regions W51 (Bieging et al 2010) and W3 (Bieging & Peters 2011); and on the lower-mass clouds in Serpens (Burleigh et al 2013) and the NGC1333 region in Perseus (Bieging et al 2014). In addition, summary results have been given for molecular clouds associated with the H II regions Sh2-254-258 ) and M17 (Povich et al 2009), and for a selection of Bok Globules (Stutz et al 2009;Lippok et al 2013). …”
Section: Introductionmentioning
confidence: 99%