@Article{Velusamy_etal2010,
author="Velusamy, T.
and Langer, W. D.
and Pineda, J. L.
and Goldsmith, P. F.
and Li, D.
and Yorke, H. W.",
title="[CII] observations of H$_{2}$ molecular layers in transition clouds",
journal="Astron. Astrophys.",
year="2010",
volume="521",
pages="L18",
optkeywords="HEB mixer applications; HIFI; Herschel; ISM: structure / ISM: molecules / ISM: atoms / submillimeter: ISM",
abstract="We present the first results on the diffuse transition clouds observed in [CII] line emission at 158 $\mu$m (1.9 THz) towards Galactic longitudes near 340{\textdegree} (5 LOSs) {\&} 20{\textdegree} (11 LOSs) as part of the HIFI tests and GOT C+ survey. Out of the total 146 [CII] velocity components detected by profile fitting we identify 53 as diffuse molecular clouds with associated 12CO emission but without 13CO emission and characterized by AV < 5 mag. We estimate the fraction of the [CII] emission in the diffuse HI layer in each cloud and then determine the [CII] emitted from the molecular layers in the cloud. We show that the excess [CII] intensities detected in a few clouds is indicative of a thick H2 layer around the CO core. The wide range of clouds in our sample with thin to thick H2 layers suggests that these are at various evolutionary states characterized by the formation of H2 and CO layers from HI and C+, respectively. In about 30{\%} of the clouds the H2 column densities ({\^a}{\texteuro}{\oe}dark gas{\^a}{\texteuro}) traced by the [CII] is 50{\%} or more than that traced by 12CO emission. On the average {\textasciitilde}25{\%} of the total H2 in these clouds is in an H2 layer which is not traced by CO. We use the HI, [CII], and 12CO intensities in each cloud along with simple chemical models to obtain constraints on the FUV fields and cosmic ray ionization rates.",
optnote="exported from refbase (https://db.rplab.ru/refbase/show.php?record=1102), last updated on Fri, 17 Jun 2016 18:01:08 -0500",
doi="10.1051/0004-6361/201015091",
opturl="https://doi.org/10.1051/0004-6361/201015091"
}