Volume 627, July 2019
|Number of page(s)||10|
|Section||Interstellar and circumstellar matter|
|Published online||05 July 2019|
Standing in the shadow of dark gas: ALMA observations of absorption from dark CO in the molecular dark neutral medium of Chamaeleon★
National Radio Astronomy Observatory,
520 Edgemont Road,
2 LERMA, Observatoire de Paris, PSL Research University, CNRS Sorbonne Universités, UPMC Université Paris 06, Ecole Normale Supérieure, 75005 Paris, France
3 Département d’Astrophysique, AIM, CEA-IRFU/CNRS/Université Paris Diderot, CEA, Saclay, 91191 Gif-sur-Yvette, France
Accepted: 1 May 2019
Context. We previously detected 89.2 GHz J = 1−0 HCO+ absorption in 12 directions lacking detected CO emission in the outskirts of the Chamaeleon cloud complex and toward one sightline with integrated CO emission WCO = 2.4 K km s−1. Eight sightlines had a much larger mean column density of dark neutral medium (DNM) – gas not represented in HI or CO emission – and were found to have much higher mean molecular column density. The five other sightlines had little or no DNM and were found to have much smaller but still detectable N(HCO+).
Aims. To determine the CO column density along previously observed Chamaeleon sightlines and to determine why CO emission was not detected in directions where molecular gas is present.
Methods. We took 12CO J = 1−0 absorption profiles toward five sightlines having higher DNM and HCO+ column densities and one sightline with smaller N(DNM) and N(HCO+). We converted the integrated HCO+ optical depths to N(H2) in the weak-excitation limit using N(HCO+)/N(H2) = 3 × 10−9 and converted the integrated CO optical depths ϒCO to CO column density using the relationship N(CO) = 1.861 × 1015 cm−2 ϒCO1.131 found along comparable lines of sight that were previously studied in J = 1−0 and J = 2−1 CO absorption and emission.
Results. CO absorption was detected along the five sightlines in the higher-DNM group, with CO column densities 4 × 1013 cm−2≲ N(CO) ≲1015 cm−2 that are generally below the detectability limit of CO emission surveys.
Conclusions. In the outskirts of the Chamaeleon complex, the presence of molecular DNM resulted primarily from small CO column densities at the onset of CO formation around the HI/H2 transition in diffuse molecular gas. CO relative abundances N(CO)/H2 ≲2 × 10−6 in the outskirts of Chamaeleon are comparable to those seen in UV absorption toward early-type stars, including in Chamaeleon.
Key words: ISM: molecules / dust, extinction / ISM: clouds
The data are only available at the CDS via anonymous ftp to cdsarc.u-strasbg.fr (18.104.22.168) or via http://cdsarc.u-strasbg.fr/viz-bin/qcat?J/A+A/627/A95
© ESO 2019
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