FIRST DETECTION OF HYDROGEN CHLORIDE TOWARD PROTOSTELLAR SHOCKS

We present the first detection of hydrogen chloride in a protostellar shock by observing the fundamental transition at 626 GHz with the HIFI spectrometer. We detected two of the three hyperfine lines from which we derived a line opacity [< or = ]1. Using a non-local thermodynamic equilibrium larg...

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Bibliographic Details
Published in:Astrophysical journal. Letters 2012-01, Vol.744 (2), p.1-5
Main Authors: Codella, C, Ceccarelli, C, Bottinelli, S, Salez, M, Vitt, S, LeFloch, B, Cabrit, S, Caux, E, Faure, A, Vasta, M, Wiesenfeld, L
Format: Article
Language:English
Subjects:
ABUNDANCE
Astrophysics
ASTROPHYSICS, COSMOLOGY AND ASTRONOMY
CHLORINE
COMPUTERIZED SIMULATION
Density
Emission
Gas phases
HYDROCHLORIC ACID
Hydrogen chlorides
INTERFEROMETERS
Mathematical models
OPACITY
Physics
PROTOSTARS
SPECTROMETERS
STAR EVOLUTION
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Summary:We present the first detection of hydrogen chloride in a protostellar shock by observing the fundamental transition at 626 GHz with the HIFI spectrometer. We detected two of the three hyperfine lines from which we derived a line opacity [< or = ]1. Using a non-local thermodynamic equilibrium large velocity gradient code, we constrained the HCl column density, temperature, and density of the emitting gas. The hypothesis that the emission originates in the molecular cloud is ruled out because it would imply a very dense gas. Conversely, assuming that the emission originates in the 10"-15" size shocked gas previously observed at the IRAM Plateau de Bure Interferometer, we obtain N(HCl) = 0.7-2 x 10 super(13) cm super(-2), temperature >15 K, and density >3 x 10 super(5) cm super(-3). Combining these with the Herschel HIFI CO(5-4) observations allows us to further constrain the gas density and temperature, 10 super(5)-10 super(6) cm super(-3) and 120-250 K, respectively, as well as the HCl column density, 2 x 10 super(13) cm super(-2), and, finally, the abundance ~3-6 x 10 super(-9). The estimated HCl abundance is consistent with that previously observed in low- and high-mass protostars. This puzzling result in the L1157-B1 shock, where species from volatile and refractory grain components are enhanced, suggests either that HCl is not the main reservoir of chlorine in the gas phase, which goes against previous chemical model predictions, or that the elemental chlorine abundance is low in L1157-B1. Astrochemical modeling suggests that HCl is in fact formed in the gas phase at low temperatures prior to the occurrence of the shock; the latter does not enhance its abundance.
ISSN:0004-637X
2041-8205
1538-4357
2041-8213
DOI:10.1088/0004-637X/744/2/164