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Menten, K. M., Wyrowski, F., Keller, D. and Kaminski, T. (2018). Widespread HCN maser emission in carbon-rich evolved stars. Astron. Astrophys., 613. LES ULIS CEDEX A: EDP SCIENCES S A. ISSN 1432-0746

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Abstract

Context. HCN is a major constituent of the circumstellar envelopes of carbon-rich evolved stars, and rotational lines from within its vibrationally excited states probe parts of these regions closest to the stellar surface. A number of such lines are known to show maser action. Historically, in one of them, the 177 GHz J = 2 -> 1 line in the l-doubled bending mode has been found to show relatively strong maser action, with results only published for a single object, the archetypical high-mass loss asymptotic giant branch (AGB) star IRC+10216. Aims. To examine how common 177 GHz HCN maser emission is, we conducted an exploratory survey for this line toward a select sample of carbon-rich asymptotic giant branch stars that are observable from the southern hemisphere. Methods. We used the Atacama Pathfinder Experiment 12 meter submillimeter Telescope (APEX) equipped with a new receiver to simultaneously observe three J = 2 -> 1 HCN rotational transitions, the (0, 1(1c), 0) and (0, 1(1d), 0) l-doublet components, and the line from the (0, 0, 0) ground state. Results. The (0, 1(1c), 0) maser line is detected toward 11 of 13 observed sources, which all show emission in the (0, 0, 0) transition. In most of the sources, the peak intensity of the (0, 1(1c), 0) line rivals that of the (0, 0, 0) line; in two sources, it is even stronger. Except for the object with the highest mass-loss rate, IRC+10216, the (0,1(1d), 0) line covers a smaller velocity range than the (0, 0, 0) line. The (0, 1(1d), 0) line, which is detected in four of the sources, is much weaker than the other two lines and covers a velocity range that is smaller yet, again except for IRC+10216. Compared to its first detection in 1989, the profile of the (0, 1(1c), 0) line observed toward IRC+10216 looks very different, and we also appear to see variability in the (0, 0, 0) line profile (at a much lower degree). Our limited information on temporal variabilitydisfavors a strong correlation of maser and stellar continuum flux. Conclusions. Maser emission in the 177 GHz J = 2 -> 1 (0, 1(1c), 0) line of HCN appears to be common in carbon-rich AGB stars. Like for other vibrationally excited HCN lines, our observations indicate that the origin of these lines is in the acceleration zone of the stellar outflow in which dust is forming. For all the stars toward which we detect the maser line, the number of photons available at 7 and 14 pm, corresponding to transitions to vibrationally excited states possibly involved in its pumping, is found to be far greater than that of the maser photons, which makes radiative pumping feasible. Other findings point to a collisional pumping scheme, however.

Item Type:	Journal Article
Creators:	Creators Email ORCID ORCID Put Code Menten, K. M. UNSPECIFIED UNSPECIFIED UNSPECIFIED Wyrowski, F. UNSPECIFIED UNSPECIFIED UNSPECIFIED Keller, D. UNSPECIFIED UNSPECIFIED UNSPECIFIED Kaminski, T. UNSPECIFIED UNSPECIFIED UNSPECIFIED
URN:	urn:nbn:de:hbz:38-185883
DOI:	10.1051/0004-6361/201732296
Journal or Publication Title:	Astron. Astrophys.
Volume:	613
Date:	2018
Publisher:	EDP SCIENCES S A
Place of Publication:	LES ULIS CEDEX A
ISSN:	1432-0746
Language:	English
Faculty:	Unspecified
Divisions:	Unspecified
Subjects:	no entry
Uncontrolled Keywords:	Keywords Language MOLECULAR LINE OBSERVATIONS; VIBRATIONALLY EXCITED HCN; V-HYDRAE; CIRCUMSTELLAR ENVELOPES; MIRA VARIABLES; BIPOLAR OUTFLOW; GROUND-STATE; IRC+10216; RADIO; IRC Multiple languages Astronomy & Astrophysics Multiple languages
Refereed:	Yes
URI:	http://kups.ub.uni-koeln.de/id/eprint/18588