2018A&A...613A..49M


C.D.S. - SIMBAD4 rel 1.7 - 2019.12.09CET21:36:59

2018A&A...613A..49M - Astronomy and Astrophysics, volume 613A, 49-49 (2018/5-1)

Widespread HCN maser emission in carbon-rich evolved stars.

MENTEN K.M., WYROWSKI F., KELLER D. and KAMINSKI T.

Abstract (from CDS):

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, 11c, 0) and (0, 11d, 0) l-doublet components, and the line from the (0, 0, 0) ground state. Results. The (0, 11c, 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, 11c, 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, 11c, 0) line covers a smaller velocity range than the (0, 0, 0) line. The (0, 11d, 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, 11c, 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 177GHz J=2-1 (0, 11c, 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 14µm, 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.

Abstract Copyright: © ESO 2018

Journal keyword(s): masers - stars: AGB and post-AGB - stars: carbon - circumstellar matter

Simbad objects: 16

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Number of rows : 16

N Identifier Otype ICRS (J2000)
RA
ICRS (J2000)
DEC
Mag U Mag B Mag V Mag R Mag I Sp type #ref
1850 - 2020
#notes
1 * omi Cet Mi* 02 19 20.79210 -02 58 39.4956   7.63 6.53 5.03   M5-9IIIe+DA 1414 0
2 V* R For C* 02 29 15.3081251463 -26 05 55.647016467   12.94 7.50     C4,3e 177 0
3 V* V571 Per LP* 03 11 23.7106154062 +38 04 09.929357618   9.05 7.35     M5: 17 0
4 RAFGL 618 pA* 04 42 53.6245215366 +36 06 53.397219192   16.32   12.59   C-rich 944 0
5 V* R Lep C* 04 59 36.3480393629 -14 48 22.511432606 15.06 13.51 7.76 4.90 3.42 C7,6e 312 0
6 RAFGL 4078 C* 07 45 02.4140089106 -71 19 45.852846228       15.92 12.72 C 44 0
7 V* X Cnc C* 08 55 22.8824572992 +17 13 52.585346790   9.63 6.40 4.29 2.90 C-N4.5 254 1
8 RAFGL 5254 C* 09 13 53.9380628049 -24 51 25.223261483           C-rich 48 0
9 IRC +10216 C* 09 47 57.406 +13 16 43.56     10.96     C9,5e 2109 0
10 V* X Vel C* 09 55 26.1119127674 -41 35 12.790399779   10.29 10.30 7.13 8.80 C-N3 61 0
11 V* RW LMi C* 10 16 02.2834693816 +30 34 18.977096332       15.27   C4,3e 377 0
12 V* U Hya C* 10 37 33.2729535 -13 23 04.352923 13.29 7.51 4.82 3.05 1.78 C-N5 282 0
13 V* V Hya C* 10 51 37.2614060865 -21 15 00.339641553   12.23 6.80     C-N:6 335 0
14 RAFGL 4211 C* 15 11 41.4387312231 -48 19 58.763122448           C-rich 46 0
15 V* X TrA C* 15 14 19.1744832785 -70 04 46.126632480 15.88 9.19 5.81     C5,5 104 0
16 WOS 48 C* 15 23 05.0744336371 -51 25 58.881494593   17.85 16.66 14.51 10.18 C 117 1

    Equat.    Gal    SGal    Ecl

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2019.12.09-21:36:59

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