2017A&A...606A.124D


C.D.S. - SIMBAD4 rel 1.7 - 2020.07.03CEST22:16:18

2017A&A...606A.124D - Astronomy and Astrophysics, volume 606A, 124-124 (2017/10-1)

Sulphur-bearing molecules in AGB stars. I. The occurrence of hydrogen sulphide.

DANILOVICH T., VAN DE SANDE M., DE BECK E., DECIN L., OLOFSSON H., RAMSTEDT S. and MILLAR T.J.

Abstract (from CDS):

Context. Sulphur is a relatively abundant element in the local Galaxy that is known to form a variety of molecules in the circumstellar envelopes of AGB stars. The abundances of these molecules vary based on the chemical types and mass-loss rates of AGB stars.
Aims. Through a survey of (sub-)millimetre emission lines of various sulphur-bearing molecules, we aim to determine which molecules are the primary carriers of sulphur in different types of AGB stars. In this paper, the first in a series, we investigate the occurrence of H2S in AGB circumstellar envelopes and determine its abundance, where possible.
Methods. We surveyed 20 AGB stars with a range of mass-loss rates and different chemical types using the Atacama Pathfinder Experiment (APEX) telescope to search for rotational transition lines of five key sulphur-bearing molecules: CS, SiS, SO, SO2, and H2S. Here we present our results for H2S, including detections, non-detections, and detailed radiative transfer modelling of the detected lines. We compared results based on various descriptions of the molecular excitation of H2S and different abundance distributions, including Gaussian abundances, where possible, and two different abundance distributions derived from chemical modelling results.
Results. We detected H2S towards five AGB stars, all of which have high mass-loss rates of M≥g5x10–6M/yr and are oxygen rich. H2S was not detected towards the carbon or S-type stars that fall in a similar mass-loss range. For the stars in our sample with detections, we find peak o-H2S abundances relative to H2 between 4x10–7 and 2.5x10–5.
Conclusions. Overall, we conclude that H2S can play a significant role in oxygen-rich AGB stars with higher mass-loss rates, but is unlikely to play a key role in stars of other chemical types or in lower mass-loss rate oxygen-rich stars. For two sources, V1300 Aql and GX Mon, H2S is most likely the dominant sulphur-bearing molecule in the circumstellar envelope.

Abstract Copyright: © ESO, 2017

Journal keyword(s): stars: AGB and post-AGB - circumstellar matter - stars: evolution - stars: mass-loss - stars: mass-loss

Simbad objects: 28

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Number of rows : 28

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 V* T Cet S* 00 21 46.2731778 -20 03 28.884826   7.32 5.74     M5-6Se 139 0
2 V* R And S* 00 24 01.9473999328 +38 34 37.326131071 10.61 9.36 7.39 4.45 2.30 S5-7/4-5e 338 0
3 IRC +10011 OH* 01 06 25.9889735162 +12 35 52.890666456   20.7   18.26 14.01 M8 396 0
4 V* R Hor Mi* 02 53 52.7746504509 -49 53 22.732999275     3.92 4.99 1.51 M5-7e 169 0
5 V* IK Tau Mi* 03 53 28.8884898148 +11 24 21.865959095 16.99 17.03 13.39 7.29 3.20 M7-11 570 0
6 V* R Lep C* 04 59 36.3480393629 -14 48 22.511432606 15.06 13.51 7.76 4.90 3.42 C7,6e 315 0
7 V* TX Cam Mi* 05 00 51.1569959503 +56 10 54.093107078       14.02   M9-9.5 328 0
8 RAFGL 865 C* 06 04 00.04728 +07 25 52.0104           C-rich 95 0
9 V* GX Mon OH* 06 52 47.0411386021 +08 25 19.131304542   15.40 15.46 10.56   M9 105 0
10 OH 231.8 +4.2 OH* 07 42 16.947 -14 42 50.20           M10III+A 503 1
11 RAFGL 4078 C* 07 45 02.4140089106 -71 19 45.852846228       15.92 12.72 C 44 0
12 IRC +10216 C* 09 47 57.40632 +13 16 43.5648     10.96     C9,5e 2133 0
13 V* TT Cen S* 13 19 35.0158270198 -60 46 46.290333346     11.50     SC5:/8+ 48 0
14 V* W Hya Mi* 13 49 02.0018313132 -28 22 03.532006894   8.97 7.70     M7.5-9e 598 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 118 1
17 RAFGL 5379 OH* 17 44 24.0038735481 -31 55 35.428622508           ~ 83 0
18 NAME Gal Center reg 17 45 40.04 -29 00 28.1           ~ 11533 0
19 IRC +10365 Mi* 18 37 19.2595666948 +10 25 42.492197977           M9 133 0
20 OH 26.5 +0.6 OH* 18 37 32.50920 -05 23 59.1936           ~ 284 0
21 IRC +20370 C* 18 41 54.5507538243 +17 41 08.481183828       13.56   C7,3e 108 0
22 IRC -30398 AB* 18 59 13.8657889129 -29 50 20.243409063   14.35 14.19 15.46   M9 42 0
23 V* W Aql S* 19 15 23.3581458294 -07 02 50.308513461   12.72 10.14     S6/6e 206 0
24 V* RR Aql Mi* 19 57 36.0628075265 -01 53 11.322802573     7.80     M7.5e 275 2
25 V* V1943 Sgr AB* 20 06 55.2458545503 -27 13 29.754314126   9.25 8.04     M7/8III 67 0
26 IRC -10529 OH* 20 10 27.8733409252 -06 16 13.757843352         15.49 M: 130 0
27 V* RZ Sgr S* 20 15 28.4028079595 -44 24 37.482236482   11.21 10.40     S4,4ep 67 0
28 V* RV Aqr C* 21 05 51.7378981699 -00 12 42.121668132     11.5     C6,3e 95 0

    Equat.    Gal    SGal    Ecl

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2020.07.03-22:16:18

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