2016A&A...596A..50G


C.D.S. - SIMBAD4 rel 1.7 - 2020.06.04CEST11:54:24

2016A&A...596A..50G - Astronomy and Astrophysics, volume 596A, 50-50 (2016/12-1)

The ALMA detection of CO rotational line emission in AGB stars in the Large Magellanic Cloud.

GROENEWEGEN M.A.T., VLEMMINGS W.H.T., MARIGO P., SLOAN G.C., DECIN L., FEAST M.W., GOLDMAN S.R., JUSTTANONT K., KERSCHBAUM F., MATSUURA M., McDONALD I., OLOFSSON H., SAHAI R., VAN LOON J.T., WOOD P.R., ZIJLSTRA A.A., BERNARD-SALAS J., BOYER M.L., GUZMAN-RAMIREZ L., JONES O.C., LAGADEC E., MEIXNER M., RAWLINGS M.G. and SRINIVASAN S.

Abstract (from CDS):

Context. Low- and intermediate-mass stars lose most of their stellar mass at the end of their lives on the asymptotic giant branch (AGB). Determining gas and dust mass-loss rates (MLRs) is important in quantifying the contribution of evolved stars to the enrichment of the interstellar medium.
Aims. This study attempts to spectrally resolve CO thermal line emission in a small sample of AGB stars in the Large Magellanic Cloud (LMC).
Methods. The Atacama Large Millimeter Array was used to observe two OH/IR stars and four carbon stars in the LMC in the CO J=2-1 line.
Results. We present the first measurement of expansion velocities in extragalactic carbon stars. All four C stars are detected and wind expansion velocities and stellar velocities are directly measured. Mass-loss rates are derived from modelling the spectral energy distribution and Spitzer/IRS spectrum with the DUSTY code. The derived gas-to-dust ratios allow the predicted velocities to agree with the observed gas-to-dust ratios. The expansion velocities and MLRs are compared to a Galactic sample of well-studied relatively low MLRs stars supplemented with extreme C stars with properties that are more similar to the LMC targets. Gas MLRs derived from a simple formula are significantly smaller than those derived from dust modelling, indicating an order of magnitude underestimate of the estimated CO abundance, time-variable mass loss, or that the CO intensities in LMC stars are lower than predicted by the formula derived for Galactic objects. This could be related to a stronger interstellar radiation field in the LMC.
Conclusions. Although the LMC sample is small and the comparison to Galactic stars is non-trivial because of uncertainties in their distances (hence luminosities), it appears that for C stars the wind expansion velocities in the LMC are lower than in the solar neighbourhood, while the MLRs appear to be similar. This is in agreement with dynamical dust-driven wind models.

Abstract Copyright: © ESO, 2016

Journal keyword(s): stars: AGB and post-AGB - stars: winds, outflows - radio continuum: stars

Status at CDS:  

Simbad objects: 29

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Number of rows : 29

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 BMB-B 75 AB* 00 52 12.933 -73 08 53.00   17.05 15.31   12.86 M6.0 22 0
2 NAME SMC G 00 52 38.0 -72 48 01   2.79 2.2     ~ 9392 1
3 RAFGL 190 C* 01 17 51.378 +67 13 53.34           C-rich 66 0
4 RAFGL 341 C* 02 33 00.34296 +58 02 06.2340           C-rich 50 0
5 NAME Magellanic Clouds GrG 03 00 -71.0           ~ 5621 1
6 LEE 259 C* 03 26 29.5050382299 +47 31 48.463099623           N 165 0
7 RAFGL 5102 C* 03 48 19.3122107756 +44 42 06.210576191           C-rich 31 0
8 IRAS 04545-7000 AB* 04 54 10.06 -69 55 58.3           ~ 24 0
9 WOH G 64 Mi* 04 55 10.5252313969 -68 20 29.998470169     18.46 15.69 12.795 M7.5 79 0
10 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
11 IRAS 05125-7035 C* 05 12 00.779 -70 32 24.03           C-rich 17 0
12 IRAS 05187-7033 C* 05 18 11.693 -70 30 26.97   20.975 20.876   20.111 C-rich 9 0
13 NAME Pictor A Sy1 05 19 49.7230919028 -45 46 43.855209977   15.73 15.77 14.85   ~ 553 1
14 NAME LMC G 05 23 34.6 -69 45 22     0.4     ~ 14760 1
15 OH 279.6 -32.6 OH* 05 27 40.78 -69 08 05.7           ~ 23 1
16 IRAS 05298-6957 pA* 05 29 24.61 -69 55 14.2           ~ 36 0
17 IRAS 05305-7251 C* 05 29 37.89 -72 49 52.9           C-rich 10 0
18 QSO B0537-441 BLL 05 38 50.36155219 -44 05 08.9389165   15.77 16.48 16   ~ 785 2
19 IRAS 05506-7053 C* 05 49 56.520 -70 53 11.75           C-rich 14 0
20 RAFGL 865 C* 06 04 00.04728 +07 25 52.0104           C-rich 95 0
21 HD 44179 pA* 06 19 58.2185496 -10 38 14.706068 9.51 9.33 9.02     B9Ib/II 714 0
22 QSO J0635-7516 QSO 06 35 46.5080299 -75 16 16.815501   15.96 15.75 15.82   ~ 507 1
23 QSO B0748+126 QSO 07 50 52.0457430 +12 31 04.828260   17.67 17.28 17.16   ~ 276 1
24 IRAS 08074-3615 C* 08 09 20.25576 -36 24 26.7588           C 35 0
25 QSO B1104-445 QSO 11 07 08.6939954176 -44 49 07.617187122   17.84 18.2 17.37   ~ 187 1
26 IRAS 12560+1656 C* 12 58 33.5125300023 +16 40 12.241266852     13.57     C 19 0
27 V* AC Her pA* 18 30 16.2374666779 +21 52 00.618442618 8.00 7.79 7.01     F4Ibp 315 0
28 RAFGL 2494 C* 20 01 09.0488458825 +40 55 39.036558501           C 63 0
29 RAFGL 3068 C* 23 19 12.60744 +17 11 33.1332           C 248 0

    Equat.    Gal    SGal    Ecl

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2020.06.04-11:54:24

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