2010A&A...513A..53L


C.D.S. - SIMBAD4 rel 1.7 - 2020.07.14CEST20:48:48

2010A&A...513A..53L - Astronomy and Astrophysics, volume 513, A53-53 (2010/4-1)

870 µm observations of evolved stars with LABOCA.

LADJAL D., JUSTTANONT K., GROENEWEGEN M.A.T., BLOMMAERT J.A.D.L., WAELKENS C. and BARLOW M.J.

Abstract (from CDS):

During their evolution, asymptotic giant branch (AGB) stars experience a high mass loss which leads to the formation of a circumstellar envelope (CSE) of dust and gas. The mass loss process is the most important phenomenon during this evolutionary stage. In order to understand it, it is important to study the physical parameters of the CSE. The emission of the CSE in the (sub)millimetre range is dominated by the dust continuum. This means that (sub)millimetre observations are a key tool in tracing the dust and improving our knowledge of the mass loss process. The aim of this study is to use new submillimetre observations of a sample of evolved stars to constrain the CSE physical parameters. We used aperture photometry to determine the fluxes at 870µm and to investigate the extended emission observed with the new APEX bolometer LABoCa. We computed the spectral energy distribution (SEDs) with the 1D radiative transfer code DUSTY, which we compared to literature data. Grain properties were calculated with both the spherical grains distribution and the continuous distribution of ellipsoids (CDE), and a comparison between the two is drawn. Synthetic surface brightness maps were derived from the modelling and were compared to the LABoCa brightness maps. A sample of nine evolved stars with different chemistry was observed with LABoCa. We detected extended emission around four stars. Physical parameters of the circumstellar envelope were derived from SED modelling, like the dust chemical composition, the dust condensation temperature and the total mass of the envelope. It proved to be difficult to fit the SED and the intensity profile simultaneously however. The use of the CDE leads to ``broad'' SEDs when compared to spherical grains, and this results in steep density distributions (∝r–2.2 typically).

Abstract Copyright:

Journal keyword(s): stars: AGB and post-AGB - stars: late-type - circumstellar matter - submillimeter: general - stars: mass-loss - dust - extinction

VizieR on-line data: <Available at CDS (J/A+A/513/A53): objects.dat images/*>

Simbad objects: 9

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Number of rows : 9

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 IRC +10011 OH* 01 06 25.9889735162 +12 35 52.890666456   20.7   18.26 14.01 M8 396 0
2 * omi Cet Mi* 02 19 20.79210 -02 58 39.4956   7.63 6.53 5.03   M5-9IIIe+DA 1438 0
3 V* VY CMa s*r 07 22 58.32877 -25 46 03.2355 12.01 10.19 7.95     M5Iae 996 0
4 IRC +10216 C* 09 47 57.40632 +13 16 43.5648     10.96     C9,5e 2134 0
5 IRAS 16342-3814 pA* 16 37 39.8700524769 -38 20 17.440442399           ~ 128 0
6 RAFGL 5379 OH* 17 44 24.0038735481 -31 55 35.428622508           ~ 83 0
7 IRC +10420 pA* 19 26 48.0981288433 +11 21 16.756524951   13.98 11.66     F8Ia+e 453 0
8 * pi.01 Gru S* 22 22 44.2112214756 -45 56 52.780402708 10.52 8.62 6.55 3.19 0.52 S5,7: 159 0
9 RAFGL 3068 C* 23 19 12.60744 +17 11 33.1332           C 249 0

    Equat.    Gal    SGal    Ecl

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2020.07.14-20:48:48

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