2015A&A...579A..76J


C.D.S. - SIMBAD4 rel 1.7 - 2019.12.10CET01:02:47

2015A&A...579A..76J - Astronomy and Astrophysics, volume 579A, 76-76 (2015/7-1)

Study of extremely reddened AGB stars in the Galactic bulge.

JIMENEZ-ESTEBAN F.M. and ENGELS D.

Abstract (from CDS):

Extremely reddened asymptotic giant branch stars (AGB) lose mass at high rates of >10–5M/yr. This is the very last stage of AGB evolution, in which stars in the mass range ∼2.0-4.0M (for solar metallicity) should have been converted to C stars already. The extremely reddened AGB stars in the Galactic bulge are however predominantly O-rich, implying that they might be either low-mass stars or stars at the upper end of the AGB mass range. Our goal is to determine the mass range of the most reddened AGB stars in the Galactic bulge. Using Virtual Observatory tools, we constructed spectral energy distributions of a sample of 37 evolved stars in the Galactic bulge with extremely red IRAS colours. We fitted DUSTY models to the observational data to infer the bolometric fluxes. Applying individual corrections for interstellar extinction and adopting a common distance, we determined luminosities and mass-loss rates, and inferred the progenitor mass range from comparisons with AGB evolutionary models. The observed spectral energy distributions are consistent with a classification as reddened AGB stars, except for two stars, which are proto-planetary nebula candidates. For the AGB stars, we found luminosities in the range ∼3000-30000L and mass-loss rates ∼10–5-3x10–4M/yr. The corresponding mass range is ∼1.1-6.0M assuming solar metallicity. Contrary to the predictions of the evolutionary models, the luminosity distribution is continuous, with many O-rich AGB stars in the mass range in which they should have been converted into C stars already. We suspect that bulge AGB stars have higher than solar metallicity and therefore may avoid the conversion to C-rich. The presence of low-mass stars in the sample shows that their termination of the AGB evolution also occurs during a final phase of very high mass-loss rate, leading to optically thick circumstellar shells.

Abstract Copyright:

Journal keyword(s): stars: AGB and post-AGB - circumstellar matter - stars: evolution - stars: variables: general - Galaxy: bulge - infrared: stars

VizieR on-line data: <Available at CDS (J/A+A/579/A76): table1.dat table2.dat>

Simbad objects: 46

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Number of rows : 46

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 M 33 GiG 01 33 50.904 +30 39 35.79 6.17 6.27 5.72     ~ 5034 1
2 NAME Magellanic Clouds GrG 03 00 -71.0           ~ 5402 1
3 NAME LMC G 05 23 34.6 -69 45 22     0.4     ~ 14380 1
4 IRAS 16582-3059 OH* 17 01 29.4 -31 04 19           ~ 4 0
5 IRAS 17030-3053 OH* 17 06 14.069 -30 57 38.32           ~ 7 0
6 IRAS 17107-3330 FIR 17 14 04.9 -33 33 59           ~ 3 0
7 IRAS 17128-3528 FIR 17 16 12.8 -35 32 12           ~ 2 0
8 IRAS 17151-3642 FIR 17 18 29.87 -36 46 08.8           ~ 4 0
9 IRAS 17171-2955 FIR 17 20 20.0 -29 58 23           ~ 3 0
10 IRAS 17207-3632 OH* 17 24 07.25496 -36 35 40.4448           ~ 8 0
11 IRAS 17251-2821 OH* 17 28 18.5 -28 23 58           ~ 8 0
12 IRAS 17276-2846 OH* 17 30 48.3374296803 -28 49 01.779662596           ~ 12 0
13 IRAS 17292-2727 OH* 17 32 23.7 -27 30 01           ~ 12 0
14 IRAS 17316-3523 OH* 17 34 57.49752 -35 25 52.5756           ~ 11 0
15 OH 354.88 -0.54 OH* 17 35 02.72 -33 33 29.4           ~ 65 1
16 IRAS 17323-2424 OH* 17 35 25.9 -24 26 25           ~ 13 2
17 IRAS 17341-3529 FIR 17 37 28.9083511464 -35 31 00.267494109           ~ 4 0
18 IRAS 17350-2413 AB* 17 38 08.7 -24 14 49           ~ 4 0
19 IRAS 17351-3429 OH* 17 38 26.1 -34 30 42           ~ 4 0
20 GLMP 602 V*? 17 39 15.2 -23 59 58           ~ 9 1
21 IRAS 17367-2722 OH* 17 39 52.42344 -27 23 31.8228           ~ 10 1
22 IRAS 17367-3633 OH* 17 40 07.62624 -36 34 41.4012           ~ 9 0
23 IRAS 17368-3515 OH* 17 40 13.1 -35 16 44           ~ 3 0
24 IRAS 17392-3020 OH* 17 42 30.53664 -30 22 07.3668           ~ 11 0
25 RAFGL 5379 OH* 17 44 24.0038735481 -31 55 35.428622508           ~ 82 0
26 OH 1.3 +1.0 OH* 17 44 58.73040 -27 14 42.8316           ~ 32 0
27 NAME Gal Center reg 17 45 40.04 -29 00 28.1           ~ 11082 0
28 IRAS 17428-2438 OH* 17 45 56.8 -24 40 00           ~ 6 0
29 [LFO93] 1749-25 AB* 17 52 39.4574953607 -25 34 37.888263108       17.0   ~ 15 0
30 IRAS 17495-2534 mul 17 52 39.6 -25 34 40           ~ 15 0
31 IRAS 17504-3312 OH* 17 53 47.0 -33 13 24           ~ 6 0
32 IRAS 17521-2938 OH* 17 55 21.8 -29 39 12           ~ 9 0
33 IRAS 17545-3056 OH* 17 57 48.4 -30 56 27           ~ 5 0
34 IRAS 17545-3317 mul 17 57 49.3 -33 17 49           ~ 4 0
35 IRAS 17583-3346 OH* 18 01 38.9 -33 46 01           ~ 5 0
36 IRAS 17584-3147 OH* 18 01 41.5 -31 47 30           ~ 9 0
37 NAME Baade Window reg 18 03.5 -30 01           ~ 516 3
38 IRAS 18019-3121 FIR 18 05 12.0 -31 21 43           ~ 5 0
39 IRAS 18040-2726 OH* 18 07 08.6 -27 25 56           ~ 8 0
40 IRAS 18040-2953 FIR 18 07 18.9 -29 53 20           ~ 4 0
41 IRAS 18091-2437 FIR 18 12 16.5 -24 36 46           ~ 6 0
42 OH 7.45 -2.62 OH* 18 12 19.3 -23 47 00           ~ 15 0
43 IRAS 18092-2508 OH* 18 12 21.866 -25 07 20.57           ~ 7 0
44 IRAS 18195-2804 OH* 18 22 40.1 -28 03 06           ~ 8 0
45 IRAS 18201-2549 FIR 18 23 12.2 -25 47 57           ~ 3 0
46 NAME Galactic Bulge reg ~ ~           ~ 3261 0

    Equat.    Gal    SGal    Ecl

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2019.12.10-01:02:47

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