2001A&A...368..239V

Query : 2001A&A...368..239V

2001A&A...368..239V - Astronomy and Astrophysics, volume 368, 239-249 (2001/3-2)

The peculiar cluster HS 327 in the Large Magellanic Cloud: can OH/IR stars and carbon stars be twins?

VAN LOON J.T., ZIJLSTRA A.A., KAPER L., GILMORE G.F., LOUP C. and BLOMMAERT J.A.D.L.

Abstract (from CDS):

The obscured OH/IR star IRAS 05298-6957 in the LMC was recently noticed to be member of the small double cluster HS 327 that also contains a carbon star (van Loon, et al., 1998A&A...329..169V). Hence they are coeval and have (nearly) the same progenitor mass, which can only be understood if Hot Bottom Burning (HBB) has prevented IRAS 05298-6957 from being a carbon star. We present extensive visual and near-IR photometric data for >104 stars in and around HS 327, and spectroscopic data for some of the brightest AGB stars amongst these. Colour-magnitude diagrams are used to estimate the age for the cluster and its members, and luminosities are derived for the stars for which spectra have been obtained. The age for IRAS 05298-6957 and the carbon star is estimated to be ∼200Myr. This corresponds to a Main-Sequence progenitor mass ∼4.0M☉ - the first direct measurement of the lower mass threshold for HBB. This agrees with stellar evolution models that, however, fail to reproduce the low luminosity of the carbon star.

Abstract Copyright: ∼

Journal keyword(s): stars: carbon - stars: evolution - stars: AGB and post-AGB - open clusters and associations: general - Magellanic Clouds - infrared: stars

Nomenclature: Text: [VZK2001] HS 327W (Nos E, W). Tables 1, 2: [VZK2001] A (Nos A-C), [VZK2001] Carbon N=1, [VZK2001] Red N=1.

CDS comments: Standard star S 121-E = GSPC S121-E

Simbad objects: 19

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Number of rows : 19
N Identifier Otype ICRS (J2000)
RA 		ICRS (J2000)
DEC 		Mag U Mag B Mag V Mag R Mag I Sp type #ref
1850 - 2024 		#notes
1 CD-28 595 PM* 01 54 50.2703221766 -27 28 35.739139915   12.06 11.51     ~ 130 0
2 HD 19445 PM* 03 08 25.5883873084 +26 19 51.400965175 8.29 8.52 8.06 7.60 7.27 G2VFe-3 771 0
3 Ross 374 PM* 03 26 59.7729638950 +23 46 35.925963580   11.36   10.6   F5 76 0
4 HD 284248 Pe* 04 14 35.5161858536 +22 21 04.252516252 9.49 9.68 9.23 8.77 8.43 sdG0 186 0
5 NAME LMC G 05 23 34.6 -69 45 22     0.4     ~ 17428 0
6 2MASS J05291132-6956150 Mi* 05 29 11.3280743568 -69 56 14.977407696     18.197 15.910 15.536 ~ 11 0
7 OGLE-CL LMC 517 Cl* 05 29 18.80 -69 54 52.5           ~ 13 0
8 2MASS J05292426-6955418 LP* 05 29 24.2689804066 -69 55 41.755858426     16.581   13.910 ~ 3 0
9 KMK88 59 Cl* 05 29 24.59 -69 55 11.8           ~ 8 0
10 IRAS 05298-6957 pA* 05 29 24.634 -69 55 13.61           ~ 41 0
11 OGLE LMC-LPV-61819 s*r 05 29 25.0015991616 -69 56 26.067831756     16.336 13.124 12.984 M5Iab-Ib 6 0
12 2MASS J05292546-6954523 LP* 05 29 25.4696077644 -69 54 52.247014649     16.280 13.954 13.86 C4.5 7 0
13 2MASS J05293634-6956060 LP* 05 29 36.3509111072 -69 56 06.010284885     17.350 14.317 14.147 ~ 5 0
14 SHV 0530080-695949 Mi* 05 29 40.3656992736 -69 57 37.387645812     19.019 15.484 15.856 C 13 0
15 GSPC S121-E * 06 29 29.1119772816 -59 39 30.728491596   13.666 13.135 13.277   ~ 12 0
16 Ross 683 PM* 08 50 27.4107904622 +07 37 17.309958783   12.06   11.1   G6 70 1
17 Ross 889 Pe* 09 40 43.2053340378 +01 00 29.511836741       10.39   sdA4 160 0
18 CD-44 12736 PM* 18 36 25.9502475648 -44 18 36.907592904   10.83 10.22     G0 211 0
19 BD-00 4470 Pe* 23 09 32.9443500338 +00 42 39.749975827   10.66   9.6   sdG2 95 2

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