Query : 2004A&A...427..945S

2004A&A...427..945S - Astronomy and Astrophysics, volume 427, 945-958 (2004/12-1)

Late-type giant variables in NGC 6522, LMC and SMC How do they differ?


Abstract (from CDS):

Complete samples of 2MASS stars in three fields of differing metallicities (and possibly differing age distributions) have been extracted and cross-correlated with MACHO and ISO data to determine their variability and mass-loss properties. In each MK histogram a fall-off in numbers is seen above the tip of the RGB. The luminosity of the tip increases with metallicity as does the average (J-K)0 at a given MK0. These quantities have been compared with the data for galactic globular clusters obtained by Ferraro et al. (2000AJ....119.1282F). In the J-H, H-K colour-colour diagrams, the increasing proportion of stars with high H-K values is conspicuous at lower metallicities. This is well-known to result from the increasing proportion of carbon stars. All three fields contain similar types of variables, mainly short-period (usually tens of days), Mira like (long-period, large amplitude) and double-period (having both long and short periods). The proportion of stars that vary decreases at lower metallicities and the minimum period associated with a given amplitude gets longer. Various trends are seen in the K, logP diagrams of each field. The Magellanic Cloud fields largely resemble each other but the Bulge field is noticeably different. The stars that follow the ``A'' K, log P relation in the Bulge hardly extend beyond MK,0Tip and the other groups also appear truncated in MK relative to their Magellanic Cloud counterparts. In the Clouds there are many stars with periods around 200-300 d that follow the ``C'' or Mira relation but have relatively small amplitudes. The mid-IR sample detected by ISOCAM during the Magellanic Cloud Mini-Survey (MCMS) appears to be reliable and complete for sources with MK more luminous than -7mag, i.e., for those close to the top of the AGB. The various colour-colour and colour-magnitude diagrams reflect the increasing dominance of carbon stars at low metallicity. Mira magnitude vs. log P relations exist at least up to 7µm. Mass-loss from longer-period and double-period SRVs occurs at similar rates in each field, in spite of the metallicity differences.

Abstract Copyright:

Journal keyword(s): stars: AGB and post-AGB - galaxies: Magellanic Clouds - Galaxy: bulge

Simbad objects: 5

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Number of rows : 5
N Identifier Otype ICRS (J2000)
ICRS (J2000)
Mag U Mag B Mag V Mag R Mag I Sp type #ref
1850 - 2023
1 NAME SMC G 00 52 38.0 -72 48 01   2.79 2.2     ~ 10692 1
2 OGLE J010046.28-725728.2 EB* 01 00 46.3047516744 -72 57 28.630823976     15.45 15.08 14.82 ~ 6 0
3 NAME LMC G 05 23 34.6 -69 45 22     0.4     ~ 16766 1
4 TLE NGC 6522 9 Mi* 18 02 34.7847285048 -29 59 58.886317140     19.056   12.455 ~ 13 0
5 NGC 6522 GlC 18 03 34.08 -30 02 02.3           ~ 507 0

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