Volume 474, Number 1, October IV 2007
|Page(s)||35 - 41|
|Published online||23 July 2007|
I. The Local Group galaxies WLM, IC 10 and NGC 6822
INAF, Osservatorio Astronomico di Roma, Viale del Parco Mellini 84, 00136 Roma, Italy e-mail: firstname.lastname@example.org
2 Département de Physique, Université de Montréal, C.P.6128, Succursale Centre-Ville, Montréal, Qc, H3C 3J7, Canada e-mail: email@example.com
3 INAF - Instituto di Radioastronomia, Largo E. Fermi 5, 50125 Firenze, Italy e-mail: firstname.lastname@example.org
Accepted: 18 July 2007
Context.The selection of AGB C and M stars from NIR colours has been done in recent years using adjustable criteria that are in needs of standardization if one wants to compare, in a coherent manner, properties of various populations.
Aims.We intend to assess the NIR colour technique to identify C and M stars.
Methods.We compare the NIR colours of several C stars previously identified from spectroscopy or narrow band techniques in WLM, IC 10 and NGC 6822.
Results.We demonstrate that very few M stars have but a non negligible number of C stars are bluer than this limit. Thus, counts of M and C stars based on such limit do not produce pure samples.
Conclusions.C/M ratios determined from NIR colours must be regarded as underestimates mainly because the M numbers include many warm C stars and also K stars if no blue limit is considered.
Key words: galaxies: individual: IC 10 / galaxies: individual: WLM / galaxies: individual: NGC 6822 / stars: carbon / stars: AGB and post-AGB / galaxies: dwarf
© ESO, 2007
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