Volume 530, June 2011
|Number of page(s)||11|
|Section||Galactic structure, stellar clusters and populations|
|Published online||03 May 2011|
Star clusters or asterisms? 2MASS CMD and structural analyses of 15 challenging targets⋆
Universidade Federal do Rio Grande do SulDepartamento de Astronomia, CP 15051, RS, Porto Alegre 91501-970, Brazil
e-mail: firstname.lastname@example.org; email@example.com
Received: 7 January 2011
Accepted: 29 March 2011
Context. Poorly-populated star clusters may have photometric and structural properties not much different from asterisms, to the point that, in some cases, widely-used databases present conflicting classifications.
Aims. We investigate the nature of a sample of challenging targets that have been classified either as star clusters or asterisms in different studies. A few objects are studied for the first time.
Methods. The analysis employs 2MASS photometry, field-star decontamination, to enhance the intrinsic colour–magnitude diagram (CMD) morphology, and colour-magnitude filters, for high contrast stellar radial density profiles (RDPs).
Results. Based on properties derived from field-star decontaminated CMDs, and structural parameters from RDPs, we find that Pismis 12, IC 1434, Juchert 10, Ruprecht 30, NGC 3519, Herschel 1, Mayer 1, and Muzzio 1 are open clusters with ages within 5 Myr − 1.3 Gyr. Ruprecht 129, 130, 140, and 146 are borderline cases, being rather poorly-populated, with evolutionary sequences and RDPs suggesting star clusters. Dolidze 39, BH 79, and Ruprecht 103, have CMDs and RDPs typical of asterisms.
Conclusions. When a low stellar population is associated with a dense field contamination and/or important differential reddening, only a thin line separates star clusters and asterisms. These cases require specific analytical tools to establish their nature.
Key words: open clusters and associations: general / Galaxy: structure
Appendices are available in electronic form at http://www.aanda.org
© ESO, 2011
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