EDP Sciences Journals List
Advanced Search
Subscriber Authentication Point
Home All issues Volume 402/2 Article
Free access article

Issue A&A
Volume 402, Number 2, May I 2003
Page(s) 549 - 564
Section Stellar clusters and associations
DOI http://dx.doi.org/10.1051/0004-6361:20030223



A&A 402, 549-564 (2003)
DOI: 10.1051/0004-6361:20030223

Photometric study of the young open cluster NGC 3293

G. Baume1, 2, R. A. Vázquez1, G. Carraro2 and A. Feinstein1

1  Facultad de Ciencias Astronómicas y Geofísicas de la UNLP, IALP-CONICET, Paseo del Bosque s/n, 1900 La Plata, Argentina
2  Dipartimento di Astronomia, Università di Padova, Vicolo Osservatorio 2, 35122 Padova, Italy

(Received 27 September 2002 / Accepted 17 January 2003 )

Abstract
Deep and extensive CCD photometric observations at $UBV(RI)_{\rm C}{\rm H}_{\alpha}$ were carried out in the area of the open cluster NGC 3293. The new data set allows to see the entire cluster sequence down to $M_{V} \approx +4.5$, revealing that stars with MV < -2 are evolving off the main sequence; stars with -2 < MV < +2 are located on the main sequence and stars with MV > +2 are placed above it. According to our analysis, the cluster distance is d = 2750   $\pm$ $250~{\rm pc}$ ( V0-MV = 12.2  $\pm$ 0.2) and its nuclear age is 8  $\pm$ 1 Myr. NGC 3293 contains an important fraction of pre-main sequence (PMS) stars distributed along a parallel band to the ZAMS with masses from 1 to $2.5~\cal M_{\odot}$ and a mean contraction age of 10 Myr. This last value does not differ too much from the nuclear age estimate. If we take into account the many factors that may affect the PMS star positions on the colour-magnitude diagram, both ages can be perfectly reconciled. The star formation rate, on the other hand, suggests that NGC 3293 stars formed surely in one single event, therefore favouring a coeval process of star formation. Using the ${\rm H}_{\alpha}$ data, we detected nineteen stars with signs of ${\rm H}_{\alpha}$ emission in the region of NGC 3293, another indication that the star formation process is still active in the region. The computed initial mass function for the cluster has a slope of $x = 1.2 \pm 0.2$ , a bit flatter than the typical slope for field stars and similar to the values found for other young open clusters.


Key words: Galaxy: open clusters and associations: individual: NGC 3293 -- stars: imaging -- stars: luminosity function, mass function

Offprint request: G. Baume, gbaume@fcaglp.fcaglp.unlp.edu.ar

SIMBAD Objects
Tables at the CDS



© ESO 2003


What is OpenURL?

The OpenURL standard is a protocol for transmission of metadata describing the resource that you wish to access. An OpenURL link contains article metadata and directs it to the OpenURL server of your choice. The OpenURL server can provide access to the resource and also offer complementary services (specific search engine, export of references...). The OpenURL link can be generated by different means.
  • If your librarian has set up your subscription with an OpenURL resolver, OpenURL links appear automatically on the abstract pages.
  • You can define your own OpenURL resolver with your EDPS Account. In this case your choice will be given priority over that of your library.
  • You can use an add-on for your browser (Firefox or I.E.) to display OpenURL links on a page (see http://www.openly.com/openurlref/). You should disable this module if you wish to use the OpenURL server that you or your library have defined.