EDP Sciences
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Volume 409, Number 2, October II 2003
Page(s) 541 - 551
Section Stellar clusters and associations
DOI http://dx.doi.org/10.1051/0004-6361:20031121

A&A 409, 541-551 (2003)
DOI: 10.1051/0004-6361:20031121

IC 2395 and BH 47: Only one open cluster in the Vela constellation

J. J. Clariá1, E. Lapasset1, A. E. Piatti2 and A. V. Ahumada1

1  Observatorio Astronómico, Universidad Nacional de Córdoba, Laprida 854, 5000 Córdoba, Argentina
    e-mail: lapasset@mail.oac.uncor.edu; andrea@mail.oac.uncor.edu
2  Instituto de Astronomía y Física del Espacio, CC 67, Suc. 28, 1428, Buenos Aires, Argentina
    e-mail: andres@iafe.uba.ar

(Received 2 May 2003 / Accepted 18 July 2003)

We report UBV photoelectric photometry for 273 stars in the fields of the open clusters IC 2395 and BH 47. Our postulate is that, rather than two different clusters in this region of Vela, there is only one, which we call $\rm IC\,2395 = BH\,47$. The cluster is centered at about $\alpha = 8^{\rm h}
42\fm 5$ , $\delta = -48\degr 06\farcm 8$ (2000), its angular diameter being ~ 19'. The analysis of the photometric data yields 61 probable cluster members and 16 possible members. Photometric membership probabilities show good agreement with those obtained from a proper motion study for 21 stars in common. The reddening across the cluster appears to be uniform, the mean E(B-V) value being  $0.09 \pm 0.02$. The true distance modulus is $(V-M_V)_0 = 9.52
\pm 0.10$ , corresponding to a distance from the Sun of ( $800 \pm 40$) pc and 48 pc below the Galactic plane. The cluster age, determined by fitting isochrones with core overshooting, turns out to be ( $6 \pm 2$) Myr. There is a strong likelihood that $\rm IC\,2395 = BH\,47$ is physically connected to the Vela OB1C association.

Key words: methods: observational -- techniques: photometric -- stars: fundamental parameters -- open clusters and associations: individual: IC 2395, BH 47

Offprint request: J. J. Clariá, claria@mail.oac.uncor.edu

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