Volume 408, Number 1, September II 2003
|Page(s)||135 - 140|
|Section||Galactic structure, stellar clusters, and populations|
|Published online||17 November 2003|
Facultad de Ciencias Astronómicas y Geofísicas, Universidad Nacional de La Plata, Paseo del Bosque s/n, 1900 La Plata, Argentina
2 Instituto de Astrofísica de La Plata, (IALP, CONICET), Paseo del Bosque s/n, 1900 La Plata, Argentina
3 Instituto de Astronomía y Física del Espacio, C. C. 67 Suc. 28, 1428 Buenos Aires, Argentina
Corresponding author: H. G. Marraco, email@example.com
Accepted: 16 May 2003
We present UBVRI polarimetric observations of stars in the direction of the open cluster Pismis 20 and WR 67. It is found that the observed members segregate polarimetrically into two groups, with different associated mean (4.31 and 6.08% respectively). Although in the literature these stars are considered as members of the same cluster, the polarized light from these groups clearly differs. There are two possible explanations: very efficient polarizing dust particles exists between certain members of the cluster; or else Pismis 20 is composed of different groupings superimposed along the line of sight. WR 67 belongs to the group more affected by the dust.
Key words: ISM: dust, extinction / open clusters and associations: individual: Pis20 / stars: individual: WR67 / technique: polarimetric
© ESO, 2003
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