Astron. Astrophys. 331, 737-741 (1998)

3. Results

The results of our observations are presented in Table 1. For the identification of the programme stars we follow the numbering system in Table II of Westerlund (1963). The polarization position angles (of the electric vector) are measured from the celestial north pole increasing towards east in the equatorial coordinate system, and from the Galactic north pole in the direction of increasing galactic longitude in the galactic coordinate system. For stars numbered 13 and 22 the observed polarization is smaller than the probable error of the measurement and therefore the polarization position angle can not be determined. The entries in Table 1 are as follows:

Table 1. Polarization measurements for stars in the region of the Puppis OB III association

For 8 of our programme stars (8,14,16,17,26,28,30 and 31) earlier polarization measurements (though in a different wave-band B, ) were made in a survey of southern early type stars by Klare & Neckel (1977). Our R band measurements generally agree with these fairly well in position angle; and are positively correlated for the degree of polarization. Because the wave-bands are different, an exact match is not expected.

© European Southern Observatory (ESO) 1998

Online publication: February 16, 1998
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