Geneva photometric boxes. III - Distances and reddenings for 43 open clusters

Details Geneva photometric boxes. III - Distances and reddenings for 43 open clusters Geneva photometric boxes. III - Distances and reddenings for 43 open clusters

Dec 1981

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1981a%26a...104..185n&link_type=abstract

Astronomy and Astrophysics, vol. 104, no. 2, Dec. 1981, p. 185-197.

Astronomy and Astrophysics

Astrophysics

55

Astrometry, Astronomical Catalogs, Open Clusters, Red Shift, Stellar Spectrophotometry, Distance, Least Squares Method, Star Distribution, Stellar Atmospheres, Stellar Evolution, Stellar Parallax, Stellar Structure, Weighting Functions

Scientific paper

An independent and homogeneous method for obtaining distances and reddenings of open clusters is presented. It is based on the Geneva photometric boxes as defined by Golay et al. (1969), Nicolet (1981, Paper I) and using data from the Rufener (1981) catalogue.
The results obtained for 43 open clusters are given in Table 5. The only fundamental data used are from the General Catalogue of trigonometric parallaxes by Jenkins (1952) and its supplement (Jenkins, 1963). As a by-product a set of systematic deviations for the parallaxes measured at Various observatories is obtained. The well known systematic difference between the parallaxes from northern and southern hemisphere observatories disappears. The method used is rather similar to that of Turon-Lacarrieu and Crézé (1977).
The computation of the distances and reddenings of the clusters is made in two steps. A least squares method is used which also provides a standard deviation. The most accurate distance moduli (m-M)0 obtained are for Praesepe: 6.166±0.040, the Pleiades: 5.683±0.048 and NGC 752: 7.830±0.054. The agreement with the best references (e.g. Mermilliod, 1981) is excellent except for the youngest clusters.
Individual parallaxes are derived for some members of the Hyades applying the box-technique based on the distance moduli of other clusters. The depth effect is investigated and the distribution of the members of the Hyades along the line of sight is found to be comparable with the tangential distribution.

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