Relative radial velocities from objective prism spectra in the region of nine southern open star clusters and a star field at Eta Carinae

Details Relative radial velocities from objective prism spectra in the region of nine southern open star clusters and a star field at Eta Carinae Relative radial velocities from objective prism spectra in the region of nine southern open star clusters and a star field at Eta Carinae

Aug 1980

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1980a%26as...41..245g&link_type=abstract

Astronomy and Astrophysics Supplement Series, vol. 41, Aug. 1980, p. 245-253. In German.

Astronomy and Astrophysics

Astrophysics

12

Astronomical Catalogs, Binary Stars, Open Clusters, Radial Velocity, Stellar Spectrophotometry, Data Reduction, Photographic Plates, Statistical Analysis, Stellar Magnitude

Scientific paper

For the investigation of spectroscopic binaries and the kinematics and dynamics of open clusters a catalogue is presented of relative radial velocities from Fehrenbach objective prism spectra of more than 500 stars in 2 by 2 square degrees fields in the region of 9 southern open clusters and one selected star field near η Carinae. The magnitude range of the stars is between photographic magnitudes 6 and 10.5, so that the brighter part of the clusters main sequences can be studied. The spectral types are selected to be between B1 and GO. The mean relative radial given in the catalogue are based on a total of about 8 000 single radial velocity measurements. A simplification of the reduction method described by Gieseking (1976) by a linear approximation of the dispersion curves between Hγ and Hδ has been applied. In Appendix lit is shown that the systematic errors introduced by this modification are completely negligible. In each of the star fields the zero point of the relative radial velocities in the mean radial velocity of a selected system of reference stars, whose members are marked by an "S" in column 2 of the catalogue. Details about this are given in Appendix 2. The entries of the catalogue are as follows:
Column 1: HD- or CPD-number of the stars.
Column 2: Identification on GPO-plates. In some cases stars with GPO-numbers are so faint (density of continuum between Hγ and Hδ < 0.4) that they mostly have not been measured. Members of the reference system are marked by an "S".
Columns 3 and 4: Plate coordinates of the stars in cm. X is parallel to declination and directed to the south, Y is parallel to right ascension and directed to the east.
Column 5: Density of the continuum of the spectra between Hγ and Hδ as measured on a representative plate.
Column 6 and 7: Blue-magnitudes of the stars. Column 6: published B-magnitudes (preferably photoelectric measurements). Column 7: GPO-magnitudes derived from characteristic curves constructed from the data in column 5 and 6 with a typical error of ± 0.1 mag.
Column 8: Spectral types from the GPO-spectra.
Column 9: Spectral types of the Michigan Spectral Catalogue Vol. 1, or from other sources.
Column 10: Mean radial velocities of the stars in km s-1 relative to the mean of the mean radial velocities of reference stars marked by an "S" in column 2. The data of stars, whose spectra are overexposed, overlapped or of bad quality by other reasons are marked by a ":".
Column 11: Standard deviation of the single measurements about their mean (column 10).
Column 12: Number of useful spectra. Very faint or very bright stars, whose spectra are sometimes underexposed or overexposed, have not been measured on all the plates. In case of a disturbance of one (or more) of the four measured spectral lines, the spectra have also been rejected for measurement.
Columns 13, 14 and 15 : Published radial velocities, number of measured spectra and the reference, respectively. In a first conclusion it is shown that the quality of the mean relative radial velocities given in the catalogue is equivalent with the quality of most published radial velocity data. In a series of forthcoming papers the detailed interpretation of this observation material will be given. In some star fields the data will be improved by further observations.

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