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III/43 Luminous Stars in the Southern Milky Way (Stephenson+ 1971)
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Beginning of ReadMe :III/43 Luminous Stars in the Southern Milky Way (Stephenson+ 1971)
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Catalogue of Luminous Stars in the Southern Milky Way
Stephenson C.B., Sanduleak N.
<Publ. Warner & Swasey Obs. 1 (1971)>
=1971PW&SO...1a...1S
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ADC_Keywords: Milky Way ; Stars, luminous ; Spectral types
Description (adapted from the Introduction of the Catalogue):
This Catalogue represents an extension to the entire Southern Milky
Way of the objective-prism survey for intrinsically luminous stars in
the Northern Milky Way III/76 that was carried out jointly by the
Hamburg and Warner and Swasey observatories.
The object has been to survey the Southern Milky Way with plates as
similar as possible to the plates used for the Northern Milky Way,
including similarity of limiting magnitude. To this end the objective
prism that was used with the Warner and Swasey Schmidt telescope for
the Northern survey was sent to Cerro Tololo, Chile, where it was used
by Sanduleak to photograph the Southern Milky Way with the Schmidt
telescope of the University of Michigan.
The survey was planned to have a minimum extent in galactic latitude
of +/-10deg. On each field three spectral plates were taken, all
intended to have spectral widening near 0.2 mm. One blue-region
(Kodak IIa-O) plate was given an exposure of 11 minutes, and another
was double-exposed for 3 minutes and 10 seconds. A red plate
(Kodak 103a-F plus Schott GG 14 filter) was also taken for the
detection of any appreciable Halpha emission, with three exposures
nominally 9 minutes, 1 minute and 10 seconds. The dispersion is 580
Angstroems/mm at Hgamma and about 1000 Angstroems/mm near Halpha;
a Michigan objective prism of 4deg angle, was used to obtain the
Halpha plates.
The spectral classification system is that discussed by Slettebak and
Stock (1957) and Nassau and Stephenson (1960). An important result of
the generally excellent quality of the new survey plates is that the
ce stars (OB stars apparently having the Balmer continuum in emission)
are easily recognised.
The magnitudes are based upon eye estimates of image density on the
blue-region spectral plates, calibrated by published magnitude
sequences, and are generally characterised by a probable error of
1/3 to 1/4 mag.
The equatorial coordinates for the stars have been derived from
measurements of the objective-prism plates, using the SAO I/131
catalogue for reference stars. The positions derived in this way are
accurate to 1" to 2" of arc, providing spectral lines are visible for
measurement. When spectral lines are not visible, the coordinate
parallel to the spectral dispersion -- always the declination --
becomes 10" or somewhat more uncertain.