An augmented system of secondary standards for bright-star spectrophotometry

Details An augmented system of secondary standards for bright-star spectrophotometry An augmented system of secondary standards for bright-star spectrophotometry

Feb 1984

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1984apjs...54..259t&link_type=abstract

Astrophysical Journal Supplement Series (ISSN 0067-0049), vol. 54, Feb. 1984, p. 259-270.

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129

Reference Stars, Stellar Spectrophotometry, Accuracy, Calibrating, Spectral Line Width, Standards

Scientific paper

This paper contains calibrations on the Hayes-Latham (1975) spectrophotometric system for 21 bright secondary standard stars. Seven of these calibrations are intended for use only with archival data, or the low sensitivity S1 photocathode, or both; the other 14 are for general use in the 3300 to 10,800 A wavelength range. The sky coverage of the calibrated stars is generally adequate for southern hemisphere observers, and is somewhat better than adequate for northern hemisphere observers. At wavelengths shorter than 6058 A, the calibrations include and extend the work of Breger. At wavelengths greater than 6058 A, the most frequently used data are from closely accordant data series given by Cochran (1981) and by the author. A status review is given for 'problem stars' calibrated in this and other papers. Several of these stars are small-amplitude variables, and Zeta Oph and (probably) 109 Vir vary intermittently by amounts which can be substantial. Other problems of calibration or use are discussed. Evidence is reviewed which suggests that, as a whole, the calibrations given in this paper have high accuracy. This implies that several of the calibrated stars may be used as standards each night; the advantages of this technique are described. Future work on secondary standards, and decisions which should be made about them, are reviewed.

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