Spectrophotometric Standards (Massey+ 1988)

Details Spectrophotometric Standards (Massey+ 1988) Spectrophotometric Standards (Massey+ 1988)

Sep 1995

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1995ycat.3116....0m&link_type=abstract

VizieR On-line Data Catalog: III/116. Originally published in: 1988ApJ...328..315M

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Spectrophotometry, Stars: Standard

Scientific paper

The stellar magnitude system is based on the brightness of Vega at each wavelength. Vega, itself, has been compared accurately with laboratory standards. Unfortunately, Vega is much too bright to be observed under the same conditions with most stars of interest. Hence, various investigators have compared carefully with Vega and a few other primary standards somewhat fainter stars to be used as secondary standards. In addition, several much fainter stars have been used as tertiary standards with lower accuracy.
With the common use of linear detectors and large telescopes, it has become important to provide spectrophotometric standards for a range of magnitudes including quite faint stars. The planning for the Hubble Space Telescope increased the necessity for fainter standards. Moreover, both the IUE and the HST require that the standards be established at the shortest wavelength reliably accessible from the ground so that ultraviolet spectrophotometry can be tied to visual spectrophotometry accurately.
Investigators at Kitt Peak National Observatory have pursued a lengthy program to provide both more accurate spectrophotometry of faint stars and a dense distribution of the wavelengths at which the fluxes are measured. The close spacing of points is essential to place the fairly short stretches of a high resolution spectrum available with a solid state detector on a standard system.
The present compilation provides improved data for nine stars previously observed by Stone (1977) or Oke (1974) and spectro- photometry of 16 new standards, eight of which are fainter than 14.0 mag. To provide red standards and still avoid stars with numerous spectral lines, a highly reddened O5 star and two substantially reddened (but bright) O5 stars are included. The observations were all referenced to either BD+28 4211 or Feige 34. For four stars in common, comparison with the data from Stone indicates that the calibration of the standard stars is good to about 0.03 mag. The internal accuracy of the data for the individual stars is substantially higher. The measurements are on the Hayes-Latham system.
Table 1 describes the stars. It is identical to Table 1 in the source reference except that V has been omitted. The number of observations per star ranges from 3 to 29, but not all observations were made under photometric conditions. Only one observation of Feige 110 was made under photometric conditions. For PG 0205+134, PG 0310+149, PG 0939+262, PG 1121+145, and PG 1545+035, only two measurements were made under photometric conditions. The magnitudes for HZ44 show a large scatter within the 29 measurements. Fig. 1, also from the source reference, provides finding fields for all stars except for the two brightest.
(26 data files).

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