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III/116 SPECTROPHOTOMETRIC STANDARDS (Massey+ 1988)
The following files can be converted to FITS (extension .fit .fit.Z .fgz)
table1 sp*.dat
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Query from: http://vizier.cds.unistra.fr/viz-bin/VizieR?-source=III/116
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drwxr-xr-x 3 cats archive 4096 Jan 12 2023 [TAR file]
-rw-r--r-- 1 cats archive 456 Dec 19 2022 .message
-r--r--r-- 1 cats archive 9459 Mar 28 2005 ReadMe
-rw-r--r-- 1 cats archive 303 Apr 16 2016 +footg5.gif
-rw-r--r-- 1 cats archive 3045 Apr 16 2016 +footg8.gif
drwxr-xr-x 2 cats archive 4096 Apr 16 2016 icons
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-r--r--r-- 1 cats archive 121466 Jun 19 1991 spectra.gz [Uncompressed]
-r--r--r-- 1 cats archive 1911 Sep 11 1995 table1.dat [txt] [txt.gz] [fits] [fits.gz] [html]
Beginning of ReadMe :III/116 Spectrophotometric Standards (Massey+ 1988)
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Spectrophotometric Standards
Massey P., Strobel K., Barnes J.V., Anderson E.
<Astrophys. J. 328, 315 (1988)>
=1988ApJ...328..315M
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ADC_Keywords: Spectrophotometry ; Stars, standard
Abstract:
Observers at the National Optical Astronomy Observatories have
provided spectrophotometry for 25 stars in the visual magnitude range
7.5 to 16.6. This document describes the machine-readable version of
their results as received from P. Massey. The magnitudes are on the
Hayes-Latham system and cover the wavelength range from 3200 to 8100
angstroms at approximately two angstrom intervals.
Description:
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.