A Correction for GALEX Spectroscopic UV Flux Distributions from Comparisons with CALSPEC and IUE. (arXiv:1901.06410v1 [astro-ph.IM])

A Correction for GALEX Spectroscopic UV Flux Distributions from Comparisons with CALSPEC and IUE. (arXiv:1901.06410v1 [astro-ph.IM])
<a href="http://arxiv.org/find/astro-ph/1/au:+Bohlin_R/0/1/0/all/0/1">Ralph C. Bohlin</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Bianchi_L/0/1/0/all/0/1">Luciana Bianchi</a>

The CALSPEC database of absolute spectral energy distributions (SEDs) from
the Hubble Space Telescope (HST) is based on pure hydrogen model atmosphere
calculations for three unreddened white dwarf (WD) stars and represents the
current UV flux calibration standard with a precision approaching 1% for well
observed stars. Following our previous work to correct IUE fluxes, this paper
provides an average correction for the GALEX spectral database that places
GALEX fluxes on the current CALSPEC scale. Our correction is derived by
comparing GALEX spectroscopic flux distributions with CALSPEC and corrected IUE
SEDs. This re-calibration is relevant for any project based on GALEX archival
spectroscopic data, including UV or multi-wavelength analyses, correlating
GALEX spectra with other existing or future databases, and planning of new
observations. The re-calibration will be applied to our planned catalog of
corrected GALEX SEDs.

The CALSPEC database of absolute spectral energy distributions (SEDs) from
the Hubble Space Telescope (HST) is based on pure hydrogen model atmosphere
calculations for three unreddened white dwarf (WD) stars and represents the
current UV flux calibration standard with a precision approaching 1% for well
observed stars. Following our previous work to correct IUE fluxes, this paper
provides an average correction for the GALEX spectral database that places
GALEX fluxes on the current CALSPEC scale. Our correction is derived by
comparing GALEX spectroscopic flux distributions with CALSPEC and corrected IUE
SEDs. This re-calibration is relevant for any project based on GALEX archival
spectroscopic data, including UV or multi-wavelength analyses, correlating
GALEX spectra with other existing or future databases, and planning of new
observations. The re-calibration will be applied to our planned catalog of
corrected GALEX SEDs.

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