Sub-percent Photometry: Faint DA White Dwarf Spectophotometric Standards for Astrophysical Observatories. (arXiv:1811.12534v1 [astro-ph.IM])
<a href="http://arxiv.org/find/astro-ph/1/au:+Narayan_G/0/1/0/all/0/1">Gautham Narayan</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Matheson_T/0/1/0/all/0/1">Thomas Matheson</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Saha_A/0/1/0/all/0/1">Abhijit Saha</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Axelrod_T/0/1/0/all/0/1">Tim Axelrod</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Calamida_A/0/1/0/all/0/1">Annalisa Calamida</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Olszewski_E/0/1/0/all/0/1">Edward Olszewski</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Claver_J/0/1/0/all/0/1">Jenna Claver</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Mandel_K/0/1/0/all/0/1">Kaisey S. Mandel</a>, <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:+Holberg_J/0/1/0/all/0/1">Jay B. Holberg</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Deustua_S/0/1/0/all/0/1">Susana Deustua</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Rest_A/0/1/0/all/0/1">Armin Rest</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Stubbs_C/0/1/0/all/0/1">Christopher W. Stubbs</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Shanahan_C/0/1/0/all/0/1">Clare E. Shanahan</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Vaz_A/0/1/0/all/0/1">Amali L. Vaz</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Zenteno_A/0/1/0/all/0/1">Alfredo Zenteno</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Strampelli_G/0/1/0/all/0/1">Giovanni Strampelli</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Hubeny_I/0/1/0/all/0/1">Ivan Hubeny</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Points_S/0/1/0/all/0/1">Sean Points</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Sabbi_E/0/1/0/all/0/1">Elena Sabbi</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Mackenty_J/0/1/0/all/0/1">John Mackenty</a>

We have established a network of 19 faint (16.5 mag < $V$ < 19 mag) northern and equatorial DA white dwarfs as spectrophotometric standards for present and future wide-field observatories. Our analysis infers SED models for the stars that are consistent with panchromatic Hubble Space Telescope (HST) photometry to better than 1%. The excellent agreement between observations and models validates the use of non-local-thermodynamic-equilibrium (NLTE) DA white dwarf atmospheres extinguished by interstellar dust as accurate spectrophotometric references. Our standards are accessible from both hemispheres and suitable for ground and space-based observatories covering the ultraviolet to the near infrared. The high-precision of these faint sources make our network of standards ideally suited for any experiment that has very stringent requirements on flux calibration, such as studies of dark energy using the Large Synoptic Survey Telescope (LSST) and the Wide-Field Infrared Survey Telescope ($mathit{WFIRST}$).

We have established a network of 19 faint (16.5 mag < $V$ < 19 mag) northern
and equatorial DA white dwarfs as spectrophotometric standards for present and
future wide-field observatories. Our analysis infers SED models for the stars
that are consistent with panchromatic Hubble Space Telescope (HST) photometry
to better than 1%. The excellent agreement between observations and models
validates the use of non-local-thermodynamic-equilibrium (NLTE) DA white dwarf
atmospheres extinguished by interstellar dust as accurate spectrophotometric
references. Our standards are accessible from both hemispheres and suitable for
ground and space-based observatories covering the ultraviolet to the near
infrared. The high-precision of these faint sources make our network of
standards ideally suited for any experiment that has very stringent
requirements on flux calibration, such as studies of dark energy using the
Large Synoptic Survey Telescope (LSST) and the Wide-Field Infrared Survey
Telescope ($mathit{WFIRST}$).

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