TOWARD A NETWORK OF FAINT DA WHITE DWARFS AS HIGH-PRECISION SPECTROPHOTOMETRIC STANDARDS
dc.contributor.author | Narayan, Gautham | |
dc.contributor.author | Axelrod, T. | |
dc.contributor.author | Holberg, J. B. | |
dc.contributor.author | Matheson, Thomas | |
dc.contributor.author | Saha, A. | |
dc.contributor.author | Olszewski, E. | |
dc.contributor.author | Claver, J. | |
dc.contributor.author | Stubbs, C. W. | |
dc.contributor.author | Bohlin, R. C. | |
dc.contributor.author | Deustua, S. | |
dc.contributor.author | Rest, A. | |
dc.date.accessioned | 2016-11-03T02:07:27Z | |
dc.date.available | 2016-11-03T02:07:27Z | |
dc.date.issued | 2016-05-05 | |
dc.identifier.citation | TOWARD A NETWORK OF FAINT DA WHITE DWARFS AS HIGH-PRECISION SPECTROPHOTOMETRIC STANDARDS 2016, 822 (2):67 The Astrophysical Journal | en |
dc.identifier.issn | 1538-4357 | |
dc.identifier.doi | 10.3847/0004-637X/822/2/67 | |
dc.identifier.uri | http://hdl.handle.net/10150/621236 | |
dc.description.abstract | We present the initial results from a program aimed at establishing a network of hot DA white dwarfs to serve as spectrophotometric standards for present and future wide-field surveys. These stars span the equatorial zone and are faint enough to be conveniently observed throughout the year with large-aperture telescopes. The spectra of these white dwarfs are analyzed in order to generate a non-local-thermodynamic-equilibrium model atmosphere normalized to Hubble Space Telescope colors, including adjustments for wavelength-dependent interstellar extinction. Once established, this standard star network will serve ground-based observatories in both hemispheres as well as space-based instrumentation from the UV to the near IR. We demonstrate the effectiveness of this concept and show how two different approaches to the problem using somewhat different assumptions produce equivalent results. We discuss the lessons learned and the resulting corrective actions applied to our program. | |
dc.description.sponsorship | NASA [NAS5-26555]; NASA Office of Space Science [NNX13AC07G]; Ministerio de Ciencia, Tecnologia e Innovacion Productiva (Argentina) [GS-2013A-Q-8, GS-2013B-Q-22] | en |
dc.language.iso | en | en |
dc.publisher | IOP PUBLISHING LTD | en |
dc.relation.url | http://stacks.iop.org/0004-637X/822/i=2/a=67?key=crossref.e75b1976b05877b5cdc758f9e0532142 | en |
dc.rights | © 2016. The American Astronomical Society. All rights reserved. | en |
dc.rights.uri | http://rightsstatements.org/vocab/InC/1.0/ | |
dc.subject | cosmology: observations | en |
dc.subject | methods: data analysis | en |
dc.subject | surveys | en |
dc.subject | white dwarfs | en |
dc.title | TOWARD A NETWORK OF FAINT DA WHITE DWARFS AS HIGH-PRECISION SPECTROPHOTOMETRIC STANDARDS | en |
dc.type | Article | en |
dc.contributor.department | Univ Arizona, Steward Observ | en |
dc.contributor.department | Univ Arizona, Lunar & Planetary Lab | en |
dc.identifier.journal | The Astrophysical Journal | en |
dc.description.collectioninformation | This item from the UA Faculty Publications collection is made available by the University of Arizona with support from the University of Arizona Libraries. If you have questions, please contact us at repository@u.library.arizona.edu. | en |
dc.eprint.version | Final published version | en |
refterms.dateFOA | 2018-08-20T11:13:12Z | |
html.description.abstract | We present the initial results from a program aimed at establishing a network of hot DA white dwarfs to serve as spectrophotometric standards for present and future wide-field surveys. These stars span the equatorial zone and are faint enough to be conveniently observed throughout the year with large-aperture telescopes. The spectra of these white dwarfs are analyzed in order to generate a non-local-thermodynamic-equilibrium model atmosphere normalized to Hubble Space Telescope colors, including adjustments for wavelength-dependent interstellar extinction. Once established, this standard star network will serve ground-based observatories in both hemispheres as well as space-based instrumentation from the UV to the near IR. We demonstrate the effectiveness of this concept and show how two different approaches to the problem using somewhat different assumptions produce equivalent results. We discuss the lessons learned and the resulting corrective actions applied to our program. |