Faint White Dwarf Flux Standards: Data and Models

Ralph C. Bohlin; Susana Deustua; Gautham Narayan; Abhijit Saha; Annalisa Calamida; Karl D. Gordon; Jay B. Holberg; Ivan Hubeny; Thomas Matheson; Armin Rest

doi:10.3847/1538-3881/ad93d8

Faint White Dwarf Flux Standards: Data and Models

Ralph C. Bohlin, Susana Deustua, Gautham Narayan, Abhijit Saha, Annalisa Calamida, Karl D. Gordon, Jay B. Holberg, Ivan Hubeny, Thomas Matheson, Armin Rest

Research output: Contribution to journal › Article › peer-review

Abstract

Fainter standard stars are essential for the calibration of larger telescopes. This work adds to the calibration spectra (CALSPEC) database of 19 faint white dwarfs (WDs) with all-sky coverage and V magnitudes between 16.5 and 18.7. Included for these stars is a new ultraviolet (UV) Hubble Space Telescope (HST) Space Telescope Imaging Spectrograph between 1150 and 3000 Å with a resolution of ∼500. Pure hydrogen WD models are fit to these UV spectra and to six-band HST/Wide Field Camera 3 photometry at 0.28-1.6 μm to construct predicted model spectral energy distributions covering wavelengths from 900 Å to the James Webb Space Telescope limit of 30 μm using well-established CALSPEC procedures for producing flux standards with the goal of 1% accuracy.

Original language	English (US)
Article number	40
Journal	Astronomical Journal
Volume	169
Issue number	1
Early online date	Dec 18 2024
DOIs	https://doi.org/10.3847/1538-3881/ad93d8
State	Published - Jan 3 2025

ASJC Scopus subject areas

Astronomy and Astrophysics
Space and Planetary Science

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abstract = "Fainter standard stars are essential for the calibration of larger telescopes. This work adds to the calibration spectra (CALSPEC) database of 19 faint white dwarfs (WDs) with all-sky coverage and V magnitudes between 16.5 and 18.7. Included for these stars is a new ultraviolet (UV) Hubble Space Telescope (HST) Space Telescope Imaging Spectrograph between 1150 and 3000 {\AA} with a resolution of ∼500. Pure hydrogen WD models are fit to these UV spectra and to six-band HST/Wide Field Camera 3 photometry at 0.28-1.6 μm to construct predicted model spectral energy distributions covering wavelengths from 900 {\AA} to the James Webb Space Telescope limit of 30 μm using well-established CALSPEC procedures for producing flux standards with the goal of 1% accuracy.",

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AU - Bohlin, Ralph C.

AU - Deustua, Susana

AU - Narayan, Gautham

AU - Saha, Abhijit

AU - Calamida, Annalisa

AU - Gordon, Karl D.

AU - Holberg, Jay B.

AU - Hubeny, Ivan

AU - Matheson, Thomas

AU - Rest, Armin

N1 - Support for this work was provided by NASA through the Space Telescope Science Institute, which is operated by AURA, Inc., under NASA contract NAS5-26555.

PY - 2025/1/3

Y1 - 2025/1/3

N2 - Fainter standard stars are essential for the calibration of larger telescopes. This work adds to the calibration spectra (CALSPEC) database of 19 faint white dwarfs (WDs) with all-sky coverage and V magnitudes between 16.5 and 18.7. Included for these stars is a new ultraviolet (UV) Hubble Space Telescope (HST) Space Telescope Imaging Spectrograph between 1150 and 3000 Å with a resolution of ∼500. Pure hydrogen WD models are fit to these UV spectra and to six-band HST/Wide Field Camera 3 photometry at 0.28-1.6 μm to construct predicted model spectral energy distributions covering wavelengths from 900 Å to the James Webb Space Telescope limit of 30 μm using well-established CALSPEC procedures for producing flux standards with the goal of 1% accuracy.

AB - Fainter standard stars are essential for the calibration of larger telescopes. This work adds to the calibration spectra (CALSPEC) database of 19 faint white dwarfs (WDs) with all-sky coverage and V magnitudes between 16.5 and 18.7. Included for these stars is a new ultraviolet (UV) Hubble Space Telescope (HST) Space Telescope Imaging Spectrograph between 1150 and 3000 Å with a resolution of ∼500. Pure hydrogen WD models are fit to these UV spectra and to six-band HST/Wide Field Camera 3 photometry at 0.28-1.6 μm to construct predicted model spectral energy distributions covering wavelengths from 900 Å to the James Webb Space Telescope limit of 30 μm using well-established CALSPEC procedures for producing flux standards with the goal of 1% accuracy.

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Faint White Dwarf Flux Standards: Data and Models

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