Skip to content Skip to navigation
University of Warwick
  • Study
  • |
  • Research
  • |
  • Business
  • |
  • Alumni
  • |
  • News
  • |
  • About

University of Warwick
Publications service & WRAP

Highlight your research

  • WRAP
    • Home
    • Search WRAP
    • Browse by Warwick Author
    • Browse WRAP by Year
    • Browse WRAP by Subject
    • Browse WRAP by Department
    • Browse WRAP by Funder
    • Browse Theses by Department
  • Publications Service
    • Home
    • Search Publications Service
    • Browse by Warwick Author
    • Browse Publications service by Year
    • Browse Publications service by Subject
    • Browse Publications service by Department
    • Browse Publications service by Funder
  • Help & Advice
University of Warwick

The Library

  • Login
  • Admin

Cool white dwarfs as standards for infrared observations

Tools
- Tools
+ Tools

Fusillo, Gentile, Pietro, Nicola, Tremblay, Pier-Emmanuel, Bohlin, Ralph C., Deustua, Susana E. and Kalirai, Jason S. (2020) Cool white dwarfs as standards for infrared observations. Monthly Notices of the Royal Astronomical Society, 491 (3). pp. 3613-3623. doi:10.1093/mnras/stz2984

[img]
Preview
PDF
WRAP-cool-white-dwarfs-standards-infrared-Tremblay-2019.pdf - Accepted Version - Requires a PDF viewer.

Download (3240Kb) | Preview
Official URL: https://doi.org/10.1093/mnras/stz2984

Request Changes to record.

Abstract

In the era of modern digital sky surveys, uncertainties in the flux of stellar standards are commonly the dominant systematic error in photometric calibration and can often affect the results of higher level experiments. The Hubble Space Telescope (HST) spectrophotometry, which is based on computed model atmospheres for three hot (Teff>30000 K) pure hydrogen (DA) white dwarfs, is currently considered the most reliable and internally consistent flux calibration. However, many next-generation facilities (e.g. Harmoni on E-ELT, Euclid, and JWST) will focus on IR observations, a regime in which white dwarf calibration has not yet been robustly tested. Cool DA white dwarfs have energy distributions that peak close to the optical or near-infrared, do not have shortcomings from UV metal line blanketing, and have a reasonably large sky density (≃4 deg−2 at G < 20), making them, potentially, excellent calibrators. Here, we present a pilot study based on STIS + WFC3 observations of two bright DA white dwarfs to test whether targets cooler than current hot primary standards (Teff<20000 K) are consistent with the HST flux scale. We also test the robustness of white dwarf models in the IR regime from an X-shooter analysis of Paschen lines and by cross-matching our previously derived Gaia white dwarf catalogue with observations obtained with 2MASS, UKIDSS, VHS, and WISE.

Item Type: Journal Article
Divisions: Faculty of Science > Physics
Journal or Publication Title: Monthly Notices of the Royal Astronomical Society
Publisher: Oxford University Press
ISSN: 0035-8711
Official Date: January 2020
Dates:
DateEvent
January 2020Published
28 November 2019Available
14 October 2019Accepted
Volume: 491
Number: 3
Page Range: pp. 3613-3623
DOI: 10.1093/mnras/stz2984
Status: Peer Reviewed
Publication Status: Published
Publisher Statement: This is a pre-copyedited, author-produced version of an article accepted for publication in Monthly Notices of the Royal Astronomical Society following peer review. The version of record Nicola Pietro Gentile Fusillo, Pier-Emmanuel Tremblay, Ralph C Bohlin, Susana E Deustua, Jason S Kalirai, Cool white dwarfs as standards for infrared observations, Monthly Notices of the Royal Astronomical Society, Volume 491, Issue 3, January 2020, Pages 3613–3623, is available online at: https://doi.org/10.1093/mnras/stz2984
Access rights to Published version: Restricted or Subscription Access
Open Access Version:
  • ArXiv

Request changes or add full text files to a record

Repository staff actions (login required)

View Item View Item

Downloads

Downloads per month over past year

View more statistics

twitter

Email us: wrap@warwick.ac.uk
Contact Details
About Us