The Astronomical Journal (Jan 2023)

The Dark Energy Survey Supernova Program: Corrections on Photometry Due to Wavelength-dependent Atmospheric Effects

  • J. Lee,
  • M. Acevedo,
  • M. Sako,
  • M. Vincenzi,
  • D. Brout,
  • B. Sanchez,
  • R. Chen,
  • T. M. Davis,
  • M. Jarvis,
  • D. Scolnic,
  • H. Qu,
  • L. Galbany,
  • R. Kessler,
  • J. Lasker,
  • M. Sullivan,
  • P. Wiseman,
  • M. Aguena,
  • S. Allam,
  • O. Alves,
  • F. Andrade-Oliveira,
  • E. Bertin,
  • S. Bocquet,
  • D. Brooks,
  • D. L. Burke,
  • A. Carnero Rosell,
  • M. Carrasco Kind,
  • J. Carretero,
  • M. Costanzi,
  • L. N. da Costa,
  • M. E. S. Pereira,
  • J. De Vicente,
  • S. Desai,
  • H. T. Diehl,
  • P. Doel,
  • S. Everett,
  • I. Ferrero,
  • D. Friedel,
  • J. Frieman,
  • J. García-Bellido,
  • D. W. Gerdes,
  • D. Gruen,
  • R. A. Gruendl,
  • G. Gutierrez,
  • S. R. Hinton,
  • D. L. Hollowood,
  • K. Honscheid,
  • D. J. James,
  • S. Kent,
  • K. Kuehn,
  • N. Kuropatkin,
  • J. Mena-Fernández,
  • R. Miquel,
  • R. L. C. Ogando,
  • A. Palmese,
  • A. Pieres,
  • A. A. Plazas Malagón,
  • M. Raveri,
  • K. Reil,
  • M. Rodriguez-Monroy,
  • E. Sanchez,
  • V. Scarpine,
  • I. Sevilla-Noarbe,
  • M. Smith,
  • E. Suchyta,
  • G. Tarle,
  • C. To,
  • N. Weaverdyck,
  • DES Collaboration

DOI
https://doi.org/10.3847/1538-3881/acca15
Journal volume & issue
Vol. 165, no. 6
p. 222

Abstract

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Wavelength-dependent atmospheric effects impact photometric supernova flux measurements for ground-based observations. We present corrections on supernova flux measurements from the Dark Energy Survey Supernova Program’s 5YR sample (DES-SN5YR) for differential chromatic refraction (DCR) and wavelength-dependent seeing, and we show their impact on the cosmological parameters w and Ω _m . We use g − i colors of Type Ia supernovae to quantify astrometric offsets caused by DCR and simulate point-spread functions (PSFs) using the GalSIM package to predict the shapes of the PSFs with DCR and wavelength-dependent seeing. We calculate the magnitude corrections and apply them to the magnitudes computed by the DES-SN5YR photometric pipeline. We find that for the DES-SN5YR analysis, not accounting for the astrometric offsets and changes in the PSF shape cause an average bias of +0.2 mmag and −0.3 mmag, respectively, with standard deviations of 0.7 mmag and 2.7 mmag across all DES observing bands ( griz ) throughout all redshifts. When the DCR and seeing effects are not accounted for, we find that w and Ω _m are lower by less than 0.004 ± 0.02 and 0.001 ± 0.01, respectively, with 0.02 and 0.01 being the 1 σ statistical uncertainties. Although we find that these biases do not limit the constraints of the DES-SN5YR sample, future surveys with much higher statistics, lower systematics, and especially those that observe in the u band will require these corrections as wavelength-dependent atmospheric effects are larger at shorter wavelengths. We also discuss limitations of our method and how they can be better accounted for in future surveys.

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