학술논문
The Dark Energy Survey Supernova Program: Corrections on Photometry Due to Wavelength-dependent Atmospheric Effects
Document Type
article
Author
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
Source
The Astronomical Journal, Vol 165, Iss 6, p 222 (2023)
Subject
Language
English
ISSN
1538-3881
Abstract
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.