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

Research output: Contribution to Journal/Magazine › Journal article › peer-review

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The Dark Energy Survey Supernova Program: Corrections on Photometry Due to Wavelength-dependent Atmospheric Effects. / Dark Energy Survey Collaboration.
In: The Astronomical Journal, Vol. 165, No. 6, 222, 01.06.2023.

Research output: Contribution to Journal/Magazine › Journal article › peer-review

Harvard

Dark Energy Survey Collaboration 2023, 'The Dark Energy Survey Supernova Program: Corrections on Photometry Due to Wavelength-dependent Atmospheric Effects', The Astronomical Journal, vol. 165, no. 6, 222. https://doi.org/10.3847/1538-3881/acca15

APA

Dark Energy Survey Collaboration (2023). The Dark Energy Survey Supernova Program: Corrections on Photometry Due to Wavelength-dependent Atmospheric Effects. The Astronomical Journal, 165(6), Article 222. https://doi.org/10.3847/1538-3881/acca15

Vancouver

Dark Energy Survey Collaboration. The Dark Energy Survey Supernova Program: Corrections on Photometry Due to Wavelength-dependent Atmospheric Effects. The Astronomical Journal. 2023 Jun 1;165(6):222. Epub 2023 May 3. doi: 10.3847/1538-3881/acca15

Author

Dark Energy Survey Collaboration. / The Dark Energy Survey Supernova Program : Corrections on Photometry Due to Wavelength-dependent Atmospheric Effects. In: The Astronomical Journal. 2023 ; Vol. 165, No. 6.

Bibtex

@article{35b9d9da25eb48b2858bdf5c164c26f3,
title = "The Dark Energy Survey Supernova Program: Corrections on Photometry Due to Wavelength-dependent Atmospheric Effects",
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 1σ 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....",
author = "{Dark Energy Survey Collaboration} and J. Lee and M. Acevedo and M. Sako and M. Vincenzi and D. Brout and B. Sanchez and R. Chen and Davis, {T. M.} and M. Jarvis and D. Scolnic and H. Qu and L. Galbany and R. Kessler and J. Lasker and M. Sullivan and P. Wiseman and M. Aguena and S. Allam and O. Alves and F. Andrade-Oliveira and E. Bertin and S. Bocquet and D. Brooks and Burke, {D. L.} and {Carnero Rosell}, A. and {Carrasco Kind}, M. and J. Carretero and M. Costanzi and {da Costa}, {L. N.} and Pereira, {M. E. S.} and {De Vicente}, J. and S. Desai and Diehl, {H. T.} and P. Doel and S. Everett and I. Ferrero and D. Friedel and J. Frieman and J. Garc{\'i}a-Bellido and Gerdes, {D. W.} and D. Gruen and Gruendl, {R. A.} and G. Gutierrez and Hinton, {S. R.} and Hollowood, {D. L.} and K. Honscheid and James, {D. J.} and S. Kent and K. Kuehn and M. Smith",
year = "2023",
month = jun,
day = "1",
doi = "10.3847/1538-3881/acca15",
language = "English",
volume = "165",
journal = "The Astronomical Journal",
issn = "0004-6256",
publisher = "IOP Publishing Ltd.",
number = "6",

}

RIS

TY - JOUR

T1 - The Dark Energy Survey Supernova Program

T2 - Corrections on Photometry Due to Wavelength-dependent Atmospheric Effects

AU - Dark Energy Survey Collaboration

AU - Lee, J.

AU - Acevedo, M.

AU - Sako, M.

AU - Vincenzi, M.

AU - Brout, D.

AU - Sanchez, B.

AU - Chen, R.

AU - Davis, T. M.

AU - Jarvis, M.

AU - Scolnic, D.

AU - Qu, H.

AU - Galbany, L.

AU - Kessler, R.

AU - Lasker, J.

AU - Sullivan, M.

AU - Wiseman, P.

AU - Aguena, M.

AU - Allam, S.

AU - Alves, O.

AU - Andrade-Oliveira, F.

AU - Bertin, E.

AU - Bocquet, S.

AU - Brooks, D.

AU - Burke, D. L.

AU - Carnero Rosell, A.

AU - Carrasco Kind, M.

AU - Carretero, J.

AU - Costanzi, M.

AU - da Costa, L. N.

AU - Pereira, M. E. S.

AU - De Vicente, J.

AU - Desai, S.

AU - Diehl, H. T.

AU - Doel, P.

AU - Everett, S.

AU - Ferrero, I.

AU - Friedel, D.

AU - Frieman, J.

AU - García-Bellido, J.

AU - Gerdes, D. W.

AU - Gruen, D.

AU - Gruendl, R. A.

AU - Gutierrez, G.

AU - Hinton, S. R.

AU - Hollowood, D. L.

AU - Honscheid, K.

AU - James, D. J.

AU - Kent, S.

AU - Kuehn, K.

AU - Smith, M.

PY - 2023/6/1

Y1 - 2023/6/1

N2 - 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 1σ 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....

AB - 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 1σ 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....

U2 - 10.3847/1538-3881/acca15

DO - 10.3847/1538-3881/acca15

M3 - Journal article

VL - 165

JO - The Astronomical Journal

JF - The Astronomical Journal

SN - 0004-6256

IS - 6

M1 - 222

ER -