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Assessment of systematic chromatic errors that impact sub-1% photometric precision in large-area sky surveys

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Assessment of systematic chromatic errors that impact sub-1% photometric precision in large-area sky surveys. / Dark Energy Survey Collaboration.

In: The Astronomical Journal, Vol. 151, No. 6, 27.05.2016.

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Dark Energy Survey Collaboration. / Assessment of systematic chromatic errors that impact sub-1% photometric precision in large-area sky surveys. In: The Astronomical Journal. 2016 ; Vol. 151, No. 6.

Bibtex

@article{8bcc0a9f675642118d6a74e8a6e1e5a2,
title = "Assessment of systematic chromatic errors that impact sub-1{\%} photometric precision in large-area sky surveys",
abstract = "Meeting the science goals for many current and future ground-based optical large-area sky surveys requires that the calibrated broadband photometry is stable in time and uniform over the sky to 1{\%} precision or better. Past surveys have achieved photometric precision of 1-2{\%} by calibrating the survey's stellar photometry with repeated measurements of a large number of stars observed in multiple epochs. The calibration techniques employed by these surveys only consider the relative frame-by-frame photometric zeropoint offset and the focal plane position-dependent illumination corrections, which are independent of the source color. However, variations in the wavelength dependence of the atmospheric transmission and the instrumental throughput induce source color-dependent systematic errors. These systematic errors must also be considered to achieve the most precise photometric measurements. In this paper, we examine such systematic chromatic errors using photometry from the Dark Energy Survey (DES) as an example. We define a natural magnitude system for DES and calculate the systematic errors on stellar magnitudes, when the atmospheric transmission and instrumental throughput deviate from the natural system. We conclude that the systematic chromatic errors caused by the change of airmass in each exposure, the change of the precipitable water vapor and aerosol in the atmosphere over time, and the non-uniformity of instrumental throughput over the focal plane, can be up to 2{\%} in some bandpasses. We compare the calculated systematic chromatic errors with the observed DES data. For the test sample data, we correct these errors using measurements of the atmospheric transmission and instrumental throughput. The residual after correction is less than 0.3{\%}. We also find that the errors for non-stellar objects are redshift-dependent and can be larger than those for stars at certain redshifts.",
keywords = "astro-ph.IM, atmospheric effects, methods: observational, surveys, techniques: photometric, RCUK, STFC",
author = "Li, {T. S.} and DePoy, {D. L.} and Marshall, {J. L.} and D. Tucker and R. Kessler and J. Annis and Bernstein, {G. M.} and S. Boada and Burke, {D. L.} and Finley, {D. A.} and James, {D. J.} and S. Kent and H. Lin and J. Marriner and N. Mondrik and D. Nagasawa and Rykoff, {E. S.} and D. Scolnic and Walker, {A. R.} and W. Wester and Abbott, {T. M. C.} and S. Allam and A. Benoit-L{\'e}vy and E. Bertin and D. Brooks and D. Capozzi and Rosell, {A. Carnero} and Kind, {M. Carrasco} and J. Carretero and M. Crocce and Cunha, {C. E.} and D'Andrea, {C. B.} and Costa, {L. N. da} and S. Desai and Diehl, {H. T.} and P. Doel and B. Flaugher and P. Fosalba and J. Frieman and E. Gaztanaga and Goldstein, {D. A.} and D. Gruen and Gruendl, {R. A.} and G. Gutierrez and K. Honscheid and K. Kuehn and N. Kuropatkin and Maia, {M. A. G.} and Nichol, {R. C.} and D. Thomas and {Dark Energy Survey Collaboration}",
note = "16 pages, 9 figures, AJ accepted",
year = "2016",
month = "5",
day = "27",
doi = "10.3847/0004-6256/151/6/157",
language = "English",
volume = "151",
journal = "The Astronomical Journal",
issn = "0004-6256",
publisher = "IOP Publishing",
number = "6",

}

RIS

TY - JOUR

T1 - Assessment of systematic chromatic errors that impact sub-1% photometric precision in large-area sky surveys

AU - Li, T. S.

AU - DePoy, D. L.

AU - Marshall, J. L.

AU - Tucker, D.

AU - Kessler, R.

AU - Annis, J.

AU - Bernstein, G. M.

AU - Boada, S.

AU - Burke, D. L.

AU - Finley, D. A.

AU - James, D. J.

AU - Kent, S.

AU - Lin, H.

AU - Marriner, J.

AU - Mondrik, N.

AU - Nagasawa, D.

AU - Rykoff, E. S.

AU - Scolnic, D.

AU - Walker, A. R.

AU - Wester, W.

AU - Abbott, T. M. C.

AU - Allam, S.

AU - Benoit-Lévy, A.

AU - Bertin, E.

AU - Brooks, D.

AU - Capozzi, D.

AU - Rosell, A. Carnero

AU - Kind, M. Carrasco

AU - Carretero, J.

AU - Crocce, M.

AU - Cunha, C. E.

AU - D'Andrea, C. B.

AU - Costa, L. N. da

AU - Desai, S.

AU - Diehl, H. T.

AU - Doel, P.

AU - Flaugher, B.

AU - Fosalba, P.

AU - Frieman, J.

AU - Gaztanaga, E.

AU - Goldstein, D. A.

AU - Gruen, D.

AU - Gruendl, R. A.

AU - Gutierrez, G.

AU - Honscheid, K.

AU - Kuehn, K.

AU - Kuropatkin, N.

AU - Maia, M. A. G.

AU - Nichol, R. C.

AU - Thomas, D.

AU - Dark Energy Survey Collaboration

N1 - 16 pages, 9 figures, AJ accepted

PY - 2016/5/27

Y1 - 2016/5/27

N2 - Meeting the science goals for many current and future ground-based optical large-area sky surveys requires that the calibrated broadband photometry is stable in time and uniform over the sky to 1% precision or better. Past surveys have achieved photometric precision of 1-2% by calibrating the survey's stellar photometry with repeated measurements of a large number of stars observed in multiple epochs. The calibration techniques employed by these surveys only consider the relative frame-by-frame photometric zeropoint offset and the focal plane position-dependent illumination corrections, which are independent of the source color. However, variations in the wavelength dependence of the atmospheric transmission and the instrumental throughput induce source color-dependent systematic errors. These systematic errors must also be considered to achieve the most precise photometric measurements. In this paper, we examine such systematic chromatic errors using photometry from the Dark Energy Survey (DES) as an example. We define a natural magnitude system for DES and calculate the systematic errors on stellar magnitudes, when the atmospheric transmission and instrumental throughput deviate from the natural system. We conclude that the systematic chromatic errors caused by the change of airmass in each exposure, the change of the precipitable water vapor and aerosol in the atmosphere over time, and the non-uniformity of instrumental throughput over the focal plane, can be up to 2% in some bandpasses. We compare the calculated systematic chromatic errors with the observed DES data. For the test sample data, we correct these errors using measurements of the atmospheric transmission and instrumental throughput. The residual after correction is less than 0.3%. We also find that the errors for non-stellar objects are redshift-dependent and can be larger than those for stars at certain redshifts.

AB - Meeting the science goals for many current and future ground-based optical large-area sky surveys requires that the calibrated broadband photometry is stable in time and uniform over the sky to 1% precision or better. Past surveys have achieved photometric precision of 1-2% by calibrating the survey's stellar photometry with repeated measurements of a large number of stars observed in multiple epochs. The calibration techniques employed by these surveys only consider the relative frame-by-frame photometric zeropoint offset and the focal plane position-dependent illumination corrections, which are independent of the source color. However, variations in the wavelength dependence of the atmospheric transmission and the instrumental throughput induce source color-dependent systematic errors. These systematic errors must also be considered to achieve the most precise photometric measurements. In this paper, we examine such systematic chromatic errors using photometry from the Dark Energy Survey (DES) as an example. We define a natural magnitude system for DES and calculate the systematic errors on stellar magnitudes, when the atmospheric transmission and instrumental throughput deviate from the natural system. We conclude that the systematic chromatic errors caused by the change of airmass in each exposure, the change of the precipitable water vapor and aerosol in the atmosphere over time, and the non-uniformity of instrumental throughput over the focal plane, can be up to 2% in some bandpasses. We compare the calculated systematic chromatic errors with the observed DES data. For the test sample data, we correct these errors using measurements of the atmospheric transmission and instrumental throughput. The residual after correction is less than 0.3%. We also find that the errors for non-stellar objects are redshift-dependent and can be larger than those for stars at certain redshifts.

KW - astro-ph.IM

KW - atmospheric effects

KW - methods: observational

KW - surveys

KW - techniques: photometric

KW - RCUK

KW - STFC

U2 - 10.3847/0004-6256/151/6/157

DO - 10.3847/0004-6256/151/6/157

M3 - Article

VL - 151

JO - The Astronomical Journal

JF - The Astronomical Journal

SN - 0004-6256

IS - 6

ER -

ID: 4767949