Photometric Characterization of the Dark Energy Camera

被引：20

作者：

Bernstein, G. M. ^{[1
]}

Abbott, T. M. C. ^{[2
]}

Armstrong, R. ^{[3
]}

Burke, D. L. ^{[4
,5
]}

Diehl, H. T. ^{[6
]}

Gruendl, R. A. ^{[7
,8
]}

Johnsons, M. D. ^{[8
]}

Li, T. S. ^{[6
]}

Rykoff, E. S. ^{[4
,5
]}

Walker, A. R. ^{[2
]}

Wester, W. ^{[6
]}

Yanny, B. ^{[6
]}

机构：

[1] Univ Penn, Dept Phys & Astron, Philadelphia, PA 19104 USA

[2] Natl Opt Astron Observ, Cerro Tololo Interamer Observ, Casilla 603, La Serena, Chile

[3] Princeton Univ, Dept Astrophys Sci, Peyton Hall, Princeton, NJ 08544 USA

[4] Stanford Univ, Kavli Inst Particle Astrophys & Cosmol, POB 2450, Stanford, CA 94305 USA

[5] SLAC Natl Accelerator Lab, Menlo Pk, CA 94025 USA

[6] Fermilab Natl Accelerator Lab, POB 500, Batavia, IL 60510 USA

[7] Univ Illinois, Dept Astron, 1002 W Green St, Urbana, IL 61801 USA

[8] Natl Ctr Supercomp Applicat, 1205 West Clark St, Urbana, IL 61801 USA

来源：

PUBLICATIONS OF THE ASTRONOMICAL SOCIETY OF THE PACIFIC | 2018年 / 130卷 / 987期

基金：

欧洲研究理事会; 澳大利亚研究理事会; 美国国家科学基金会; 英国科学技术设施理事会;

关键词：

instrumentation: detectors; methods: data analysis; techniques: photometric; ALL-SKY; CALIBRATION;

D O I：

10.1088/1538-3873/aaa753

中图分类号：

P1 [天文学];

学科分类号：

0704 ;

摘要：

We characterize the variation in photometric response of the Dark Energy Camera (DECam) across its 520 Mpix science array during 4 years of operation. These variations are measured using high signal-to-noise aperture photometry of >10(7) stellar images in thousands of exposures of a few selected fields, with the telescope dithered to move the sources around the array. A calibration procedure based on these results brings the rms variation in aperture magnitudes of bright stars on cloudless nights down to 2-3 mmag, with <1 mmag of correlated photometric errors for stars separated by >= 20 ''. On cloudless nights, any departures of the exposure zeropoints from a secant airmass law exceeding <1 mmag are plausibly attributable to spatial/temporal variations in aperture corrections. These variations can be inferred and corrected by measuring the fraction of stellar light in an annulus between 6 '' and 8 '' diameter. Key elements of this calibration include: correction of amplifier nonlinearities; distinguishing pixel-area variations and stray light from quantum-efficiency variations in the flat fields; field-dependent color corrections; and the use of an aperture-correction proxy. The DECam response pattern across the 2 degrees field drifts over months by up to +/- 9 mmag, in a nearly wavelength-independent low-order pattern. We find no fundamental barriers to pushing global photometric calibrations toward mmag accuracy.

引用

页数：22

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