Astrometric Calibration and Performance of the Dark Energy Camera

Bernstein, G M and Armstrong, R and Plazas, A A and Walker, A R and Abbott, T M C and Allam, S and Bechtol, K and Benoit-Lévy, A and Brooks, D and Burke, D L and Rosell, A C and Kind, M C and Carretero, J and Cunha, C E and Costa, L N da and DePoy, D L and Desai, Shantanu and et al, . (2017) Astrometric Calibration and Performance of the Dark Energy Camera. Publications of the Astronomical Society of the Pacific, 129 (977). 074503. ISSN 0004-6280

Full text not available from this repository. (Request a copy)

Abstract

We characterize the ability of the Dark Energy Camera (DECam) to perform relative astrometry across its 500. Mpix, 3-deg(2) science field of view and across four years of operation. This is done using internal comparisons of similar to 4 x10(7) measurements of high signal-to-noise ratio stellar images obtained in repeat visits to fields of moderate stellar density, with the telescope dithered to move the sources around the array. An empirical astrometric model includes terms for optical distortions; stray electric fields in the CCD detectors; chromatic terms in the instrumental and atmospheric optics; shifts in CCD relative positions of up to approximate to 10 mu m when the DECam temperature cycles; and low-order distortions to each exposure from changes in atmospheric refraction and telescope alignment. Errors in this astrometric model are dominated by stochastic variations with typical amplitudes of 10-30. mas (in a 30 s exposure) and 5'-10' coherence length, plausibly attributed to Kolmogorov-spectrum atmospheric turbulence. The size of these atmospheric distortions is not closely related to the seeing. Given an astrometric reference catalog at density approximate to 0.7 arcmin(-2), e.g., from Gaia, the typical atmospheric distortions can be interpolated to approximate to 7 mas rms accuracy (for 30 s exposures) with 1' coherence length in residual errors. Remaining detectable error contributors are 2- 4. mas rms from unmodelled stray electric fields in the devices, and another 2- 4. mas rms from focal plane shifts between camera thermal cycles. Thus the astrometric solution for a single DECam exposure is accurate to 3- 6. mas (approximate to 0.02 pixels, or approximate to 300 nm) on the focal plane, plus the stochastic atmospheric distortion.

[error in script]
IITH Creators:
IITH CreatorsORCiD
Desai, Shantanuhttp://orcid.org/0000-0002-0466-3288
Item Type: Article
Uncontrolled Keywords: astrometry; atmospheric effects; instrumentation: detectors; methods: data analysis
Subjects: Physics > Astronomy Astrophysics
Divisions: Department of Physics
Depositing User: Team Library
Date Deposited: 22 Jun 2017 04:51
Last Modified: 05 Sep 2017 06:05
URI: http://raiith.iith.ac.in/id/eprint/3277
Publisher URL: https://doi.org/10.1088/1538-3873/aa6c55
OA policy: http://www.sherpa.ac.uk/romeo/issn/0004-6280/
Related URLs:

Actions (login required)

View Item View Item
Statistics for RAIITH ePrint 3277 Statistics for this ePrint Item