THE DARK ENERGY CAMERA

被引：599

作者：

Flaugher, B. ^{[1
]}

Diehl, H. T. ^{[1
]}

Honscheid, K. ^{[2
,3
]}

Abbott, T. M. C. ^{[4
]}

Alvarez, O. ^{[1
]}

Angstadt, R. ^{[1
]}

Annis, J. T. ^{[1
]}

Antonik, M. ^{[5
]}

Ballester, O. ^{[6
]}

Beaufore, L. ^{[3
]}

Bernstein, G. M. ^{[7
]}

Bernsteing, R. A. ^{[8
]}

Bigelow, B. ^{[9
]}

Bonati, M. ^{[4
]}

Boprie, D. ^{[9
]}

Brooks, D. ^{[5
]}

Buckley-Geer, E. J. ^{[1
]}

Campa, J. ^{[10
]}

Cardiel-Sas, L. ^{[6
]}

Castander, F. J. ^{[11
]}

Castilla, J. ^{[10
]}

Cease, H. ^{[1
]}

Cela-Ruiz, J. M. ^{[10
]}

Chappa, S. ^{[1
]}

Chi, E. ^{[1
]}

Cooper, C. ^{[9
]}

da Costa, L. N. ^{[12
,13
]}

Dede, E. ^{[9
]}

Derylo, G. ^{[1
]}

DePoy, D. L. ^{[14
,15
]}

de Vicente, J. ^{[10
]}

Doel, P. ^{[5
]}

Drlica-Wagner, A. ^{[1
]}

Eiting, J. ^{[3
]}

Elliott, A. E. ^{[3
]}

Emes, J. ^{[16
]}

Estrada, J. ^{[1
]}

Neto, A. Fausti ^{[12
]}

Finley, D. A. ^{[1
]}

Flores, R. ^{[1
]}

Frieman, J. ^{[1
,17
]}

Gerdes, D. ^{[9
]}

Gladders, M. D. ^{[17
]}

Gregory, B. ^{[4
]}

Gutierrez, G. R. ^{[1
]}

Hao, J. ^{[1
]}

Holland, S. E. ^{[16
]}

Holm, S. ^{[1
]}

Huffman, D. ^{[1
]}

Jackson, C. ^{[1
]}

机构：

[1] Fermilab Natl Accelerator Lab, Batavia, IL 60510 USA

[2] Ohio State Univ, Ctr Cosmol & Astroparticle Phys, Columbus, OH 43210 USA

[3] Ohio State Univ, Dept Phys, Columbus, OH 43210 USA

[4] Cerro Tololo Interamer Observ, Natl Opt Astron Observ, La Serena, Chile

[5] UCL, Dept Phys & Astron, London WC1E 6BT, England

[6] Univ Autonoma Barcelona, Inst Fis Altes Energies, E-08193 Barcelona, Spain

[7] Univ Penn, Dept Astron & Astrophys, Philadelphia, PA 19104 USA

[8] Carnegie Inst Washington Observ, Pasadena, CA 91101 USA

[9] Univ Michigan, Dept Phys, Ann Arbor, MI 48109 USA

[10] CIEMAT, E-28040 Madrid, Spain

[11] Fac Ciencies, Campus UAB, IEEC CSIC, Inst Ciencies lEspai, E-08193 Barcelona, Spain

[12] Lab Interinstituc eAstron LIneA, BR-20921400 Rio De Janeiro, Brazil

[13] Obser Nacl, BR-20921400 Rio De Janeiro, Brazil

[14] Texas A&M Univ, George P & Cynthia Woods Mitchell Inst Fundamenta, College Stn, TX 77843 USA

[15] Texas A&M Univ, Dept Phys & Astron, College Stn, TX 77843 USA

[16] Univ Calif Berkeley, Lawrence Berkeley Natl Lab, Berkeley, CA 94720 USA

[17] Univ Chicago, Kavli Inst Cosmol Phys, Chicago, IL 60637 USA

[18] Univ Illinois, Dept Phys, Urbana, IL 61801 USA

[19] Australian Astron Observ, N Ryde, NSW 2113, Australia

[20] Argonne Natl Lab, Lemont, IL 60439 USA

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

[22] Inst Catalana Recerca & Estudis Avancats, Barcelona E-08010, Spain

[23] Univ Portsmouth, Inst Cosmol & Gravitat, Portsmouth PO1 3FX, Hants, England

[24] Brookhaven Natl Lab, Upton, NY 11973 USA

[25] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA

[26] Stanford Univ, Kavli Inst Particle Astrophys & Cosmol, Stanford, CA 94305 USA

来源：

ASTRONOMICAL JOURNAL | 2015年 / 150卷 / 05期

基金：

美国国家科学基金会; 英国科学技术设施理事会;

关键词：

atlases; catalogs; cosmology: observations; instrumentation: detectors; instrumentation: photometers; surveys; CHARGE-COUPLED-DEVICES; DATA RELEASE; TELESCOPE; SYSTEM; DECAM; CCDS;

D O I：

10.1088/0004-6256/150/5/150

中图分类号：

P1 [天文学];

学科分类号：

0704 ;

摘要：

The Dark Energy Camera is a new imager with a 2 degrees.2 diameter field of view mounted at the prime focus of the Victor M. Blanco 4 m telescope on Cerro Tololo near La Serena, Chile. The camera was designed and constructed by the Dark Energy Survey Collaboration. and meets or exceeds the stringent requirements designed for the wide-field and supernova surveys for which the collaboration uses it. The camera consists of a five-element optical corrector, seven filters, a shutter with a 60 cm aperture, and a charge-coupled device (CCD) focal plane of 250 mu m thick fully depleted CCDs cooled inside a vacuum Dewar. The 570 megapixel focal plane comprises 62 2k x 4k CCDs for imaging and 12 2k x 2k CCDs for guiding and focus. The CCDs have 15 mu m x 15 mu m pixels with a plate scale of 0 ''.263 pixel(-1). A hexapod system provides state-of-the-art focus and alignment capability. The camera is read out in 20 s with 6-9 electron. readout noise. This paper provides a technical description of the camera's engineering, construction, installation, and current status.

引用

页数：43

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