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The Atacama Cosmology Telescope: Data Characterization and Map Making
NTRS Full-Text: Click to View  [PDF Size: 3.1 MB]
External Online Source: doi:10.1088/0004-637X/762/1/10
Author and Affiliation:
Duenner, Rolando(Pontificia Univ. Catolica de Chile, Dept. de Astronomia y Astrofisica, Santiago, Chile);
Hasselfield, Matthew(British Columbia Univ., Dept. of Physics and Astronomy, Vancouver, British Columbia Canada);
Marriage, Tobias A.(Princeton Univ., Dept. of Astrophysical Sciences, Princeton, NJ, United States);
Sievers, Jon(Princeton Univ., Joseph Henry Laboratories of Physics, Princeton, NJ, United States);
Acquaviva, Viviana(Princeton Univ., Dept. of Astrophysical Sciences, Princeton, NJ, United States);
Addison, Graeme E.(Oxford Univ., Dept. of Astrophysics, Oxford, United Kingdom);
Ade, Peter A. R.(Cardiff Univ., School of Physics and Astronomy, United Kingdom);
Aguirre, Paula(Pontificia Univ. Catolica de Chile, Dept. de Astronomia y Astrofisica, Santiago, Chile);
Amiri, Mandana(British Columbia Univ., Dept. of Physics and Astronomy, Vancouver, British Columbia Canada);
Appel, John William(Princeton Univ., Joseph Henry Laboratories of Physics, Princeton, NJ, United States);
Barrientos, L. Felipe(Pontificia Univ. Catolica de Chile, Dept. de Astronomia y Astrofisica, Santiago, Chile);
Battistelli, Elia S.(British Columbia Univ., Dept. of Physics and Astronomy, Vancouver, British Columbia Canada);
Bond, J. Richard(Toronto Univ., Canadian Inst. for Theoretical Astrophysics, Ontario Canada);
Brown, Ben(Pittsburgh Univ., Dept. of Physics and Astronomy, Pittsburgh, PA, United States);
Burger, Bryce(British Columbia Univ., Dept. of Physics and Astronomy, Vancouver, British Columbia Canada);
Chervenak, Jay(NASA Goddard Space Flight Center, Greenbelt, MD, United States);
Calabrese, Erminia(Oxford Univ., Dept. of Astrophysics, Oxford, United Kingdom);
Das, Sudeep(Princeton Univ., Dept. of Astrophysical Sciences, Princeton, NJ, United States);
Devlin, Mark J.(Pennsylvania Univ., Dept. of Physics and Astronomy, Philadelphia, PA, United States);
Dicker, Simon R.(Pennsylvania Univ., Dept. of Physics and Astronomy, Philadelphia, PA, United States);
Doriese, W. Bertrand(National Inst. of Standards and Technology, Quantum Devices Group, Boulder, CO, United States);
Dunkley, Joanna(Princeton Univ., Dept. of Astrophysical Sciences, Princeton, NJ, United States);
Essinger-Hileman, Thomas(Princeton Univ., Joseph Henry Labs. of Physics, Princeton, NJ, United States);
Moseley, Harvey(NASA Goddard Space Flight Center, Greenbelt, MD, United States);
Wollack, Ed(NASA Goddard Space Flight Center, Greenbelt, MD, United States);
et al.
Abstract: We present a description of the data reduction and mapmaking pipeline used for the 2008 observing season of the Atacama Cosmology Telescope (ACT). The data presented here at 148 GHz represent 12% or the 90 TB collected by ACT from 2007 to 2010. In 2008 we observed for 136 days, producing a total of 142h of data (11 TB for the 148 GHz band only), with a daily average of 10.5 h of observation. From these, 108.5 h were devoted to 850 sq deg stripe (11.2 h by 9 deg.1) centered on a declination of -52 deg.7, while 175 h were devoted to a 280 square deg stripe (4.5 h by 4 deg.8) centered at the celestial equator. We discuss sources of statistical and systematic noise, calibration, telescope pointing and data selection. Out of 1260 survey hours and 1024 detectors per array, 816 h and 593 effective detectors remain after data selection for this frequency band, yielding a 38 % survey efficiency. The total sensitivity in 2008, determined from the noise level between 5 Hz and 20 Hz in the time-ordered data stream (TOD), is 32 muK square root of s in CMB units. Atmospheric brightness fluctuations constitute the main contaminant in the data and dominate the detector and noise covariance at low frequencies in the TOD. The maps were made by solving the lease squares problem using the Preconditioned Conjugate Gradient method, incorporating the details of the detector and noise correlations. Cross-correlation with WMAP sky maps as well as analysis from simulations reveal the our maps are unbiased at l > 300. This paper accompanies the public release of the 148 GHz southern stripe maps from 2008. The techniques described here will be applied to future maps and data releases.
Publication Date: Jan 01, 2012
Document ID:
20120015668
(Acquired Nov 15, 2012)
Subject Category: ASTRONOMY
Report/Patent Number: GSFC.JA.7097.2012
Document Type: Preprint
Contract/Grant/Task Num: DE-AC3-76SF00515; FONDECYT-11100147; FONDAP 15010003; NSF AST-0408696; NSF AST-0965625; NSF PHY-0855887; NSF PHY-1214379; NSF AST-0807790; NSF PHY-0114422
Financial Sponsor: NASA Goddard Space Flight Center; Greenbelt, MD, United States
National Science Foundation; Arlington, VA, United States
Department of Energy; United States
FONDECYT; Brazil
Organization Source: NASA Goddard Space Flight Center; Greenbelt, MD, United States
Description: 20p; In English; Original contains color and black and white illustrations
Distribution Limits: Unclassified; Publicly available; Unlimited
Rights: Copyright; Distribution as joint owner in the copyright
NASA Terms: DATA REDUCTION; TELESCOPES; SKY SURVEYS (ASTRONOMY); ASTRONOMICAL OBSERVATORIES; COSMIC MICROWAVE BACKGROUND RADIATION; MICROWAVE ANISOTROPY PROBE; DATA FLOW ANALYSIS
Miscellaneous Notes: Prepared by the ACT Collaboration. Sponsored in part from Centro de Astrofisica FONDAP; Rhodes Trust and Christ Church; Princeton Univ; Pensylvania Univ; and a Canada Foundation for Innovation (CFI); and the Government of Ontario, the Ontario Research Fund and the University of Toronto. To be published in the Astrophysical Journal
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