The Atacama Cosmology Telescope: two-season ACTPol extragalactic point sources and their polarization properties

被引：32

作者：

Datta, Rahul ^{[1
,18
]}

Aiola, Simone ^{[2
]}

Choi, Steve K. ^{[2
]}

Devlin, Mark ^{[3
]}

Dunkley, Joanna ^{[2
]}

Dunner, Rolando ^{[4
,5
]}

Gallardo, Patricio A. ^{[6
]}

Gralla, Megan ^{[7
]}

Halpern, Mark ^{[8
]}

Hasselfield, Matthew ^{[9
,10
]}

Hilton, Matt ^{[11
]}

Hincks, Adam D. ^{[12
]}

Ho, Shuay-Pwu P. ^{[2
]}

Hubmayr, Johannes ^{[13
]}

Huffenberger, Kevin M. ^{[14
]}

Hughes, John P. ^{[15
]}

Kosowsky, Arthur ^{[16
]}

Lopez-Caraballo, Carlos H. ^{[4
,5
]}

Louis, Thibaut ^{[17
]}

Lungu, Marius ^{[2
]}

Marriage, Tobias ^{[18
]}

Maurin, Loic ^{[4
,5
]}

McMahon, Jeff ^{[19
]}

Moodley, Kavilan ^{[11
]}

Naess, Sigurd K. ^{[20
]}

Nati, Federico ^{[3
]}

Niemack, Michael D. ^{[6
]}

Page, Lyman A. ^{[2
]}

Partridge, Bruce ^{[21
]}

Prince, Heather ^{[2
]}

Staggs, Suzanne T. ^{[2
]}

Switzer, Eric R. ^{[1
]}

Wollack, Edward J. ^{[1
]}

Farren, Gerrit ^{[21
]}

机构：

[1] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA

[2] Princeton Univ, Joseph Henry Labs Phys, Jadwin Hall, Princeton, NJ 08544 USA

[3] Univ Penn, Dept Phys & Astron, 209 South 33rd St, Philadelphia, PA 19104 USA

[4] Pontificia Univ Catolica Chile, Fac Fis, Inst Astrofis, Av Vicuna Mackenna 4860, Santiago 7820436, Chile

[5] Pontificia Univ Catolica Chile, Fac Fis, Ctr Astroingn, Av Vicuna Mackenna 4860, Santiago 7820436, Chile

[6] Cornell Univ, Dept Phys, Ithaca, NY 14953 USA

[7] Univ Arizona, Steward Observ, 933 N Cherry Ave, Tucson, AZ 85721 USA

[8] Univ British Columbia, Dept Phys & Astron, Vancouver, BC V6T 1Z4, Canada

[9] Penn State Univ, Dept Astron & Astrophys, 525 Davey Lab, University Pk, PA 16802 USA

[10] Penn State Univ, Inst Gravitat & Cosmos, University Pk, PA 16802 USA

[11] Univ KwaZulu Natal, Sch Math Stat & Comp Sci, Astrophys & Cosmol Res Unit, Westville Campus, ZA-4041 Durban, South Africa

[12] Univ Roma La Sapienza, Dept Phys, Piazzale Aldo Moro 5, I-00185 Rome, Italy

[13] NIST Quantum Devices Grp, 325 Broadway,Mailcode 817-03, Boulder, CO 80305 USA

[14] Florida State Univ, Dept Phys, Tallahassee, FL 32306 USA

[15] Rutgers State Univ, Dept Phys & Astron, Piscataway, NJ 08854 USA

[16] Univ Pittsburgh, Dept Phys & Astron, Pittsburgh, PA 15260 USA

[17] Univ Paris Saclay, Univ Paris Sud, CNRS, Lab Accelerateur Lineaire, Orsay, France

[18] Johns Hopkins Univ, Dept Phys & Astron, 3400 N Charles St, Baltimore, MD 21218 USA

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

[20] Ctr Computat Astrophys, 162 5th Ave, New York, NY 10003 USA

[21] Haverford Coll, Dept Phys & Astron, Haverford, PA 19041 USA

来源：

MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY | 2019年 / 486卷 / 04期

基金：

美国国家科学基金会; 新加坡国家研究基金会;

关键词：

polarization; techniques: polarimetric; catalogues; surveys; galaxies: active; cosmology: observations; STAR-FORMING GALAXIES; RADIO-SOURCES; HIGH-FREQUENCY; LINEAR-POLARIZATION; INTERVAL ESTIMATION; SOURCE COUNTS; PREDICTIONS; POLARIMETRY; STATISTICS; SKY;

D O I：

10.1093/mnras/sty2934

中图分类号：

P1 [天文学];

学科分类号：

0704 ;

摘要：

We report on measurements of the polarization of extragalactic sources at.148 GHz made during the first two seasons of the Atacama Cosmology Telescope Polarization (ACTPol) survey. The survey covered 680 deg(2) of the sky on the celestial equator. Polarization measurements of 169 intensity-selected sources brighter than 30 mJy, that are predominantly active galactic nuclei, are presented. Above a total flux of 215 mJy where the noise bias removal in the polarization measurement is reliable, we detect 2.6 sources, 14 of which have a detection of linear polarization at greater than 3 sigma-significance. The distribution of the fractional polarization as a function of total source intensity is analysed. Our result is consistent with the scenario that the fractional polarization of our measured radio source population is independent of total intensity down to the limits of our measurements and well described by a Gaussian distribution with a mean fractional polarization p(m) = 0.02.8 +/- 0.005 and standard deviation sigma(pm) = 0.054, truncated at p = 0. Extrapolating this model for the distribution of source polarization below the ACTPol detection threshold, we predict: that one could get a clean measure of the E mode polarization power spectrum. of the microwave background out to l approximate to 6000 with 1 HK-arcminute maps over 10% of the sky from a future stu-vey. We also study the spectral energy distribution of the total and polarized source flux densities by cross-matching with low.radio frequency catalogues. We do not find any correlation between the spectral indices for total flux and polarized flux.

引用

页码：5239 / 5262

页数：24

共 33 条

[31] The XMM large scale structure survey: properties and two-point angular correlations of point-like sources
Gandhi, P.
Garcet, O.
Disseau, L.
Pacaud, F.
Pierre, M.
Gueguen, A.
Alloin, D.
Chiappetti, L.
Gosset, E.
Maccagni, D.
Surdej, J.
Valtchanov, I.
ASTRONOMY & ASTROPHYSICS, 2006, 457 (02) : 393 - 404
[32] Predictions of the angular power spectrum of clustered extragalactic point sources at cosmic microwave background frequencies from flat and all-sky two-dimensional simulations
González-Nuevo, J
Toffolatti, L
Argüeso, F
ASTROPHYSICAL JOURNAL, 2005, 621 (01): : 1 - 14
[33] Deep 610-MHz Giant Metrewave Radio Telescope observations of the Spitzer extragalactic First Look Survey field - III. The radio properties of infrared-faint radio sources
Garn, Timothy
Alexander, Paul
MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY, 2008, 391 (02) : 1000 - 1008

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