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The NuSTAR Extragalactic Surveys: Overview and catalog from the COSMOS field

Civano, F. and Hickox, R. C. and Puccetti, S. and Comastri, A. and Mullaney, J. R. and Zappacosta, L. and LaMassa, S. M. and Aird, J. and Alexander, D. M. and Ballantyne, D. R. and Bauer, F. E. and Brandt, W. N. and Boggs, S. E. and Christensen, F. E. and Craig, W. W. and Del-Moro, A. and Elvis, M. and Forster, K. and Gandhi, P. and Grefenstette, B. W. and Hailey, C. J. and Harrison, F. A. and Lansbury, G. B. and Luo, B. and Madsen, K. K. and Saez, C. and Stern, D. and Treister, E. and Urry, M. C. and Wik, D. R. and Zhang, W. W. (2015) The NuSTAR Extragalactic Surveys: Overview and catalog from the COSMOS field. Astrophysical Journal, 808 (2). Art. No. 185. ISSN 0004-637X. doi:10.1088/0004-637X/808/2/185.

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To provide the census of the sources contributing to the X-ray background peak above 10 keV, Nuclear Spectroscopic Telescope Array (NuSTAR) is performing extragalactic surveys using a three-tier “wedding cake” approach. We present the NuSTAR survey of the COSMOS field, the medium sensitivity, and medium area tier, covering 1.7 deg^2 and overlapping with both Chandra and XMM-Newton data. This survey consists of 121 observations for a total exposure of ∼3 Ms. To fully exploit these data, we developed a new detection strategy, carefully tested through extensive simulations. The survey sensitivity at 20% completeness is 5.9, 2.9, and 6.4 × 10^(−14) erg cm^(-2) s^(-1) in the 3–24, 3–8, and 8–24 keV bands, respectively. By combining detections in 3 bands, we have a sample of 91 NuSTAR sources with 1042–1045.5 erg s^(-1) luminosities and redshift z = 0.04–2.5. Thirty-two sources are detected in the 8–24 keV band with fluxes ∼100 times fainter than sources detected by Swift-BAT. Of the 91 detections, all but 4 are associated with a Chandra and/or XMM-Newton point-like counterpart. One source is associated with an extended lower energy X-ray source. We present the X-ray (hardness ratio and luminosity) and optical-to-X-ray properties. The observed fraction of candidate Compton-thick active galactic nuclei measured from the hardness ratio is between 13%–20%. We discuss the spectral properties of NuSTAR J100259+0220.6 (ID 330) at z = 0.044, with the highest hardness ratio in the entire sample. The measured column density exceeds 1024 cm^(−2), implying the source is Compton-thick. This source was not previously recognized as such without the >10 keV data.

Item Type:Article
Related URLs:
URLURL TypeDescription Paper
Civano, F.0000-0002-2115-1137
Hickox, R. C.0000-0003-1468-9526
Puccetti, S.0000-0002-2734-7835
Comastri, A.0000-0003-3451-9970
Mullaney, J. R.0000-0002-3126-6712
Zappacosta, L.0000-0002-4205-6884
LaMassa, S. M.0000-0002-5907-3330
Aird, J.0000-0003-1908-8463
Alexander, D. M.0000-0002-5896-6313
Ballantyne, D. R.0000-0001-8128-6976
Bauer, F. E.0000-0002-8686-8737
Brandt, W. N.0000-0002-0167-2453
Boggs, S. E.0000-0001-9567-4224
Christensen, F. E.0000-0001-5679-1946
Forster, K.0000-0001-5800-5531
Gandhi, P.0000-0003-3105-2615
Grefenstette, B. W.0000-0002-1984-2932
Harrison, F. A.0000-0003-2992-8024
Lansbury, G. B.0000-0002-5328-9827
Luo, B.0000-0002-9036-0063
Madsen, K. K.0000-0003-1252-4891
Stern, D.0000-0003-2686-9241
Treister, E.0000-0001-7568-6412
Urry, M. C.0000-0002-0745-9792
Wik, D. R.0000-0001-8952-676X
Zhang, W. W.0000-0002-1426-9698
Additional Information:© 2015. The American Astronomical Society. Received 2015 February 27; accepted 2015 June 17; published 2015 August 3. We thank the anonymous referee for interesting comments and A. Goulding and M. Rose for useful discussions. This work made use of data from the NuSTAR mission, a project led by the California Institute of Technology, managed by the Jet Propulsion Laboratory, and funded by the National Aeronautics and Space Administration. We thank the NuSTAR Operations, Software and Calibration teams for support with the execution and analysis of these observations. This research has made use of the NuSTAR Data Analysis Software (NUSTARDAS) jointly developed by the ASI Science Data Center (ASDC, Italy) and the California Institute of Technology (USA). We acknowledge support from the NASA grants 11-ADAP11-0218 and GO3-14150C (FC); from the Science and Technology Facilities Council ST/I001573/1 (ADM, DMA); NSF award AST 1008067 (DRB); NuSTAR grant 44A-1092750, NASA ADP grant NNX10AC99G, and the V.M. Willaman Endowment (WNB, BL); CONICYT-Chile grants Basal-CATA PFB-06/2007 (FEB), FONDECYT 1141218 (FEB), and "EMBIGGEN" Anillo ACT1101 (FEB, ET); the Ministry of Economy, Development, and Tourism's Millennium Science Initiative through grant IC120009, awarded to The Millennium Institute of Astrophysics, MAS (FEB); the Center of Excellence in Astrophysics and Associated Technologies (PFB 06) and by the FONDECYT regular grant 1120061 (ET); financial support under ASI/INAF contract I/037/12/0 (LZ).
Group:NuSTAR, Space Radiation Laboratory
Funding AgencyGrant Number
Science and Technology Facilities Council (STFC)ST/I001573/1
NASAAST 1008067
Caltech NuSTAR subcontract44A-1092750
V. M. Willaman EndowmentUNSPECIFIED
Iniciativa Científica Milenio del Ministerio de Economía, Fomento y TurismoIC120009
Fondo Nacional de Desarrollo Científico y Tecnológico (FONDECYT)1120061
Agenzia Spaziale Italiana (ASI)I/037/12/0 011/13
Other Numbering System:
Other Numbering System NameOther Numbering System ID
Space Radiation Laboratory2015-43
Issue or Number:2
Record Number:CaltechAUTHORS:20150907-154658360
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Usage Policy:No commercial reproduction, distribution, display or performance rights in this work are provided.
ID Code:60087
Deposited By: Joy Painter
Deposited On:09 Sep 2015 22:18
Last Modified:10 Nov 2021 22:29

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