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The NuSTAR Extragalactic Surveys: Initial Results and Catalog from the Extended Chandra Deep Field South

Mullaney, J. R. and Del-Moro, A. and Aird, J. and Alexander, D. M. and Civano, F. M. and Hickox, R. C. and Lansbury, G. B. and Ajello, M. and Assef, R. and Ballantyne, D. R. and Baloković, M. and Bauer, F. E. and Brandt, W. N. and Boggs, S. E. and Brightman, M. and Christensen, F. E. and Comastri, A. and Craig, W. W. and Elvis, M. and Forster, K. and Gandhi, P. and Grefenstette, B. W. and Hailey, C. J. and Harrison, F. A. and Koss, M. and LaMassa, S. M. and Luo, Bin and Madsen, K. K. and Puccetti, S. and Saez, C. and Stern, D. and Treister, E. and Urry, C. M. and Wik, D. R. and Zappacosta, L. and Zhang, W. W. (2015) The NuSTAR Extragalactic Surveys: Initial Results and Catalog from the Extended Chandra Deep Field South. Astrophysical Journal, 808 (2). Art. No. 184. ISSN 0004-637X.

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We present the initial results and the source catalog from the Nuclear Spectroscopic Telescope Array (NuSTAR) survey of the Extended Chandra Deep Field South (hereafter, ECDFS)—currently the deepest contiguous component of the NuSTAR extragalactic survey program. The survey covers the full ≈30' × 30' area of this field to a maximum depth of ≈360 ks (≈ 220 ks when corrected for vignetting at 3–24 keV), reaching sensitivity limits of ≈ 1.3 X 10^(-14) erg s^(-1) cm^(-2) (3–8 keV), ≈ 3.4 X 10^ s^(-1)}, cm^(-2) (8–24 keV), and ~3 X 10^(-14) erg, s^(-1) cm^(-2) (3–24 keV). A total of 54 sources are detected over the full field, although five of these are found to lie below our significance threshold once contaminating flux from neighboring (i.e., blended) sources is taken into account. Of the remaining 49 that are significant, 19 are detected in the 8–24 keV band. The 8–24 to 3–8 keV band ratios of the 12 sources that are detected in both bands span the range 0.39–1.7, corresponding to a photon index range of Γ ≈ 0.5-2.3, with a median photon index of Γ[bar]} = 1.70 ± 0.52. The redshifts of the 49 sources in our main sample span the range z = 0.21-2.7, and their rest-frame 10–40 keV luminosities (derived from the observed 8–24 keV fluxes) span the range L_(10-40 keV) ≈ (0.7-300) X 10^(43) erg s^(-1), sampling below the "knee" of the X-ray luminosity function out to sim 0.8-1. Finally, we identify one NuSTAR source that has neither a Chandra nor an XMM-Newton counterpart, but that shows evidence of nuclear activity at infrared wavelengths and thus may represent a genuine, new X-ray source detected by NuSTAR in the ECDFS.

Item Type:Article
Related URLs:
URLURL TypeDescription Paper
Mullaney, J. R.0000-0002-3126-6712
Aird, J.0000-0003-1908-8463
Alexander, D. M.0000-0002-5896-6313
Lansbury, G. B.0000-0002-5328-9827
Assef, R.0000-0002-9508-3667
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
Comastri, A.0000-0003-3451-9970
Gandhi, P.0000-0003-3105-2615
Harrison, F. A.0000-0003-2992-8024
Koss, M.0000-0002-7998-9581
Luo, Bin0000-0002-9036-0063
Madsen, K. K.0000-0003-1252-4891
Puccetti, S.0000-0002-2734-7835
Stern, D.0000-0003-2686-9241
Urry, C. M.0000-0002-0745-9792
Additional Information:© 2015. The American Astronomical Society. Received 2015 March 2; accepted 2015 June 19; published 2015 August 3. We thank the anonymous referee for their careful reading of the manuscript and comments that improved the clarity of the text. 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). A.D.M. and D.M.A. gratefully acknowledge financial support from the Science and Technology Facilities Council (ST/I001573/1). J.A. acknowledges support from a COFUND Junior Research Fellowship from the Institute of Advanced Study, Durham University, and ERC Advanced Grant FEEDBACK at the University of Cambridge. F.M.C. acknowledges support from NASA grants 11-ADAP11-0218 and GO3-14150C. D.R.B. is supported in part by NSF award AST 1008067. W.N.B. and B.L. thank NuSTAR grant 44A-1092750, NASA ADP grant NNX10AC99G, and the V. M. Willaman Endowment. We acknowledge support from CONICYT-Chile grants Basal-CATA PFB-06/2007 (FEB), FONDECYT 1141218 (FEB) and 1120061 (ET), and "EMBIGGEN" Anillo ACT1101 (FEB, ET); and the Ministry of Economy, Development, and Tourism's Millennium Science Initiative through grant IC120009, awarded to The Millennium Institute of Astrophysics, MAS (FEB). Support for the work of E.T. was also provided by the Center of Excellence in Astrophysics and Associated Technologies (PFB 06). A.C., S.P., and L.Z. acknowledge support from the ASI/INAF grant I/037/12/0 011/13. A.C. acknowledges the Caltech Kingsley visitor program. M.B. acknowledges support from NASA Headquarters under the NASA Earth and Space Science Fellowship Program, grant NNX14AQ07H.
Group:NuSTAR, Space Radiation Laboratory
Funding AgencyGrant Number
Science and Technology Facilities Council (STFC)ST/I001573/1
Durham UniversityUNSPECIFIED
European Research Council (ERC)UNSPECIFIED
V. M. Willaman EndowmentUNSPECIFIED
Caltech NuSTAR subcontract44A-1092750
Fondo Nacional de Desarrollo Científico y Tecnológico (FONDECYT)1141218
Comisión Nacional de Investigación Científica y Tecnológica (CONICYT)ACT1101
Iniciativa Científica Milenio del Ministerio de Economía, Fomento y TurismoIC120009
Center of Excellence in Astrophysics and Associated Technologies (CATA)UNSPECIFIED
Agenzia Spaziale Italiana (ASI)I/037/12/0 011/13
NASA Earth and Space Science FellowshipNNX14AQ07H
Caltech Kingsley Foundation FellowshipUNSPECIFIED
Other Numbering System:
Other Numbering System NameOther Numbering System ID
Space Radiation Laboratory2015-44
Record Number:CaltechAUTHORS:20150907-151739240
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Official Citation:J. R. Mullaney et al 2015 ApJ 808 184
Usage Policy:No commercial reproduction, distribution, display or performance rights in this work are provided.
ID Code:60086
Deposited By: Joy Painter
Deposited On:09 Sep 2015 22:53
Last Modified:21 Mar 2019 18:59

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