Utilizza questo identificativo per citare o creare un link a questo documento:
http://hdl.handle.net/20.500.12386/23701
Campo DC | Valore | Lingua |
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dc.contributor.author | Civano, F. | en_US |
dc.contributor.author | Hickox, R. C. | en_US |
dc.contributor.author | Puccetti, S. | en_US |
dc.contributor.author | COMASTRI, Andrea | en_US |
dc.contributor.author | Mullaney, J. R. | en_US |
dc.contributor.author | ZAPPACOSTA, Luca | en_US |
dc.contributor.author | LaMassa, S. M. | en_US |
dc.contributor.author | Aird, J. | en_US |
dc.contributor.author | Alexander, D. M. | en_US |
dc.contributor.author | Ballantyne, D. R. | en_US |
dc.contributor.author | Bauer, F. E. | en_US |
dc.contributor.author | Brandt, W. N. | en_US |
dc.contributor.author | Boggs, S. E. | en_US |
dc.contributor.author | Christensen, F. E. | en_US |
dc.contributor.author | Craig, W. W. | en_US |
dc.contributor.author | Del-Moro, A. | en_US |
dc.contributor.author | Elvis, M. | en_US |
dc.contributor.author | Forster, K. | en_US |
dc.contributor.author | Gandhi, P. | en_US |
dc.contributor.author | Grefenstette, B. W. | en_US |
dc.contributor.author | Hailey, C. J. | en_US |
dc.contributor.author | Harrison, F. A. | en_US |
dc.contributor.author | Lansbury, G. B. | en_US |
dc.contributor.author | Luo, B. | en_US |
dc.contributor.author | Madsen, K. | en_US |
dc.contributor.author | Saez, C. | en_US |
dc.contributor.author | Stern, D. | en_US |
dc.contributor.author | Treister, E. | en_US |
dc.contributor.author | Urry, M. C. | en_US |
dc.contributor.author | Wik, D. R. | en_US |
dc.contributor.author | Zhang, W. | en_US |
dc.date.accessioned | 2020-03-30T12:55:02Z | - |
dc.date.available | 2020-03-30T12:55:02Z | - |
dc.date.issued | 2015 | en_US |
dc.identifier.issn | 0004-637X | en_US |
dc.identifier.uri | http://hdl.handle.net/20.500.12386/23701 | - |
dc.description | 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). | en |
dc.description.abstract | 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<SUP>2</SUP> 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<SUP>-14</SUP> {erg} {{cm}}<SUP>-2</SUP> {{{s}}}<SUP>-1</SUP> 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 10<SUP>42</SUP>-10<SUP>45.5</SUP> {erg} {{{s}}}<SUP>-1</SUP> 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 10<SUP>24</SUP> cm<SUP>-2</SUP>, implying the source is Compton-thick. This source was not previously recognized as such without the >10 keV data. | en_US |
dc.language.iso | eng | en_US |
dc.title | The Nustar Extragalactic Surveys: Overview and Catalog from the COSMOS Field | en_US |
dc.type | Article | - |
dc.identifier.doi | 10.1088/0004-637X/808/2/185 | en_US |
dc.identifier.scopus | 2-s2.0-84942163474 | en_US |
dc.identifier.isi | 000371002400081 | en_US |
dc.identifier.url | https://iopscience.iop.org/article/10.1088/0004-637X/808/2/185/ | en_US |
dc.relation.medium | STAMPA | en_US |
dc.relation.volume | 808 | en_US |
dc.relation.issue | 2 | en_US |
dc.relation.firstpage | 185 | en_US |
dc.relation.lastpage | 204 | en_US |
dc.relation.numberofpages | 20 | en_US |
dc.type.referee | REF_1 | en_US |
dc.description.numberofauthors | 31 | en_US |
dc.description.international | sì | en_US |
dc.contributor.country | ITA | en_US |
dc.contributor.country | USA | en_US |
dc.relation.scientificsector | FIS/05 - ASTRONOMIA E ASTROFISICA | en_US |
dc.relation.journal | THE ASTROPHYSICAL JOURNAL | en_US |
dc.type.miur | 262 Articolo in rivista | - |
dc.identifier.adsbibcode | 2015ApJ...808..185C | en_US |
dc.relation.ercsector | Scienze Fisiche Settori ERC (ERC) di riferimento::PE9 Universe sciences: astro-physics/chemistry/biology; solar systems; stellar, galactic and extragalactic astronomy, planetary systems, cosmology, space science, instrumentation | en_US |
dc.description.apc | sì | en_US |
dc.description.oa | 1 – prodotto con file in versione Open Access (allegherò il file al passo 5-Carica) | en_US |
item.grantfulltext | open | - |
item.openairecristype | http://purl.org/coar/resource_type/c_18cf | - |
item.fulltext | With Fulltext | - |
item.languageiso639-1 | en | - |
item.openairetype | Article | - |
item.cerifentitytype | Publications | - |
crisitem.journal.journalissn | 0004-637X | - |
crisitem.journal.ance | E016252 | - |
crisitem.author.dept | OAS Bologna | - |
crisitem.author.dept | O.A. Roma | - |
crisitem.author.orcid | 0000-0003-3451-9970 | - |
crisitem.author.orcid | 0000-0002-4205-6884 | - |
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