J/ApJS/185/433ivo://CDS.VizieR/J/ApJS/185/433doi:10.26093/cds/vizier.21850433CDSWilkes B.J.Kilgard R.Kim D.-W.Kim M.Polletta M.Lonsdale C.,Smith H.E.Surace J.Owen F.N.Franceschini A.Siana B.Shupe D.2017-11-10T11:16:31Z2010-05-31T20:26:16ZCDS support team

CDS, Observatoire de Strasbourg, 11 rue de l'Universite, F-67000 Strasbourg, France

cds-question@unistra.frx-ray-sourcesinfrared-photometryvisible-astronomyWide-band photometryastronomical-object-identificationsurveysactive-galactic-nucleiWe report a moderate-depth (70ks), contiguous 0.7deg^2^ Chandra survey in the Lockman Hole Field of the Spitzer/SWIRE Legacy Survey coincident with a completed, ultra-deep VLA survey with deep optical and near-infrared imaging in-hand. The primary motivation is to distinguish starburst galaxies and active galactic nuclei (AGNs), including the significant, highly obscured (logN_H_>23) subset. Chandra has detected 775 X-ray sources to a limiting broadband (0.3-8keV) flux ~4x10^-16^erg/cm^2^/s. We present the X-ray catalog, fluxes, hardness ratios, and multi-wavelength fluxes. The logN versus logS agrees with those of previous surveys covering similar flux ranges. The Chandra and Spitzer flux limits are well matched: 771 (99%) of the X-ray sources have infrared (IR) or optical counterparts, and 333 have MIPS 24um detections. There are four optical-only X-ray sources and four with no visible optical/IR counterpart. The very deep (~2.7uJy rms) VLA data yield 251 (>4{sigma}) radio counterparts, 44% of the X-ray sources in the field. More than 40% of the X-ray sources in the VLA field are radio-loud using the classical definition, RL. The majority of these are red and relatively faint in the optical so that the use of RL to select those AGNs with the strongest radio emission becomes questionable. Using the 24um to radio flux ratio (q_24_) instead results in 13 of the 147 AGNs with sufficient data being classified as radio-loud, in good agreement with the ~10% expected for broad-lined AGNs based on optical surveys. We conclude that q_24_ is a more reliable indicator of radio-loudness. Use of RL should be confined to the optically selected type 1 AGN.2009ApJS..185..433Whttps://cdsarc.cds.unistra.fr/viz-bin/cat/J/ApJS/185/433CatalogResearchIsServedByTAP VizieR generic serviceIsServedByConesearch servicerelated-toJ/AJ/129/2074 : Faint Chandra sources in SWIRE (Franceschini+, 2005)J/ApJ/642/673 : IR-selected obscured AGN candidates (Polletta+, 2006)http://cosmosdb.iasf-milano.inaf.it/CHANDRA-SWIRE/index.jsp : SWIRE/Chandrahttps://cds.unistra.fr/vizier-org/licences_vizier.htmlhttps://vizier.cds.unistra.fr/viz-bin/VizieR-2?-source=J/ApJS/185/433https://vizier.iucaa.in/viz-bin/VizieR-2?-source=J/ApJS/185/433http://vizieridia.saao.ac.za/viz-bin/VizieR-2?-source=J/ApJS/185/433https://vizier.cds.unistra.fr/viz-bin/votable?-source=J/ApJS/185/433https://vizier.iucaa.in/viz-bin/votable?-source=J/ApJS/185/433http://vizieridia.saao.ac.za/viz-bin/votable?-source=J/ApJS/185/433GETtext/xml+votablehttps://tapvizier.cds.unistra.fr/TAPVizieR/tapCone search capability for table J/ApJS/185/433/survey (SWIRE and X-ray sources in Lockman Hole (tables 3, 4 and 7 of the paper))https://vizier.cds.unistra.fr/viz-bin/conesearch/J/ApJS/185/433/survey?https://vizier.iucaa.in/viz-bin/conesearch/J/ApJS/185/433/survey?http://vizieridia.saao.ac.za/viz-bin/conesearch/J/ApJS/185/433/survey?GETtext/xml+votable180.050000true161.621958358.99480560.0055555555555555566/6077 60799.932213363424795e-25 4.653515163505597e-19https://cdsarc.cds.unistra.fr/viz-bin/moc/J/ApJS/185/433?format=asciiX-rayOpticalInfrareddefaultJ/ApJS/185/433/surveySWIRE and X-ray sources in Lockman Hole (tables 3, 4 and 7 of the paper)NotesNotesmeta.notecharrecnoRecord number assigned by the VizieR team. Should Not be used for identification.meta.recordintCXOSWSource identification (JHHMMSS.s+DDMMSS)meta.id;meta.mainchare_posPosition errorarcsecstat.errorfloatXctsNet 0.3-8.0keV countsctphot.count;em.X-rayfloate_XctsError on Xctsctstat.errorfloatXrateNet 0.3-8.0keV count ratect/sphot.count;em.X-raydoublee_XrateError on Xratect/sstat.error;phot.count;em.X-raydoubleS1keVThe 1keV flux density (1)mW.m**-2.Hz**-1phot.flux;em.X-raydoubleFbroadBroad 0.3-8.0keV flux (1)mW.m**-2phot.flux;em.X-raydoubleFsoft? Soft 0.3-2.5keV flux (1)mW.m**-2phot.flux;em.X-raydoublenullableFhard? Hard 2.5-8.0keV flux (1)mW.m**-2phot.flux;em.X-raydoublenullableHRHardness ratio (2)phot.flux;arith.ratiofloatE_HRUpper error on HRstat.error;stat.maxfloate_HRLower error on HRstat.errorfloatSWIRE? SWIRE identificationmeta.id.crossintnullableDPOS? Distance between X-ray and SWIRE sourcesarcsecpos.angDistancefloatnullablermagThe r' band magnitude (1)magphot.mag;em.opt.Rfloate_rmag? The error in rmagmagstat.error;phot.mag;em.opt.RfloatnullablegmagThe g' band magnitude (1)magphot.mag;em.opt.Bfloate_gmag? The error in gmagmagstat.error;phot.mag;em.opt.BfloatnullableF3.6The 3.6 micron flux density (1)uJyphot.mag;em.IR.3-4umfloate_F3.6? The error in F3.6uJystat.errorfloatnullableF8.0The 8.0 micron flux density (1)uJyphot.flux.density;em.IR.8-15umfloate_F8.0? The error in F8.0uJystat.errorfloatnullableF24The 24 micron flux density (1)uJyphot.flux.density;em.IR.15-30umfloate_F24? The error in F24uJystat.errorfloatnullableF20cmThe 20cm flux density (1)uJyphot.flux.density;em.radio.750-1500MHzfloate_F20cm? The error in F20cmuJystat.errorfloatnullableSimbadSimbad column added by the CDScharRAJ2000Hours of Right Ascention (J2000)pos.eq.ra;meta.mainDEJ2000Degree of Declination (J2000)pos.eq.dec;meta.main