J/ApJ/836/99 NuSTAR serendipitous survey: the 40-month catalog (Lansbury+, 2017)
The NuSTAR serendipitous survey: the 40-month catalog and the properties of the distant high-energy X-ray source population. Lansbury G.B., Stern D., Aird J., Alexander D.M., Fuentes C., Harrison F.A., Treister E., Bauer F.E., Tomsick J.A., Balokovic M., Del Moro A., Gandhi P., Ajello M., Annuar A., Ballantyne D.R., Boggs S.E., Brandt W.N., Brightman M., Chen C.-T.J., Christensen F.E., Civano F., Comastri A., Craig W.W., Forster K., Grefenstette B.W., Hailey C.J., Hickox R.C., Jiang B., Jun H.D., Koss M., Marchesi S., Melo A.D., Mullaney J.R., Noirot G., Schulze S., Walton D.J., Zappacosta L., Zhang W.W. <Astrophys. J., 836, 99-99 (2017)> =2017ApJ...836...99L (SIMBAD/NED BibCode)
ADC_Keywords: Active gal. nuclei ; BL Lac objects ; X-ray sources ; Redshifts ; Photometry, infrared ; Spectroscopy ; Surveys Mission_Name: NuSTAR Keywords: catalogs; galaxies: active; galaxies: nuclei; quasars: general; surveys; X-rays: general Abstract: We present the first full catalog and science results for the Nuclear Spectroscopic Telescope Array (NuSTAR) serendipitous survey. The catalog incorporates data taken during the first 40 months of NuSTAR operation, which provide ∼20Ms of effective exposure time over 331 fields, with an areal coverage of 13deg2, and 497 sources detected in total over the 3-24keV energy range. There are 276 sources with spectroscopic redshifts and classifications, largely resulting from our extensive campaign of ground-based spectroscopic follow-up. We characterize the overall sample in terms of the X-ray, optical, and infrared source properties. The sample is primarily composed of active galactic nuclei (AGNs), detected over a large range in redshift from z=0.002 to 3.4 (median of <z≥0.56), but also includes 16 spectroscopically confirmed Galactic sources. There is a large range in X-ray flux, from log(f3-24keV/erg/s/cm2)~-14 to -11, and in rest-frame 10-40keV luminosity, from log(L10-40keV/erg/s)∼39 to 46, with a median of 44.1. Approximately 79% of the NuSTAR sources have lower-energy (<10keV) X-ray counterparts from XMM-Newton, Chandra, and Swift XRT. The mid-infrared (MIR) analysis, using WISE all-sky survey data, shows that MIR AGN color selections miss a large fraction of the NuSTAR-selected AGN population, from ∼15% at the highest luminosities (LX>1044erg/s) to ∼80% at the lowest luminosities (LX<1043erg/s). Our optical spectroscopic analysis finds that the observed fraction of optically obscured AGNs (i.e., the type 2 fraction) is FType2=53-15+14% , for a well-defined subset of the 8-24keV selected sample. This is higher, albeit at a low significance level, than the type 2 fraction measured for redshift- and luminosity-matched AGNs selected by <10keV X-ray missions. Description: Over the period from 2012 July to 2015 November, which is the focus of the current study, there are 510 individual NuSTAR exposures that have been incorporated into the serendipitous survey. These exposures were performed over 331 unique fields (i.e., 331 individual sky regions, each with contiguous coverage composed of one or more NuSTAR exposures), yielding a total sky area coverage of 13deg2. Table 1 lists the fields chronologically. The fields have a cumulative exposure time of 20.4Ms. We have undertaken a campaign of dedicated spectroscopic follow-up in the optical-IR bands, obtaining spectroscopic identifications for a large fraction (56%) of the total sample. Since NuSTAR performs science pointings across the whole sky, a successful ground-based follow-up campaign requires the use of observatories at a range of geographic latitudes, and preferably across a range of dates throughout the sidereal year. This has been achieved through observing programs with, primarily, the following telescopes over a multiyear period (2012 Oct 10 to 2016 Jul 10): the Hale Telescope at Palomar Observatory (5.1m; PIs F. A. Harrison and D. Stern); Keck I and II at the W. M. Keck Observatory (10m; PIs F. A. Harrison and D. Stern); the New Technology Telescope (NTT) at La Silla Observatory (3.6m; PI G. B. Lansbury); the Magellan I (Baade) and Magellan II (Clay) Telescopes at Las Campanas Observatory (6.5m; PIs E. Treister and F. E. Bauer); and the Gemini-South observatory (8.1m; PI E. Treister). File Summary:
FileName Lrecl Records Explanations
ReadMe 80 . This file table1.dat 82 591 Details of the individual NuSTAR observations which make up the serendipitous survey table5.dat 903 498 The primary NuSTAR serendipitous source catalog table6.dat 234 303 Summary of the optical spectroscopy for the NuSTAR serendipitous survey sources table7.dat 377 64 The secondary NuSTAR serendipitous source catalog table8.dat 234 46 Summary of the optical spectroscopy for the secondary catalog sources
See also: IX/15 : Einstein EMSS Survey (Gioia+ 1990, Stocke+ 1991) I/284 : The USNO-B1.0 Catalog (Monet+ 2003) VII/259 : 6dF galaxy survey final redshift release (Jones+, 2009) II/311 : WISE All-Sky Data Release (Cutri+ 2012) IX/45 : The Chandra Source Catalog, Release 1.1 (Evans+ 2012) II/319 : UKIDSS-DR9 LAS, GCS and DXS Surveys (Lawrence+ 2012) IX/50 : XMM-Newton Serendipitous Source Catalogue 3XMM-DR6 (XMM-SSC, 2016) J/A+AS/97/483 : Optical spectroscopy of 1Jy, S4 and S5 sources (Stickel+ 1993) J/ApJ/518/656 : ASCA Large Sky Survey (Ueda+, 1999) J/MNRAS/327/771 : BeppoSAX HELLAS survey. II. (Fiore+, 2001) J/ApJ/554/742 : Chandra Deep Survey of the HDF-N (Hornschemeier+, 2001) J/A+A/371/833 : ROSAT Ultra Deep Survey (Lehmann+, 2001) J/AJ/126/539 : The Chandra Deep Fields North and South (Alexander+, 2003) J/AJ/126/632 : UBVRIz'HK' photometry of 2Ms CDFN X-ray sources (Barger+, 2003) J/A+A/409/79 : HELLAS2XMM survey. IV. (Fiore+, 2003) J/ApJ/596/944 : SEXSI catalog (Harrison+, 2003) J/MNRAS/342/802 : Chandra survey of 13-h XMM/ROSAT survey (McHardy+, 2003) J/ApJ/582/615 : SHEEP survey (Nandra+, 2003) J/ApJS/150/19 : ChaMP. I. First X-ray source catalog (Kim+, 2004) J/A+A/418/465 : Mid-infrared and hard X-ray emission in AGN (Lutz+, 2004) J/ApJS/161/21 : Extended Chandra Deep Field-South survey (Lehmer+, 2005) J/MNRAS/356/568 : Deep Chandra survey of the Groth Strip (Nandra+, 2005) J/ApJS/161/185 : GIS catalog project : source catalog II (Ueda+, 2005) J/ApJS/165/19 : SEXSI catalog. III (Eckart+, 2006) J/A+A/448/L9 : Position catalogue of Swift XRT afterglows (Moretti+, 2006) J/ApJS/166/128 : Narrow line Seyfert 1 galaxies from SDSS-DR3 (Zhou+, 2006) J/A+A/476/1191 : XMM-Newton serendipitous survey. IV (Barcons+, 2007) J/A+A/475/775 : INTEGRAL all-sky survey of hard X-ray sources (Krivonos+, 2007) J/ApJ/678/102 : BAT X-ray survey. I. (Ajello+, 2008) J/ApJ/681/113 : Swift BAT survey of AGNs (Tueller+, 2008) J/ApJS/180/102 : AEGIS-X: Chandra deep survey (Laird+, 2009) J/A+A/495/691 : Multifrequency catalog of blazars, Roma-BZCAT (Massaro+, 2009) J/A+A/493/339 : XMM-Newton serendipitous Survey. V. (Watson+, 2009) J/ApJ/713/970 : Low-resolution SED templates for AGNs & galaxies (Assef+, 2010) J/ApJ/708/584 : SEXSI Spitzer catalog (Eckart+, 2010) J/ApJ/728/58 : Swift-BAT survey of AGNs (Burlon+, 2011) J/ApJS/195/10 : The CDF-S survey: 4Ms source catalogs (Xue+, 2011) J/ApJS/201/34 : Swift-INTEGRAL X-ray (SIX) survey (Bottacini+, 2012) J/ApJ/754/45 : IR properties of Swift/BAT X-ray AGNs (Ichikawa+, 2012) J/MNRAS/426/1750 : INTEGRAL/IBIS AGN catalogue (Malizia+, 2012) J/ApJ/753/104 : AGN identifications from AKARI and Swift (Matsuta+, 2012) J/ApJ/758/129 : 4Ms Chandra Deep Field South 6-8keV galaxies (Xue+, 2012) J/ApJ/772/26 : AGN with WISE. II. The NDWFS Bootes field (Assef+, 2013) J/ApJS/207/19 : Hard X-ray survey from Swift-BAT 2004-2010 (Baumgartner+, 2013) J/ApJ/779/104 : Luminous dust-poor SDSS QSOs at z<4.5 (Jun+, 2013) J/ApJ/765/L26 : Swift/BAT ultra-hard X-ray data from GOALS LIRGs (Koss+, 2013) J/ApJ/763/111 : X-ray spectral analysis of Swift/BAT AGNs (Vasudevan+, 2013) J/ApJ/808/185 : NuSTAR surveys: COSMOS catalog (Civano+, 2015) J/ApJ/808/184 : NuSTAR surveys: ECDF-S catalog (Mullaney+, 2015) J/ApJ/815/L13 : Compton-thick AGNs from 70-month Swift/BAT obs. (Ricci+, 2015) J/ApJ/807/129 : X-ray to MIR luminosities relation of AGNs (Stern, 2015) Byte-by-byte Description of file: table1.dat
Bytes Format Units Label Explanations
1- 4 A4 --- Field Field identifier (1) 6- 28 A23 --- Target Primary science target identifier 30- 31 I2 --- NObs [1/15]? Number of individual exposures in Field 33- 43 I11 --- ObsID ? Observation identifier 45- 54 A10 "Y/M/D" Date ? Field observation start UT date 56- 61 F6.2 deg RAdeg ? Aim point Right Ascension (J2000) 63- 68 F6.2 deg DEdeg ? Aim point Declination (J2000) 70- 75 F6.1 ks Exp [1.8/1104] Exposure time (2) 77- 78 I2 --- N [0/12]? Number of serendipitous sources detected 80 I1 --- A15 [0/1]? Aird+ 2015ApJ...815...66A flag (3) 82 I1 --- H16 [0/1]? Harrison+ 2016ApJ...831..185H flag (3)
Note (1): For fields with multiple NuSTAR exposures (i.e., Nobs>1), each individual component exposure is listed with a letter suffixed to the field ID (e.g., 3a and 3b). Note (2): For a single focal plane module (i.e., averaged over FPMA and FPMB). Note (3): Binary flags to highlight the serendipitous survey fields used for the Aird+ 2015ApJ...815...66A and Harrison+ 2016ApJ...831..185H studies.
Byte-by-byte Description of file: table5.dat
Bytes Format Units Label Explanations
1- 3 I3 --- Seq [1/498] Running sequence number 5- 10 A6 --- --- [NuSTAR] 11- 24 A14 --- NuSTAR Unique NuSTAR source name (JHHMMSS+DDMM.m) 26- 35 F10.6 deg RAdeg Right Ascension in decimal degrees (J2000) 37- 46 F10.6 deg DEdeg Declination in decimal degrees (J2000) 48 I1 --- SFl [0/1] Soft (3-8keV) band detection flag (1) 50 I1 --- HFl [0/1] Hard (8-24keV) band detection flag (1) 52 I1 --- FFl [0/1] Full (3-24keV) band detection flag (1) 54 I1 --- SdbFl [0/1] Deblended soft band detection flag (2) 56 I1 --- HdbFl [0/1] Deblended hard band detection flag (2) 58 I1 --- FdbFl [0/1] Deblended full band detection flag (2) 60- 67 F8.3 [-] logSP [-44/-0.003]?=-999 Log of soft band false probability; Section 2.3 69- 76 F8.3 [-] logHP [-42/-0.03]?=-999 Log of hard band false probability; Section 2.3 78- 85 F8.3 [-] logFP [-44/-1.7]?=-999 Log of full band false probability; Section 2.3 87- 94 F8.3 [-] logSdbP [-306/-0.003]?=-999 Log of deblended soft band false probability 96-103 F8.3 [-] logHdbP [-231/-0.03]?=-999 Log of deblended hard band false probability 105-112 F8.3 [-] logFdbP [-246/-1.7]?=-999 Log of deblended full band false probability 114 I1 --- dbFl [0/1] Source remains significant after deblending flag (3) 116-122 F7.1 ct Scts [8/11132] Total soft (3-8keV) band counts (4) 124-130 F7.3 ct e_Scts [3/107] The 84% confidence level in Scts 132-139 F8.3 ct SBck [10/2568] Soft background counts scaled to source aperture (4) 141-148 F8.3 ct SNet [5/9881] Net soft (3-8keV) band counts; Scts-SBck (4) 150-156 F7.3 ct e_SNet [-99/107] The error in SNet (5) 158-163 F6.1 ct Hcts [15/6680] Total hard (8-24keV) band counts (4) 165-170 F6.3 ct e_Hcts [4/83] The 84% confidence level in Hcts 172-179 F8.3 ct HBck [7/1620] Hard background counts scaled to source aperture (4) 181-188 F8.3 ct HNet [5/5854] Net hard (8-24keV) band counts; Hcts-HBck (4) 190-196 F7.3 ct e_HNet [-99/83] The error in HNet (5) 198-204 F7.1 ct Fcts [32/17765] Total full (3-24keV) band counts (4) 206-212 F7.3 ct e_Fcts [6/135] The 84% confidence level in Fcts 214-221 F8.3 ct FBck [18/4178] Full background counts scaled to source aperture (4) 223-231 F9.3 ct FNet [18/15694] Net full (3-24keV) band counts; Fcts-FBck (4) 233-239 F7.3 ct e_FNet [-99/135] The error in FNet (5) 241-247 F7.1 ct Sdbcts [8/11132] Total deblended soft band counts (4) 249-256 F8.3 ct e_Sdbcts [10/2568] The 84% confidence level in Sdbcts 258-265 F8.3 ct SdbNet [5/9881] Net deblended soft band counts; Sdbcts-SdbBck (4) 267-273 F7.3 ct e_SdbNet [-99/107] The error in SdbNet (5) 275-280 F6.1 ct Hdbcts [15/6680] Total deblended hard band counts (4) 282-289 F8.3 ct e_Hdbcts [7/1620] The 84% confidence level in Hdbcts 291-298 F8.3 ct HdbNet [5/5854] Net deblended hard band counts; Hdbcts-HdbBck (4) 300-306 F7.3 ct e_HdbNet [-99/83] The error in HdbNet (5) 308-314 F7.1 ct Fdbcts [32/17765] Total deblended full band counts (4) 316-323 F8.3 ct e_Fdbcts [18/4178] The 84% confidence level in Fdbcts 325-333 F9.3 ct FdbNet [18/15694] Net deblended full band counts; Fdbcts-FdbBck (4) 335-341 F7.3 ct e_FdbNet [-99/135] The error in FdbNet (5) 343-351 F9.1 s Sexp [12556/] Soft band exposure time (6) 353-361 F9.1 s Hexp [10166/] Hard band exposure time (6) 363-371 F9.1 s Fexp [10172/] Full band exposure time (6) 373-381 E9.3 ct/s SCR [0.0004/0.06] Total soft band count rate (7) 383-391 E9.3 ct/s e_SCR [/0.002] The 84% confidence level in SCR 393-401 E9.3 ct/s SCRBck [0.0004/0.007] Soft background count rate (7) 403-411 E9.3 ct/s SNCR [/0.06] Net soft count rate (7) 413-422 E10.3 ct/s e_SNCR [-99/0.002] The error in SNCR (5) 424-432 E9.3 ct/s HCR [0.0005/0.05] Total hard band count rate (7) 434-442 E9.3 ct/s e_HCR [/0.001] The 84% confidence level in HCR 444-452 E9.3 ct/s HCRBck [0.0006/0.005] Hard background count rate (7) 454-462 E9.3 ct/s HNCR [/0.04] Net hard count rate (7) 464-473 E10.3 ct/s e_HNCR [-99/0.001] The error in HNCR (5) 475-483 E9.3 ct/s FCR [0.001/0.2] Total full band count rate (7) 485-493 E9.3 ct/s e_FCR [/0.002] The 84% confidence level in FCR 495-503 E9.3 ct/s FCRBck [0.001/0.02] Full background count rate (7) 505-513 E9.3 ct/s FNCR [0.0001/0.1] Net full count rate (7) 515-524 E10.3 ct/s e_FNCR [-99/0.002] The error in FNCR (5) 526-534 E9.3 ct/s SdbNCR [/0.06] Deblended net soft count rate (7) 536-545 E10.3 ct/s e_SdbNCR [-99/0.002] The 84% confidence level in SdbNCR 547-555 E9.3 ct/s HdbNCR [/0.04] Deblended net hard count rate (7) 557-566 E10.3 ct/s e_HdbNCR [-99/0.001] The 84% confidence level in HdbNCR 568-576 E9.3 ct/s FdbNCR [0.0001/0.1] Deblended net full count rate (7) 578-587 E10.3 ct/s e_FdbNCR [-99/0.002] The 84% confidence level in FdbNCR 589-593 F5.3 --- H/S [/7.5]?=0 Hard to Soft band ratio 595-601 F7.3 --- E_H/S [-99/1] Upper error on H/S (8) 603-609 F7.3 --- e_H/S [-99/1] Lower error on H/S (8) 611-616 F6.3 --- gamma [-0.5/3]? Effective photon index 618-624 F7.3 --- E_gamma [-99/1]? Upper error on gamma (8) 626-632 F7.3 --- e_gamma [-99/0.6]? Lower error on gamma (8) 634-642 E9.3 mW/m2 SFlux Observed-frame soft flux (9) 644-653 E10.3 mW/m2 e_SFlux ?=-99 The 84% confidence level in SFlux 655-663 E9.3 mW/m2 HFlux Observed-frame hard flux (9) 665-674 E10.3 mW/m2 e_HFlux ?=-99 The 84% confidence level in HFlux 676-684 E9.3 mW/m2 FFlux Observed-frame full flux (9) 686-695 E10.3 mW/m2 e_FFlux ?=-99 The 84% confidence level in FFlux 697-704 A8 --- XOrig Soft X-ray counterpart code (10) 706-715 F10.6 deg RAXdeg ? Soft X-ray counterpart Right Ascension in decimal degrees (J2000) 717-726 F10.6 deg DEXdeg ? Soft X-ray counterpart Declination in decimal degrees (J2000) 728-732 F5.2 arcsec XOff [0.5/37]? Soft X-ray and NuSTAR position offset 734-742 E9.3 mW/m2 XFlux [0/2e-12]? Observed-frame 3-8 keV X-ray counterpart flux (11) 744-752 E9.3 mW/m2 XTFlux [0/2e-12]? Total combined 3-8 keV X-ray flux within 30" of NUSTAR 754-763 F10.6 deg RAWdeg ? WISE counterpart Right Ascension in decimal degrees (J2000) 765-774 F10.6 deg DEWdeg ? WISE counterpart Declination in decimal degrees (J2000) 776-780 F5.3 arcsec IROff [0.05/6]? WISE and NuSTAR position offset 782-787 F6.3 mag W1mag [5.6/18.8]? WISE W1 band, 3.4um, profile-fit Vega magnitude 789-793 F5.3 mag e_W1mag [0.02/0.3]? Error in W1mag (12) 795-800 F6.3 mag W2mag [3.8/17.4]? WISE W2 band, 4.6um, profile-fit Vega magnitude 802-806 F5.3 mag e_W2mag ? Error in W2mag (12) 808-813 F6.3 mag W3mag [4/14]? WISE W3 band, 12 micron, profile-fit Vega magnitude 815-819 F5.3 mag e_W3mag ? Error in W3mag (12) 821-826 F6.3 mag W4mag [1.7/10.2]? WISE W4 band, 22um, profile-fit Vega magnitude 828-832 F5.3 mag e_W4mag ? Error in W4mag (12) 834-842 A9 --- OOrig Adopted optical counterpart code (13) 844-855 F12.8 deg RAOdeg ? Optical counterpart Right Ascension in decimal degrees (J2000) 857-868 F12.8 deg DEOdeg ? Optical counterpart Declination in decimal degrees (J2000) 870-874 F5.3 arcsec OOff [0.02/6]? Optical and NuSTAR position offset 876-882 F7.3 mag Rmag [-99/24.3]? Optical counterpart R band Vega magnitude (14) 884-888 F5.3 --- zsp [0/3.5]? Spectroscopic redshift (15) 890-899 E10.3 10-7W XLum ? Rest-frame 10-40 keV luminosity (16) 901 I1 --- PFl [0/1] Source associated with primary science target (17) 903 I1 --- A15Fl [0/1] Aird+ 2015ApJ...815...66A flag (18)
Note (1): A binary flag indicating whether the source is detected with a false probability lower than our threshold of log(PFalse)=-6. Note (2): Same as previous columns but after deblending has been performed to account for contamination of the source counts from very nearby sources (see Section 2.4 of this paper, and Section 2.3.2 of Mullaney+ (2015, J/ApJ/808/184). Deblending only affects a very small fraction of the overall sample (e.g., see Section 2.4). Note (3): A binary flag indicating whether the NuSTAR detected source remains significant after deblending, in at least one of the three standard energy bands. Note (4): Calculated at the source coordinates, and using a source aperture of 30" radius (see Section 2.4). The values are non-aperture-corrected; i.e., they correspond to the 30" values, and have not been corrected to the full PSF values. Note (5): For the net source counts, we give 90% CL upper limits for sources not detected in a given band. Throughout the table, upper limits are flagged with a -99 value in the error column. Note (6): The average net, vignetting-corrected exposure time at the source coordinates. These correspond to the A+B data, so should be divided by two to obtain the average exposure per FPM. Note (7): Non-aperture-corrected. Determined from the photometric values and the exposure times. Note (8): Upper limits, lower limits, and sources with no constraints are flagged with -99, -88, and -77 values, respectively, in the error columns. Note (9): After deblending has been performed. These are aperture corrected values (i.e., they correspond to the full NuSTAR PSF), and are calculated from the count rates using the conversion factors listed in Section 2.4. Note (10): An abbreviated code indicating the origin of the adopted soft (i.e., low energy; <10keV) X-ray counterpart. Code as follows: CXO_CSC = counterparts from the Chandra Source Catalog (CSC; 82 occurrences; Evans+ 2010, Cat. IX/45). XMM_3XMM = counterparts from the third XMM-Newton serendipitous source catalog (3XMM; 203 occurrences; Watson+ 2009, J/A+A/493/339 ; Rosen+ 2016, IX/50). CXO_MAN = sources manually identified using archival Chandra (27 occurrences) XMM_MAN = sources manually identified using archival XMM-Newton (24 occurrences) XRT_MAN = sources manually identified using archival Swift XRT data (60 occurrences). Section 3.1 details the counterpart matching. Note (11): For sources with counterparts in the CSC and 3XMM catalogs. For CSC sources we convert to the 3-8keV flux from the 2-7keV flux using a conversion factor of 0.83, and for the 3XMM sources we convert from the 4.5-12keV flux using a conversion factor of 0.92. Note (12): Blanks in the errors indicates the magnitude is a WISE upper limit. Note (13): An abbreviated code indicating the origin of the adopted optical counterpart to the NuSTAR source. Code as follows: SDSS = sources with soft X-ray counterparts and successful matches in the SDSS DR7 catalog (York+ 2000AJ....120.1579Y); 127 occurrences USNO = sources with soft X-ray counterparts and successful matches in the USNOB1 catalog (Monet+ 2003, I/284); 166 occurrences MAN = sources with a soft X-ray counterpart and a corresponding optical counterpart manually identified in the available optical coverage; 181 occurrences SDSS_WISE = there is no soft X-ray counterpart to the NuSTAR position, but a WISE AGN candidate is identified within the NuSTAR error circle and successfully matched to the SDSS DR7 (these are mainly used as candidates for spectroscopic followup); 11 occurrences. USNO_WISE = there is no soft X-ray counterpart to the NuSTAR position, but a WISE AGN candidate is identified within the NuSTAR error circle and successfully matched to the USNOB1 catalog (these are mainly used as candidates for spectroscopic followup; 6 occurrences). We give a detailed description of the procedure used to identify optical counterparts in Section 3.2. Note (14): For the SDSS DR7 matches, this is calculated as R=r-0.16. For the USNOB1 matches, this is taken as the mean of the two independent photographic plate measurements, R1mag and R2mag. For the manual identifications, the magnitude is taken from another optical catalog or manually determined from the imaging data. Note (15): The large majority of the redshifts were obtained through our own campaign of ground-based spectroscopic followup of NuSTAR serendipitous survey sources (see Section 3.3.1 and the "Description" section above). Note (16): Estimated from the observed-frame fluxes, following the procedure outlined in Section 2.4. Negative values indicate upper limits. The luminosities are observed values, uncorrected for any absorption along the line of sight. The intrinsic luminosities may therefore be higher, for highly absorbed AGNs. Note (17): A binary flag indicating the few sources which show evidence for being associated with the primary science targets of their respective NuSTAR observations, according to the definition in Section 2.3 [Δ(cz)<0.05cz]. Note (18): A binary flag highlighting the sources used in the Aird+ (2015ApJ...815...66A) study.
Byte-by-byte Description of file: table.dat
Bytes Format Units Label Explanations
1- 3 I3 --- Seq [1/498] Unique source identification number 5- 10 A6 --- --- [NuSTAR] 11- 24 A14 --- NuSTAR Unique NuSTAR source name (JHHMMSS+DDMM.m) 26- 30 F5.3 --- z [0/3.5]? Source spectroscopic redshift 32- 38 A7 --- Type Classification (1) 41-162 A122 --- Lines Emission/absorption lines identified (2) 164-231 A68 --- Notes Source notes and literature spectra references 233-234 A2 --- Run Unique observing run identification number (3)
Note (1): Classification (for primary sources) as follows: BL = broad-line AGN (151 occurrences + 11 BL?) NL = narrow-line AGN (84 occurrences + 13 NL?) BL Lac? = BL Lac object candidate (1 occurrence) Gal = galaxies (16 occurrences) See Section 3.3.2 for further details. Note (2): Absorption line/feature marked with "dg" footnote. Note (3): As defined in Table 4 ("S" and "L" mark spectra obtained from the SDSS and from elsewhere in the literature, respectively).
Byte-by-byte Description of file: table7.dat
Bytes Format Units Label Explanations
1- 2 I2 --- Seq [1/64] Unique source identification number 4- 9 A6 --- --- [NuSTAR] 10- 23 A14 --- NuSTAR Unique NuSTAR source name (JHHMMSS+DDMM.m) 25- 34 F10.6 deg RAdeg Right Ascension in decimal degrees (J2000) 36- 45 F10.6 deg DEdeg Declination in decimal degrees (J2000) 47- 54 F8.3 ct Scts [36/7049]? Total soft band (3-8keV) counts (1) 56- 63 F8.3 ct SBck ? Soft background counts (1) 65- 72 F8.3 ct SNet [16/6633]? Net soft band counts (1) 74- 80 F7.3 ct e_SNet [-99/85]? The error in SNet (2) 82- 89 F8.3 ct Hcts ? Total hard band (8-24 keV) counts (1) 91- 98 F8.3 ct HBck ? Hard background counts (1) 100-107 F8.3 ct HNet [13/4306]? Net hard band counts (1) 109-115 F7.3 ct e_HNet [-99/69]? The error in HNet (2) 117-125 F9.3 ct Fcts [85/11617]? Total full band (3-24keV) counts (1) 127-134 F8.3 ct FBck ? Full background counts (1) 136-144 F9.3 ct FNet [22/10900]? Net full band counts (1) 146-152 F7.3 ct e_FNet [-99/109]? The error in FNet (2) 154-161 F8.1 s Sexp [14375/643091]? Soft band exposure time (3) 163-170 F8.1 s Hexp ? Hard band exposure time (3) 172-179 F8.1 s Fexp ? Full band exposure time (3) 181-189 E9.3 ct/s SNCR [0.0003/0.5]? Net soft count rate, aperture-corrected (4) 191-200 E10.3 ct/s e_SNCR [-99/0.006]? The error in SNCR (2) 202-210 E9.3 ct/s HNCR [0.0003/0.4]? Net hard count rate, aperture-corrected (4) 212-221 E10.3 ct/s e_HNCR [-99/0.006]? The error in HNCR (2) 223-231 E9.3 ct/s FNCR [0.0005/1]? Net full count rate, aperture-corrected (4) 233-242 E10.3 ct/s e_FNCR [-99/0.01]? The error in FNCR (2) 244-252 E9.3 mW/m2 SFlux ? Observed-frame soft flux (5) 254-263 E10.3 mW/m2 e_SFlux [-99/]? The 84% confidence level in SFlux 265-273 E9.3 mW/m2 HFlux ? Observed-frame hard flux (5) 275-284 E10.3 mW/m2 e_HFlux [-99/]? The 84% confidence level in HFlux 286-294 E9.3 mW/m2 FFlux ? Observed-frame full flux (5) 296-305 E10.3 mW/m2 e_FFlux [-99/]? The 84% confidence level in FFlux 307-309 A3 --- XName Lower energy X-ray counterpart observatory name 311-320 F10.6 deg RAXdeg ? Lower energy X-ray counterpart Right Ascension in decimal degrees (J2000) 322-331 F10.6 deg DEXdeg ? Lower energy X-ray counterpart Declination in decimal degrees (J2000) 333-336 A4 --- OName Other, optical or WISE, counterpart observatory name 338-347 F10.6 deg RAOdeg ? Other counterpart Right Ascension in decimal degrees (J2000) 349-358 F10.6 deg DEOdeg ? Other counterpart Declination in decimal degrees (J2000) 360-364 F5.3 --- zsp [0/1.9]? Spectroscopic redshift (6) 366-375 E10.3 10-7W XLum ? Non-absorption-corrected, rest-frame 10-40keV luminosity (7) 377 A1 --- Fl Primary catalog code (8)
Note (1): Calculated at the source coordinates. The values are non-aperture-corrected. Note (2): For the net source counts, we give 90% CL upper limits for sources not detected in a given band. Throughout the table, upper limits are flagged with a -99 value in the error column. The photometric columns are blank where the A+B data prohibit reliable photometric constraints. Note (3): The average net, vignetting-corrected exposure time at the source coordinates. These correspond to the A+B data, so should be divided by two to obtain the average exposure per FPM. Note (4): Determined from the photometric values and the exposure times. Note (5): After deblending has been performed. These are aperture corrected values (i.e., they correspond to the full NuSTAR PSF), and are calculated from the count rates using the conversion factors listed in Section 2.4. Note (6): The large majority of the redshifts were obtained through our own campaign of ground-based spectroscopic followup of NuSTAR serendipitous survey sources (see Section 3.3.1 and the "Description" section above). Note (7): Estimated from the observed-frame fluxes, following the procedure outlined in Section 2.4. Negative values indicate upper limits. The luminosities are observed values, uncorrected for any absorption along the line of sight. The intrinsic luminosities may therefore be higher, for highly absorbed AGNs. Note (8): A character indicating the reason for not being included in the primary catalog. These are categorised into four groups as follows: E = the source is within or very close to the peripheral region of the NuSTAR mosaic, which is excluded from the primary source detection (33% of cases); T = the source is narrowly offset from the central science target position for the NuSTAR observation (and thus automatically excluded; see Section 2.3), or from another bright source in the field (11%); X = the source lies in a region which is masked out, or in a NuSTAR field which is excluded, from the primary source detection (44%; e.g., due to highly contaminating stray light or a bright science target); or L = the source has a comparatively low detection significance (12%).
History: From electronic version of the journal
(End) Prepared by [AAS], Emmanuelle Perret [CDS] 15-Sep-2017
|The document above follows the rules of the Standard Description for Astronomical Catalogues.From this documentation it is possible to generate f77 program to load files into arrays or line by line|