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 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 =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 2015ApJ...815...66A flag (3)
82 I1 --- H16 [0/1]? Harrison+ 2016ApJ...831..185H 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 2015ApJ...815...66A and Harrison+ 2016ApJ...831..185H 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 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 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 2015ApJ...815...66A) study.
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Byte-by-byte Description of file: table[68].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)
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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 = Galactic objects (z=0; 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).
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Byte-by-byte Description of file: table7.dat
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Bytes Format Units Label Explanations
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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)
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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%).
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History:
From electronic version of the journal
(End) Prepared by [AAS], Emmanuelle Perret [CDS] 15-Sep-2017