J/ApJ/850/66 Stripe 82X survey multiwavelength catalog (Ananna+, 2017)
AGN populations in large-volume X-ray surveys:
photometric redshifts and population types found in the Stripe 82X survey.
Ananna T.T., Salvato M., Lamassa S., Urry C.M., Cappelluti N.,
Cardamone C., Civano F., Farrah D., Gilfanov M., Glikman E., Hamilton M.,
Kirkpatrick A., Lanzuisi G., Marchesi S., Merloni A., Nandra K.,
Natarajan P., Richards G.T., Timlin J.
<Astrophys. J., 850, 66-66 (2017)>
=2017ApJ...850...66A 2017ApJ...850...66A (SIMBAD/NED BibCode)
ADC_Keywords: Galaxy catalogs ; Active gal. nuclei ; X-ray sources ; Redshifts ;
Photometry, SDSS ; Photometry, infrared ; Ultraviolet
Keywords: catalogs - quasars: absorption lines - quasars: emission lines -
quasars: general - techniques: photometric - techniques: spectroscopic
Abstract:
Multiwavelength surveys covering large sky volumes are necessary to
obtain an accurate census of rare objects such as high-luminosity
and/or high-redshift active galactic nuclei (AGNs). Stripe 82X is a
31.3 X-ray survey with Chandra and XMM-Newton observations overlapping
the legacy Sloan Digital Sky Survey Stripe 82 field, which has a rich
investment of multiwavelength coverage from the ultraviolet to the
radio. The wide-area nature of this survey presents new challenges for
photometric redshifts for AGNs compared to previous work on
narrow-deep fields because it probes different populations of objects
that need to be identified and represented in the library of
templates. Here we present an updated X-ray plus multiwavelength
matched catalog, including Spitzer counterparts, and estimated
photometric redshifts for 5961 (96% of a total of 6181) X-ray sources
that have a normalized median absolute deviation, σnmad=0.06,
and an outlier fraction, η=13.7%. The populations found in this
survey and the template libraries used for photometric redshifts
provide important guiding principles for upcoming large-area surveys
such as eROSITA and 3XMM (in X-ray) and the Large Synoptic Survey
Telescope (optical).
Description:
We fitted SED templates to 5961 X-ray objects (96.4%) in the Stripe
82X survey (LaMassa et al. 2013, Cat. J/MNRAS/436/3581,
2013MNRAS.432.1351L 2013MNRAS.432.1351L, 2016, J/ApJ/817/172) and calculated photometric
redshifts with an outlier fraction of 13.69% and a σnmad
of 0.06. This is the largest-volume X-ray survey to date for which
photometric redshifts have been calculated, and as such, it has given
us important insights, such as optimizing template selection for the
higher-flux population found in large-area, shallow surveys.
File Summary:
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FileName Lrecl Records Explanations
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ReadMe 80 . This file
table13.dat 1475 6181 Catalog (final version, 21/08/2019)
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See also:
J/ApJS/219/39 : QSOs selection from SDSS and WISE (Richards+, 2015)
J/ApJ/817/172 : X-ray Observations of Stripe 82 (LaMassa+, 2016)
J/MNRAS/456/1359 : IAC Stripe 82 Legacy Project: Photometry (Fliri+, 2016)
J/ApJS/225/1 : SpIES: the Spitzer IRAC Equatorial Survey (Timlin+, 2016)
Byte-by-byte Description of file: table13.dat
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Bytes Format Units Label Explanations
--------------------------------------------------------------------------------
1- 6 I6 --- ID ID number for each source as assigned in
LM16 (Lamassa et al. 2016,
Cat. J/ApJ/817/172)
8- 19 A12 --- Cat Name of the original X-ray survey from
Lamassa et al. 2016, Cat. J/ApJ/817/172
(AO10, AO13, Chandra) or archival XMM
21- 40 F20.16 deg RAdeg Rigth ascension (J2000) of X-ray source
42- 63 E22.15 deg DEdeg Declination (J2000) of X-ray source
65- 75 F11.8 deg ePos Error in position of X-ray source
77- 98 E22.15 10-17W/m2 FSoft ?=0 X-ray flux in 0.5-2keV band
100- 123 E24.19 --- SoftDetml ?=0 Significance of detection in 0.5-2keV
band: detml = -ln(Prandom)
125- 146 E22.15 10-17W/m2 FHard ?=0 X-ray flux in 2-10 keV band
148- 169 E22.15 10-17W/m2 FFull ?=0 Total X-ray flux in 0.5-10 keV band
171- 178 A8 --- AssocCat This field indicates how many catalogs
agree that the association we selected
for the X-ray object is the correct
association (1)
180- 184 A5 --- r_RAcdeg When we select RA and DE for the best
X-ray association, we look at all the
catalogs that agree and choose
coordinates from the one with the best
astrometric accuracy (SDSS, than VHS,
than IRAC)
186- 205 F20.16 deg RAcdeg ?=-99 Right ascension of the best
associations for the X-ray object
207- 228 E22.15 deg DEcdeg ?=-99 Declination of the best
associations for the X-ray object
230- 232 F3.1 --- QF Quality flag (2)
234- 236 I3 --- Nearobj ?=-99 Number of nearby objects with 6"
238- 251 F14.10 arcsec DXrayCtp ?=-99 Distance between X-ray coordinates
and counterparts
253- 265 A13 --- SDSSClass Reliability class for SDSS, counterpart
(Secure/Ambiguous/Sub-threshold)
267- 279 A13 --- VHSClass Reliability class VHS counterpart
(Secure/Ambiguous/Sub-threshold)
281- 293 A13 --- IRACClass Reliability class for IRAC counterpart
(Secure/Ambiguous/Sub-threshold)
295- 304 F10.6 mag FUVmag ?=-99 Extinction-corrected GALEX FUV
SEXTRACTOR AUTO magnitude (AB)
306- 319 F14.10 mag e_FUVmag ?=-99 Extinction-corrected GALEX FUV
SEXTRACTOR AUTO magnitude error (AB)
321- 331 F11.7 mag NUVmag ?=-99 Extinction-corrected GALEX NUV
SEXTRACTOR AUTO magnitude (AB)
333- 344 E12.10 mag e_NUVmag ?=-99 Extinction-corrected GALEX NUV
SEXTRACTOR AUTO magnitude error (AB)
346- 356 F11.7 mag umag ?=-99 SDSS coadded (SEXTRACTOR AUTO)
u magnitude (4)
358- 365 E8.4 mag e_umag ?=-99 SDSS coadded (SEXTRACTOR AUTO)
u magnitude error (4)
367- 377 F11.7 mag gmag ?=-99 SDSS coadded (SEXTRACTOR AUTO)
g magnitude (4)
379- 384 E6.2 mag e_gmag ?=-99 SDSS coadded (SEXTRACTOR AUTO)
g magnitude error (4)
386- 396 F11.7 mag rmag ?=-99 SDSS coadded (SEXTRACTOR AUTO)
r magnitude (4)
398- 403 E6.2 mag e_rmag ?=-99 SDSS coadded (SEXTRACTOR AUTO)
r magnitude error (4)
405- 415 F11.7 mag imag ?=-99 SDSS coadded (SEXTRACTOR AUTO)
i magnitude (4)
417- 422 E6.2 mag e_imag ?=-99 SDSS coadded (SEXTRACTOR AUTO)
i magnitude error (4)
424- 434 F11.7 mag zmag ?=-99 SDSS coadded (SEXTRACTOR AUTO)
z magnitude (4)
436- 443 E8.4 mag e_zmag ?=-99 SDSS coadded (SEXTRACTOR AUTO)
z magnitude error (4)
445- 455 F11.7 mag Jmag ?=-99 Extinction-corrected J magnitude
from the VISTA VHS survey (5)
457- 468 E12.8 mag e_Jmag ?=-99 Extinction-corrected J magnitude
error from the VISTA VHS survey (5)
470- 480 F11.7 mag Hmag ?=-99 Extinction-corrected H magnitude
from the VISTA VHS survey (5)
482- 493 E12.8 mag e_Hmag ?=-99 Extinction-corrected H magnitude
error from the VISTA VHS survey (5)
495- 505 F11.7 mag Kmag ?=-99 Extinction-corrected K magnitude
from the ISTA VHS survey (5)
507- 518 E12.8 mag e_Kmag ?=-99 Extinction-corrected K magnitude
error from the VISTA VHS survey (5)
520- 530 F11.7 mag JmagUK ?=-99 Extinction-corrected J magnitude
from the UKIDSS Large Area Survey
catalog (5)
532- 543 E12.8 mag e_JmagUK ?=-99 Extinction-corrected J magnitude
error from the UKIDSS LAS catalog (5)
545- 555 F11.7 mag HmagUK ?=-99 Extinction-corrected H magnitude
from the UKIDSS Large Area Survey
catalog (5)
557- 568 E12.8 mag e_HmagUK ?=-99 Extinction-corrected H magnitude
error from the UKIDSS LAS catalog (5)
570- 580 F11.7 mag KmagUK ?=-99 Extinction-corrected K magnitude
from the UKIDSS LAS catalog (5)
582- 593 E12.8 mag e_KmagUK ?=-99 Extinction-corrected K magnitude
error from the UKIDSS LAS catalog (5)
595- 605 F11.7 mag IRAC1Sp ?=-99 IRAC CH1 magnitude (SEXTRACTOR
AUTO; not extinction-corrected) from
Timlin et al. (2016, J/ApJS/225/1)
607- 618 E12.8 mag e_IRAC1Sp ?=-99 IRAC1 magnitude error (SEXTRACTOR
AUTO; not extinction-corrected) from
Timlin et al. (2016, J/ApJS/225/1)
620- 630 F11.7 mag IRAC2Sp ?=-99 IRAC2 magnitude (SEXTRACTOR AUTO;
not extinction-corrected) from
Timlin et al. (2016, J/ApJS/225/1)
632- 643 E12.8 mag e_IRAC2Sp ?=-99 IRAC2 magnitude error (SEXTRACTOR
AUTO; not extinction-corrected) from
Timlin et al. (2016, J/ApJS/225/1)
645- 655 F11.7 mag IRAC1Sh ?=-99 IRAC1 magnitude (SEXTRACTOR
AUTO; not extinction-corrected) from
Papovich et al. (2016ApJS..224...28P 2016ApJS..224...28P)
657- 668 E12.8 mag e_IRAC1Sh ?=-99 IRAC1 magnitude error (SEXTRACTOR
AUTO; not extinction-corrected) from
Papovich et al. (2016ApJS..224...28P 2016ApJS..224...28P)
670- 680 F11.7 mag IRAC2Sh ?=-99 IRAC2 magnitude (SEXTRACTOR
AUTO; not extinction-corrected) from
Papovich et al. (2016ApJS..224...28P 2016ApJS..224...28P)
682- 693 E12.8 mag e_IRAC2Sh ?=-99 IRAC2 magnitude error (SEXTRACTOR
AUTO; not extinction-corrected) from
Papovich et al. (2016ApJS..224...28P 2016ApJS..224...28P)
695- 705 F11.7 mag W1mag ?=-99 AllWISE (mpro) W1 magnitude
(not extinction-corrected)
707- 713 F7.3 mag e_W1mag ?=-99 AllWISE (mpro) W1 magnitude error
(not extinction-corrected)
715- 725 F11.7 mag W2mag ?=-99 AllWISE (mpro) W2 magnitude
(not extinction-corrected)
727- 733 F7.3 mag e_W2mag ?=-99 AllWISE (mpro) W2 magnitude error
(not extinction-corrected)
735- 740 I6 --- Context LePhare needs this field to understand
which filters to use to calculate
photometry (6)
742- 753 E12.8 --- zsp ?=-99 Spectroscopic redshift
755- 775 E21.9 --- e_zsp []?=-99 Spectroscopic redshift error
777- 803 A27 --- r_zsp Source of spectroscopic data
(e.g., SDSS DR13, DR12Q)
805- 827 A23 --- ObjId SDSS spectra object ID DR12Q, DR13, DR14
830- 836 A7 --- SpClass SDSS spectroscopic classification of
this object
838- 858 A21 --- Subclass SDSS Additional spectroscopic data on
object type
860- 862 I3 --- zwarning ?=-99 Warning on redshift. Only
ZWARNING = 0 was used in our training
sample
864- 874 F11.7 mag W3mag ?=-99 AllWISE (mpro) W3 magnitude
(not extinction-corrected) (7)
876- 882 F7.3 mag e_W3mag ?=-99 AllWISE (mpro) W3 magnitude error
(not extinction-corrected) (7)
884- 894 F11.7 mag W4mag ?=-99 AllWISE (mpro) W4 magnitude
(not extinction-corrected) (7)
896- 902 F7.3 mag e_W4mag ?=-99 AllWISE (mpro) W4 magnitude error
(not extinction-corrected) (7)
904- 905 I2 --- Nfilter [0/12] Number of filters
907- 909 I3 --- Fliriflag ?=-99 SEXTRACTOR extraction flag from
FT16 (Fliri & Trujillo, 2016,
J/MNRAS/456/1359) catalog
911- 914 A4 --- r_ExtCorr Extinction correction origin (8)
916- 918 I3 --- NUVart ?=-99 GALEX NUV artifact flags (9)
920- 922 I3 --- FUVart ?=-99 GALEX FUV artifact flags (9)
924- 943 F20.16 pix FWHMNUV ?=-99 FWHM for GALEX NUV,
measured in pixels
945- 965 F21.17 pix FWHMFUV ?=-99 FWHM for GALEX FUV,
measured in pixels
967- 969 I3 --- FlagNUV ?=-99 SEXTRACTOR flags for NUV
971- 973 I3 --- FlagFUV ?=-99 SEXTRACTOR flags for FUV
975- 977 I3 --- GCLass ?=-99 GALEX object classification
979- 981 I3 --- GFlag ?=-99 GALEX manual flag
983- 995 F13.9 pix uFWHM ?=-99 FWHM for u SDSS band from Jiang et
al. (2014ApJS..213...12J 2014ApJS..213...12J, J14)
997-1008 F12.8 pix gFWHM ?=-99 FWHM for g SDSS band from Jiang et
al. (2014ApJS..213...12J 2014ApJS..213...12J, J14)
1010-1022 F13.9 pix RFWHM ?=-99 FWHM for r SDSS band from Jiang et
al. (2014ApJS..213...12J 2014ApJS..213...12J, J14)
1024-1035 F12.8 pix iFWHM ?=-99 FWHM for i SDSS band from Jiang et
al. (2014ApJS..213...12J 2014ApJS..213...12J, J14)
1037-1048 F12.8 pix zFWHM ?=-99 FWHM for z SDSS band from Jiang et
al. (2014ApJS..213...12J 2014ApJS..213...12J, J14)
1050-1058 E9.5 --- NNV ?=-99 Variability information for optical
sources, varies from 0 to 1
(-1 for completely nonvarying sources)
1060-1062 I3 --- VHSMClass ?=-99 Class flag from available
measurements (10)
1064-1075 E12.8 --- VHSPstar ?=-99 VHS pipeline probability that an
object is a star
1077-1088 E12.8 --- VHSpgal ?=-99 VHS pipeline probability that an
object is a galaxy
1090-1092 I3 --- IRAC1FlgSp ?=-99 SEXTRACTOR flags for IRAC1
1094-1096 I3 --- IRAC2FlgSp ?=-99 SEXTRACTOR flags for IRAC2
1098-1109 E12.8 --- ClassSp ?=-99 SpIES object classification
1111-1115 F5.1 --- RelIRAC1Sp ?=-99 Reliability of IRAC1 SpIES
(Timlin et al. 2016, J/ApJS/225/1) data
1117-1121 F5.1 --- RelIRAC2Sp ?=-99 Reliability of IRAC2 SpIES
(Timlin et al. 2016, J/ApJS/225/1) data
1123-1125 I3 --- IRAC1FlgSh ?=-99 Reliability of IRAC1 SHELA
(Papovich et al., 2016ApJS..224...28P 2016ApJS..224...28P)
data
1127-1129 I3 --- IRAC2FlgSh ?=-99 Reliability of IRAC2 SHELA
(Papovich et al., 2016ApJS..224...28P 2016ApJS..224...28P)
data
1131-1143 E13.9 --- XO ?=-99 X-ray-to-optical ratio (11)
1145-1147 A3 --- Coadded Indicates whether the photometry we use
is from FT16 or J14. We prefer FT16 and
use it when available
1149-1151 I3 --- Jiangflag ?=-99 Jiang et al. (2014ApJS..213...12J 2014ApJS..213...12J,
J14) r-band SEXTRACTOR flag
1153-1155 I3 --- NN ?=-99 This is the remainder of the Jiang
et al. (2014ApJS..213...12J 2014ApJS..213...12J)
SEXTRACTOR flag (12)
1157-1166 A10 --- Class Classification according to Figure 10
1168-1170 I3 --- PS [0/1]?=-99 PS code
1172-1179 F8.4 --- zph ?=-99 Best-fit photometric redshift
1181-1188 F8.4 --- e_zph ?=-99 1sigma lower bound on photometric
redshift (68% confidence level)
1190-1197 F8.4 --- E_zph ?=-99 1sigma upper bound on photometric
redshift (68% confidence level)
1199-1206 F8.4 --- zphML ?=-99 Best-fit photometric redshift ML
1208-1215 F8.4 --- e_zphML ?=-99 1sigma lower bound on photometric
redshift ML (68% confidence level)
1217-1224 F8.4 --- E_zphML ?=-99 1sigma upper bound on photometric
redshift ML (68% confidence level)
1226-1236 E11.6 --- Chibest ?=-99 χ2 value for our best-fit SED
1238-1242 F5.1 --- Modbest ?=-99 Best-fit SED
1244-1248 F5.1 --- ExtlawBest [0/1]?=-99 Extinction law used for
best-fit SED (1 for Prevot et al.
1984A&A...132..389P 1984A&A...132..389P and 0 for none)
1250-1255 F6.2 --- EBVbest ?=-99 Color excess for host galaxy of AGN
1257-1263 F7.3 --- PDZbest ?=-99 Described in Section 5. Can also be
taken as LePhare's confidence on zph
1265-1270 F6.2 --- zphsec ?=-99 Secondary redshift for SED with
χ2 value very close to best-fit {
chi}2 value
1272-1282 E11.6 --- Chisec ?=-99 χ2 value for second-best fit
1284-1289 F6.1 --- Modsec ?=-999 SED for second-best fit
1291-1296 F6.2 --- EBVsec ?=-99 Color excess used in second-best
fit
1298-1304 F7.3 --- PDZsec ?=-99 Check Section 3
1306-1315 E10.6 --- Chistar ?=-99 χ2 value for best star
template fit
1317-1319 I3 --- Nband ?=-99 Number of bands used by Lephare to
determine zph
1321 I1 --- Morph [0/7] Morphology according to template
fitting (13)
1323-1325 A3 --- CMorp LaMassa et al. (2016ApJ...818...88L 2016ApJ...818...88L)
color morphology: extragalactic or star
1327-1347 A21 --- SEDname Name of the best-fit template
1349-1354 F6.2 --- zphP ?=-99 Peters et al. (2015ApJ...811...95P 2015ApJ...811...95P)
photometric redshift
1356-1367 F12.8 --- zphB ?=-99 Bovy et al. (2012ApJ...749...41B 2012ApJ...749...41B)
photometric redshift
1369-1375 F7.3 --- zphR ?=-99 Richards et al. (2015,
J/ApJS/219/39) photometric redshift
1377-1397 E21.15 --- LDph ?=0 Luminosity distance calculated using
zph
1399-1416 F18.15 [10-7W] lgLXph ?=0 Full-flux X-ray luminosity calculated
using zph
1418-1438 E21.15 --- LDsp ?=0 Luminosity distance calculated using
zsp
1440-1457 F18.15 [10-7W] lgLXsp ?=0 Full-flux X-ray luminosity calculated
using zsp
1459 I1 --- DupFlag [-2/2] Duplication flag (14)
1461-1467 I7 --- DupID1 ?=9999999 ID of duplicate X-ray source
1469-1475 I7 --- DupID2 ?=9999999 Duplicate X-ray source ID if
there is a second duplicate source
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Note (1): "Sp," "Sh," "V," "F," and "J" stand for SpIES, SHELA, VHS, and SDSS
and coadded catalogs FT16 ((Fliri & Trujillo, 2016, J/MNRAS/456/1359) and
J14 (Jiang et al., 2014ApJS..213...12J 2014ApJS..213...12J), respectively.
"SpVJr" indicates that IRAC, VHS, and J14 (Jiang et al., 2014ApJS..213...12J 2014ApJS..213...12J)
r band agree and there is no conflict with the association of this X-ray
object.
"V" might indicate that we only have VHS data for this object or that we found
a VHS counterpart to be the most likely counterpart.
LM16 indicates that these sources were added from the LM16 catalog (Lamassa
et al., 2016, Cat. J/ApJ/817/172)- we did not find them through our MLE
matches, but these sources exist in SDSS DR13 in at least one single-epoch
frame. Details of how we arrived at these results are discussed in
Section 2.5.
Note (2): this field indicates whether or not there was a conflict in
association. Described in detail in Figure 6.
Note (4): If the field "Coadded" is set to "FT16," the data come from Fliri &
Trujillo, 2016, J/MNRAS/456/1359, and if it is set to "J14," the photometry
comes from Jiang et al. (2014ApJS..213...12J 2014ApJS..213...12J). We allow all photometry
data from the former catalog, and when no photometry is available, we look at
the latter and take all data with SEXTRACTOR flags set to 0 or 2. We tried to
correct for galactic extinction whenever extinction information was available.
If extinction was not available, sdssextcorr is set to "N/A."
Note (5): 2."8 and 5."6 radius aperture magnitude for point-like and extended
sources, respectively.
Note (6): For example, if we just need to use filters FUV (filter number 0),
SDSS i (5), and CH1 SpIES (13), the context is set to 20+25+2^13%.
In the catalogs, we use this column to indicate which bands we used for
final template fitting by LePhare.
Note (7): The W3 and W4 magnitude errors are blank if the profile-fit magnitude
is a 95% confidence upper limit or the source is not measurable
(http://wise2.ipac.caltech.edu/docs/release/allwise/expsup/sec2_1a.html).
Note (8): The coadded SDSS catalogs do not come with extinction information.
At the same time, if we can find an extinction match in SDSS DR7, this field
is set to "SDSS." If we cannot, we use the EBV from the VHS catalog to
calculate extinction, in which case this flag is set to "VHS."
Note (9): as described here:
http://www.galex.caltech.edu/DATA/gr1_docs/GR1Pipelineandadvanceddatadescriptionv2.htm
Note (10): Class flag as follows:
1 = galaxy
-1 = stellar
-2 = probableStar
-3 = probableGalaxy
Note (11): as explained in Appendix C. This ratio is for X-ray hardband
(0.5-2 keV) to SDSS r band.
Note (12): 1 indicates that there is a nearby neighbor bright enough to
significantly impact photometry. We exclude these objects from the training
set. (NearbyNeighborSEXTRACTOR)
Note (13): Morphology code as follows:
1 = Stars
2 = Ellipticals
3 = Spirals
4 = Type 2
5 = Starbursts
6 = Type 1
7 = QSOs
Note (14): Duplication flag as follows:
0 = the object is unique.
1 = one of a duplicate pair of X-ray sources. We identify the same
counterpart for both X-ray observations.
-1 = one of a duplicate pair of X-ray sources. We identify the same
counterpart for both X-ray observations.
2 = duplicate pairs - these sources find different counterparts for
X-ray sources.
-2 = duplicate pairs - these sources find different counterparts for
X-ray sources.
The positive flags (1, 2) indicate more reliable X-ray positions -
we use only values of 0 or above to calculate outlier fractions/accuracy.
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History:
From electronic version of the journal and from
Tonima Tasnim Ananna, tonimatasnim.ananna(at)yale.edu
(End) Patricia Vannier [CDS] 01-Mar-2019