J/MNRAS/493/3341 X-ray and radio activity of Ly α emitters (Calhau+, 2020)
The X-ray and radio activity of typical and luminous Ly α emitters from
z∼2 to z∼6: evidence for a diverse, evolving population.
Calhau J., Sobral D., Santos S., Matthee J., Paulino-Afonso A., Stroe A.,
Simmons B., Barlow-Hall C., Adams B.
<Mon. Not. R. Astron. Soc., 493, 3341-3362 (2020)>
=2020MNRAS.493.3341C 2020MNRAS.493.3341C (SIMBAD/NED BibCode)
ADC_Keywords: Active gal. nuclei ; Galaxies ; X-ray sources ; Radio sources ;
Infrared
Keywords: galaxies: active - galaxies: evolution - galaxies: high-redshift -
quasars: supermassive black holes - galaxies: star formation -
cosmology: observations - X-rays: galaxies
Abstract:
Despite recent progress in understanding Ly α emitters (LAEs),
relatively little is known regarding their typical black hole activity
across cosmic time. Here, we study the X-ray and radio properties of
∼4000 LAEs at 2.2<z<6 from the SC4K survey in the COSMOS field. We
detect 254 (6.8 per cent ± 0.4 per cent) LAEs individually in the
X-rays (S/N>3) with an average luminosity of 1044.31±0.01erg/s and
average black hole accretion rate (BHAR) of 0.72±0.01M☉/yr,
consistent with moderate to high accreting active galactic nuclei
(AGNs). We detect 120 sources in deep radio data (radio AGN fraction
of 3.2 per cent ± 0.3 per cent). The global AGN fraction (8.6 per
cent ± 0.4 per cent) rises with Ly α luminosity and declines
with increasing redshift. For X-ray-detected LAEs, Ly α
luminosities correlate with the BHARs, suggesting that Ly α
luminosity becomes a BHAR indicator. Most LAEs (93.1 per cent ± 0.6
per cent) at 2<z<6 have no detectable X-ray emission
(BHARs<0.017M☉/yr). The median star formation rate (SFR) of
star-forming LAEs from Ly α and radio luminosities is
7.6+6.6-2.8M☉/yr. The black hole to galaxy growth ratio
(BHAR/SFR) for LAEs is <0.0022, consistent with typical star-forming
galaxies and the local BHAR/SFR relation. We conclude that LAEs at
2<z<6 include two different populations: an AGN population, where Ly
α luminosity traces BHAR, and another with low SFRs which remain
undetected in even the deepest X-ray stacks but is detected in the
radio stacks.
Description:
We use a large sample of LAEs selected over a redshift range of z∼2-6
in the COSMOS field (SC4K; Sobral et al. 2018MNRAS.476.4725S 2018MNRAS.476.4725S, Cat.
J/MNRAS/476/4725). SC4K also includes the CALYMHA COSMOS sample at
z=2.2 (Sobral et al. 2017MNRAS.466.1242S 2017MNRAS.466.1242S, Cat. J/MNRAS/466/1242), with
Hα coverage from HiZELS (Geach et al. 2008MNRAS.388.1473G 2008MNRAS.388.1473G;
Sobral et al. 2013MNRAS.428.1128S 2013MNRAS.428.1128S, Cat. J/MNRAS/428/1128). The LAEs
were detected using a compilation of 16 narrow and medium band (MB)
data taken with the Subaru and the Isaac Newton Telescopes. Sources
were selected as LAEs through a combination of photometric and
spectroscopic redshifts as well as colour-colour diagnostics.
The Chandra COSMOS-Legacy survey (Elvis et al. 2009ApJS..184..158E 2009ApJS..184..158E,
Cat. J/ApJS/184/158; Civano et al. 2016ApJ...819...62C 2016ApJ...819...62C, Cat.
J/ApJ/819/62) covers the COSMOS field (e.g. Capak et al.
2007ApJS..172...99C 2007ApJS..172...99C, Cat. II/284; Scoville et al. 2007ApJS..172....1S 2007ApJS..172....1S)
over a total area of 2.2deg2. The deep X-ray data allow us to track
X-ray emission from processes like bremsstrahlung and inverse Compton
scattering, and thus to identify AGN X-ray emission.
The VLA-COSMOS Survey (Schinnerer et al. 2004AJ....128.1974S 2004AJ....128.1974S, Cat.
J/AJ/128/1974, 2007ApJS..172...46S 2007ApJS..172...46S, Cat. J/ApJS/172/46; Bondi et al.
2008ApJ...681.1129B 2008ApJ...681.1129B; Schinnerer et al. 2010ApJS..188..384S 2010ApJS..188..384S, Cat.
J/ApJS/188/384) used the National Radio Astronomy Observatory's Very
Large Array (VLA) to conduct deep, wide-field imaging with ∼1.5arcsec
resolution at 1.4GHz continuum of the 2deg2 COSMOS field.
Usage of the 3GHz VLA data allows us to further probe the existence of
radio-emitting AGNs over a larger area, as this survey covers the
entirety of SC4K. In addition, by removing radio-detected AGNs and
obtaining deep radio stacks, radio data will allow us a
dust-independent determination of the SFRs of SC4K LAEs.
File Summary:
--------------------------------------------------------------------------------
FileName Lrecl Records Explanations
--------------------------------------------------------------------------------
ReadMe 80 . This file
tablec1.dat 1311 3705 The full table of LAEs in our SC4K
tablec2.dat 613 84 The results for the stacking analysis of the
radio emission of LAEs
tablec3.dat 1227 138 The results of our stacking analysis of the
X-ray emission of LAEs
--------------------------------------------------------------------------------
See also:
J/MNRAS/476/4725 : SC4K catalogue of candidate LAEs (Sobral+, 2018)
J/MNRAS/466/1242 : CALYMHA survey. I. (Sobral+, 2017)
J/MNRAS/428/1128 : UDS/COSMOS HiZELS galaxies (Sobral+, 2013)
J/ApJS/184/158 : Chandra COSMOS survey I. (Elvis+, 2009)
J/ApJ/819/62 : The COSMOS-Legacy Survey (CLS) catalog (Civano+, 2016)
J/ApJ/864/56 : "Super-deblended" dust emission in gal. II. COSMOS
(Jin+, 2018)
J/AJ/128/1974 : The VLA-COSMOS survey (Schinnerer+, 2004)
J/ApJS/172/46 : VLA-COSMOS survey. II. (Schinnerer+, 2007)
J/A+A/602/A1 : VLA-COSMOS 3 GHz Large Project (Smolcic+, 2017)
Byte-by-byte Description of file: tablec1.dat
--------------------------------------------------------------------------------
Bytes Format Units Label Explanations
--------------------------------------------------------------------------------
1- 18 A18 --- Name Name of the source (SC4K-IANNN-NNNNNN,
SC4K-IANNN-nNNNNNN or SC4K-NBNNN-NNNNNN)
20- 34 F15.11 deg RAdeg Right ascension (J2000)
36- 48 F13.11 deg DEdeg Declination (J2000)
50- 67 E18.12 0.1nm EW0 Ly α rest-frame equivalent width
69- 86 F18.12 0.1nm E_EW0 Upper error on EW0
88- 104 E17.12 0.1nm e_EW0 Lower error on EW0
106- 118 F13.10 [10-7W] logLLya Logarithm of the Ly α luminosity
120- 135 F16.14 [10-7W] E_logLLya Upper error on logLLya
137- 153 F17.14 [10-7W] e_logLLya Lower error on logLLya
155- 176 F22.17 --- SFRSM19 Ly α star formation rate estimated
following Sobral & Matthee
(2019A&A...623A.157S 2019A&A...623A.157S)
178- 190 F13.11 --- z Redshift
192- 209 E18.12 [mW/m2] FXfull Logarithm of the full band X-ray flux (1)
211- 227 E17.12 [mW/m2] E_FXfull Upper error on FXfull
229- 245 E17.12 [mW/m2] e_FXfull Lower error on FXfull
247- 263 E17.12 [mW/m2] FXhard Logarithm of the hard band X-ray flux (1)
265- 281 E17.12 [mW/m2] E_FXhard Upper error on FXhard
283- 299 E17.12 [mW/m2] e_FXhard Lower error on FXhard
301- 318 E18.12 [mW/m2] FXsoft Logarithm of the soft band X-ray flux (1)
320- 336 E17.12 [mW/m2] E_FXsoft Upper error on FXsoft
338- 354 E17.12 [mW/m2] e_FXsoft Lower error on FXsoft
356- 372 E17.12 [10-7W] LXfull Logarithm of the full band X-ray
luminosity (2)
374- 390 E17.12 [10-7W] E_LXfull Upper error on LXfull
392- 408 E17.12 [10-7W] e_LXfull Lower error on LXfull
410- 426 E17.12 [10-7W] LXhard Logarithm of the hard band X-ray
luminosity (2)
428- 444 E17.12 [10-7W] E_LXhard Upper error on LXhard
446- 462 E17.12 [10-7W] e_LXhard Lower error on LXhard
464- 480 E17.12 [10-7W] LXsoft Logarithm of the soft band X-ray
luminosity (2)
482- 498 E17.12 [10-7W] E_LXsoft Upper error on LXsoft
500- 516 E17.12 [10-7W] e_LXsoft Lower error on LXsoft
518- 535 E18.12 --- XrayHR ?=-99 Hardness ratio (3)
537- 554 E18.12 --- E_XrayHR ?=-99 Upper error on XrayHR
556- 573 E18.12 --- e_XrayHR ?=-99 Lower error on XrayHR
575- 592 E18.12 Msun/yr XrayBHAR Black hole accretion rate (4)
594- 611 E18.12 Msun/yr E_XrayBHAR ?=-99 Upper error on XrayBHAR
613- 630 E18.12 Msun/yr e_XrayBHAR ?=-99 Lower error on XrayBHAR
632- 649 E18.12 ct/s CRfull Chandra full band count rate
651- 668 E18.12 ct/s CRHE ?=-99 Chandra High Energy Transmission
Grating (HETG) count rate
670- 687 E18.12 ct/s CRLE ?=-99 Chandra Low Energy Transmission
Grating (LETG) count rate
689 I1 --- Detfull [0/1] Indicates if the source is detected
in the Chandra full band
(1: True 252/3705, 0: False 3453/3705)
691 I1 --- Detsoft [0/1] Indicates if the source is detected
in the Chandra soft band
(1: True 269/3705, 0: False 3436/3705)
693 I1 --- Dethard [0/1] Indicates if the source is detected
in the Chandra hard band
(1: True 227/3705, 0: False 3478/3705)
695- 712 E18.12 --- SNfull Signal-to-noise ratio on the Chandra
full band
714- 731 E18.12 --- SNsoft ?=-99 Signal-to-noise ratio on the
Chandra soft band
733- 750 E18.12 --- SNhard ?=-99 Signal-to-noise ratio on the
Chandra hard band
752- 759 A8 --- IDciv Source identifier in Civano et al.
(2016ApJ...819...62C 2016ApJ...819...62C, Cat. J/ApJ/819/62)
(lid_NNNN or cid_NNNN)
761- 769 E9.3 [mW/m2] Fbciv ?=-99 0.5-10keV flux from Civano et al.
(2016ApJ...819...62C 2016ApJ...819...62C, Cat. J/ApJ/819/62)
771- 779 E9.3 [mW/m2] e_Fbciv ?=-99 Error on Fbciv
781- 789 E9.3 [mW/m2] Fsciv ?=-99 0.5-2keV flux from Civano et al.
(2016ApJ...819...62C 2016ApJ...819...62C, Cat. J/ApJ/819/62)
791- 799 E9.3 [mW/m2] e_Fsciv ?=-99 Error on Fhciv
801- 809 E9.3 [mW/m2] Fhciv ?=-99 2-10keV flux from Civano et al.
(2016ApJ...819...62C 2016ApJ...819...62C, Cat. J/ApJ/819/62)
811- 819 E9.3 [mW/m2] e_Fhciv ?=-99 Error on Fsciv
821 I1 --- Detciv [0/1] Indicates if the source is detected
by Civano et al. (2016ApJ...819...62C 2016ApJ...819...62C,
Cat. J/ApJ/819/62)
823- 835 F13.9 Jy F250 ?=-99 Super-deblended Herschel/SPIRE
250um flux from Jin et al.
(2018ApJ...864...56J 2018ApJ...864...56J, Cat. J/ApJ/864/56)
837- 848 E12.6 Jy e_F250 ?=-99 Error on F250
850- 862 F13.9 Jy F350 ?=-99 Super-deblended Herschel/SPIRE
350um flux from Jin et al.
(2018ApJ...864...56J 2018ApJ...864...56J, Cat. J/ApJ/864/56)
864- 875 E12.6 Jy e_F350 ?=-99 Error on F350
877- 889 F13.9 Jy F500 ?=-99 Super-deblended Herschel/SPIRE
500um flux from Jin et al.
(2018ApJ...864...56J 2018ApJ...864...56J, Cat. J/ApJ/864/56)
891- 902 E12.6 Jy e_F500 ?=-99 Error on F500
904- 916 F13.9 Jy F100 ?=-99 Super-deblended Herschel/PACS
100um flux from Jin et al.
(2018ApJ...864...56J 2018ApJ...864...56J, Cat. J/ApJ/864/56)
918- 929 E12.6 Jy e_F100 ?=-99 Error on F100
931- 943 F13.9 Jy F160 ?=-99 Super-deblended Herschel/PACS
160um flux from Jin et al.
(2018ApJ...864...56J 2018ApJ...864...56J, Cat. J/ApJ/864/56)
945- 956 E12.6 Jy e_F160 ?=-99 Error on F160
958- 964 F7.2 Msun/yr SFRjin ?=-99 Star formation rate from Jin et al.
(2018ApJ...864...56J 2018ApJ...864...56J, Cat. J/ApJ/864/56)
966- 977 E12.6 Msun/yr e_SFRjin ?=-99 Error on SFRjin
979- 986 I8 --- IDjin ? Source identifier in Jin et al.
(2018ApJ...864...56J 2018ApJ...864...56J, Cat. J/ApJ/864/56)
988 I1 --- Detjin [0/1] Indicates if the source is detected
by Jin et al. (2018ApJ...864...56J 2018ApJ...864...56J,
Cat. J/ApJ/864/56)
990- 1008 E19.13 Jy F1.4GHz Flux at 1.4GHz
1010- 1027 E18.12 Jy E_F1.4GHz ?=-99 Upper error on F1.4GHz
1029- 1046 E18.12 Jy e_F1.4GHz ?=-99 Lower error on F1.4GHz
1048 I1 --- Det1.4GHz [0/1] Indicates if the source is detected
in the 1.4GHz VLA-COSMOS data
1050- 1068 E19.13 Jy F3GHz Flux at 3GHz
1070- 1087 E18.12 Jy E_F3GHz ?=-99 Upper error on F3GHz
1089- 1106 E18.12 Jy e_F3GHz ?=-99 Lower error on F3GHz
1108 I1 --- Det3GHz [0/1] Indicates if the source is detected
in the 3GHz VLA-COSMOS data
1110- 1130 F21.17 --- 1.4-3 ?=-99 Radio spectral index (5)
1132- 1152 F21.17 --- e_1.4-3 ?=-99 Error on 1.4-3
1154- 1172 F19.14 --- SN3GHz Signal to noise ratio on the 3GHz band
1174- 1191 F18.14 --- SN1.4GHz ?=-99 Signal to noise ratio on the
1.4GHz band
1193- 1212 A20 --- IDschin Source identifier in Schinnerer et al.
(2007ApJS..172...46S 2007ApJS..172...46S,
Cat. J/ApJS/172/46)
1214- 1234 F21.17 Jy S1.4GHz ?=-99 Flux at 1.4GHz from
Schinnerer et al. (2007ApJS..172...46S 2007ApJS..172...46S,
Cat. J/ApJS/172/46)
1236- 1256 F21.17 Jy e_S1.4GHz ?=-99 Error on S1.4GHz
1258- 1277 A20 --- IDsmol Source identifier in Smolcic et al.
(2017A&A...602A...1S 2017A&A...602A...1S, Cat. J/A+A/602/A1)
1279- 1289 F11.7 Jy S3GHz ?=-99 Flux at 3GHz from Smolcic et al.
(2017A&A...602A...1S 2017A&A...602A...1S, Cat. J/A+A/602/A1)
1291- 1301 F11.7 Jy e_S3GHz ?=-99 Error on S3GHz
1303 I1 --- Detsmol [0/1] Indicates if the source is detected
by Smolcic et al. (2017A&A...602A...1S 2017A&A...602A...1S,
Cat. J/A+A/602/A1)
1305 I1 --- Detschin [0/1] Indicates if the source is detected
by Schinnerer et al.
(2007ApJS..172...46S 2007ApJS..172...46S,
Cat. J/ApJS/172/46)
1307 I1 --- Detradio [0/1] Indicates if the source is detected
in radio
1309 I1 --- radiocont [0/1] Indicates if the source is
radio contaminated
1311 I1 --- vcheck [0/1] Visual check pass
--------------------------------------------------------------------------------
Note (1): We convert our counts/s into flux by using the method detailed in
Elvis et al. (2009ApJS..184..158E 2009ApJS..184..158E, Cat. J/ApJS/184/158) and
Civano et al. (2016ApJ...819...62C 2016ApJ...819...62C, Cat. J/ApJ/819/62). See section
3.1.3 of the article for more details.
Note (2): We convert the fluxes to observed X-ray luminosity by using
LX=4π(FX)dL2 (erg/s), where dL is the luminosity
distance in cm. See section 3.1.5 of the article for more details.
Note (3): In order to estimate the hardness ratio of our sources, we adopt the
standard definition (see Park et al. 2006ApJ...652..610P 2006ApJ...652..610P):
HR=(H-S)/(H+S), where H and S are the count rates in the hard (2-7keV)
and soft band (0.5-2keV), respectively.
Note (4): See section 3.1.6 of the article for details on the calculation of
the black hole accretion rate.
Note (5): We calculate the radio spectral index α, estimated between 1.4
and 3.0GHz, as α=log(F3GHz/F1.4GHz)/log(3/1.4), where
F3GHz and F1.4GHz are the aperture corrected fluxes in the 3GHz
and 1.4GHz bands respectively. See section 3.2.4 of the article for
more details.
--------------------------------------------------------------------------------
Byte-by-byte Description of file: tablec2.dat
--------------------------------------------------------------------------------
Bytes Format Units Label Explanations
--------------------------------------------------------------------------------
1- 31 A31 --- Subsample Stacked subsample
33- 37 I5 --- Pix [10000] Sigma-clipping
39- 42 I4 --- Ns Number of stacked sources
44- 47 F4.1 [10-7W] b_logLLya []? Minimum value of logLLya
49- 52 F4.1 [10-7W] B_logLLya []? Maximum value of logLLya
54- 66 F13.10 [10-7W] logLLya Logarithm of the median Ly α
luminosity
68- 81 F14.12 [10-7W] E_logLLya Upper error on logLLya
83- 96 F14.12 [10-7W] e_logLLya Lower error on logLLya
98- 111 F14.10 0.1nm EW Median Ly α rest-frame equivalent
width
113- 129 E17.12 0.1nm E_EW Upper error on EW
131- 147 E17.12 0.1nm e_EW Lower error on EW
149- 161 F13.11 --- z Median redshift
163- 180 E18.12 --- E_z ? Upper error on z
182- 199 E18.12 --- e_z ? Lower error on z
201- 215 F15.13 --- Fcor1.4GHz Flux correction at 1.4GHz
217- 233 E17.12 Jy F1.4GHz Median flux at 1.4GHz
235- 251 E17.12 Jy E_F1.4GHz Upper error on F1.4GHz
253- 269 E17.12 Jy e_F1.4GHz Lower error on F1.4GHz
271- 283 F13.10 [W/Hz] logL1.4 Logarithm of the median 1.4GHz luminosity
285- 301 E17.12 [W/Hz] E_logL1.4 ? Upper error on logL1.4
303- 319 E17.12 [W/Hz] e_logL1.4 ? Lower error on logL1.4
321- 335 F15.10 Msun/yr SFR1.4 Median star formation rate at 1.4GHz
337- 350 F14.10 Msun/yr E_SFR1.4 ?=-99 Upper error on SFR1.4
352- 365 F14.10 Msun/yr e_SFR1.4 ?=-99 Lower error on SFR1.4
367- 384 E18.12 --- SN1.4GHz ?=-99 Median signal to noise ratio at
1.4GHz
386 I1 --- Det1.4GHz [0/1] Indicates if the stack is detected
in the 1.4GHz band (G1)
388- 399 E12.6 --- Bkg1.4GHz Background stack on the 1.4GHz band
401 I1 --- Aper1.4GHz [8] Aperture radius used on the 1.4GHz
band
403- 417 F15.13 --- Fcor3GHz Flux correction at 3GHz
419- 435 E17.12 Jy F3GHz Median flux at 3GHz
437- 453 E17.12 Jy E_F3GHz Upper error on F3GHz
455- 471 E17.12 Jy e_F3GHz Lower error on F3GHz
473- 485 F13.10 [W/Hz] logL3 Logarithm of the median 3GHz luminosity
487- 503 E17.12 [W/Hz] E_logL3 ? Upper error on logL3
505- 521 E17.12 [W/Hz] e_logL3 ? Lower error on logL3
523- 539 E17.12 Msun/yr SFR3 Median star formation rate at 3GHz
541- 558 E18.12 Msun/yr E_SFR3 ?=-99 Upper error on SFR3
560- 577 E18.12 Msun/yr e_SFR3 ?=-99 Upper error on SFR3
579- 596 E18.12 --- SN3GHz Median signal to noise ratio at 3GHz
598 I1 --- Det3GHz [0/1] Indicates if the stack is detected
in the 3GHz band (G1)
600- 611 E12.6 --- Bkg3GHz Background stack on the 3GHz band
613 I1 --- Aper3GHz [3] Aperture radius used on the 3GHz band
--------------------------------------------------------------------------------
Byte-by-byte Description of file: tablec3.dat
--------------------------------------------------------------------------------
Bytes Format Units Label Explanations
--------------------------------------------------------------------------------
1- 48 A48 --- Subsample Stacked subsample
50- 55 I6 --- Pix [100000] Sigma-clipping
57- 60 I4 --- Ns Number of stacked sources
62- 65 F4.1 [10-7W] b_logLLya ? Minimum value of logLLya
67- 70 F4.1 [10-7W] B_logLLya ? Maximum value of logLLya
72- 84 F13.10 [10-7W] logLLya Logarithm of the median Ly α
luminosity
86- 99 F14.12 [10-7W] E_logLLya Upper error on logLLya
101- 114 F14.12 [10-7W] e_logLLya Lower error on logLLya
116- 129 F14.10 0.1nm EW Median Ly α rest-frame equivalent
width
131- 147 E17.12 0.1nm E_EW Upper error on EW
149- 165 E17.12 0.1nm e_EW Lower error on EW
167- 179 F13.11 --- z Median redshift
181- 198 E18.12 --- E_z ? Upper error on z
200- 216 E17.12 --- e_z Lower error on z
218- 220 F3.1 --- Tphoton [1.4] Photon index
222- 224 F3.1 --- epsilon [0.1] Accretion efficiency
226- 230 F5.3 --- CFHE [0.687] Conversion factor for the hard
band
232- 248 E17.12 h TexpHE Exposure time on the hard band
250- 266 E17.12 [mW/m2] FXhard Logarithm of the median hard band X-ray
flux
268- 284 E17.12 [mW/m2] E_FXhard Upper error on FXhard
286- 302 E17.12 [mW/m2] e_FXhard Lower error on FXhard
304- 320 E17.12 [10-7W] LXhard Logarithm of the median hard band X-ray
luminosity
322- 338 E17.12 [10-7W] E_LXhard Upper error on LXhard
340- 356 E17.12 [10-7W] e_LXhard Lower error on LXhard
358- 374 E17.12 [10-7W] LXhardcor Logarithm of the median corrected hard
band X-ray luminosity
376- 392 E17.12 [10-7W] E_LXhardcor Upper error on LXhardcor
394- 410 E17.12 [10-7W] e_LXhardcor Lower error on LXhardcor
412- 428 E17.12 Msun/yr BHARhard Median of the hard band black hole
accretion rate
430- 446 E17.12 Msun/yr E_BHARhard Upper error on BHARhard
448- 464 E17.12 Msun/yr e_BHARhard Lower error on BHARhard
466- 482 E17.12 ct/s CRHE Median Chandra High Energy Transmission
Grating (HETG) count rate
484- 500 E17.12 --- NoiseHEmax Maximum Noise on the hard band
502- 518 E17.12 --- NoiseHEmin Minimum Noise on the hard band
520- 537 E18.12 --- SNhard Median Signal-to-noise ratio on the
Chandra hard band
539 I1 --- Dethard [0/1] Indicates if the stack is detected
in the Chandra hard band (G1)
541- 557 E17.12 --- BkgHE Background stack on the Chandra hard band
559 I1 --- AperHE [4] Aperture radius used on the Chandra
hard band
561- 564 F4.2 --- CFLE [3.05] Conversion factor for the soft
band
566- 582 E17.12 h TexpLE Exposure time on the soft band
584- 600 E17.12 [mW/m2] FXsoft Logarithm of the median soft band X-ray
flux
602- 618 E17.12 [mW/m2] E_FXsoft Upper error on FXsoft
620- 636 E17.12 [mW/m2] e_FXsoft Lower error on FXsoft
638- 654 E17.12 [10-7W] LXsoft Logarithm of the median soft band X-ray
luminosity
656- 672 E17.12 [10-7W] E_LXsoft Upper error on LXsoft
674- 690 E17.12 [10-7W] e_LXsoft Lower error on LXsoft
692- 708 E17.12 [10-7W] LXsoftcor Logarithm of the median corrected soft
band X-ray luminosity
710- 726 E17.12 [10-7W] E_LXsoftcor Upper error on LXsoftcor
728- 744 E17.12 [10-7W] e_LXsoftcor Lower error on LXsoftcor
746- 762 E17.12 Msun/yr BHARsoft Median of the soft band black hole
accretion rate
764- 780 E17.12 Msun/yr E_BHARsoft Upper error on BHARsoft
782- 798 E17.12 Msun/yr e_BHARsoft Lower error on BHARsoft
800- 816 E17.12 ct/s CRLE Median Chandra Low Energy Transmission
Grating (LETG) count rate
818- 834 E17.12 --- NoiseLEmax Maximum Noise on the soft band
836- 852 E17.12 --- NoiseLEmin Minimum Noise on the soft band
854- 871 E18.12 --- SNsoft Median Signal-to-noise ratio on the
Chandra soft band
873 I1 --- Detsoft [0/1] Indicates if the stack is detected
in the Chandra soft band (G1)
875- 891 E17.12 --- BkgLE Background stack on the Chandra soft band
893 I1 --- AperLE [4] Aperture radius used on the Chandra
soft band
895- 898 F4.2 --- CFfull [1.64] Conversion factor for the full
band
900- 916 E17.12 h Texpfull Exposure time on the full band
918- 934 E17.12 [mW/m2] FXfull Logarithm of the median full band X-ray
flux
936- 952 E17.12 [mW/m2] E_FXfull Upper error on FXfull
954- 970 E17.12 [mW/m2] e_FXfull Lower error on FXfull
972- 988 E17.12 [10-7W] LXfull Logarithm of the median full band X-ray
luminosity
990- 1006 E17.12 [10-7W] E_LXfull Upper error on LXfull
1008- 1024 E17.12 [10-7W] e_LXfull Lower error on LXfull
1026- 1042 E17.12 [10-7W] LXfullcor Logarithm of the median corrected full
band X-ray luminosity
1044- 1060 E17.12 [10-7W] E_LXfullcor Upper error on LXfullcor
1062- 1078 E17.12 [10-7W] e_LXfullcor Lower error on LXfullcor
1080- 1096 E17.12 Msun/yr BHARfull Median of the full band black hole
accretion rate
1098- 1114 E17.12 Msun/yr E_BHARfull Upper error on BHARfull
1116- 1132 E17.12 Msun/yr e_BHARfull Lower error on BHARfull
1134- 1150 E17.12 ct/s CRfull Median count rate on Chandra full band
1152- 1168 E17.12 --- NoiseFmax Maximum Noise on the full band
1170- 1186 E17.12 --- NoiseFmin Minimum Noise on the full band
1188- 1205 E18.12 --- SNfull Median Signal-to-noise ratio on the
Chandra full band
1207 I1 --- Detfull [0/1] Indicates if the stack is detected
in the Chandra full band (G1)
1209- 1225 E17.12 --- Bkgfull Background stack on the Chandra full band
1227 I1 --- Aperfull [4] Aperture radius used on the Chandra
full band
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Global Notes:
Note (G1): A stack is considered as having a detection when the S/N≥3. For
stacks with lower S/N, we provide the 3σ upper limit.
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History:
From electronic version of the journal
(End) Ana Fiallos [CDS] 24-Apr-2023