J/MNRAS/493/3341 X-ray and radio activity of Ly {alpha} emitters (Calhau+, 2020)
================================================================================
The X-ray and radio activity of typical and luminous Ly {alpha} 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    (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 {alpha} 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 10^44.31+/-0.01^erg/s and
    average black hole accretion rate (BHAR) of 0.72+/-0.01M_{sun}_/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 {alpha} luminosity and declines
    with increasing redshift. For X-ray-detected LAEs, Ly {alpha}
    luminosities correlate with the BHARs, suggesting that Ly {alpha}
    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_{sun}_/yr). The median star formation rate (SFR) of
    star-forming LAEs from Ly {alpha} and radio luminosities is
    7.6^+6.6^_-2.8_M_{sun}_/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
    {alpha} 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, Cat.
    J/MNRAS/476/4725). SC4K also includes the CALYMHA COSMOS sample at
    z=2.2 (Sobral et al. 2017MNRAS.466.1242S, Cat. J/MNRAS/466/1242), with
    H{alpha} coverage from HiZELS (Geach et al. 2008MNRAS.388.1473G;
    Sobral et al. 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,
    Cat. J/ApJS/184/158; Civano et al. 2016ApJ...819...62C, Cat.
    J/ApJ/819/62) covers the COSMOS field (e.g. Capak et al.
    2007ApJS..172...99C, Cat. II/284; Scoville et al. 2007ApJS..172....1S)
    over a total area of 2.2deg^2^. 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, Cat.
    J/AJ/128/1974, 2007ApJS..172...46S, Cat. J/ApJS/172/46; Bondi et al.
    2008ApJ...681.1129B; Schinnerer et al. 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 2deg^2^ 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 {alpha} 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 {alpha} 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 {alpha} star formation rate estimated
                                        following Sobral & Matthee
                                        (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, 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, 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, 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, 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,
                                        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, 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, 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, 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, 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, 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, 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, Cat. J/ApJ/864/56)
       988 I1     ---       Detjin     [0/1] Indicates if the source is detected
                                        by Jin et al. (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,
                                        Cat. J/ApJS/172/46)
1214- 1234 F21.17 Jy        S1.4GHz    ?=-99 Flux at 1.4GHz from 
                                        Schinnerer et al.  (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, Cat. J/A+A/602/A1)
1279- 1289 F11.7  Jy        S3GHz      ?=-99 Flux at 3GHz from Smolcic et al.
                                        (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,
                                        Cat. J/A+A/602/A1)
      1305 I1     ---       Detschin   [0/1] Indicates if the source is detected
                                        by Schinnerer et al.
                                        (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, Cat. J/ApJS/184/158) and
          Civano et al. (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
          L_X_=4{pi}(F_X_)d_L_^2^ (erg/s), where d_L_ 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):
          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 {alpha}, estimated between 1.4
          and 3.0GHz, as {alpha}=log(F_3GHz_/F_1.4GHz_)/log(3/1.4), where
          F_3GHz_ and F_1.4GHz_ 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 {alpha}
                                       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 {alpha} 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 {alpha}
                                        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 {alpha} 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
--------------------------------------------------------------------------------

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 3{sigma} upper limit.
--------------------------------------------------------------------------------

History:
    From electronic version of the journal

================================================================================
(End)                                           Ana Fiallos [CDS]    24-Apr-2023