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J/A+A/358/77   Hamburg/ESO survey for bright QSOs. III.      (Wisotzki+, 2000)
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The Hamburg/ESO survey for bright QSOs. III.
A large flux-limited sample of QSOs.
    Wisotzki L., Christlieb N., Bade N., Beckmann V., Koehler T.,
    Vanelle C., Reimers D.
   <Astron. Astrophys. 358, 77 (2000)>
   =2000A&A...358...77W
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ADC_Keywords: QSOs ; Galaxies, Seyfert ; Redshifts
Keywords: quasars: general - galaxies: photometry - galaxies: Seyfert -
          cosmology: observations - surveys

Description:
    Appendix to the above paper, containing the two large tables
    A.1 and B.1 described in the paper. Table A.1 gives the basic
    properties of the 207 survey fields used to construct the flux-limited
    sample, including field-dependent magnitude limits and adopted
    extinction values. Table B.1 lists the 415 QSOs and Seyfert 1 galaxies
    that form the sample, with positions, redshift and magnitudes, plus a
    cross-identification with the 1995 version of the AGN catalogue by
    Veron-Cetty & Veron (see Cat. <VII/215>).

File Summary:
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 FileName      Lrecl  Records   Explanations
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ReadMe            80        .   This file
tablea1.dat       53      207   HES survey fields
tableb1.dat       80      415   Quasar list
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See also:
  J/A+AS/115/235 : The Hamburg/ESO survey for bright QSOs. II. (Reimers+, 1996)
         VII/215 : Quasars and Active Galactic Nuclei (9th Ed.) (Veron+ 2000)

Byte-by-byte Description of file: tablea1.dat
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   Bytes Format Units    Label     Explanations
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   4-  6  I3    ---      Field     ESO/UKST field number
   8- 12  I5    ---      Plate     ESO Schmidt plate number
  16- 17  I2    h        RAh       Right ascension (J2000) (1)
  19- 20  I2    min      RAm       Right ascension (J2000) (1)
  22- 23  I2    s        RAs       Right ascension (J2000) (1)
      26  A1    ---      DE-       Declination sign
  27- 28  I2    deg      DEd       Declination (J2000) (1)
  30- 31  I2    arcmin   DEm       Declination (J2000) (1)
  33- 34  I2    arcsec   DEs       Declination (J2000) (1)
  37- 42  F6.2  mag      maglim    B_J magnitude limit of the plate (2)
  44- 47  F4.1 10+20cm-2 NHI       HI column density (4) (3)
  49- 53  F5.2  mag      ABj       Adopted extinction per field (4)
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Note (1): Positions are *nominal* field centres; actual plate centroids may
           deviate by several arcmin.
Note (2): The magnitude limits correspond to the 5 sigma `completeness limits'
           described in the paper.
Note (3): HI column densities are in units of 10^20^cm^-2^, taken from
           Dickey & Lockman (1990ARA&A..28..215D)
Note (4): The conversion to extinction was performed assuming
           A_Bj_ = 3.9 N_H_ / 58 (Bohlin et al., 1978ApJ...224..132B)
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Byte-by-byte Description of file: tableb1.dat
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   Bytes Format Units   Label     Explanations
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   1- 12  A12   ---     HEname    Name according to HES convention
  15- 29  A15   ---     VVname    Name as listed by Veron-Cetty & Veron
                                  (1995, see Cat. <VII/215>)
  32- 33  I2    h       RAh       Right ascension (J2000)
  35- 36  I2    min     RAm       Right ascension (J2000)
  38- 41  F4.1  s       RAs       Right ascension (J2000)
      43  A1    ---     DE-       Declination sign (J2000)
  44- 45  I2    deg     DEd       Declination (J2000)
  47- 48  I2    arcmin  DEm       Declination (J2000)
  50- 51  I2    arcsec  DEs       Declination (J2000)
  54- 56  I3    ---     Field     ESO/UKST field number (1)
  59- 64  F6.3  ---     z         Geocentric redshift (2)
      66  A1    ---   f_z         [+] Redshift origin flag (2)
  68- 73  F6.2  mag     BJmag     Photographic B_J magnitude
  75- 80  F6.2  mag     BJmagc    B_J_ magnitude, corrected for extinction
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Note (1): The field number is needed for cross-identification with table A1.
Note (2): The redshifts are from our own measurements whenever spectra were
           available. These redshifts have an accuracy of up to +/-0.001
           (see more detailed discussion in the paper) and are marked with
           a flag "+" in the following column. All other redshifts were taken
           from the literature and are essentially of unknown accuracy.
           Among the latter group there are certainly several cases where
           trailing zeroes have no significance.
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Acknowledgements: Lutz Wisotzki <lutz@astro.physik.uni-potsdam.de>

References:
       Hagen et al., Paper I   1995A&AS..111..195H
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(End)     L. Wisotzki [Hamburger Sternwarte], Patricia Bauer [CDS]   20-Jun-2000