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J/MNRAS/246/433     CCD photometry & APM parameters for galaxies  (Maddox+ 1990)
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The APM galaxy survey. II. Photometric corrections.
     Maddox S.J., Efstathiou G., Sutherland W.J.
    <Mon. Not. R. Astron. Soc. 246, 433 (1990)>
    =1990MNRAS.246..433M        (SIMBAD/NED BibCode)
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ADC_Keywords: Galaxies, photometry

Description:
    The sequences for UKS fields 152 246 and 249 appear to be discrepant
    with the plate matching in the APM survey, and so may not be
    completely reliable.

File Summary:
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 FileName       Lrecl  Records   Explanations
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ReadMe             80        .   This file
table3             80      301   CCD photometry and APM parameters for galaxies
                                  in the calibration sequences
table3.tex        108      372   TeX version of table3
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Byte-by-byte Description of file: table3
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   Bytes Format Units   Label    Explanations
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   1-  5  A5    ---     Name     Galaxy name
   7-  8  I2    h       RAh      Right ascension (B1950)
  10- 11  I2    min     RAm      Right ascension (B1950)
  13- 16  F4.1  s       RAs      Right ascension (B1950)
      18  A1    ---     DE-      Declination sign
  19- 20  I2    deg     DEd      Declination (B1950)
  22- 23  I2    arcmin  DEm      Declination (B1950)
  25- 28  F4.1  arcsec  DEs      Declination (B1950)
  30- 34  F5.2  mag     Bmag     B magnitude
  36- 40  F5.2  mag     Vmag     V magnitude
  42- 46  F5.2  mag     bJ       bJ magnitude
  48- 52  F5.2  mag     m        APM magnitude
  54- 61  F8.2  ---     Class    Class, phi, as defined in Maddox et al. (1990)
                                  (Paper I) (-5000 flags merged images) (1)
  63- 70  F8.1  8um     Xpos     X coordinate (2)
  72- 79  F8.1  8um     Ypos     Y coordinate (2)
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Note (1): A simple way of using all the APM parameters is to treat each 
    of the levels, A_i_, and the peak density, P, as different
    measurements of the surface brightness profile, and use nine separate
    pairwise plots against magnitude. The radius of gyration is included
    as a tenth plot against magnitude. For each parameter p_i_ (where
    p_i_=A_i_, 1<=i<=8, p_9_=P, p_10_=K), a scatter plot of p_i_ against m
    is produced, the stellar locus is located as a function of magnitude,
    giving p_i_*(m).
    The final profile residual, phi, which is equivalent to the
    integrated difference between the particular image profile and the
    stellar profile at the same magnitude, is given by:
          phi = 1000log(sum(1to10){w_i_(m)[p_i_(m)-p_i_*(m)]^2^}),
    where w_i_ are the weighting factors, defined as
          w_i_=1/{delta}_i_^2^, with {delta}_i_ the estimated error in p_i_.
Note (2): Position measured in 8 micron units from the centre of each plate
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Courtesy: Steve Maddox <sjm@ast.cam.ac.uk>

References:
  Maddox S.J. et al., 1990, MNRAS 243, 692  =1990MNRAS.243..692M
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(End)                                         Patricia Bauer  [CDS]  06-Sep-1996