J/MNRAS/246/433 CCD photometry & APM parameters for galaxies (Maddox+ 1990)
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 1990MNRAS.246..433M
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.dat 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.dat
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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, Ai, 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 pi (where
pi=Ai, 1≤i≤8, p9=P, p10=K), a scatter plot of pi against m
is produced, the stellar locus is located as a function of magnitude,
giving pi*(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){wi(m)[pi(m)-pi*(m)]2}),
where wi are the weighting factors, defined as
wi=1/δi2, with δi the estimated error in pi.
Note (2): Position measured in 8 micron units from the centre of each plate
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Courtesy: Steve Maddox
References:
Maddox S.J. et al., 1990, MNRAS 243, 692 =1990MNRAS.243..692M 1990MNRAS.243..692M
(End) Patricia Bauer [CDS] 06-Sep-1996