Automated galaxy surface photometry. V - Detection of very low surface brightness galaxies

Details Automated galaxy surface photometry. V - Detection of very low surface brightness galaxies Automated galaxy surface photometry. V - Detection of very low surface brightness galaxies

Jul 1990

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1990mnras.245..289i&link_type=abstract

Monthly Notices of the Royal Astronomical Society (ISSN 0035-8711), vol. 245, July 15, 1990, p. 289-304. Research supported by S

Astronomy and Astrophysics

Astronomy

77

Astronomical Photometry, Charge Coupled Devices, Galactic Clusters, Surface Properties, Astronomical Catalogs, Brightness Distribution, Data Processing, Photographic Plates

Scientific paper

It is shown that APM measurement of a standard deep UKSTU plate is equally as successful as photographic amplification in the detection of very low surface brightness galaxies. This method has the advantage of allowing the detection and quantitative measurement of images at the same time. Suitable median filtering techniques allow galaxies with scale sizes of a few arcseconds and central surface brightnesses as low as 26.5 B mag/sq arcsec to be detected. As suggested by previous work, detected galaxies occupy the whole of the parameter space which is accessible by the present method, again emphasizing the point that objectively determined selection boundaries are crucial in such studies. In particular there is no evidence for a correlation between galaxy scale size and surface brightness, and no sign of a cut-off in galaxy numbers as a function of surface brightness at these very faint levels.

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