On Magnitude Limits for Point Source Detections

Details On Magnitude Limits for Point Source Detections On Magnitude Limits for Point Source Detections

Aug 1995

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1995aj....110..916s&link_type=abstract

Astronomical Journal v.110, p.916

Astronomy and Astrophysics

Astronomy

5

Methods: Observational

Scientific paper

The notion of magnitude limits is formalized as a compromise between incompleteness and spurious detections. The best possible detection performance for given signal to noise is then computed for different point spread functions and pixel sizes. The resulting theoretical magnitude limits are much shallower than simple 3σ arguments would predict (and the reason for this is explained), but are (as expected) somewhat deeper than magnitude limits achieved in practice.

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