Noise-induced bias in magnitude determinations

Details Noise-induced bias in magnitude determinations Noise-induced bias in magnitude determinations

Jan 1996

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1996mnras.278..635c&link_type=abstract

Monthly Notices of the Royal Astronomical Society, Volume 278, pp. 635-643

Astronomy and Astrophysics

Astronomy

4

Techniques: Photometric -- Stars: Fundamental Parameters

Scientific paper

Because of the logarithmic nature of magnitude scales, noise on the basic flux measurements at the telescope introduces bias into determinations of stellar magnitudes and colour indices. Expressions have been derived to allow approximate calculation of the scale of the bias associated with magnitude difference estimators based on the mean, barΔm, and on the most probable value or mode, circumflex-barΔm, associated with the probability density distribution of magnitude difference measurements. Noise-induced bias has also been explored by computer simulations and various observational situations have been mimicked. ___ It is demonstrated that the bias associated with barΔm is usually insignificantly small in relation to random observational errors. For many stellar studies, however, the experimental procedures provide values for magnitude differences which are only estimates of barΔm or which correspond to circumflex-barΔm. The scale of the bias of circumflex-barΔm runs from ˜-0.0005 to ˜-0.01 mag over the range of flux measurements that may be met in observational practice. For the explored cases, the scale of mode bias is generally one-third the standard deviation of a magnitude measurement and is significant, its effect requiring consideration and assessment in precision photometry.

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