Talk:Limiting magnitude

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For background limited observations, the limiting magnitude can be predicted from the derived zeropoints according to the formula (see McLean 1997):

mlim = zp-2.5log(S/N(nB/t)^1/2)

where: zp is the zeropoint magnitude (for 1 electron/sec), S/N is the requested signal-to-noise ratio, B is the background level (in electrons per second per pixel), t is the total on-source integration time and n is the number of pixels:

for point source: n = 3.1415 * (FWHM/pixel_size)^2 for extended source: n = (1/pixel_size)^2

Merge languages

This page should be merged with Grenzgröße on the German wiki, but that one is linked to another language, and I can't figure out how to merge the two wikidata pages.Ckyba (talk) 10:57, 10 September 2014 (UTC)

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Errors in section 'Calculating limiting magnitude'

Not only does this article need improved references, there are glaring errors. I have hidden Section 'Calculating limiting magnitude' until I can find son decent refs so I don't make the mistake of relying on my memory rather than reliable sources. Please, anyone, jump in here. — Neonorange (Phil) 06:09, 18 June 2021 (UTC)

Below is likely a better source:

TELESCOPIC LIMITING MAGNITUDES

BRADLEY E. SCHAEFER

Publications of the Astronomical Society of the Pacific Vol. 102, No. 648 (February 1990), pp. 212-229 (18 pages) Published By: Astronomical Society of the Pacific

The complete article is behind a paywall at JSTOR, I will read the article this weekend and then try to improve the article. — Neonorange (Phil) 11:48, 18 June 2021 (UTC)

I have added a new section on modelling limiting magnitude based on the 2014 MNRAS paper by Crumey - https://doi.org/10.1093/mnras/stu992 - which supersedes Schaefer's work and is cited in the most recent work on light pollution etc. StormBarn23 (talk) 17:00, 6 April 2023 (UTC)

I've added another on telescopic limiting magnitudes, based on the same paper. StormBarn23 (talk) 10:16, 7 April 2023 (UTC)