On Computing Upper Limits to Source Intensities.¶
Kashyap, V. L., van Dyk, D. A., Connors, A., Freeman, P. E., Siemiginowska, A., Xu, J., & Zezas, A. (2010). On Computing Upper Limits to Source Intensities. The Astrophysical Journal, 719(1), 900-914.
Cited by¶
1 citation across 1 artifact.
Each citation links to the sentence it supports in the citing article.
Primes¶
- Absence Of Evidence Vs Evidence Of Absence
- Instead the non-detection is converted into an upper limit: the sensitivity curve says the instrument would have detected, with high probability, any source brighter than flux F, so the result is "any source present is fainter than F" — a measured exclusion, not silence.
This sourceStandard reference distinguishing a flux upper limit (a calibration of the detection process) from an upper bound, formalizing how a non-detection is converted into a constraint via a characterized instrument sensitivity.
Supported in partVerified against the work's full text
Kashyap et al. show how a non-detection is converted to an upper limit via detection probability, but stress that the limit is not a bound on the source's actual intensity.
“We emphasize that the upper limit is not meant to be an estimate or even a bound on the intensity of the source”
- Instead the non-detection is converted into an upper limit: the sensitivity curve says the instrument would have detected, with high probability, any source brighter than flux F, so the result is "any source present is fainter than F" — a measured exclusion, not silence.
Verification¶
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Registry ID ref:1283e26a8c63 · see in the full table