The atmospheric extinction in photoelectric photometry

Stock, J.

doi:10.1016/0083-6656(69)90008-7

Cited by 9 publications

(5 citation statements)

References 5 publications

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“…One should note that the air mass depends slightly on the vertical structure of the atmosphere (Stone, 1996;Nijegorodov and Luhanga, 1996): an effect which is particularly distinctive in a polar environment. The relative errors due to such environmental variations are, however, below 0.2 % up to z 82 • (m 7) and below 1 % at z 87 • (m 15) (Tomasi and Petkov, 2014).…”

Section: Air Mass (X) Accuracymentioning

confidence: 99%

Accuracy in starphotometry

et al. 2021

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Abstract. Starphotometry, the night-time counterpart of sunphotometry, has not yet achieved the commonly sought observational error level of 1 %: a spectral optical depth (OD) error level of 0.01. In order to address this issue, we investigate a large variety of systematic (absolute) uncertainty sources. The bright-star catalogue of extraterrestrial references is noted as a major source of errors with an attendant recommendation that its accuracy, particularly its spectral photometric variability, be significantly improved. The small field of view (FOV) employed in starphotometry ensures that it, unlike sun- or moonphotometry, is only weakly dependent on the intrinsic and artificial OD reduction induced by scattering into the FOV by optically thin clouds. A FOV of 45 arcsec (arcseconds) was found to be the best trade-off for minimizing such forward-scattering errors concurrently with flux loss through vignetting. The importance of monitoring the sky background and using interpolation techniques to avoid spikes and to compensate for measurement delay was underscored. A set of 20 channels was identified to mitigate contamination errors associated with stellar and terrestrial atmospheric gas absorptions, as well as aurora and airglow emissions. We also note that observations made with starphotometers similar to our High Arctic instrument should be made at high angular elevations (i.e. at air masses less than 5). We noted the significant effects of snow crystal deposition on the starphotometer optics, how pseudo OD increases associated with this type of contamination could be detected, and how proactive techniques could be employed to avoid their occurrence in the first place. If all of these recommendations are followed, one may aspire to achieve component errors that are well below 0.01: in the process, one may attain a total 0.01 OD target error.

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Section: Air Mass (X) Accuracymentioning

confidence: 99%

Accuracy in starphotometry

et al. 2021

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“…If, in contrast, the instrument throughput is known to be stable, the acquisition of a large set of TSM measurements may enable an accurate calibration under variable τ conditions. Several TSM-based procedures optimizing S 0 retrieval are detailed in Stock (1969) and Mironov (2008), while an iterative algorithm, employed at the Pulkovo observatory, is detailed in Novikov (2021). Such retrievals of sets of S 0 are equivalent to building a new M 0 catalogue.…”

Section: Tsmmentioning

confidence: 99%

“…Gutierrez-Moreno and Stock (1966) introduced the TSM variant to reduce TSM error propagation associated with errors in M 0 (see Stock, 1969, for further TSM details and Sect. 4 for a discussion of M 0 errors).…”

Section: Tsmmentioning

confidence: 99%

“…The near-synchronicity minimizes potential OD variations and the impact of rapid throughput degradation incited by phenomena such as optical transmission degradation.7 Introduced by Gutierrez-Moreno andStock (1966), detailed inStock (1969), applied to starphotometry byLeiterer et al (1998), and patented in Russia byLebedev et al (2016).https://doi.org/10.5194/amt-14-6561-2021 Atmos. Meas.…”

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confidence: 99%

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Accuracy in starphotometry

Ivanescu

Baibakov

O’Neill

et al. 2021

Preprint

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Abstract. Starphotometry, the nightime counterpart of sunphotometry, has not yet achieved the commonly sought observational error level of 1%: a spectral optical depth (OD) error level of 0.01. In order to address this issue, we investigate a large variety of systematic (absolute) uncertainty sources. The bright star catalog of extraterrestrial references is noted as a major source of errors with an attendant recommendation that its accuracy, as well as its spectral photometric variability, be significantly improved. The small Field of View (FOV) employed in starphotometry ensures that starphotometry, unlike sun- or moonphotometry, is only weakly dependent on the intrinsic and artificial OD reduction induced by scattering into the FOV by optically thin clouds. A FOV of 45 arc-seconds was found to be the best tradeoff for minimizing such forward scattering errors concurrently with flux loss through vignetting. The importance of monitoring the sky background and using interpolation techniques to avoid spikes and to compensate for measurement delay was underscored. A set of 20 channels was identified to mitigate contamination errors associated with stellar and terrestrial-atmospheric gas absorptions, as well as aurora and airglow emissions. We also note that observations for starsphotometers similar to our high-Arctic starphotometer should be made at high angular elevations, i.e. at airmasses lower than 5. We noted the significant effects of snow crystal deposition on the starphotometer optics, how pseudo OD increases associated with this type of contamination could be detected and how proactive techniques could be employed to avoid their occurrence in the first place. If all these recommendations are followed, one may aspire to achieve component errors that are well below 0.01: in the process one may attain a total 0.01 OD target error.

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“…Observations (41) have found significant and systematic variations in the ultraviolet extinction during the night. Stock (42) has discussed the subject of atmospheric extinction in photoelectric photometry in some detail. The usual procedures are satisfactory for reducing observations to a uniform instrumental system but can lead to significant errors when used to compute extra-atmospheric values.…”

Section: Wide B a N D Photometrymentioning

confidence: 99%

25. Stellar Photometry

Cousins¹,

Crawford²,

Argue³

et al. 1970

Trans. Int. Astron. Union

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During the past three years there has been increased activity in many fields where photometric methods are employed; more telescopes have been commissioned or adapted for photometric measurements and new magnitude systems have been proposed and tried, but much of the observing is now of a routine nature. Most of this continues to be done in the wide-band UBV system, but more measurements are now being made in the red and infra-red.More interest is being shown in narrower band-widths that emphasize particular features of a stellar spectrum, because these offer better prospects of separating the effects of temperature, luminosity, interstellar reddening, composition and duplicity. Attention has been given to finding the most useful bands and practical ways of measuring them, both photoelectrically and photographically.

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The atmospheric extinction in photoelectric photometry

Cited by 9 publications

References 5 publications

Accuracy in starphotometry

Accuracy in starphotometry

Accuracy in starphotometry

25. Stellar Photometry

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