Field studies of the correlation between the atmospheric aerosol content and the light polarization at the zenith of the daytime sky

Шукуров, А. Х.; Shukurov, K. A.

doi:10.1134/s0001433806010063

“…Aerosol particle optical properties and vertical distributions also vary (cf. Wu & Jin 1997, Shukurov & Shukurov 2006, Vermeulen et al 2000, Ougolnikov & Maslov 2002, 2005a,b, 2009a,b, Ugolnikov et al 2004). The polarization can change across atmospheric absorption bands or can be influenced by other scattering mechanisms (cf.…”

Section: The Polarized Sky As a Calibrationmentioning

confidence: 99%

Deriving Telescope Mueller Matrices Using Daytime Sky Polarization Observations

Harrington

¹

,

Kuhn

²

,

Hall

³

2011

Publications of the Astronomical Society of the Pacific

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Telescopes often modify the input polarization of a source so that the measured circular or linear output state of the optical signal can be signficantly different from the input. This mixing, or polarization "cross-talk", is defined by the optical system Mueller matrix. We describe here an efficient method for recovering the input polarization state of the light and the full 4 × 4 Mueller matrix of the telescope with an accuracy of a few percent without external masks or telescope hardware modification. Observations of the bright, highly polarized daytime sky using the Haleakala 3.7m AEOS telescope and a coudé spectropolarimeter demonstrate the technique.

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“…The first subset of telescope pointings were chosen starting North-South with a 60 • spacing for azimuths of: [060, 120, 180, 240, 300, 360] and elevations of: [10,25,50,75]. The second subset of telescope pointings were chosen starting East-West with azimuths of: [030, 090, 150, 210, 270, 330] and elevations of [20,35,60,89].…”

Section: The Hivis Daytime Sky Observing Campaignmentioning

confidence: 99%

“…[67][68][69][70][71][72] Aerosol particle optical properties and vertical distributions also vary. 58,[73][74][75][76][77][78][79][80][81][82] The polarization can change across atmospheric absorption bands or can be influenced by other scattering mechanisms. [83][84][85][86][87] Deviations from a single scattering Rayleigh model grow as the aerosol, cloud, ground or sea-surface scattering sources affect the telescope line-of-sight.…”

Section: Sunmentioning

confidence: 99%

Daytime sky polarization calibration limitations

Harrington

¹

,

Kuhn

²

,

Ariste

³

2017

J. Astron. Telesc. Instrum. Syst

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The daytime sky has been recently demonstrated as a useful calibration tool for deriving polarization cross-talk properties of large astronomical telescopes. The Daniel K Inouye Solar Telescope (DKIST) and other large telescopes under construction can benefit from precise polarimetric calibration of large mirrors. Several atmospheric phenomena and instrumental errors potentially limit the techniques accuracy. At the 3.67m AEOS telescope on Haleakala, we have performed a large observing campaign with the HiVIS spectropolarimeter to identify limitations and develop algorithms for extracting consistent calibrations. Effective sampling of the telescope optical configurations and filtering of data for several derived parameters provide robustness to the derived Mueller matrix calibrations. Second-order scattering models of the sky show that this method is relatively insensitive to multiple-scattering in the sky provided calibration observations are done in regions of high polarization degree. The technique is also insensitive to assumptions about telescope induced polarization provided the mirror coatings are highly reflective. Zemax-derived polarization models show agreement between the functional dependence of polarization predictions and the corresponding on-sky calibrations.

show abstract

“…• spacing for azimuths of: [060, 120, 180, 240, 300, 360] and elevations of: [10,25,50,75]. The second subset of telescope pointings were chosen starting East-West with azimuths of: [030, 090, 150, 210, 270, 330] and elevations of [20,35,60,89].…”

Section: The Hivis Daytime Sky Observing Campaignmentioning

confidence: 99%

Daytime sky polarization calibration limitations

Harrington

¹

,

Kuhn

²

,

Ariste

³

2016

View full text Add to dashboard Cite

The daytime sky has been recently demonstrated as a useful calibration tool for deriving polarization cross-talk properties of large astronomical telescopes. The Daniel K Inouye Solar Telescope (DKIST) and other large telescopes under construction can benefit from precise polarimetric calibration of large mirrors. Several atmospheric phenomena and instrumental errors potentially limit the techniques accuracy. At the 3.67m AEOS telescope on Haleakala, we have performed a large observing campaign with the HiVIS spectropolarimeter to identify limitations and develop algorithms for extracting consistent calibrations. Effective sampling of the telescope optical configurations and filtering of data for several derived parameters provide robustness to the derived Mueller matrix calibrations. Second-order scattering models of the sky show that this method is relatively insensitive to multiple-scattering in the sky provided calibration observations are done in regions of high polarization degree. The technique is also insensitive to assumptions about telescope induced polarization provided the mirror coatings are highly reflective. Zemax-derived polarization models show agreement between the functional dependence of polarization predictions and the corresponding on-sky calibrations.

show abstract

Field studies of the correlation between the atmospheric aerosol content and the light polarization at the zenith of the daytime sky

Cited by 6 publications

References 0 publications

Deriving Telescope Mueller Matrices Using Daytime Sky Polarization Observations

Deriving Telescope Mueller Matrices Using Daytime Sky Polarization Observations

Daytime sky polarization calibration limitations

Daytime sky polarization calibration limitations

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