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Wavelength-dependent PSFs and their impact on weak lensing measurements

Author(s): Carlsten, SG; Strauss, Michael A; Lupton, Robert H; Meyers, Joshua E; Miyazaki, Satoshi

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dc.contributor.authorCarlsten, SG-
dc.contributor.authorStrauss, Michael A-
dc.contributor.authorLupton, Robert H-
dc.contributor.authorMeyers, Joshua E-
dc.contributor.authorMiyazaki, Satoshi-
dc.date.accessioned2022-01-25T15:04:58Z-
dc.date.available2022-01-25T15:04:58Z-
dc.date.issued2018-06-21en_US
dc.identifier.citationCarlsten, SG, Strauss, Michael A, Lupton, Robert H, Meyers, Joshua E, Miyazaki, Satoshi. (2018). Wavelength-dependent PSFs and their impact on weak lensing measurements. \mnras, 479 (1491 - 1504. doi:10.1093/mnras/sty1636en_US
dc.identifier.urihttp://arks.princeton.edu/ark:/88435/pr1cc0tt01-
dc.description.abstractWe measure and model the wavelength dependence of the point spread function (PSF) in the Hyper Suprime-Cam Subaru Strategic Program survey. We find that PSF chromaticity is present in the redder stars that appear smaller than bluer stars in the g, r, and i bands at the 1–2 per cent level and in the z and y bands at the 0.1–0.2 per cent level. From the color dependence of the PSF, we fit a model between the monochromatic PSF size based on weighted second moments, R, and wavelength of the form R(λ) ∝λ−b. We find values of b between 0.2 and 0.5, depending on the epoch and filter. This is consistent with the expectations of a turbulent atmosphere with an outer scale length of ∼10 − 100 m, indicating that the atmosphere is dominating the chromaticity. In the best seeing data, we find that the optical system and detector also contribute some wavelength dependence. Meyers & Burchat showed that b must be measured to an accuracy of ∼0.02 not to dominate the systematic error budget of the Large Synoptic Survey Telescope (LSST) weak lensing (WL) survey. Using simple image simulations, we find that b can be inferred with this accuracy in the r and i-bands for all positions in the LSST focal plane, assuming a stellar density of 1 star arcmin−2 and that the optical component of the PSF can be accurately modeled. Therefore, it is possible to correct for most, if not all, of the bias that the wavelength-dependent PSF will introduce into an LSST-like WL survey.en_US
dc.format.extent1491 - 1504en_US
dc.language.isoen_USen_US
dc.relationhttps://ui.adsabs.harvard.edu/abs/2018MNRAS.479.1491C/abstracten_US
dc.relation.ispartofMonthly Notices of the Royal Astronomical Societyen_US
dc.rightsFinal published version. Article is made available in OAR by the publisher's permission or policy.en_US
dc.titleWavelength-dependent PSFs and their impact on weak lensing measurementsen_US
dc.typeJournal Articleen_US
dc.identifier.doidoi:10.1093/mnras/sty1636-
dc.date.eissued2018-09en_US
pu.type.symplectichttp://www.symplectic.co.uk/publications/atom-terms/1.0/journal-articleen_US

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