Pith. sign in

REVIEW 1 cited by

Dark Energy Survey Year 3 Results: Point-Spread Function Modeling

Not yet reviewed by Pith; the record is open.

Re-run · record.json Download PDF Read on arXiv ↗

This paper has not been read by Pith yet. Machine review is queued; the pith claim, tier, and objections will appear here once it completes.

SPECIMEN: schema-true, not a live event

T0 review · schema-true

One-sentence machine reading of the paper's core claim.

pith:XXXXXXXX · record.json · timestamp

arxiv 2011.03409 v2 pith:SKIPEPMB submitted 2020-11-06 astro-ph.IM astro-ph.CO

Dark Energy Survey Year 3 Results: Point-Spread Function Modeling

M. Jarvis , G. M. Bernstein , A. Amon , C. Davis , P. F. L\'eget , K. Bechtol , I. Harrison , M. Gatti
show 74 more authors
A. Roodman C. Chang R. Chen A. Choi S. Desai A. Drlica-Wagner D. Gruen R. A. Gruendl A. Hernandez N. MacCrann J. Meyers A. Navarro-Alsina S. Pandey A. A. Plazas L. F. Secco E. Sheldon M. A. Troxel S. Vorperian K. Wei J. Zuntz T. M. C. Abbott M. Aguena S. Allam S. Avila S. Bhargava S. L. Bridle D. Brooks A. Carnero Rosell M. Carrasco Kind J. Carretero M. Costanzi L. N. da Costa J. De Vicente H. T. Diehl P. Doel S. Everett B. Flaugher P. Fosalba J. Frieman J. Garc\'ia-Bellido E. Gaztanaga D. W. Gerdes G. Gutierrez S. R. Hinton D. L. Hollowood K. Honscheid D. J. James S. Kent K. Kuehn N. Kuropatkin O. Lahav M. A. G. Maia M. March J. L. Marshall P. Melchior F. Menanteau R. Miquel R. L. C. Ogando F. Paz-Chinch\'on E. S. Rykoff E. Sanchez V. Scarpine M. Schubnell S. Serrano I. Sevilla-Noarbe M. Smith E. Suchyta M. E. C. Swanson G. Tarle T. N. Varga A. R. Walker W. Wester R.D. Wilkinson DES Collaboration
This is my paper
classification astro-ph.IM astro-ph.CO
keywords modelingerrorspiffresultsanalysisdarkdescribeenergy
verification ladder T0 review T1 audit T2 compute T3 formal T4 reserved
0 comments
read the original abstract

We introduce a new software package for modeling the point-spread function (PSF) of astronomical images, called Piff (PSFs In the Full FOV), which we apply to the first three years (known as Y3) of the Dark Energy Survey (DES) data. We describe the relevant details about the algorithms used by Piff to model the PSF, including how the PSF model varies across the field of view (FOV). Diagnostic results show that the systematic errors from the PSF modeling are very small over the range of scales that are important for the DES Y3 weak lensing analysis. In particular, the systematic errors from the PSF modeling are significantly smaller than the corresponding results from the DES year one (Y1) analysis. We also briefly describe some planned improvements to Piff that we expect to further reduce the modeling errors in future analyses.

discussion (0)

Sign in with ORCID, Apple, or X to comment. Anyone can read and Pith papers without signing in.

Forward citations

Cited by 1 Pith paper

Reviewed papers in the Pith corpus that reference this work. Sorted by Pith novelty score.

  1. Dark Energy Survey Year 3 Results: Cosmological Constraints from Galaxy Clustering and Weak Lensing

    astro-ph.CO 2021-05 accept novelty 6.0

    DES Y3 3x2pt analysis constrains S8=0.776±0.017 and Ωm=0.339±0.032 in flat ΛCDM, consistent with Planck CMB results at p=0.13-0.48.