Near-IR Weak-lensing (NIRWL) Measurements in the CANDELS Fields. I. Point-spread Function Modeling and Systematics
We have undertaken a near-IR weak-lensing (NIRWL) analysis of the CANDELS HST/WFC3-IR F160W observations. With the Gaia proper motion–corrected catalog as an astrometric reference, we updated the astrometry of the five CANDELS mosaics and achieved an absolute alignment within 0.″02 ± 0.″02, on avera...
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| Format: | Article |
| Language: | English |
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IOP Publishing
2023-01-01
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| Series: | The Astrophysical Journal |
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| Online Access: | https://doi.org/10.3847/1538-4357/acfafd |
| _version_ | 1827293238628712448 |
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| author | Kyle Finner Bomee Lee Ranga-Ram Chary M. James Jee Christopher Hirata Giuseppe Congedo Peter Taylor Kim HyeongHan |
| author_facet | Kyle Finner Bomee Lee Ranga-Ram Chary M. James Jee Christopher Hirata Giuseppe Congedo Peter Taylor Kim HyeongHan |
| author_sort | Kyle Finner |
| collection | DOAJ |
| description | We have undertaken a near-IR weak-lensing (NIRWL) analysis of the CANDELS HST/WFC3-IR F160W observations. With the Gaia proper motion–corrected catalog as an astrometric reference, we updated the astrometry of the five CANDELS mosaics and achieved an absolute alignment within 0.″02 ± 0.″02, on average, which is a factor of several superior to existing mosaics. These mosaics are available to download ( https://drive.google.com/drive/folders/1k9WEV3tBOuRKBlcaTJ0-wTZnUCisS__r ). We investigated the systematic effects that need to be corrected for weak-lensing measurements. We find that the largest contributing systematic effect is caused by undersampling. We find a subpixel centroid dependence on the PSF shape that causes the PSF ellipticity and size to vary by up to 0.02 and 3%, respectively. Using the UDS as an example field, we show that undersampling induces a multiplicative shear bias of −0.025. We find that the brighter-fatter effect causes a 2% increase in the size of the PSF and discover a brighter-rounder effect that changes the ellipticity by 0.006. Based on the small range of slopes in a galaxy’s spectral energy distribution (SED) within the WFC3-IR bandpasses, we suggest that the impact of the galaxy SED on the PSF is minor. Finally, we model the PSF of WFC3-IR F160W for weak lensing using a principal component analysis. The PSF models account for temporal and spatial variations of the PSF. The PSF corrections result in residual ellipticities and sizes, ∣ de _1 ∣ < 0.0005 ± 0.0003, ∣ de _2 ∣ < 0.0005 ± 0.0003, and ∣ dR ∣ < 0.0005 ± 0.0001, that are sufficient for the upcoming NIRWL search for massive overdensities in the five CANDELS fields. |
| first_indexed | 2024-03-11T11:46:54Z |
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| institution | Directory Open Access Journal |
| issn | 1538-4357 |
| language | English |
| last_indexed | 2024-04-24T13:21:54Z |
| publishDate | 2023-01-01 |
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| series | The Astrophysical Journal |
| spelling | doaj.art-ce7d912a3eb34601b07207f2b460c5a12024-04-04T13:31:42ZengIOP PublishingThe Astrophysical Journal1538-43572023-01-0195813310.3847/1538-4357/acfafdNear-IR Weak-lensing (NIRWL) Measurements in the CANDELS Fields. I. Point-spread Function Modeling and SystematicsKyle Finner0https://orcid.org/0000-0002-4462-0709Bomee Lee1https://orcid.org/0000-0003-1954-5046Ranga-Ram Chary2https://orcid.org/0000-0001-7583-0621M. James Jee3https://orcid.org/0000-0002-5751-3697Christopher Hirata4https://orcid.org/0000-0002-2951-4932Giuseppe Congedo5https://orcid.org/0000-0003-2508-0046Peter Taylor6https://orcid.org/0000-0001-6999-4718Kim HyeongHan7https://orcid.org/0000-0002-2550-5545IPAC, California Institute of Technology , 1200 East California Boulevard, Pasadena, CA 91125, USA ; kfinner@caltech.eduKorea Astronomy and Space Science Institute (KASI) , 776 Daedeokdae-ro, Yuseong-gu, Daejeon 34055, Republic of KoreaIPAC, California Institute of Technology , 1200 East California Boulevard, Pasadena, CA 91125, USA ; kfinner@caltech.eduDepartment of Astronomy, Yonsei University , 50 Yonsei-ro, Seodaemun-gu, Seoul 03722, Republic of Korea; Department of Physics and Astronomy, University of California , Davis, One Shields Avenue, Davis, CA 95616, USACenter for Cosmology and Astroparticle Physics, The Ohio State University , 191 West Woodruff Avenue, Columbus, OH 43210, USA; Department of Physics, The Ohio State University , 191 West Woodruff Avenue, Columbus, OH 43210, USA; Department of Astronomy, The Ohio State University , 140 West 18th Avenue, Columbus, OH 43210, USAInstitute for Astronomy, University of Edinburgh , Royal Observatory, Blackford Hill, Edinburgh, EH9 3HJ, UKCenter for Cosmology and Astroparticle Physics, The Ohio State University , 191 West Woodruff Avenue, Columbus, OH 43210, USA; Department of Physics, The Ohio State University , 191 West Woodruff Avenue, Columbus, OH 43210, USA; Department of Astronomy, The Ohio State University , 140 West 18th Avenue, Columbus, OH 43210, USADepartment of Astronomy, Yonsei University , 50 Yonsei-ro, Seodaemun-gu, Seoul 03722, Republic of KoreaWe have undertaken a near-IR weak-lensing (NIRWL) analysis of the CANDELS HST/WFC3-IR F160W observations. With the Gaia proper motion–corrected catalog as an astrometric reference, we updated the astrometry of the five CANDELS mosaics and achieved an absolute alignment within 0.″02 ± 0.″02, on average, which is a factor of several superior to existing mosaics. These mosaics are available to download ( https://drive.google.com/drive/folders/1k9WEV3tBOuRKBlcaTJ0-wTZnUCisS__r ). We investigated the systematic effects that need to be corrected for weak-lensing measurements. We find that the largest contributing systematic effect is caused by undersampling. We find a subpixel centroid dependence on the PSF shape that causes the PSF ellipticity and size to vary by up to 0.02 and 3%, respectively. Using the UDS as an example field, we show that undersampling induces a multiplicative shear bias of −0.025. We find that the brighter-fatter effect causes a 2% increase in the size of the PSF and discover a brighter-rounder effect that changes the ellipticity by 0.006. Based on the small range of slopes in a galaxy’s spectral energy distribution (SED) within the WFC3-IR bandpasses, we suggest that the impact of the galaxy SED on the PSF is minor. Finally, we model the PSF of WFC3-IR F160W for weak lensing using a principal component analysis. The PSF models account for temporal and spatial variations of the PSF. The PSF corrections result in residual ellipticities and sizes, ∣ de _1 ∣ < 0.0005 ± 0.0003, ∣ de _2 ∣ < 0.0005 ± 0.0003, and ∣ dR ∣ < 0.0005 ± 0.0001, that are sufficient for the upcoming NIRWL search for massive overdensities in the five CANDELS fields.https://doi.org/10.3847/1538-4357/acfafdWeak gravitational lensingGalaxy clustersAstrometryGalaxy groupsHubble Space TelescopeInfrared astronomy |
| spellingShingle | Kyle Finner Bomee Lee Ranga-Ram Chary M. James Jee Christopher Hirata Giuseppe Congedo Peter Taylor Kim HyeongHan Near-IR Weak-lensing (NIRWL) Measurements in the CANDELS Fields. I. Point-spread Function Modeling and Systematics The Astrophysical Journal Weak gravitational lensing Galaxy clusters Astrometry Galaxy groups Hubble Space Telescope Infrared astronomy |
| title | Near-IR Weak-lensing (NIRWL) Measurements in the CANDELS Fields. I. Point-spread Function Modeling and Systematics |
| title_full | Near-IR Weak-lensing (NIRWL) Measurements in the CANDELS Fields. I. Point-spread Function Modeling and Systematics |
| title_fullStr | Near-IR Weak-lensing (NIRWL) Measurements in the CANDELS Fields. I. Point-spread Function Modeling and Systematics |
| title_full_unstemmed | Near-IR Weak-lensing (NIRWL) Measurements in the CANDELS Fields. I. Point-spread Function Modeling and Systematics |
| title_short | Near-IR Weak-lensing (NIRWL) Measurements in the CANDELS Fields. I. Point-spread Function Modeling and Systematics |
| title_sort | near ir weak lensing nirwl measurements in the candels fields i point spread function modeling and systematics |
| topic | Weak gravitational lensing Galaxy clusters Astrometry Galaxy groups Hubble Space Telescope Infrared astronomy |
| url | https://doi.org/10.3847/1538-4357/acfafd |
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