Morphological Parameters and Associated Uncertainties for 8 Million Galaxies in the Hyper Suprime-Cam Wide Survey

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dc.article.number134
dc.contributor.authorGhosh, Aritra
dc.contributor.authorUrry, C. Megan
dc.contributor.authorMishra, Aayush
dc.contributor.authorPerreault-Levasseur, Laurence
dc.contributor.authorNatarajan, Priyamvada
dc.contributor.authorSanders, David B.
dc.contributor.authorNagai, Daisuke
dc.contributor.authorTian, Chuan
dc.contributor.authorCappelluti, Nico
dc.contributor.authorKartaltepe, Jeyhan S.
dc.contributor.authorPowell, Meredith C.
dc.contributor.authorRau, Amrit
dc.contributor.authorTreister, Ezequiel
dc.date.accessioned2024-04-15T08:00:17Z
dc.date.available2024-04-15T08:00:17Z
dc.date.issued2023
dc.description.abstractWe use the Galaxy Morphology Posterior Estimation Network (GaMPEN) to estimate morphological parameters and associated uncertainties for & SIM;8 million galaxies in the Hyper Suprime-Cam Wide survey with z & LE; 0.75 and m & LE; 23. GaMPEN is a machine-learning framework that estimates Bayesian posteriors for a galaxy's bulge-to-total light ratio (L ( B )/L ( T )), effective radius (R ( e )), and flux (F). By first training on simulations of galaxies and then applying transfer learning using real data, we trained GaMPEN with <1% of our data set. This two-step process will be critical for applying machine-learning algorithms to future large imaging surveys, such as the Rubin-Legacy Survey of Space and Time, the Nancy Grace Roman Space Telescope, and Euclid. By comparing our results to those obtained using light profile fitting, we demonstrate that GaMPEN's predicted posterior distributions are well calibrated (& LSIM;5% deviation) and accurate. This represents a significant improvement over light profile fitting algorithms, which underestimate uncertainties by as much as & SIM;60%. For an overlapping subsample, we also compare the derived morphological parameters with values in two external catalogs and find that the results agree within the limits of uncertainties predicted by GaMPEN. This step also permits us to define an empirical relationship between the Sersic index and L ( B )/L ( T ) that can be used to convert between these two parameters. The catalog presented here represents a significant improvement in size (& SIM;10x), depth (& SIM;4 mag), and uncertainty quantification over previous state-of-the-art bulge+disk decomposition catalogs. With this work, we also release GaMPEN's source code and trained models, which can be adapted to other data sets.
dc.description.funderPontificia Universidad Catolica de Chile
dc.format.extent32 páginas
dc.fuente.origenWOS
dc.identifier.doi10.3847/1538-4357/acd546
dc.identifier.eissn1538-4357
dc.identifier.isbn978-1-119-52131-0
dc.identifier.issn0004-637X
dc.identifier.pubmedidMEDLINE:34444039
dc.identifier.scopusidSCOPUS_ID:85140131661
dc.identifier.urihttps://doi.org/10.3847/1538-4357/acd546
dc.identifier.urihttps://repositorio.uc.cl/handle/11534/85067
dc.identifier.wosidWOS:001047913900001
dc.information.autorucInstituto de Astrofísica; Treister, Ezequiel; 0000-0001-7568-6412; 1031846
dc.issue.numero2
dc.language.isoen
dc.nota.accesoContenido completo
dc.pagina.final21
dc.pagina.inicio8
dc.publisherWiley
dc.relation.ispartofCuadernos de Geografia: Revista Colombiana de Geografia
dc.revistaThe Astrophysical Journal
dc.rightsacceso abierto
dc.subjectVivienda progresiva
dc.subjectApego barrial
dc.subjectRedes sociales vecinales
dc.subject.ddc520
dc.subject.deweyAstronomíaes_ES
dc.titleMorphological Parameters and Associated Uncertainties for 8 Million Galaxies in the Hyper Suprime-Cam Wide Survey
dc.typeartículo
dc.volumen953
sipa.codpersvinculados1031846
sipa.indexWOS
sipa.trazabilidadCarga WOS-SCOPUS;15-04-2024
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