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dc.contributor.authorPandya, Viraj
dc.contributor.authorPrimack, Joel
dc.contributor.authorBehroozi, Peter
dc.contributor.authorDekel, Avishai
dc.contributor.authorZhang, Haowen
dc.contributor.authorEckholm, Elliot
dc.contributor.authorFaber, Sandra M
dc.contributor.authorFerguson, Henry C
dc.contributor.authorGiavalisco, Mauro
dc.contributor.authorGuo, Yicheng
dc.contributor.authorHathi, Nimish
dc.contributor.authorKodra, Dritan
dc.contributor.authorKoekemoer, Anton M
dc.contributor.authorKoo, David C
dc.contributor.authorNewman, Jeffrey
dc.contributor.authorvan der Wel, Arjen
dc.date.accessioned2019-10-09T19:28:43Z
dc.date.available2019-10-09T19:28:43Z
dc.date.issued2019-08-02
dc.identifier.citationViraj Pandya, Joel Primack, Peter Behroozi, Avishai Dekel, Haowen Zhang, Elliot Eckholm, Sandra M Faber, Henry C Ferguson, Mauro Giavalisco, Yicheng Guo, Nimish Hathi, Dritan Kodra, Anton M Koekemoer, David C Koo, Jeffrey Newman, Arjen van der Wel, Can intrinsic alignments of elongated low-mass galaxies be used to map the cosmic web at high redshift?, Monthly Notices of the Royal Astronomical Society, Volume 488, Issue 4, October 2019, Pages 5580–5593, https://doi.org/10.1093/mnras/stz2129en_US
dc.identifier.issn0035-8711
dc.identifier.doi10.1093/mnras/stz2129
dc.identifier.urihttp://hdl.handle.net/10150/634712
dc.description.abstractHubble Space Telescope observations show that low-mass () galaxies at high redshift (z= 1.0-2.5) tend to be elongated (prolate) rather than disky (oblate) or spheroidal. This is explained in zoom-in cosmological hydrodynamical simulations by the fact that these galaxies are forming in cosmic web filaments where accretion happens preferentially along the direction of elongation. We ask whether the elongated morphology of these galaxies allows them to be used as effective tracers of cosmic web filaments at high redshift via their intrinsic alignments. Using mock light cones and spectroscopically confirmed galaxy pairs from the Cosmic Assembly Near-infared Deep Extragalactic Legacy Survey (CANDELS), we test two types of alignments: (1) between the galaxy major axis and the direction to nearby galaxies of any mass and (2) between the major axes of nearby pairs of low-mass, likely prolate, galaxies. The mock light cones predict strong signals in 3D real space, 3D redshift space, and 2D projected redshift space for both types of alignments (assuming prolate galaxy orientations are the same as those of their host prolate haloes), but we do not detect significant alignment signals in CANDELS observations. However, we show that spectroscopic redshifts have been obtained for only a small fraction of highly elongated galaxies, and accounting for spectroscopic incompleteness and redshift errors significantly degrades the 2D mock signal. This may partly explain the alignment discrepancy and highlights one of several avenues for future work.en_US
dc.description.sponsorshipNational Science FoundationNational Science Foundation (NSF) [1339067]; NASA from the Space Telescope Science Institute [HST-AR-14578.001-A]; NASANational Aeronautics & Space Administration (NASA) [NAS 5-26555]en_US
dc.language.isoenen_US
dc.publisherOXFORD UNIV PRESSen_US
dc.rightsCopyright © 2019 The Author(s) Published by Oxford University Press on behalf of the Royal Astronomical Society.en_US
dc.subjectgalaxies: dwarfen_US
dc.subjectgalaxies: high-redshiften_US
dc.subjectgalaxies: statisticsen_US
dc.subjectgalaxies: structureen_US
dc.subjectdark matteren_US
dc.subjectlarge-scale structure of Universeen_US
dc.titleCan intrinsic alignments of elongated low-mass galaxies be used to map the cosmic web at high redshift?en_US
dc.typeArticleen_US
dc.contributor.departmentUniv Arizona, Dept Astronen_US
dc.contributor.departmentUniv Arizona, Steward Observen_US
dc.identifier.journalMONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETYen_US
dc.description.collectioninformationThis item from the UA Faculty Publications collection is made available by the University of Arizona with support from the University of Arizona Libraries. If you have questions, please contact us at repository@u.library.arizona.edu.en_US
dc.eprint.versionFinal published versionen_US
dc.source.volume488
dc.source.issue4
dc.source.beginpage5580-5593
refterms.dateFOA2019-10-09T19:28:44Z


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