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dc.contributor.authorEndsley, Ryan
dc.contributor.authorBehroozi, Peter
dc.contributor.authorStark, Daniel P
dc.contributor.authorWilliams, Christina C
dc.contributor.authorRobertson, Brant E
dc.contributor.authorRieke, Marcia
dc.contributor.authorGottlöber, Stefan
dc.contributor.authorYepes, Gustavo
dc.date.accessioned2020-04-13T20:59:46Z
dc.date.available2020-04-13T20:59:46Z
dc.date.issued2020-02-04
dc.identifier.citationRyan Endsley, Peter Behroozi, Daniel P Stark, Christina C Williams, Brant E Robertson, Marcia Rieke, Stefan Gottlöber, Gustavo Yepes, Clustering with JWST: Constraining galaxy host halo masses, satellite quenching efficiencies, and merger rates at z = 4−10, Monthly Notices of the Royal Astronomical Society, Volume 493, Issue 1, March 2020, Pages 1178–1196, https://doi.org/10.1093/mnras/staa324en_US
dc.identifier.issn0035-8711
dc.identifier.doi10.1093/mnras/staa324
dc.identifier.urihttp://hdl.handle.net/10150/640968
dc.description.abstractGalaxy clustering measurements can be used to constrain many aspects of galaxy evolution, including galaxy host halo masses, satellite quenching efficiencies, and merger rates. We simulate JWST galaxy clustering measurements at z similar to 4-10 by utilizing mock galaxy samples produced by an empirical model, the UNIVERSEMACHINE. We also adopt the survey footprints and typical depths of the planned joint NIRCam and NIRSpec Guaranteed Time Observation program planned for Cycle 1 to generate realistic JWST survey realizations and to model high-redshift galaxy selection completeness. We find that galaxy clustering will be measured with greater than or similar to 5 sigma significance at z similar to 4-10. Halo mass precisions resulting from Cycle 1 angular clustering measurements will be similar to 0.2 dex for faint (-18 greater than or similar to M-UV greater than or similar to -19) galaxies at z similar to 4-10 as well as similar to 0.3 dex for bright (M-UV similar to -20) galaxies at z similar to 4-7. Dedicated spectroscopic follow-up over similar to 150 arcmin(2) would improve these precisions by similar to 0.1 dex by removing chance projections and low-redshift contaminants. Future JWST observations will therefore provide the first constraints on the stellar-halo mass relation in the epoch of reionization and substantially clarify how this relation evolves at z > 4. We also find that similar to 1000 individual satellites will be identifiable at z similar to 4-8 with JWST, enabling strong tests of satellite quenching evolution beyond currently available data (z less than or similar to 2). Finally, we find that JWST observations can measure the evolution of galaxy major merger pair fractions at z similar to 4-8 with similar to 0.1-0.2 dex uncertainties. Such measurements would help determine the relative role of mergers to the build-up of stellar mass into the epoch of reionization.en_US
dc.language.isoenen_US
dc.publisherOXFORD UNIV PRESSen_US
dc.rightsCopyright © 2020 The Author(s). Published by Oxford University Press on behalf of the Royal Astronomical Society.en_US
dc.rights.urihttp://rightsstatements.org/vocab/InC/1.0/
dc.subjectgalaxies: high-redshiften_US
dc.subjectdark agesen_US
dc.subjectreionizationen_US
dc.subjectfirst starsen_US
dc.subjectcosmology: large-scale structure of Universeen_US
dc.titleClustering with JWST: Constraining galaxy host halo masses, satellite quenching efficiencies, and merger rates at z  = 4−10en_US
dc.typeArticleen_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.journaltitleMonthly Notices of the Royal Astronomical Society
dc.source.volume493
dc.source.issue1
dc.source.beginpage1178
dc.source.endpage1196
refterms.dateFOA2020-04-13T20:59:48Z


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