Please use this identifier to cite or link to this item:
http://hdl.handle.net/20.500.12386/31809
DC Field | Value | Language |
---|---|---|
dc.contributor.author | Reeves, Andrew M. M. | en_US |
dc.contributor.author | Balogh, Michael L. | en_US |
dc.contributor.author | van der Burg, Remco F. J. | en_US |
dc.contributor.author | Finoguenov, Alexis | en_US |
dc.contributor.author | Kukstas, Egidijus | en_US |
dc.contributor.author | McCarthy, Ian G. | en_US |
dc.contributor.author | Webb, Kristi | en_US |
dc.contributor.author | Muzzin, Adam | en_US |
dc.contributor.author | McGee, Sean | en_US |
dc.contributor.author | Rudnick, Gregory | en_US |
dc.contributor.author | BIVIANO, ANDREA | en_US |
dc.contributor.author | Cerulo, Pierluigi | en_US |
dc.contributor.author | Chan, Jeffrey C. C. | en_US |
dc.contributor.author | Cooper, M. C. | en_US |
dc.contributor.author | Demarco, Ricardo | en_US |
dc.contributor.author | Jablonka, Pascale | en_US |
dc.contributor.author | DE LUCIA, GABRIELLA | en_US |
dc.contributor.author | Vulcani, Benedetta | en_US |
dc.contributor.author | Wilson, Gillian | en_US |
dc.contributor.author | Yee, Howard K. C. | en_US |
dc.contributor.author | Zaritsky, Dennis | en_US |
dc.date.accessioned | 2022-03-22T15:37:16Z | - |
dc.date.available | 2022-03-22T15:37:16Z | - |
dc.date.issued | 2021 | en_US |
dc.identifier.issn | 0035-8711 | en_US |
dc.identifier.uri | http://hdl.handle.net/20.500.12386/31809 | - |
dc.description.abstract | We use photometric redshifts and statistical background subtraction to measure stellar mass functions in galaxy group-mass (4.5-8 × 10<SUP>13</SUP> M<SUB>⊙</SUB>) haloes at 1 < z < 1.5. Groups are selected from COSMOS and SXDF, based on X-ray imaging and sparse spectroscopy. Stellar mass (M<SUB>stellar</SUB>) functions are computed for quiescent and star-forming galaxies separately, based on their rest-frame UVJ colours. From these we compute the quiescent fraction and quiescent fraction excess (QFE) relative to the field as a function of M<SUB>stellar</SUB>. QFE increases with M<SUB>stellar</SUB>, similar to more massive clusters at 1 < z < 1.5. This contrasts with the apparent separability of M<SUB>stellar</SUB> and environmental factors on galaxy quiescent fractions at z ~ 0. We then compare our results with higher mass clusters at 1 < z < 1.5 and lower redshifts. We find a strong QFE dependence on halo mass at fixed M<SUB>stellar</SUB>; well fit by a logarithmic slope of d(QFE)/dlog (M<SUB>halo</SUB>) ~ 0.24 ± 0.04 for all M<SUB>stellar</SUB> and redshift bins. This dependence is in remarkably good qualitative agreement with the hydrodynamic simulation BAHAMAS, but contradicts the observed dependence of QFE on M<SUB>stellar</SUB>. We interpret the results using two toy models: one where a time delay until rapid (instantaneous) quenching begins upon accretion to the main progenitor ('no pre-processing') and one where it starts upon first becoming a satellite ('pre-processing'). Delay times appear to be halo mass-dependent, with a significantly stronger dependence required without pre-processing. We conclude that our results support models in which environmental quenching begins in low-mass (<10<SUP>14</SUP>M<SUB>⊙</SUB>) haloes at z > 1. | en_US |
dc.language.iso | eng | en_US |
dc.title | The GOGREEN survey: dependence of galaxy properties on halo mass at z > 1 and implications for environmental quenching | en_US |
dc.type | Article | - |
dc.identifier.doi | 10.1093/mnras/stab1955 | en_US |
dc.identifier.scopus | 2-s2.0-85112584022 | en_US |
dc.identifier.url | https://academic.oup.com/mnras/article/506/3/3364/6318877 | en_US |
dc.identifier.url | http://arxiv.org/abs/2107.03425v1 | en_US |
dc.relation.medium | STAMPA | en_US |
dc.relation.volume | 506 | en_US |
dc.relation.issue | 3 | en_US |
dc.relation.firstpage | 3364 | en_US |
dc.relation.lastpage | 3384 | en_US |
dc.type.referee | REF_1 | en_US |
dc.description.international | sì | en_US |
dc.relation.scientificsector | FIS/05 - ASTRONOMIA E ASTROFISICA | en_US |
dc.relation.journal | MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY | en_US |
dc.type.miur | 262 Articolo in rivista | - |
dc.identifier.adsbibcode | 2021MNRAS.506.3364R | en_US |
dc.relation.ercsector | ERC sectors::Physical Sciences and Engineering::PE9 Universe sciences: astro-physics/chemistry/biology; solar systems; stellar, galactic and extragalactic astronomy, planetary systems, cosmology, space science, instrumentation | en_US |
dc.description.apc | no | en_US |
dc.description.oa | 1 – prodotto con file in versione Open Access (allegare il file al passo 5-Carica) | en_US |
item.openairecristype | http://purl.org/coar/resource_type/c_18cf | - |
item.openairetype | Article | - |
item.languageiso639-1 | en | - |
item.cerifentitytype | Publications | - |
item.grantfulltext | open | - |
item.fulltext | With Fulltext | - |
crisitem.author.dept | O.A. Trieste | - |
crisitem.author.dept | O.A. Trieste | - |
crisitem.author.dept | O.A. Padova | - |
crisitem.author.orcid | 0000-0002-0857-0732 | - |
crisitem.author.orcid | 0000-0002-6220-9104 | - |
crisitem.author.orcid | 0000-0003-0980-1499 | - |
crisitem.journal.journalissn | 0035-8711 | - |
crisitem.journal.ance | E112946 | - |
Appears in Collections: | 1.01 Articoli in rivista |
Files in This Item:
File | Description | Size | Format | |
---|---|---|---|---|
2107.03425.pdf | preprint | 2.91 MB | Adobe PDF | View/Open |
stab1955.pdf | Pdf editoriale | 7.26 MB | Adobe PDF | View/Open |
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