Cosmic filaments delay quenching inside clusters
Entidad
UAM. Departamento de Física TeóricaEditor
Royal Astronomical Society; Oxford University PressFecha de edición
2022-02-10Cita
10.1093/mnras/stac300
Monthly Notices of the Royal Astronomical Society 512.1 (2022): 926-944
ISSN
0035-8711 (print); 1365-2966 (online)DOI
10.1093/mnras/stac300Proyecto
info:eu-repo/grantAgreement/EC/H2020/734374/EU//LACEGAL; Gobierno de España. PGC2018-094975-C21Versión del editor
https://doi.org/10.1093/mnras/stac300Materias
Galaxies: Clusters: General; Galaxies: Star Formation; Large-Scale Structure of Universe; FísicaNota
This is a pre-copyedited, author-produced PDF of an article accepted for publication in Monthly Notices of the Royal Astronomical Society following peer review. The version of record Monthly Notices of the Royal Astronomical Society 512.1 (2022): 926-944 is available online at: https://academic.oup.com/mnras/article-abstract/512/1/926/6526336Derechos
© 2022 The Author(s) Published by Oxford University Press on behalf of Royal Astronomical SocietyResumen
We investigate how large-scale cosmic filaments impact the quenching of galaxies within one virial radius of 324 simulated clusters from The Three Hundred project. We track cosmic filaments with the versatile, observation-friendly program DisPerSE and identify haloes hosting galaxies with VELOCIRaptor. We find that cluster galaxies close to filaments tend to be more star forming, bluer, and contain more cold gas than their counterparts further away from filaments. This effect is recovered at all stellar masses. This is in stark contrast with galaxies residing outside of clusters, where galaxies close to filaments show clear signs of density related pre-processing. We first show that the density contrast of filaments is reduced inside the intra-cluster medium. Moreover, examination of flows around and into cluster galaxies shows that the gas flows in intra-cluster filaments are colder and tend to stream along with galaxies in their midst, partially shielding them from strangulation by the hot, dense intra-cluster medium. This also preserves accretion on to satellites and limit ram pressure
Lista de ficheros
Google Scholar:Kotecha, Sachin
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Welker, Charlotte
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Zhou, Zihan
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Wadsley, James
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Kraljic, Katarina
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Sorce, Jenny
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Rasia, Elena
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Roberts, Ian
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Gray, Meghan
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Yepes Alonso, Gustavo
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Cui, Weiguang
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