Spectroscopic Confirmation of a Protocluster at z = 3.37 with a High Fraction of Quiescent Galaxies

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dc.contributor.authorMcConachie, I.
dc.contributor.authorWilson, G.
dc.contributor.authorForrest, B.
dc.contributor.authorMarsan, Z.
dc.contributor.authorMuzzin, A.
dc.contributor.authorCooper, M.
dc.contributor.authorAnnunziatella, M.
dc.contributor.authorMarchesini, D.
dc.contributor.authorChan, J.
dc.contributor.authorGomez, P.
dc.contributor.authorAbdullah, M.
dc.contributor.authorSaracco, P.
dc.contributor.authorNantais, J.
dc.date.accessioned2022-08-02T17:50:54Z
dc.date.available2022-08-02T17:50:54Z
dc.date.issued2022-02
dc.descriptionIndexación: Scopus.es
dc.description.abstractWe report the discovery of MAGAZ3NE J095924+022537, a spectroscopically confirmed protocluster at z=3.3665-0.0012+0.0009 around a spectroscopically confirmed UVJ-quiescent ultramassive galaxy (UMG; M=2.34-0.34+0.23×1011MȮ ) in the COSMOS UltraVISTA field. We present a total of 38 protocluster members (14 spectroscopic and 24 photometric), including the UMG. Notably, and in marked contrast to protoclusters previously reported at this epoch that have been found to contain predominantly star-forming members, we measure an elevated fraction of quiescent galaxies relative to the coeval field ( 73.3-16.9+26.7% versus 11.6-4.9+7.1% for galaxies with stellar mass M ≥ 1011 M Ȯ). This high quenched fraction provides a striking and important counterexample to the seeming ubiquitousness of star-forming galaxies in protoclusters at z > 2 and suggests, rather, that protoclusters exist in a diversity of evolutionary states in the early universe. We discuss the possibility that we might be observing either "early mass quenching"or nonclassical "environmental quenching."We also present the discovery of MAGAZ3NE J100028+023349, a second spectroscopically confirmed protocluster, at a very similar redshift of z=3.3801-0.0281+0.0213 . We present a total of 20 protocluster members, 12 of which are photometric and eight spectroscopic including a poststarburst UMG ( M=2.95-0.20+0.21×1011MȮ ). Protoclusters MAGAZ3NE J0959 and MAGAZ3NE J1000 are separated by 18′ on the sky (35 comoving Mpc), in good agreement with predictions from simulations for the size of "Coma"-type cluster progenitors at this epoch. It is highly likely that the two UMGs are the progenitors of Brightest Cluster Galaxies seen in massive virialized clusters at lower redshift.es
dc.description.urihttps://iopscience-iop-org.recursosbiblioteca.unab.cl/article/10.3847/1538-4357/ac2b9f
dc.identifier.citationAstrophysical Journal, Volume 926, Issue 11, February 2022, Article number 37es
dc.identifier.doi10.3847/1538-4357/ac2b9f
dc.identifier.issn0004-637X
dc.identifier.urihttps://repositorio.unab.cl/xmlui/handle/ria/23413
dc.language.isoenes
dc.publisherIOP Publishing Ltdes
dc.rights.licenseAttribution 4.0 International (CC BY 4.0)
dc.rights.urihttps://journals.aas.org/article-charges-and-copyright/#licensing
dc.subjectStar Formationes
dc.subjectGalaxieses
dc.subjectGalactic Evolutiones
dc.titleSpectroscopic Confirmation of a Protocluster at z = 3.37 with a High Fraction of Quiescent Galaxieses
dc.typeArtículoes
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