English (United Kingdom)

https://curated-unify.zendy.io/wp-json/zendy-region/v1/featured_content/oa?rat=en

https://curated-unify.zendy.io/wp-json/zendy-region/v1/highlighted_journal/

Global: Zendy Plus annual

Presents the access of premium content as premium feature

Premium Content

Presents the keyphrase highlighting as premium feature

Keyphrase Highlighting

Presents the summarisation as premium feature

Summarisation

Insights

Presents the pdf analysis as premium feature

PDF Analysis

Presents the zaia usage as premium feature

ZAIA

Global: Zendy Tools annual

Global: Zendy Free Plan

Global: Zendy Tools monthly

Global: Zendy Plus monthly

In order to connect galaxy clusters to their progenitor protoclusters, wemust constrain the star formation histories within their member galaxies andthe timescale of virial collapse. In this paper we characterize the complexstar-forming properties of a $z=2.5$ protocluster in the COSMOS field usingALMA dust continuum and new VLA CO(1-0) observations of two filamentsassociated with the structure, sometimes referred to as the "Hyperion"protocluster. We focus in particular on the protocluster "core" which haspreviously been suggested as the highest redshift bona fide galaxy clustertraced by extended X-ray emission in a stacked Chandra/XMM image. We re-analyzethis data and refute these claims, finding that at least 40 $\pm$ 17% ofextended X-ray sources of similar luminosity and size at this redshift ariseinstead from Inverse Compton scattering off recently extinguished radiogalaxies rather than intracluster medium. Using ancillary COSMOS data, we alsoconstrain the SEDs of the two filaments' eight constituent galaxies from therest-frame UV to radio. We do not find evidence for enhanced star formationefficiency in the core and conclude that the constituent galaxies are alreadymassive (M$_{\star} \approx 10^{11} M_{\odot}$), with molecular gas reservoirs$>10^{10} M_{\odot}$ that will be depleted within 200-400 Myr. Finally, wecalculate the halo mass of the nested core at $z=2.5$ and conclude that it willcollapse into a cluster of 2-9 $\times 10^{14} M_{\odot}$, comparable to thesize of the Coma cluster at $z=0$ and accounting for at least 50% of the totalestimated halo mass of the extended "Hyperion" structure.

Comprehensive Gas Characterization of a $z= 2.5$ Protocluster: A Cluster Core Caught in the Beginning of Virialization?