NOEMA formIng Cluster survEy (NICE): Characterizing eight massive galaxy groups at $1.5 &lt; z &lt; 4$ in the COSMOS field
Creators: name: Sillassen, Nikolaj B.
name: Jin, Shuowen
name: Magdis, Georgios E.
name: Daddi, Emanuele
name: Wang, Tao
name: Lu, Shiying
name: Sun, Hanwen
name: Arumugam, Vinod
name: Liu, Daizhong
name: Brinch, Malte
name: D'Eugenio, Chiara
name: Gobat, Raphael
name: Gómez-Guijarro, Carlos
name: Rich, Michael
name: Schinnerer, Eva
name: Strazzullo, Veronica
name: Tan, Qinghua
name: Valentino, Francesco
name: Wang, Yijun
name: Xiao, Mengyuan
name: Zhou, Luwenjia
name: Blánquez-Sesé, David
name: Cai, Zheng
name: Chen, Yanmei
name: Ciesla, Laure
name: Dai, Yu
name: Delvecchio, Ivan
name: Elbaz, David
name: Finoguenov, Alexis
name: Gao, Fangyou
name: Gu, Qiusheng
name: Hale, Catherine
name: Hao, Qiaoyang
name: Huang, Jiasheng
name: Jarvis, Matt
name: Kalita, Boris
name: Ke, Xu
name: Bail, Aurelien Le
name: Magnelli, Benjamin
name: Shi, Yong
name: Vaccari, Mattia
name: Whittam, Imogen
name: Yang, Tiancheng
name: Zhang, Zhiyu
Publisher: name: arXiv
Year: 2024
Subjects: subject: Astrophysics of Galaxies (astro-ph.GA)
subject: FOS: Physical sciences
subject: FOS: Physical sciences

description: The NOEMA formIng Cluster survEy (NICE) is a large program targeting 69 massive galaxy group candidates at $z&gt;2$ in six deep fields. We report spectroscopic confirmation of eight groups at $1.65\leq z\leq3.61$ in COSMOS. Homogeneously selected as significant overdensities of red IRAC sources with red Herschel colors, four groups are confirmed by CO and [CI] with NOEMA 3mm observations, three are confirmed with ALMA, and one is confirmed by H$α$ from Subaru/FMOS. We constructed the integrated FIR SEDs for the eight groups, obtaining total IR SFR $=260-1300~{\rm M_\odot}$~yr$^{-1}$. We adopted six methods to estimate the dark matter masses, including stellar mass to halo mass relations, overdensity with galaxy bias, and NFW profile fitting to radial stellar mass density. We found the radial stellar mass density are consistent with a NFW profile, supporting that they are collapsed structures hosted by a single dark matter halo. The best halo mass estimates are $\log(M_{\rm h}/{\rm M_\odot})=12.8-13.7$ with uncertainty of 0.3 dex. From halo mass estimates, we derive baryonic accretion rate ${\rm BAR}=(1-8)\times10^{3}\,{\rm M_{\odot}/yr}$ for this sample. We find a quasi-linear correlation between the integrated SFR/BAR and the theoretical halo mass limit for cold streams, $M_{\rm stream}/M_{\rm h}$, with ${\rm SFR/BAR}=10^{-0.46\pm0.22}\left({M_{\rm stream}/M_{\rm h}}\right)^{0.71\pm0.16}$ with a scatter of $0.40\,{\rm dex}$. Further, we compare halo masses and stellar masses with simulations, and find all structures are consistent with being progenitors of $M_{\rm h}(z=0)&gt;10^{14}\,{\rm M_{\odot}}$ galaxy clusters, and the most massive central galaxies have stellar masses consistent with brightest cluster galaxies (BCGs) progenitors in the TNG300 simulation. The results strongly suggest these structures are forming massive galaxy clusters via baryonic and dark matter accretion.
description: 44 pages (27pp appendix), 32 figures, 18 tables, accepted for publication in A&amp;A