TY - JOUR
T1 - NOEMA formIng Cluster survEy (NICE)
T2 - Characterizing eight massive galaxy groups at 1.5 < z < 4 in the COSMOS field
AU - Sillassen, Nikolaj B.
AU - Jin, Shuowen
AU - Magdis, Georgios E.
AU - Daddi, Emanuele
AU - Wang, Tao
AU - Lu, Shiying
AU - Sun, Hanwen
AU - Arumugam, Vinod
AU - Liu, Daizhong
AU - Brinch, Malte
AU - D'eugenio, Chiara
AU - Gobat, Raphael
AU - Gómez-Guijarro, Carlos
AU - Rich, Michael
AU - Schinnerer, Eva
AU - Strazzullo, Veronica
AU - Tan, Qinghua
AU - Valentino, Francesco
AU - Wang, Yijun
AU - Xiao, Mengyuan
AU - Zhou, Luwenjia
AU - Blánquez-Sesé, David
AU - Cai, Zheng
AU - Chen, Yanmei
AU - Ciesla, Laure
AU - Dai, Yu
AU - Delvecchio, Ivan
AU - Elbaz, David
AU - Finoguenov, Alexis
AU - Gao, Fangyou
AU - Gu, Qiusheng
AU - Hale, Catherine
AU - Hao, Qiaoyang
AU - Huang, Jiasheng
AU - Jarvis, Matt
AU - Kalita, Boris
AU - Ke, Xu
AU - Le Bail, Aurelien
AU - Magnelli, Benjamin
AU - Shi, Yong
AU - Vaccari, Mattia
AU - Whittam, Imogen
AU - Yang, Tiancheng
AU - Zhang, Zhiyu
N1 - Publisher Copyright:
© The Authors 2024.
PY - 2024
Y1 - 2024
N2 - The Northern Extended Millimeter Array (NOEMA) formIng Cluster survEy (NICE) is a NOEMA large programme targeting 69 massive galaxy group candidates at z > 2 over six deep fields with a total area of 46 deg2. Here we report the spectroscopic confirmation of eight massive galaxy groups at redshifts 1.65 ≤ z ≤ 3.61 in the Cosmic Evolution Survey (COSMOS) field. Homogeneously selected as significant overdensities of red IRAC sources that have red Herschel colours, four groups in this sample are confirmed by CO and [CI] line detections of multiple sources with NOEMA 3 mm observations, three are confirmed with Atacama Large Millimeter Array (ALMA) observations, and one is confirmed by Ha emission from Subaru/FMOS spectroscopy. Using rich ancillary data in the far-infrared and sub-millimetre, we constructed the integrated farinfrared spectral energy distributions for the eight groups, obtaining a total infrared star formation rate (SFR) of 260-1300 M⊙ yr-1. We adopted six methods for estimating the dark matter masses of the eight groups, including stellar mass to halo mass relations, overdensity with galaxy bias, and NFW profile fitting to radial stellar mass densities. We find that the radial stellar mass densities of the eight groups are consistent with a NFW profile, supporting the idea that they are collapsed structures hosted by a single dark matter halo. The best halo mass estimates are log(Mh/M⊙) = 12.8-13.7 with a general uncertainty of 0.3 dex. Based on the halo mass estimates, we derived baryonic accretion rates (BARs) of (1-8) × 103 M⊙/yr for this sample. Together with massive groups in the literature, we find a quasi-linear correlation between the integrated SFR/BAR ratio and the theoretical halo mass limit for cold streams, Mstream/Mh, with SFR/BAR = 10-0.46±0.22 (Mstream/Mh)0.71±0.16 with a scatter of 0.40 dex. Furthermore, we compared the halo masses and the stellar masses with simulations, and find that the halo masses of all structures are consistent with those of progenitors of Mh(z = 0) > 1014 M⊙ galaxy clusters, and that the most massive central galaxies have stellar masses consistent with those of the brightest cluster galaxy progenitors in the TNG300 simulation. Above all, the results strongly suggest that these massive structures are in the process of forming massive galaxy clusters via baryonic and dark matter accretion.
AB - The Northern Extended Millimeter Array (NOEMA) formIng Cluster survEy (NICE) is a NOEMA large programme targeting 69 massive galaxy group candidates at z > 2 over six deep fields with a total area of 46 deg2. Here we report the spectroscopic confirmation of eight massive galaxy groups at redshifts 1.65 ≤ z ≤ 3.61 in the Cosmic Evolution Survey (COSMOS) field. Homogeneously selected as significant overdensities of red IRAC sources that have red Herschel colours, four groups in this sample are confirmed by CO and [CI] line detections of multiple sources with NOEMA 3 mm observations, three are confirmed with Atacama Large Millimeter Array (ALMA) observations, and one is confirmed by Ha emission from Subaru/FMOS spectroscopy. Using rich ancillary data in the far-infrared and sub-millimetre, we constructed the integrated farinfrared spectral energy distributions for the eight groups, obtaining a total infrared star formation rate (SFR) of 260-1300 M⊙ yr-1. We adopted six methods for estimating the dark matter masses of the eight groups, including stellar mass to halo mass relations, overdensity with galaxy bias, and NFW profile fitting to radial stellar mass densities. We find that the radial stellar mass densities of the eight groups are consistent with a NFW profile, supporting the idea that they are collapsed structures hosted by a single dark matter halo. The best halo mass estimates are log(Mh/M⊙) = 12.8-13.7 with a general uncertainty of 0.3 dex. Based on the halo mass estimates, we derived baryonic accretion rates (BARs) of (1-8) × 103 M⊙/yr for this sample. Together with massive groups in the literature, we find a quasi-linear correlation between the integrated SFR/BAR ratio and the theoretical halo mass limit for cold streams, Mstream/Mh, with SFR/BAR = 10-0.46±0.22 (Mstream/Mh)0.71±0.16 with a scatter of 0.40 dex. Furthermore, we compared the halo masses and the stellar masses with simulations, and find that the halo masses of all structures are consistent with those of progenitors of Mh(z = 0) > 1014 M⊙ galaxy clusters, and that the most massive central galaxies have stellar masses consistent with those of the brightest cluster galaxy progenitors in the TNG300 simulation. Above all, the results strongly suggest that these massive structures are in the process of forming massive galaxy clusters via baryonic and dark matter accretion.
KW - Galaxies: clusters: general
KW - Galaxies: evolution
KW - Galaxies: high-redshift
KW - Submillimeter: galaxies
U2 - 10.1051/0004-6361/202450760
DO - 10.1051/0004-6361/202450760
M3 - Journal article
AN - SCOPUS:85206331827
SN - 0004-6361
VL - 690
JO - Astronomy and Astrophysics
JF - Astronomy and Astrophysics
M1 - A55
ER -