COALAS - III. The ATCA CO(1–0) look at the growth and death of Hα emitters in the Spiderweb protocluster at z = 2.16

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Volume 696 (April 2025)

A&A, 696 (2025) A236

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Table A.2.

List of protocluster (PCL), protocluster core (PCL-core), cluster (CL), and field samples with CO(1-0) emitters from the literature at z > 1.5.

Name	Type	Redshift	N	$\tilde{{L'}_{CO (1 - 0)}}$ $\widetilde{{L\prime}_{\mathrm{CO(1-0)}}}$ ^a	Area	Facility	Reference
				(10¹⁰ K km s⁻¹ pc²)	(arcmin²)
PKS 1138-262	PCL	2.16	46	3.5 ± 2.2	25.8	ATCA	Jin et al. (2021)
CLJ 1001+0220^b	PCL	2.51	14	2.2 ± 4.2	5.1^a	VLA	Wang et al. (2018)
CLJ 1001+0220	PCL	2.51	8	1.7 ± 1.4	2.6	VLA	Champagne et al. (2021)
USS 1558-003	PCL	2.53	3	1.5 ± 1.0	1.5	VLA	Tadaki et al. (2014)
HXMM20	PCL-core	2.60	5	5.0 ± 2.6	1.6	VLA	Gómez-Guijarro et al. (2019)
XMM-LSS J02182-05102	CL	1.62	2	1.7 ± 1.3	0.8	VLA	Rudnick et al. (2017)

COSMOS	Field	1.6 < z < 3.0	10	4.8 ± 2.2	-	VLA	Kaasinen et al. (2019)
HUDF	Field	2.0 < z < 2.7	6	1.7 ± 1.0	2.4	VLA	Riechers et al. (2020)
COSMOS, GOODS-N	Field	2.0 < z < 2.8	51	2.9 ± 3.4	-	VLA	Pavesi et al. (2018)
HDF	Field	2.2 < z < 2.5	5	7.6 ± 3.5	4.3	VLA	Ivison et al. (2011)
COSMOS, UDS, GOODS-N, EGS	Field	2.2 < z < 4.4	13	10.6 ± 3.7	-	VLA	Frias Castillo et al. (2023)

Notes.

^(a)

Median CO(1-0) luminosity ( $\tilde{{L'}_{CO (1 - 0)}}$ $\widetilde{{L\prime}_{\mathrm{CO(1-0)}}}$ ) and standard deviation.

^(b)

Wang et al. (2018) detect sources within twice the full width at half power (FWHP) per pointing and thus, its surveyed area takes this into account. Other works cited in this table restrict their surveyed areas to a single FWHP per pointing.

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