ALMA survey of a massive node of the Cosmic Web at z ∼ 3 - II. A dynamically cold and massive disk galaxy in the proximity of a hyper-luminous quasar

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Volume 701 (September 2025)

A&A, 701 (2025) A120

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Table 1.

Line and continuum flux measurements, luminosity estimates, and derived quantities of the sources.

	QSO CTS G18.01			MQN01-QC
RA (ICRS)	00:41:31.443			00:41:31.463
Dec (ICRS)	−49:36:11.703			−49:36:12.943

Line ⁽¹⁾	CO(4−3)		CO(9−8)	CO(4−3) ^( † )	CO(9−8) ^( ‡ )
	systemic comp.	blueshifted broad comp.

Δv_QSO (km s⁻¹)	−	$- 307_{- 137}^{+ 125}$ $-307^{+125}_{-137}$	$- 36_{- 44}^{+ 40}$ $-36^{+40}_{-44}$	$- 241_{- 70}^{+ 77}$ $-241^{+77}_{-70}$	−
z_CO	$3 . 2510_{- 0.0004}^{+ 0.0004}$ $3.2510^{+0.0004}_{-0.0004}$	$3 . 2468_{- 0.0022}^{+ 0.0018}$ $3.2468^{+0.0018}_{-0.0022}$	$3 . 2504_{- 0.0004}^{+ 0.0005}$ $3.2504^{+0.0005}_{-0.0004}$	$3 . 2475_{- 0.0010}^{+ 0.0012}$ $3.2475^{+0.0012}_{-0.0010}$	−
FWHM_CO (km s⁻¹)	$404_{- 66}^{+ 64}$ $404^{+64}_{-66}$	$717_{- 187}^{+ 225}$ $717^{+225}_{-187}$	$556_{- 115}^{+ 128}$ $556^{+128}_{-115}$	$796_{- 44}^{+ 55}$ $796^{+55}_{-44}$	−
F_CO (Jy km s⁻¹) ⁽¹⁾	$0 . 48_{- 0.16}^{+ 0.13}$ $0.48^{+0.13}_{-0.16}$	$0 . 32_{- 0.14}^{+ 0.17}$ $0.32^{+0.17}_{-0.14}$	$1 . 06_{- 0.18}^{+ 0.20}$ $1.06^{+0.20}_{-0.18}$	$1 . 1_{- 0.3}^{+ 0.3}$ $1.1^{+0.3}_{-0.3}$	< 0.3
L_CO (10⁸ L_⊙)	$0 . 44_{- 0.15}^{+ 0.12}$ $0.44^{+0.12}_{-0.15}$	$0 . 30_{- 0.13}^{+ 0.16}$ $0.30^{+0.16}_{-0.13}$	$2 . 2_{- 0.4}^{+ 0.4}$ $2.2^{+0.4}_{-0.4}$	$1 . 0_{- 0.2}^{+ 0.3}$ $1.0^{+0.3}_{-0.2}$	< 0.3
L′_CO (10¹⁰ K km s⁻¹ pc²)	$1 . 4_{- 0.5}^{+ 0.4}$ $1.4^{+0.4}_{-0.5}$	$1 . 0_{- 0.4}^{+ 0.5}$ $1.0^{+0.5}_{-0.4}$	$0 . 62_{- 0.10}^{+ 0.12}$ $0.62^{+0.12}_{-0.10}$	$3 . 3_{- 0.8}^{+ 0.8}$ $3.3^{+0.8}_{-0.8}$	< 0.9

Continuum ⁽²⁾	3 mm		1.2 mm	3 mm	1.2 mm

F_peak (mJy beam⁻¹)	0.072 ± 0.004		0.99 ± 0.04	0.043 ± 0.004	1.63 ± 0.04
F_2σ (mJy)	0.092 ± 0.008		−	0.091 ± 0.008	−

Notes. ⁽¹⁾In the case of the CO(4−3) line of the QSO host and MQN01-QC galaxy, the best-fit parameters of the composite model are reported. ⁽²⁾The measurements of the 1.2 mm continuum fluxes are taken from Paper I, where the low spatial resolution of the band 6 mosaic observations makes the emission from the two sources partially blended. The reported measurements were obtained through a single-pixel analysis, thus minimizing the flux contamination. ^( † )The parameter estimates reported in this column are the flux-weighted average velocity shift and redshift, the total full width at half maximum, and the flux and luminosity of the best-fit composite model of the line profile, respectively. ^( ‡ )The reported values correspond to 3σ upper limits assuming FWHM = 750 km s⁻¹.

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