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 2.

Mass budgets, dust characteristics, and morphological sizes of the quasar host and the MQN01-QC galaxy.

	QSO CTS G18.01	MQN01-QC
M_dyn(< r) (10¹¹ M_⊙)	disp: $0 . 13_{- 0.04}^{+ 0.06}$ $0.13^{+0.06}_{-0.04}$	$2 . 5_{- 1.1}^{+ 0.6}$ $2.5^{+0.6}_{-1.1}$ (< 4.1 kpc)
M_dyn(< r) (10¹¹ M_⊙)	rot: $0 . 7_{- 0.3}^{+ 0.8} (< 1.3 kpc)$ $0.7^{+0.8}_{-0.3}\,({ < }1.3\,\mathrm{kpc})$ ^( † )

M_⋆(< r) (10¹⁰ M_⊙)	−		$9 . 1_{- 1.1}^{+ 1.4}$ $9.1^{+1.4}_{-1.1}$ (< 2.3 kpc)

M_H2⁽¹⁾ (10¹⁰ (α_CO/1.7) M_⊙)	total: $4 . 6_{- 1.8}^{+ 2.0}$ $\,4.6^{+2.0}_{-1.8}$
	sys: $2 . 5_{- 1.4}^{+ 1.7}$ $\,2.5^{+1.7}_{-1.4}$	$6_{- 2}^{+ 3}$ $6^{+3}_{-2}$
	bulk: $3 . 5_{- 1.4}^{+ 2.0}$ $3.5^{+2.0}_{-1.4}$	$6_{- 2}^{+ 3}$ $6^{+3}_{-2}$

T_dust⁽²⁾ (K)	35 ± 5
log(M_dust/M_⊙)	$8 . 88_{- 0.09}^{+ 0.11}$ $8.88^{+0.11}_{-0.09}$	$8 . 83_{- 0.09}^{+ 0.11}$ $\mathbf{8.83^{+0.11}_{-0.09}}$
β	$1 . 01_{- 0.12}^{+ 0.13}$ $1.01^{+0.13}_{-0.12}$	$1 . 56_{- 0.11}^{+ 0.12}$ $\mathbf{1.56^{+0.12}_{-0.11}}$
L_FIR⁽³⁾ (10¹³ L_⊙)	$0 . 08_{- 0.03}^{+ 0.04}$ $0.08^{+0.04}_{-0.03}$	$0 . 27_{- 0.10}^{+ 0.15}$ $\mathbf{0.27^{+0.15}_{-0.10}}$
SFR_IR (M_⊙ yr⁻¹)	$124_{- 41}^{+ 60}$ $124^{+60}_{-41}$	$405_{- 149}^{+ 216}$ $\mathbf{405^{+216}_{-149}}$

T_dust⁽²⁾ (K)	45 ± 5
log(M_dust/M_⊙)	$8 . 73_{- 0.08}^{+ 0.08}$ $\mathbf{8.73^{+0.08}_{-0.08}}$	$8 . 68_{- 0.08}^{+ 0.08}$ $8.68^{+0.08}_{-0.08}$
β	$0 . 92_{- 0.11}^{+ 0.12}$ $\mathbf{0.92^{+0.12}_{-0.11}}$	$1 . 47_{- 0.11}^{+ 0.11}$ $1.47^{+0.11}_{-0.11}$
L_FIR⁽³⁾ (10¹³ L_⊙)	$0 . 16_{- 0.05}^{+ 0.07}$ $\mathbf{0.16^{+0.07}_{-0.05}}$	$0 . 6_{- 0.2}^{+ 0.3}$ $0.6^{+0.3}_{-0.2}$
SFR_IR (M_⊙ yr⁻¹)	$237_{- 69}^{+ 97}$ $\mathbf{237^{+97}_{-69}}$	$862_{- 293}^{+ 403}$ $862^{+403}_{-293}$

R_{1/2, CO(4 − 3)} (kpc)	1.31 ± 0.15	2.52 ± 0.01 ^( ‡ )
R_{1/2, 3 mm} (kpc)	1.1 ± 0.2	2.2 ± 0.3

Notes. The mass budgets are estimated within a given radius r. Where not specified, they represent the total mass of the observable emission as described in the main text. ⁽¹⁾The reported molecular gas masses are derived assuming a CO(4−3)-to-CO(1−0) line luminosity ratio of r₄₁ = 0.87 and a CO-to-H₂ conversion factor of α_CO = 1.7 M_⊙ (K km s⁻¹ pc²)⁻¹ (Carilli & Walter 2013; Montoya Arroyave et al. 2023). The uncertainties do not account for systematics on L′_{CO(4 − 3)}-to-M_H2 conversion factors (see Sect. 3.3). For the quasar host we report values of the total molecular gas mass, that accounting only for the CO(4−3) luminosity of the systematic component (“sys”), and the one excluding the blue side of the broad component (“bulk”, see Sect. 3.3). ⁽²⁾Mean and the standard deviation of the Gaussian prior employed in the fit of the dust SED. ⁽³⁾The FIR luminosity within the rest-frame wavelength range 8 − 1000 μm. The fiducial characteristic values for the dust properties are reported in boldface. ^( † )The dynamical mass are estimated assuming dispersion-dominated system (“disp”) and rotationally supported galaxy disk (“rot”). ^( ‡ )Half-light radius as derived from GALPAK^3D modeling (see Sect. 4.1.2).

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