JWST’s PEARLS: A z ≃ 6 quasar in a train-wreck galaxy merger system

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Table 4.

Physical properties calculated for the emission line regions: SFR from the constrained (SFR_Hα, min) and unconstrained (SFR_Hα, max) Hα models, mass-to-light ratio, M_*/L, in the HST/WFC3 F160W filter, stellar age, t, metal abundance, [M/H], stellar dust attenuation, A_V, and stellar mass, M_*.

Region	SFR_Hα, min	SFR_Hα, max	M_*/L	t	[M/H]	A_V	M_*
	(M_⊙ yr⁻¹)	(M_⊙ yr⁻¹)	(10⁻⁴ M_⊙/L_⊙)	(Myr)		(mag)	(10¹⁰ M_⊙)
1	14.7±1.3	26.7±3.0	$14_{- 1}^{+ 3}$ $14^{+3}_{-1}$	$65_{- 4}^{+ 9}$ $65^{+9}_{-4}$	> −0.1	$0 . 41_{- 0.05}^{+ 0.04}$ $0.41^{+0.04}_{-0.05}$	$36_{- 3}^{+ 6}$ $36^{+6}_{-3}$
2 (2*)	11.2±0.7	21.8±1.7	$1 . 6_{- 0.7}^{+ 2.0}$ $1.6^{+2.0}_{-0.7}$	$8_{- 4}^{+ 10}$ $8^{+10}_{-4}$	–	–	–
3	52.1±4.6	60.4±5.1	–	–	–	–	–
4 (4*)	42.4±1.0	65.1±1.9	$0 . 7_{- 0.1}^{+ 0.2}$ $0.7^{+0.2}_{-0.1}$	$6 . 7_{- 1.8}^{+ 1.8}$ $6.7^{+1.8}_{-1.8}$	< − 0.8	$1 . 2_{- 0.1}^{+ 0.1}$ $1.2^{+0.1}_{-0.1}$	$1 . 9_{- 0.4}^{+ 0.4}$ $1.9^{+0.4}_{-0.4}$

Notes. The SFRs are based on the Hα narrow-line fluxes listed in Table 3 following the equation in Section 4.2.2. The true SFRs are likely to be smaller than the calculated values because the quasar contributes to the photoionisation. The stellar population properties t, [M/H], and A_V are calculated from the PPXF SPS modelling (Section 4.3). These models use the smaller regions 2* and 4* to avoid contamination by the quasar. These SPS quantities are light-weighted values. The stellar mass M_* is calculated from the SPS mass-to-light-ratio and the HST/WFC3 F160W H-band magnitude of the two companion galaxies. Region 2 was undetected in the H-band images, prohibiting a stellar mass estimate. Region 3 is dominated by the quasar emission, and no SPS fitting is possible.

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