A remarkable ruby: Absorption in dense gas, rather than evolved stars, drives the extreme Balmer break of a little red dot at z = 3.5

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Table 3.

Stellar population fitting results.

Parameter	`Prospector`	`Prospector`	Labbé et al.	Labbé et al.
	(galaxy-only/no AGN)	(galaxy + AGN)	(galaxy + AGN)	(galaxy + AGN; extreme dust)
log(M_*/M_⊙)	$10 . 586_{- 0.048}^{+ 0.009}$ $10.586_{-0.048}^{+0.009}$	$10 . 39_{- 0.03}^{+ 0.03}$ $10.39_{-0.03}^{+0.03}$	$10 . 531_{- 0.008}^{+ 0.007}$ $10.531_{-0.008}^{+0.007}$	$10 . 434_{- 0.049}^{+ 0.014}$ $10.434_{-0.049}^{+0.014}$
age [Gyr]	$0 . 90_{- 0.42}^{+ 0.11}$ $0.90_{-0.42}^{+0.11}$	$0 . 69_{- 0.11}^{+ 0.11}$ $0.69_{-0.11}^{+0.11}$	$0 . 65_{- 0.04}^{+ 0.04}$ $0.65_{-0.04}^{+0.04}$	$0 . 66_{- 0.19}^{+ 0.10}$ $0.66_{-0.19}^{+0.10}$
log(Z/Z_⊙)	$- 1 . 95_{- 0.02}^{+ 0.14}$ $-1.95_{-0.02}^{+0.14}$	$- 1 . 84_{- 0.09}^{+ 0.08}$ $-1.84_{-0.09}^{+0.08}$	$- 0 . 986_{- 0.010}^{+ 0.023}$ $-0.986_{-0.010}^{+0.023}$	$- 0 . 83_{- 0.12}^{+ 0.3}$ $-0.83_{-0.12}^{+0.3}$
SFR [M_⊙ yr⁻¹]	$7 . 3_{- 4.0}^{+ 6.0}$ $7.3_{-4.0}^{+6.0}$	$0 . 43_{- 0.40}^{+ 0.95}$ $0.43_{-0.40}^{+0.95}$
log(τ/yr)			$6 . 9_{- 0.3}^{+ 0.3}$ $6.9_{-0.3}^{+0.3}$	$7 . 0_{- 0.4}^{+ 0.3}$ $7.0_{-0.4}^{+0.3}$
A_V (stars)	$1 . 63_{- 0.08}^{+ 0.13}$ $1.63_{-0.08}^{+0.13}$	$1 . 43_{- 0.05}^{+ 0.05}$ $1.43_{-0.05}^{+0.05}$	$1 . 34_{- 0.02}^{+ 0.02}$ $1.34_{-0.02}^{+0.02}$	$1 . 06_{- 0.03}^{+ 0.04}$ $1.06_{-0.03}^{+0.04}$
dust index	$- 0 . 991_{- 0.007}^{+ 0.013}$ $-0.991_{-0.007}^{+0.013}$	$- 0 . 97_{- 0.02}^{+ 0.03}$ $-0.97_{-0.02}^{+0.03}$	–1.8	$- 2 . 47_{- 0.02}^{+ 0.04}$ $-2.47_{-0.02}^{+0.04}$

Notes. The dust index corresponds the power-law slope for the Labbe et al. (2024) models. For the Prospector models it instead corresponds to the corrective power-law slope to the Calzetti dust law (i.e. δ in the parametrisation of Noll et al. 2009).

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