JOYS: Unlocking accretion-rate diagnostics for high-mass protostars using JWST/MIRI HI lines

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Table 5.

Accretion for the detected H I lines derived using Gaussian fits (Figures 4, A.2, A.3, and A.4).

IR source	S/N^*	FWHM^**	$\frac{L_{proto}}{L_{bkg}}$ $Mathematical equation: $ \frac{L_{\mathrm{proto}}}{L_{\mathrm{bkg}}} $$	L_{line, obs}	L_line	$L_{acc}^{1}$ $Mathematical equation: $ L_{\mathrm{acc}}^{\,\,\,1} $$	$L_{acc}^{2}$ $Mathematical equation: $ L_{\mathrm{acc}}^{\,\,\,2} $$	L $_{acc}^{3}$ $Mathematical equation: $ _{\mathrm{acc}}^{\,\,\,3} $$	${\dot{M}}_{acc}^{1}$ $Mathematical equation: $ \dot{M}_{\mathrm{acc}}^{\,\,\,1} $$	${\dot{M}}_{acc}^{2}$ $Mathematical equation: $ \dot{M}_{\mathrm{acc}}^{\,\,\,2} $$	${\dot{M}}_{acc}^{3}$ $Mathematical equation: $ \dot{M}_{\mathrm{acc}}^{\,\,\,3} $$
IR source		[km s⁻¹]		log[ L_⊙]	log[ L_⊙]	log[ L_⊙ ]			log[ L_⊙ yr⁻¹ ]
Pfund α H I 6–5

G28P1 A	4.5 (6.3)	69	1.84	−3.81	−2.47	−	−	2.02	−	−	−5.2
					−2.35	−	−	2.16	−	−	−5.1

IRAS23385 A	4.9 (7.2)	164	15.7	−2.92	−1.66	−	−	2.90	−	−	−4.8
					−1.54	−	−	3.02	−	−	−4.7

Humphreys β H I 8–6

G28IRS2	8.7 (–)	107	≫1	−2.83	−0.96	−	−	3.84	−	−	−3.4
					−0.79	−	−	[4.03]	−	−	−

G28P1 B	3.3 (–)	108	≫1	−3.50	−1.62	−	−	[3.12]	−	−	−
					−1.45	–	−	[3.31]	−	−	−

IRAS23385 A	5.9 (4.4)	78	2.27	−3.44	−2.17	−	−	2.51	−	−	−5.2
					−2.06	−	−	2.64	−	−	−5.1

Humphreys α H I 7–6

G28IRS2	7.4 (8.2)	75	1.6	−4.30	−0.57	[8.56]	[8.41]	[4.44]	−	−	−
					−1.96	[5.66]	[5.62]	2.95	−	−	−4.3

G28P1 A	3.3 (9.2)	72	1.17	−5.00	−2.30	[4.96]	[4.96]	2.59	−	−	−4.6
					−3.31	[2.86]	[2.94]	1.52	−	−	−5.7

G28P1 B	4.7 (15)	70	1.01	−5.85	−2.09	[5.40]	[5.37]	2.82	−	−	−4.4
					−3.50	2.47	2.56	1.31	−5.1	−5.0	−5.9

IRAS23385 A	2.5 (0)	90	≫1	−4.24	−1.70	[6.21]	[6.16]	3.24	−	−	−4.5
					–2.65	[4.24]	[4.26]	2.22	–	−	−5.5

H I 10 - 7

G28P1 B^!!	4.2 (–)	177	≫1	−3.40	0.47	−	[7.20]	[5.22]	−	−	−
					−0.59	−	[5.78]	[4.16]	−	−	−

IRAS18089 C^!!	3.2 (–)	123	6.88	−4.29	2.38	−	[9.78]	[7.13]	−	−	−
					0.56	−	[7.33]	[5.31]	−	−	−

Notes. Duplicated cells in the seven columns from the right display the two values given by the extinction curves of KP5 (upper) and M09 (lower). The L_acc values in square brackets indicate that they surpass their region’s L_bol (Table 1). ^* S/N towards the protostar and background (in parenthesis). ^** Not corrected by instrumental broadening. ^!! Dubious detection (Appendix A). ¹ Calculated using calibration of Rigliaco et al. (2015); ²Tofflemire et al. (2025); ³ or Shridharan et al. (2026).

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