Determining stellar accretion rates from Paα and Brβ emission lines with JWST NIRSpec - Accretion of pre-main-sequence stars in NGC 3603

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Table 1.

Physical properties of the PMS stars considered in this analysis and the EWs of the three recombination lines.

ID	RA	Dec	T_eff (K)	Group	M_* (M_⊙)	EW Pa_α (Å)	EW Br_γ (Å)	EW Br_β (Å)	log₁₀(L_acc) (L_⊙)
727	168.8096466	−61.263581	3800 ±150	TT	0.5 ±0.06	−23.1 ±2.2	−0.8 ±0.2	−9.7 ±1.9	−1.42 ±0.75
654	168.7541941	−61.2514463	4600 ±150	TT	0.75 ±0.07	−3.6 ±0.4	−0.4 ±0.1	−3.8 ±0.7	−1.42 ±0.72
4595	168.8129136	−61.2625111	3600 ±150	TT	0.47 ±0.05	−22.2 ±2	−2.4 ±0.7	−26 ±4.7	−1.4 ±0.74
996	168.7973597	−61.2640824	5200 ±150	TT	0.97 ±0.08	−8.9 ±0.7	−0.5 ±0.2	−2.9 ±0.5	−1.11 ±0.74
1497	168.7688519	−61.25128	6000 ±100	TT	1.3 ±0.04	−24.2 ±2	−2.9 ±0.5	−17.1 ±2.9	−1.08 ±0.71
1457	168.7310205	−61.2672106	5400 ±100	TT	1.05 ±0.04	−45.5 ±3.8	−10.7 ±1.3	−61 ±10.5	−0.75 ±0.69
1038	168.7957658	−61.2643274	5400 ±150	TT	1.05 ±0.08	−54.2 ±4.6	−3.6 ±0.5	−12.2 ±2	−0.75 ±0.68
1339	168.8197744	−61.2630422	4400 ±150	TT	0.7 ±0.06	−12 ±1	−5.7 ±0.7	−45 ±7.8	−0.73 ±0.69
858	168.7365507	−61.2702015	9600 ±200	HAe/Be	3.3 ±0.14	−82.6 ±6.9	−7.6 ±0.8	−33.5 ±5.9	−0.67 ±0.48
1813	168.8037358	−61.246069	5600 ±150	TT	1.1 ±0.08	−48 ±4.1	−5.6 ±0.7	−38 ±6.7	−0.65 ±0.69
1442	168.8120917	−61.2671703	4200 ±150	TT	0.65 ±0.06	−11 ±0.9	−1 ±0.2	−2.4 ±0.4	−0.65 ±0.69
1997	168.8052566	−61.2510052	4400 ±200	TT	0.7 ±0.06	−14.8 ±1.3	−1.3 ±0.2	−3.2 ±0.6	−0.61 ±0.69
1717	168.8138352	−61.2507679	5800 ±200	TT	1.2 ±0.08	−24.6 ±2.1	−3.4 ±0.6	−6.7 ±1.2	−0.61 ±0.76
4649	168.7420813	−61.2585345	3600 ±150	TT	0.47 ±0.05	−128.7 ±11.7	−10.6 ±1.8	−59.3 ±10.6	−0.53 ±0.67
1271	168.7330151	−61.2635352	4600 ±200	TT	0.75 ±0.07	−70.6 ±6	−9 ±1.1	−17.5 ±3.1	−0.47 ±0.67
2326	168.7438995	−61.2588048	3800 ±150	TT	0.5 ±0.06	−114.3 ±10.1	−25.7 ±4.4	−86.3 ±16.3	−0.41 ±0.67
1134	168.7353906	−61.2705277	5600 ±150	TT	1.13 ±0.08	−125.1 ±10.5	−10.1 ±1.2	−45.4 ±8.1	−0.37 ±0.67
2673	168.7975961	−61.2649162	4400 ±100	TT	0.7 ±0.03	−34.2 ±3	−3.5 ±0.5	−7.3 ±1.4	−0.36 ±0.67
1854	168.7292443	−61.2600537	4200 ±150	TT	0.75 ±0.07	−225.1 ±19.7	−22.8 ±2.9	−127.9 ±22.3	−0.36 ±0.67
2492	168.7427501	−61.2714228	5000 ±100	TT	0.9 ±0.04	−245 ±21.8	−57.6 ±7	−79.2 ±14.7	−0.27 ±0.66
977	168.8092518	−61.2623119	5000 ±150	TT	0.9 ±0.07	−19.1 ±1.6	−2 ±0.3	−5.8 ±1.1	−0.03 ±0.67
354	168.7704651	−61.2626355	10 600 ±2000	HAe/Be		−22.5 ±2.1	−5 ±1.3	−5.6 ±1.3	0.07 ±0.49
853	168.7643462	−61.2488318	5400 ±100	TT	1.05 ±0.04	−18.2 ±1.5	−2.1 ±0.3	−5.9 ±0.9	0.15 ±0.64
2166	168.7944201	−61.2661562	5000 ±150	TT	0.9 ±0.07	−69.1 ±6.2	−6.5 ±0.8	−15.3 ±2.6	0.27 ±0.64
152	168.7817328	−61.2648809	9400 ±1800	HAe/Be		−14.9 ±1.2	−1.5 ±0.2	−2.2 ±0.4	0.42 ±0.44
1350	168.8031179	−61.2483281	5000 ±2000	TT/HAe	0.9 ±0.7	−53.6 ±4.4	−8.2 ±1	−11.1 ±2	0.66 ±0.63
1354	168.7519521	−61.2645637	6600 ±1400	TT/HAe		−20.8 ±1.7	−3.5 ±0.4	−5 ±0.8	0.9 ±0.62
823	168.7623889	−61.2710101	7200 ±1400	HAe		−33.8 ±2.9	−6 ±0.7	−9 ±1.5	1.79 ±0.43
238	168.8151779	−61.2550836	7000 ±1800	HAe/Be		−76 ±6.3	−13.5 ±2.1	−23.6 ±4.2	2.06 ±0.39
185	168.7627924	−61.2625057	8200 ±1800	HAe/Be		−82.2 ±6.8	−9.4 ±1.1	−14.1 ±2.3	2.13 ±0.37
469	168.7941589	−61.2779717	8600 ±1800	HAe/Be		−216.9 ±45.1	−16.2 ±2	−17.2 ±3.1	2.52 ±0.36
251	168.7684956	−61.2531283	6400 ±1800	TT/HAe		−124.9 ±10.6	−13.7 ±1.6	−17.6 ±3.1	2.75 ±0.37

Notes. The sources have been ordered in terms of increasing accretion luminosity. The Group column indicates whether the sources are classified as T Tauri or Herbig AeBe. For the T Tauri stars, the temperatures, masses and associated uncertainties come directly from the Phoenix stellar models based on the five best fitting model spectra. For the Herbig AeBe stars, the temperatures and masses come from the photometry of B10. The uncertainty in mass for each source has been calculated based on . The uncertainty in temperature for the Herbig AeBe stars has been determined from the Phoenix models, such that the range of temperatures reproduces the upper and lower mass limit for each source. Source 1350 could not be classified by spectroscopic or photometric means and so, a temperature of 5000 K was assumed with an uncertainty of 2000 K.

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