New insights on the near-infrared veiling of young stars using CFHT/SPIRou data

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Table 2.

Parameters of the targets derived in this work.

Star	Std	v_rad	r_Y	r_J	r_H	r_K	EW_HeI^(a)	EW_Paβ^(a)	EW_Brγ^(a)	Ṁ_Paβ	Ṁ_Brγ	α_{2_8}^(b)
										×10⁻⁸	×10⁻⁸
		(km s⁻¹)					(Å)	(Å)	(Å)	(M_⊙ yr⁻¹)	(M_⊙ yr⁻¹)
CI Tau	V819TAU	16.3 ± 0.5	0.53 ± 0.28	0.49 ± 0.17	0.39 ± 0.09	0.92 ± 0.23	9.5 ± 3.2	14.0 ± 2.6	7.9 ± 1.8	2.2	4.2	−0.84
DoAr 44	V819TAU	−6.1 ± 0.7	0.20 ± 0.09	0.48 ± 0.10	0.60 ± 0.06	1.28 ± 0.05	5.4 ± 1.4	9.1 ± 0.8	3.8 ± 0.5	1.7	1.5	−1.09
GQ Lup	TWA9A	−3.0 ± 0.3	0.19 ± 0.09	0.58 ± 0.11	0.78 ± 0.14	1.87 ± 0.26	0.9 ± 2.0	6.3 ± 1.6	2.0 ± 0.7	2.5	1.9	−0.89
TW Hya	TWA25	12.4 ± 0.1	0.08 ± 0.07	0.09 ± 0.06	0.10 ± 0.05	0.23 ± 0.11	5.1 ± 4.9	15.9 ± 6.2	6.8 ± 2.6	0.6	0.3	−1.92
V2129 Oph	V819TAU	−7.1 ± 0.6	0.05 ± 0.10	0.11 ± 0.06	0.25 ± 0.07	0.76 ± 0.16	0.9 ± 1.1	1.0 ± 0.7	0.5 ± 0.3	0.2	0.1	−1.62
BP Tau	V819TAU	15.2 ± 0.6	0.22 ± 0.09	0.36 ± 0.06	0.36 ± 0.09	0.78 ± 0.10	3.9 ± 1.4	7.7 ± 1.4	3.2 ± 0.8	1.3	1.1	−1.69
DG Tau	TWA9A	15.1 ± 3.4	0.29 ± 0.22	0.80 ± 0.20	1.09 ± 0.16	2.90 ± 0.51	11.7 ± 2.7	16.3 ± 2.1	6.8 ± 1.0	6.4	7.6	−0.26
RU Lup	TWA9A	−1.3 ± 1.4	1.14 ± 0.51	1.70 ± 0.65	1.65 ± 0.44	6.27 ± 2.97	23.2 ± 4.0	30.1 ± 3.0	12.2 ± 1.5	7.8	11.9	−0.21
V2247 Oph	TWA25	−5.8 ± 0.5	−0.02 ± 0.07	−0.06 ± 0.01	0.01 ± 0.03	−0.03 ± 0.02	0.0 ± 0.2	0.1 ± 0.1	−0.1 ± 0.2	0.009	–	−2.54
DO Tau	TWA25	16.1 ± 1.0	0.50 ± 0.40	0.78 ± 0.41	1.07 ± 0.32	2.33 ± 0.61	1.0 ± 1.8	12.7 ± 3.9	4.0 ± 1.9	2.3	3.4	−0.54
V347 Aur	TWA25	8.1 ± 0.6	0.31 ± 0.19	0.46 ± 0.26	0.37 ± 0.15	1.12 ± 0.31	−0.9 ± 1.1	6.7 ± 2.1	2.9 ± 1.0	7.1	7.3	−0.62
J1604	V819TAU	−5.8 ± 0.8	−0.14 ± 0.11	0.20 ± 0.07	0.22 ± 0.13	0.81 ± 0.23	−2.6 ± 1.8	−0.1 ± 0.2	0.3 ± 0.1	–	0.013	−2.81
PDS 70	TWA9A	5.0 ± 0.4	0.02 ± 0.11	0.18 ± 0.04	0.19 ± 0.07	0.34 ± 0.08	−0.7 ± 0.9	0.2 ± 0.2	0.1 ± 0.2	0.007	0.003	–
GM Aur	TWA9A	14.5 ± 0.3	−0.00 ± 0.06	0.13 ± 0.09	0.11 ± 0.06	0.31 ± 0.10	3.4 ± 2.8	10.2 ± 3.2	4.7 ± 1.9	1.3	1.0	–

Notes.

^(a)

We used the convention of positive equivalent width for emission lines, and negative values for absorption lines.

^(b)

Slope of the spectral energy distribution measured between 2 and 8 μm.

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