The accretion luminosity of Class I protostars | Astronomy & Astrophysics (A&A)

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Volume 703 (November 2025)

A&A, 703 (2025) A277

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Table 2

Properties of the newly observed Class I/F and those from Beck (2007) (below the horizontal line).

	Name	α₂₀₀₀	δ₂₀₀₀	Region	d ^a	Class ^b	A_K,fg ^c	T_bol ^c	T_bol ^c
					(pc)		(mag)	(K)	(L_⊙)
1	SSTc2d j162621.3-242304	16 26 21.38	−24 23 04.0	Oph L1688	139.4	I	2.2	$320_{- 64}^{+ 137}$ $320_{ - 64}^{ + 137}$	$18_{- 4}^{+ 7}$ $18_{ - 4}^{ + 7}$
2	SSTc2d j162702.3-243727	16 27 02.33	−24 37 27.2	Oph L1688	139.4	I	3.1	$939_{- 262}^{+ 511}$ $939_{ - 262}^{ + 511}$	$16_{- 6}^{+ 18}$ $16_{ - 6}^{ + 18}$
3	SSTc2d j162709.4-243718	16 27 09.43	−24 37 18.8	Oph L1688	139.4	I	1.7	$455_{- 53}^{+ 80}$ $455_{ - 53}^{ + 80}$	$29_{- 9}^{+ 14}$ $29_{ - 9}^{ + 14}$
4	SSTc2d j162721.7-242953	16 27 21.80	−24 29 53.4	Oph L1688	139.4	I	2.0	$534_{- 54}^{+ 67}$ $534_{ - 54}^{ + 67}$	$2_{- 0.6}^{+ 1}$ $2_{ - 0.6}^{ + 1}$
5	SSTc2d j162726.9-244050	16 27 26.91	−24 40 50.8	Oph L1688	139.4	I	2.5	$408_{- 81}^{+ 117}$ $408_{ - 81}^{ + 117}$	$6_{- 1.5}^{+ 2}$ $6_{ - 1.5}^{ + 2}$
6	SSTc2d j162727.9-243933	16 27 27.89	−24 39 43.9	Oph L1688	139.4	I	2.2	$314_{- 26}^{+ 45}$ $314_{ - 26}^{ + 45}$	$13_{- 3.5}^{+ 5}$ $13_{ - 3.5}^{ + 5}$
7	SSTc2d j162730.1-242743	16 27 30.18	−24 27 43.4	Oph L1688	139.4	F	2.2	$814_{- 171}^{+ 288}$ $814_{ - 171}^{ + 288}$	$3_{- 1}^{+ 2.5}$ $3_{ - 1}^{ + 2.5}$
8	SSTc2d j163135.6-240129	16 31 35.66	−24 01 29.5	Oph L1709	139.4	F	1.1	$387_{- 110}^{+ 168}$ $387_{ - 110}^{ + 168}$	${2.5}_{- 0.5}^{+ 0.9}$ $2.5_{ - 0.5}^{ + 0.9}$
9	SSTc2d j163200.9-245642	16 32 00.99	−24 56 42.0	Oph L1689	139.4	I	1.1	$133_{- 27}^{+ 45}$ $133_{ - 27}^{ + 45}$	$6_{- 0.5}^{+ 0.7}$ $6_{ - 0.5}^{ + 0.7}$
10	IRAS 04016+2610	4 04 43.07	+26 18 56.4	Tau F	146	I	0.4	$427_{- 22}^{+ 81}$ $427_{ - 22}^{ + 81}$	$19_{- 2.1}^{+ 8.5}$ $19_{ - 2.1}^{ + 8.5}$
11	MHO 1	4 14 26.27	+28 06 03.3	Tau A	130.5	I	0.9	$1064_{- 562}^{+ 6330}$ $1064_{ - 562}^{ + 6330}$	$23_{- 8}^{+ 3900}$ $23_{ - 8}^{ + 3900}$
12	MHO 2	4 14 26.40	+28 05 59.6	Tau A	130.5	I	0.9	$1136_{- 604}^{+ 6206}$ $1136_{ - 604}^{ + 6206}$	$23_{- 8}^{+ 4000}$ $23_{ - 8}^{ + 4000}$
13	SSTtau 041430.5+280514	4 14 30.55	+28 05 14.6	Tau A	130.5	F	1.0	$2490_{- 1860}^{+ 5000}$ $2490_{ - 1860}^{ + 5000}$	$25_{- 15}^{+ 1100}$ $25_{ - 15}^{ + 1100}$
14	SSTtau 042107.9+270220	4 21 07.97	+27 02 20.1	Tau A	130.5		2.7	$1284_{- 556}^{+ 921}$ $1284_{ - 556}^{ + 921}$	$17_{- 8}^{+ 38}$ $17_{ - 8}^{ + 38}$
15	SSTtau 042111.4+270109	4 21 11.47	+27 01 09.4	Tau A	130.5	I	2.7	$1274_{- 443}^{+ 1015}$ $1274_{ - 443}^{ + 1015}$	$8_{- 4}^{+ 19}$ $8_{ - 4}^{ + 19}$
15	SSTtau 043232.0+225726	4 32 32.05	+22 57 26.7	Tau B	131	I	2.1	$838_{- 349}^{+ 719}$ $838_{ - 349}^{ + 719}$	$9_{- 3}^{+ 11}$ $9_{ - 3}^{ + 11}$
17	SSTtau 043935.1+254144	4 39 35.19	+25 41 44.7	Tau B	131	^I	0.4	$337_{- 19}^{+ 54}$ $337_{ - 19}^{ + 54}$	$13_{- 1.4}^{+ 4.6}$ $13_{ - 1.4}^{ + 4.6}$
18	IRAS04108+2803B	4 13 54.72	+28 11 32.9	Tau A	130.5	I	0.9	$270_{- 55}^{+ 110}$ $270_{ - 55}^{ + 110}$	${6.0}_{- 1}^{+ 1.8}$ $6.0_{ - 1}^{ + 1.8}$

18	IRAS04158+2805	4 18 58.13	+28 12 23.4	Tau A	130.5	I	0.6	$1172_{- 700}^{+ 6058}$ $1172_{ - 700}^{ + 6058}$	$2_{- 0.6}^{+ 3800}$ $2_{ - 0.6}^{ + 3800}$
20	IRAS04181+2654A	4 21 11.47	+27 01 09.4	Tau E	160.2	F	1.1	$434_{- 124}^{+ 235}$ $434_{ - 124}^{ + 235}$	$8_{- 1.9}^{+ 3.5}$ $8_{ - 1.9}^{ + 3.5}$
21	IRAS04239+2436	4 26 56.30	+24 43 35.3	Tau B	131	I	0.4	$311_{- 28}^{+ 961}$ $311_{ - 28}^{ + 961}$	$13_{- 1.3}^{+ 7}$ $13_{ - 1.3}^{ + 7}$
22	IRAS04295+2251	4 32 32.05	+22 57 26.7	Tau E	160.2	F	2.1	$1544_{- 1016}^{+ 3060}$ $1544_{ - 1016}^{ + 3060}$	$23_{- 11}^{+ 6770}$ $23_{ - 11}^{ + 6770}$
23	IRAS04361+2547	4 39 13.89	+25 53 20.9	Tau B	131	I	0.4	$163_{- 10}^{+ 36}$ $163_{ - 10}^{ + 36}$	$28_{- 1.8}^{+ 5.5}$ $28_{ - 1.8}^{ + 5.5}$
24	IRAS04365+2535	4 39 35.19	+25 41 44.7	Tau B	131	I	0.4	$369_{- 27}^{+ 89}$ $369_{ - 27}^{ + 89}$	$11_{- 1.2}^{+ 4.3}$ $11_{ - 1.2}^{ + 4.3}$

Notes. ^(a) Distances are the average cloud distance for Ophiuchus and average distances of each sub-cloud for Taurus (see Testi et al. 2022; Grasser et al. 2021; Roccatagliata et al. 2020).^(b) The literature young stellar object classification is based on Dunham et al. (2015), Rebull et al. (2010), and Beck (2007). ^(c) From this paper (see Sect. 4.3).

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