Early Planet Formation in Embedded Disks (eDisk) - XX. Constraining the chemical tracers of young protostellar sources

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Volume 704 (December 2025)

A&A, 704 (2025) A133

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Table 2

Summary of the eDisk sources.


Source name	Hereafter	Class	Distance (pc)	T_bol (K)	L_bol (L_⊙)	Inclination (°)	v_sys (km s⁻¹)	References
BHR 71 IRS1	BHR71 IRS1	0	176	66	10	39	−4.45	(1)
BHR 71 IRS2	BHR71 IRS2	0	176	39	1.1	31	−4.45	(1)
Ced110 IRS4^†	Ced110IRS4	0	189	68	1.0	75	4.67	(2)
GSS30 IRS3	GSS30IRS3	0	138	50	1.7	72	2.84	(3)
IRAS 04166+2706	IRAS 04166	0	156	61	0.4	47	6.80	(4)
IRAS 15398–3359	IRAS 15398	0	155	50	1.4	51	5.40	(5)
IRAS 16253–2429	IRAS 16253	0	139	42	0.16	68	4.00	(6)
IRAS 16544–1604	IRAS 16544	0	151	50	0.89	73	4.96	(7)
L1527 IRS	L1527	0	140	41	1.3	75	5.90	(8)
R CrA IRAS 32^†	IRAS32	0	150	64	1.6	69	5.86	(9)
R CrA IRS5N	IRS5N	0	147	59	1.4	65	6.65	(10)
IRAS 04169+2702	IRAS 04169	I	156	163	1.5	44	6.90	(11)
IRAS 04302+2247	IRAS 04302	I	160	88	0.43	84	5.70	(12)
L1489 IRS	L1489	I	146	213	3.4	71	7.38	(13)
Oph IRS43^†	OphIRS43	I	137	193	4.1	78	3.90	(14)
Oph IRS63	OphIRS63	I	132	348	1.3	47	2.80	(15)
R CrA IRS7B^†	IRS7B	I	152	88	5.1	68	5.90	(16, 17)

B335	B335	0	165	41	1.4	37	8.30	(9)
TMC-1A	TMC1A	I	137	183	2.3	52	6.80	(9)

Notes. ^† These sources have close binaries with projected seperations of ~ $1_{\cdot}^{''} 30$ $\[1^{\prime\prime}_\cdot30\]$ (~250 au) for Ced110IRS4, ~ $1_{\cdot}^{''} 38$ $\[1^{\prime\prime}_\cdot38\]$ (~207 au) for IRAS32, ~ $0_{\cdot}^{''} 55$ $\[0^{\prime\prime}_\cdot55\]$ (~74 au) for OphIRS43, and ~ $0_{\cdot}^{''} 70$ $\[0^{\prime\prime}_\cdot70\]$ (~106 au) for IRS7B. The inclination angle for these binaries are based on their primary companion. (1) Gavino et al. (2024); (2) Sai et al. (2023); (3) Santamaría-Miranda et al. (2024); (4) Phuong et al. (2025); (5) Thieme et al. (2023); (6) Aso et al. (2023); (7) Kido et al. (2023); (8) van’t Hoff et al. (2023); (9) Ohashi et al. (2023); (10) Sharma et al. (2023); (11) Han et al. (2025); (12) Lin et al. (2023); (13) Yamato et al. (2023); (14) Narayanan et al. (2023); (15) Flores et al. (2023); (16) Takakuwa et al. (2024); (17) Ohashi et al. (2023).

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