Candidate young stellar objects in the S-cluster: Kinematic analysis of a subpopulation of the low-mass G objects close to Sgr A*

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Volume 686 (June 2024)

A&A, 686 (2024) A235

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Table 7.

Best-fit properties of the candidate YSOs investigated using HYPERION.

ID	Mass [M_⊙]	Luminosity [10³ × L_⊙]	Radius [R_⊙]	Disk size [AU]	Envelope size [AU]
D2	0.5 ± 0.1	2000 $_{- 200}^{+ 100}$ $^{+100}_{-200}$	2.09 $_{- 0.19}^{+ 0.11}$ $^{+0.11}_{-0.19}$	(6–125) ± 5	(7–300) ± 20
D23	0.5 ± 0.1	2000 $_{- 200}^{+ 200}$ $^{+200}_{-200}$	2.09 $_{- 0.10}^{+ 0.10}$ $^{+0.10}_{-0.10}$	(6–125) ± 5	(7–300) ± 20
D3	0.3 ± 0.1	1500 $_{- 100}^{+ 100}$ $^{+100}_{-100}$	2.09 $_{- 0.09}^{+ 0.11}$ $^{+0.11}_{-0.09}$	(4–75) ± 5	(7–150) ± 10
D5	0.3 ± 0.1	1500 $_{- 100}^{+ 100}$ $^{+100}_{-100}$	0.80 $_{- 0.10}^{+ 0.10}$ $^{+0.10}_{-0.10}$	(4–75) ± 5	(7–150) ± 10
G2/DSO	0.4 ± 0.2	1300 $_{- 200}^{+ 200}$ $^{+200}_{-200}$	0.30 $_{- 0.20}^{+ 0.20}$ $^{+0.20}_{-0.20}$	(4–70) ± 5	(7–180) ± 20
X7	2.0 ± 0.5	2600 $_{- 200}^{+ 200}$ $^{+200}_{-200}$	2.00 $_{- 0.50}^{+ 0.50}$ $^{+0.50}_{-0.50}$	(4–75) ± 5	(7–400) ± 50
X7.1	1.0 ± 0.1	2000 $_{- 300}^{+ 300}$ $^{+300}_{-300}$	1.00 $_{- 0.20}^{+ 0.20}$ $^{+0.20}_{-0.20}$	(4–100) ± 10	(7–200) ± 10
X8	1.0 ± 0.2	3000 $_{- 400}^{+ 400}$ $^{+400}_{-400}$	1.00 $_{- 0.20}^{+ 0.20}$ $^{+0.20}_{-0.20}$	(4–80) ± 5	(7–200) ± 20

Notes. For these fit parameters, we derive the indicated uncertainty ranges, which are represented by three different SEDs displayed in Fig. 9. Due to the challenging observation of the OS sources close to the detection limit, we excluded them from this analysis. As mentioned, G1 will be analyzed in detail in Melamed et al. (in prep.). For all remaining sources, the radiative transfer code suggests a low-mass classification that was discussed in Ciurlo et al. (2020).

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