Analysing the SEDs of protoplanetary disks with machine learning

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Volume 672 (April 2023)

A&A, 672 (2023) A30

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Table 2

Assumed stellar parameters for the analysed sample.

Object	SpTyp⁽¹⁾	d (pc)⁽²⁾	Av⁽³⁾	Teff (K)⁽³⁾	L_⋆ (L_sun)⁽⁴⁾	M_⋆ [M_sun]⁽¹⁾	age (Myr)⁽¹⁾
HD 97048	B9	184.4 ± 0.8	1.28	10000	45.82	2.6	4.5
HD 100546	B9⁽⁵⁾	108.1 ± 0.4	0.22	10470	33.55	2.5⁽⁵⁾	> 4.8⁽⁵⁾
AB Aur	B9	155.9 ± 0.9	0.42	9550	49.35	2.6	3.9
HD 95881	A1⁽⁶⁾	111.0 ± 2.4	0.89	9900	14.43	2.5⁽⁶⁾	> 5.8⁽⁶⁾
HD 163296	A1⁽⁶⁾	101.0 ± 0.4	0.48	9000	25.17	2.5⁽⁶⁾	> 5.8⁽⁶⁾
49 Cet	A2	57.23 ± 0.18	0.00	8770	15.58	1.99	10
MWC 480	A5	156.2 ± 1.3	0.16	8250	17.81	1.99	4.9 × 10²
HD 169142	A7⁽⁷⁾	114.87 ± 0.35	0.06	7800	6.15	1.74⁽⁷⁾	> 15 ⁽⁷⁾
CQ Tau	A9	149.4 ± 1.3	2.53	7231	11.58	1.76	9.4
HD 142666	F1	146.3 ± 0.5	0.81	7050	10.02	1.7	1.7 × 10³
HD 135344B	F3	135.0 ± 0.4	0.40	6620	7.07	1.58	12
V 1149 Sco	F9	167.3 ± 0.5	0.71	6080	3.75	1.33	16
PDS 66	K0	97.89 ± 0.12	1.01	5205	1.42	1.25	15
Lk Ca 15	K3⁽⁸⁾	157.2 ± 0.7	1.7	4730	1.51	1.5⁽⁸⁾	> 5.5⁽⁸⁾
RY Lup	K4	153.5 ± 1.4	0.29	4420	1.95	1.23	1.9
Usco J 1604–2130	K4	145.3 ± 0.6	1.0	4550	0.76	1.0	10
CI Tau	K6	160.3 ± 0.5	1.77	4200	1.21	0.90	1.9
TW Cha	K6	183.1 ± 0.4	1.61	4110	0.78	0.82	2.8
TW Hya	K7	60.14 ± 0.05	0.20	4000	0.34	0.75	7.8
RU Lup	K7	157.5 ± 1.0	0.00	4060	1.49	0.73	1.1
AA Tau	K7	134.7 ± 1.6	0.99	4010	0.78	0.71	2.3
GM Aur	K7	158.1 ± 1.2	0.30	4000	0.77	0.70	2.3
DN Tau	K7	128.6 ± 0.4	0.71	3986	0.71	0.69	2.4
BP Tau	K7	127.4 ± 0.6	0.57	3950	0.74	0.65	2.0
DF Tau	K7	176 ± 16	1.27	3900	3.89	0.61	0.36
DO Tau	M0	138.5 ± 0.7	2.6	3800	0.90	0.52	1.1
DM Tau	M0	144.0 ± 0.5	0.55	3780	0.25	0.52	5.4
CY Tau	M1	126.33 ± 0.33	0.10	3640	0.29	0.42	2.8
FT Tau	M3	130.2 ± 0.4	1.09	3400	0.26	0.30	2.2
RECX 15	M3	103.4 ± 2.4	0.65	3400	0.11	0.29	5.2

Notes. ⁽¹⁾Spectral type, stellar mass and age for every object is derived using the updated luminosity and pre-main-sequence tracks by Siess et al. (2000) for solar-metallicity. ⁽²⁾Distances are taken from Gaia Collaboration (2021). ⁽³⁾Taken from Woitke et al. (2019). ⁽⁴⁾Updated luminosity: Luminosity used by Woitke et al. (2019) scaled according to new distances. ⁽⁵⁾No tracks from Siess et al. (2000) match, values are taken from the closest point at T_eff = 9650 K and L_⋆ = 42 L_sun. ⁽⁶⁾No tracks from Siess et al. (2000) match, values are taken from the closest point at T_eff = 9000 K and L_⋆ = 30 L_sun. ⁽⁷⁾No tracks from Siess et al. (2000) match, values are taken from the closest point at T_eff = 7800 K and L_⋆ = 9 L_sun. ⁽⁸⁾No tracks from Siess et al. (2000) match, values are taken from the closest point at T_eff = 4730 K and L_⋆ = 1.6 L_sun.

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