Using autoencoders and deep transfer learning to determine the stellar parameters of 286 CARMENES M dwarfs

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Volume 687 (July 2024)

A&A, 687 (2024) A205

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Table 3

Low-metallicity stars identified in Fig. 8.

Karmn		Name	[Fe/H]^(a)_AE	[Fe/H]^(b)_DTL	[Fe/H]^(c)_Mann15	[Fe/H]^(d)_corr,Mar21	[Fe/H]^(e)_Schw19
			(dex)	(dex)	(dex)	(dex)	(dex)
J00183+440	GX And	$- {0.33}_{- 0.17}^{+ 0.06}$ $- 0.33_{ - 0.17}^{ + 0.06}$	$- {0.26}_{- \dots}^{+ \dots}$ $- 0.26_{ - \ldots }^{ + \ldots }$	−0. 30 ± 0 .08	−0.52 ± 0.11	−0.25 ± 0.16	D
J02123+035	BD+02 348	$- {0.35}_{- 0.10}^{+ 0.12}$ $- 0.35_{ - 0.10}^{ + 0.12}$	$- {0.33}_{- 0.01}^{+ 0.01}$ $- 0.33_{ - 0.01}^{ + 0.01}$	−0. 36 ± 0 .08	−0.49 ± 0.06	−0.05 ± 0.16	TD
J06371+175	HD 260655	$- {0.41}_{- 0.13}^{+ 0.11}$ $- 0.41_{ - 0.13}^{ + 0.11}$	$- {0.37}_{- 0.02}^{+ 0.02}$ $- 0.37_{ - 0.02}^{ + 0.02}$	−0. 34 ± 0 .08	−0.43 ± 0.04	−0.42 ± 0.16	TD-D
J11033+359	Lalande 21185	$- {0.34}_{- 0.13}^{+ 0.08}$ $- 0.34_{ - 0.13}^{ + 0.08}$	$- {0.31}_{- \dots}^{+ \dots}$ $- 0.31_{ - \ldots }^{ + \ldots }$	−0.38 ± 0.08	−0.49 ± 0.10	−0.09 ± 0.16	TD
J11054+435	BD+44 2051A	$- {0.40}_{- 0.18}^{+ 0.07}$ $- 0.40_{ - 0.18}^{ + 0.07}$	$- {0.35}_{- \dots}^{+ \dots}$ $- 0.35_{ - \ldots }^{ + \ldots }$	−0.37 ± 0.08	−0.56 ± 0.09	−0.3 ± 0.16	TD-D
J12248−182^(g)	Ross 695	$- {0.33}_{- 0.18}^{+ 0.06}$ $- 0.33_{ - 0.18}^{ + 0.06}$	$- {0.40}_{- 0.04}^{+ 0.02}$ $- 0.40_{ - 0.04}^{ + 0.02}$	…	−0.60 ± 0.09	−0.17 ± 0.16	TD
J13450+176	BD+18 2776	$- {0.53}_{- 0.27}^{+ 0.09}$ $- 0.53_{ - 0.27}^{ + 0.09}$	$- {0.46}_{- 0.05}^{+ 0.06}$ $- 0.46_{ - 0.05}^{ + 0.06}$	−0.54 ± 0.08	−0.54 ± 0.03	−0.43 ± 0.16	TD
J16254+543^(g)	GJ 625	$- {0.33}_{- 0.15}^{+ 0.05}$ $- 0.33_{ - 0.15}^{ + 0.05}$	$- {0.32}_{- 0.03}^{+ 0.02}$ $- 0.32_{ - 0.03}^{ + 0.02}$	−0.35 ± 0.08	−0.28 ± 0.07	−0.26 ± 0.16	YD
J17378+185	BD+18 3421	$- {0.33}_{- 0.08}^{+ 0.11}$ $- 0.33_{ - 0.08}^{ + 0.11}$	$- {0.23}_{- 0.03}^{+ 0.01}$ $- 0.23_{ - 0.03}^{ + 0.01}$	−0.25 ± 0.08	−0.40 ± 0.07	−0.23 ± 0.16	D
J19070+208^(g)	Ross 730	$- {0.34}_{- 0.18}^{+ 0.05}$ $- 0.34_{ - 0.18}^{ + 0.05}$	$- {0.32}_{- 0.02}^{+ 0.01}$ $- 0.32_{ - 0.02}^{ + 0.01}$	−0.33 ± 0.08	−0.46 ± 0.07	−0.20 ± 0.16	D
J19072+208^(g)	HD 349726	$- {0.32}_{- 0.17}^{+ 0.05}$ $- 0.32_{ - 0.17}^{ + 0.05}$	$- {0.32}_{- 0.02}^{+ 0.02}$ $- 0.32_{ - 0.02}^{ + 0.02}$	−0.35 ± 0.08	−0.46 ± 0.06	−0.23 ± 0.16	D
J23492+024	BR Psc	$- {0.43}_{- 0.12}^{+ 0.11}$ $- 0.43_{ - 0.12}^{ + 0.11}$	$- {0.40}_{- 0.03}^{+ 0.02}$ $- 0.40_{ - 0.03}^{ + 0.02}$	−0.45 ± 0.08	−0.55 ± 0.08	−0.13 ± 0.16	TD

Notes. As explained in Passegger et al. (2020, 2022), our [M/H] results directly translate into [Fe/H] values. ^(a)From this work. ^(b)From Bello23. ^(c)From Mann et al. (2015). ^(d)From Mar21, corrected from the α enhancement. ^(e)From Schw19.^(f)Galactic populations, including the thick disc (TD), the thick disc-thin disc transition (TD-D), the thin disc (D), and the young disc (YD), following Cortés-Contreras et al. (in prep.).^(g)Reported to have a behaviour akin to subdwarfs in Mar21 or Schw19. In particular, J19070+208 and J19072+208 are both components of the wide binary system LDS 1017, and Houdebine (2008) already identified them as subdwarfs.

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