Understanding post-red giant branch binaries through stable mass transfer

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Volume 703 (November 2025)

A&A, 703 (2025) A294

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Table C.2.

SED fitting results of the Galactic post-AGB and post-RGB binary sample.

IRAS	Name	T_eff/K	D/pc	E(B − V)	L/L_⊙	L_IR/L_* (%)
...	EZ Gem	6555	4216 $_{- 521}^{+ 630}$ $_{-521}^{+630}$	0.43 $_{- 0.27}^{+ 0.04}$ $_{-0.27}^{+0.04}$	50 $_{- 29}^{+ 25}$ $_{-29}^{+25}$	53
13258-8103	...	6000	1608 $_{- 385}^{+ 704}$ $_{-385}^{+704}$	1.58 $_{- 0.7}^{+ 0.39}$ $_{-0.7}^{+0.39}$	50 $_{- 41}^{+ 251}$ $_{-41}^{+251}$	284
21216+1803	AU Peg	5750	597 $_{- 6}^{+ 6}$ $_{-6}^{+6}$	0.08 $_{- 0.08}^{+ 0.14}$ $_{-0.08}^{+0.14}$	74 $_{- 11}^{+ 27}$ $_{-11}^{+27}$	19
06108+2743	SU Gem	5750	1703 $_{- 146}^{+ 238}$ $_{-146}^{+238}$	0 $_{- 0}^{+ 0.22}$ $_{-0}^{+0.22}$	90 $_{- 15}^{+ 97}$ $_{-15}^{+97}$	792
08011-3627	AR Pup	6000	661 $_{- 63}^{+ 82}$ $_{-63}^{+82}$	0.15 $_{- 0.15}^{+ 0.56}$ $_{-0.15}^{+0.56}$	90 $_{- 32}^{+ 322}$ $_{-32}^{+322}$	915
20131+2554	EF Vul	4250	1790 $_{- 51}^{+ 60}$ $_{-51}^{+60}$	0.16 $_{- 0.16}^{+ 0.22}$ $_{-0.16}^{+0.22}$	124 $_{- 27}^{+ 55}$ $_{-27}^{+55}$	35
22327-1731	HD 213985; HM Aqr	8250	702 $_{- 22}^{+ 28}$ $_{-22}^{+28}$	0.11 $_{- 0.04}^{+ 0.11}$ $_{-0.04}^{+0.11}$	144 $_{- 22}^{+ 76}$ $_{-22}^{+76}$	45
06489-0118	SZ Mon	4700	1437 $_{- 103}^{+ 118}$ $_{-103}^{+118}$	0.01 $_{- 0.01}^{+ 0.09}$ $_{-0.01}^{+0.09}$	193 $_{- 27}^{+ 72}$ $_{-27}^{+72}$	38
17233-4330	V1504 Sco	6250	2485 $_{- 359}^{+ 495}$ $_{-359}^{+495}$	0.25 $_{- 0.25}^{+ 0.08}$ $_{-0.25}^{+0.08}$	203 $_{- 118}^{+ 148}$ $_{-118}^{+148}$	469
(...)	(...)	(...)	(...)	(...)	(...)	(...)

Notes. The table lists the following information for each object: its IRAS name, alternative identifications, effective temperature T_eff, distance D, reddening E(B − V), luminosity L, and IR-to-stellar luminosity ratio L_IR/L_*. The effective temperatures are taken from Kluska et al. (2022) and have a formal error of ±250 K. The distances correspond to the geometric distances from Bailer-Jones et al. (2021). The whole table is available at CDS.

^(a)

Luminosities are taken from Men’shchikov et al. (2002), as no distance is available from Bailer-Jones et al. (2021) due to the lack of a Gaia parallax measurement.

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