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.8.

Estimated post-mass-transfer ages of the Galactic post-RGB binary subsample.

Name	$t_{pRGB}^{mean} / kyr$ $t_{\mathrm{pRGB}}^{\mathrm{mean}}/\mathrm{kyr}$	$t_{pRGB}^{\min} / kyr$ $t_{\mathrm{pRGB}}^{\mathrm{min}}/\mathrm{kyr}$	$t_{pRGB}^{\max} / kyr$ $t_{\mathrm{pRGB}}^{\mathrm{max}}/\mathrm{kyr}$	$t_{pRGB}^{mean} / kyr$ $t_{\mathrm{pRGB}}^{\mathrm{mean}}/\mathrm{kyr}$	$t_{pRGB}^{\min} / kyr$ $t_{\mathrm{pRGB}}^{\mathrm{min}}/\mathrm{kyr}$	$t_{pRGB}^{\max} / kyr$ $t_{\mathrm{pRGB}}^{\mathrm{max}}/\mathrm{kyr}$
	Z = 0.02	Z = 0.02	Z = 0.02	Z = 0.00142	Z = 0.00142	Z = 0.00142
EZ Gem	4000	3000	10000	3000	1000	10000
AU Peg	2000	2000	3000	1000	700	2000
EF Vul	0	0	600	0	0	0
IRAS 13258-8103	1000	100	9000	600	70	6000
HD 213985; HM Aqr	1000	600	1000	900	500	1000
SZ Mon	500	400	800	0	0	100
BT Lac	500	200	800	200	0	400
IRAS 22251+5406	200	200	300	200	100	200
IRAS 06165+3158	200	100	200	200	100	200
HD 186438	200	100	200	100	100	200
AY Lep	90	0	100	0	0	0
R Sge	200	90	200	100	70	100
CC Lyr	200	100	200	100	80	200
DY Ori	200	100	200	100	80	200
DF Cyg	100	100	200	70	0	100
IRAS 06452-3456	100	60a	500	100	60a	300
UY Ara	100	80	200	100	60	100
SU Gem	100	90	200	100	30	100
ST Pup	100	100	200	100	80	100
HD 340949	100	90	300	70	0	200
AR Pup	100	60a	200	80	60a	100
EZ Aql	100	90	300	70	70	200
GK Car	100	80	200	90	60	100
V1504 Sco	100	80	300	90	70	200
SX Cen	100	90	100	90	30	100
V Vul	100	60a	200	70	50a	100
IRAS 20094+3721	100	80	100	80	60a	100
V1711 Sgr	90	70	100	60	40	80
TW Cam	80	70	100	20	0	70
CN Cen	80	50a	100	60	40a	90
GZ Nor	70	50a	100	40	0	80
GP Cha	80	60a	100	60	50a	80
V1333 Sco	80	60a	90	60b	30a	60
RV Tau	70	50a	80	20b	0	50
RS Sge	80	60a	100	60b	60a	90
HD 114855; V956 Cen	60	60a	90	60b	60a	70
HD 137569	60b	60a	90	70b	70a	80

Notes. The table lists the following information for each object: its name and estimated mean, minimum, and maximum post-mass-transfer age t_pRGB determined from its position in the HRD for both metallicities (see Sect. 4.2).

^(a)

Upper limit on the minimum post-mass-transfer age, as the luminosity upper limit of the object is larger than the maximum luminosity of the binary models.

^(b)

Upper limit on the mean post-mass-transfer age, as the luminosity of the object is larger than the maximum luminosity of the binary models.

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