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.7.

Estimated orbital periods and post-mass-transfer ages of the post-RGB binary candidate subsamples in the LMC and SMC.

Object	Host	P_orb/ days	$P_{orb}^{\min} / days$ $P_{\mathrm{orb}}^{\mathrm{min}}/\mathrm{\,days}$	$P_{orb}^{\max} / days$ $P_{\mathrm{orb}}^{\mathrm{max}}/\mathrm{\,days}$	$t_{pRGB}^{mean} / kyr$ $t_{\mathrm{pRGB}}^{\mathrm{mean}}/\mathrm{kyr}$	$t_{pRGB}^{\min} / kyr$ $t_{\mathrm{pRGB}}^{\mathrm{min}}/\mathrm{kyr}$	$t_{pRGB}^{\max} / kyr$ $t_{\mathrm{pRGB}}^{\mathrm{max}}/\mathrm{kyr}$	$t_{pRGB}^{mean} / kyr$ $t_{\mathrm{pRGB}}^{\mathrm{mean}}/\mathrm{kyr}$	$t_{pRGB}^{\min} / kyr$ $t_{\mathrm{pRGB}}^{\mathrm{min}}/\mathrm{kyr}$	$t_{pRGB}^{\max} / kyr$ $t_{\mathrm{pRGB}}^{\mathrm{max}}/\mathrm{kyr}$
					Z = 0.02	Z = 0.02	Z = 0.02	Z = 0.00142	Z = 0.00142	Z = 0.00142
J045745.46-683724.1	LMC	41	40	93	2000	700	2000	2000	500	2000
J054144.88-712351.7	LMC	44	44	76	2000	700	2000	0	0	1000
J053811.63-680824.9	LMC	46	39	59	2000	1000	2000	800	0	1000
J053030.78-701805.5	LMC	48	47	64	1000	600	1000	0	0	0
J051412.13-702026.0	LMC	54	48	122	2000	500	2000	1000	300	1000
J051751.41-713507.3	LMC	58	34	105	1000	600	3000	1000	500	3000
J045736.84-705127.2	LMC	63	47	77	1000	1000	2000	1000	1000	2000
J052107.90-714104.4	LMC	63	39	102	1000	700	3000	1000	600	3000
J045058.16-671634.4	LMC	76	59	231	1000	200	1000	700	200	900
(...)	(...)	(...)	(...)	(...)	(...)	(...)	(...)	(...)	(...)	(...)

Notes. The table lists the following information for each object: its identification, host Magellanic Cloud, estimated orbital period P_orb determined from its luminosity (see Appendix A), and the estimated post-mass-transfer age t_pRGB determined from its position in the HRD for both metallicities (see Sect. 5.3). $P_{orb}^{\min}$ $P_{\mathrm{orb}}^{\mathrm{min}}$ and $P_{orb}^{\max}$ $P_{\mathrm{orb}}^{\mathrm{max}}$ correspond to the orbital periods estimated using the luminosity upper and lower limits, respectively. We do not estimate the orbital periods of OGLE-LMC-T2CEP-032 and OGLE-LMC-T2CEP-200, as these have already been photometrically determined. The whole table is available at CDS.

^(a)

Lower limit on the maximum orbital period, as the luminosity upper limit of the object is larger than the maximum luminosity of the binary models.

^(b)

Lower limit on the orbital period, as the luminosity of the object is larger than the maximum luminosity of the binary models.

^(c)

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.

^(d)

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.

^(e)

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

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