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.6.

Estimated orbital periods of the Galactic post-RGB binary subsample without observed orbital periods.

Name	P_orb/ days	$P_{orb}^{\min} / days$ $P_{\mathrm{orb}}^{\mathrm{min}}/\mathrm{\,days}$	$P_{orb}^{\max} / days$ $P_{\mathrm{orb}}^{\mathrm{max}}/\mathrm{\,days}$	P_orb/ days	$P_{orb}^{\min} / days$ $P_{\mathrm{orb}}^{\mathrm{min}}/\mathrm{\,days}$	$P_{orb}^{\max} / days$ $P_{\mathrm{orb}}^{\mathrm{max}}/\mathrm{\,days}$
	Z = 0.02	Z = 0.02	Z = 0.02	Z = 0.00142	Z = 0.00142	Z = 0.00142
EZ Gem	32	13	48	20	9	29
EF Vul	80	62	116	47	37	67
IRAS 13258-8103	92	16	568	54	10	296
SZ Mon	125	107	173	72	62	97
IRAS 22251+5406	273	221	368	149	122	197
HD 186438	356	313	463	191	169	244
CC Lyr	428	297	757	227	161	387
UY Ara	469	354	1029	247	190	516
HD 340949	529	227	872	276	125	442
EZ Aql	571	234	863	297	129	437
GK Car	581	310	1078	302	168	538
V Vul	720	382	1556a	369	204	633a
IRAS 20094+3721	739	499	1323	378	262	633a
V1711 Sgr	754	611	1155	385	317	574
CN Cen	1097	504	1556a	548	264	633a
GZ Nor	1175	510	1556a	584	267	633a
HD 114855; V956 Cen	1456	1049	1556a	633b	525	...

Notes. The table lists the following information for each object: its name and estimated orbital period P_orb determined from its luminosity for both metallicities (see Sect. 4.2). $P_{orb}^{\min}$ $P_{\mathrm{orb}}^{\mathrm{min}}$ and $P_{orb}^{\max}$ $P_{\mathrm{orb}}^{\mathrm{max}}$ correspond to the orbital periods estimated using the luminosity upper and lower limits, respectively.

^(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.

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