The most metal-poor tail of the Galactic halo: Hypothesis for its origin from precise spectral analysis

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Table A.2

Effective temperature determinations from diverse methods, spectral resolution and signal-to-noise ratio.

Star	T_eff (B − RP)	T_eff (G − BP)	$T_{eff}^{phot} / T_{eff}^{int} / T_{eff}^{IRFM}$ $T_\frame{\frame{\text{eff~}}}^\frame{\frame{\text{phot~}}}/T_\frame{\frame{\text{eff~}}}^\frame{\frame{\text{int~}}}/T_\frame{\frame{\text{eff~}}}^\frame{\frame{\text{IRFM~}}}$	T_eff (Hα)	⟨T_eff⟩	$δ T_{eff}^{E (B - V)}$ $\delta T_\frame{\frame{\text{eff~}}}^\frame{E(B - V)}$	comments	R	S/N
BD+24 1676	—	—	— / — / 6387 ± 92	6440 ± 33	6433 ± 23	—	—	56990	489
BD-10 388	—	—	—/—/6260±61	6293 ± 43	6285 ± 19	—	—	51690	528
BPS CS22166-030	—	—	—/—/6039±59	6255 ± 39	6203 ± 130	—	—	51690	544
CD-35 14849	—	—	—/—/6396±65	6377 ± 34	6380 ± 10	—	—	51690	526
BD+03 740	—	—	— / — / 6419 ± 83	6385 ± 48	6388 ± 13	—	—	51690	655
BD-13 3442	—	—	— / — / 6434 ± 80	6446 ± 34	6444 ± 6	—	—	56990	778
BD+26 2621	—	—	—/—/6336±72	6457 ± 31	6436 ± 65	—	—	51690	381
CD-33 1173	—	—	—/—/6685±68	6602 ± 32	6617 ± 46	—	—	51690	564
CD-71 1234	—	—	—/—/6408±69	6432 ± 31	6427 ± 13	—	—	51690	547
HE 0926−0508	6645 ± 31	6481 ± 69	—/ —/ 6451 ± 79	6458 ± 32	6457 ± 3	77	—	42310	178
LP 815−43	—	—	—/ —/ 6535 ± 68	6539 ± 41	6538 ± 2	—	—	107200	665
LP 831−70	—	—	—/ —/ 6408 ± 67	6379 ± 35	6384 ± 16	—	—	51690	315
UCAC2 20056019	6390 ± 27	6412 ± 68	—/ —/ 6393 ± 14	6443 ± 33	6401 ± 25	9	—	42310	124
Wolf 1492	6513±32	6577 ± 75	—/—/6523±52	6592 ± 32	6572 ± 44	41	—	42310	226
HD 140283	—	—	— / 5792 ± 55/ —	5810±32	5805 ± 11	—	—	14000	955
BPSBS16023−046	6497 ± 30	6524 ± 73	— / — / 6501 ± 7	6526 ± 83	6502 ± 7	13	—	42310	46
BPS BS16968−061	6241 ± 32	6276 ± 72	—/ —/ 6247 ± 37	6267 ± 69	6252 ± 12	32	—	42310	169
BPS CS22177−009	6368 ± 34	6398 ± 76	—/ —/ 6373 ± 35	6415 ± 92	6353 ± 74	31	—	42310	140
BPS CS22953−037	6505 ± 30	6529 ± 73	—/ —/ 6508 ± 23	6537 ± 103	6510±9	20	—	42310	97
BPS CS29518−043	6513±30	6543 ± 74	—/ —/ 6517 ± 20	6579±115	6519 ± 15	14	—	42310	98

BPS BS 17569−049	4798 ± 20	4800 ± 33	4798 ± 61 / —/ —	4790 ± 55	4794 ± 6	12	—	42310	275
BPS CS 22953−003	5171 ± 19	5189±40	5174 ± 72/ —/ —	5155±47	5160 ± 12	39	—	42310	171
HD 186478	4769 ± 34	4770 ± 45	4770 ± 111 /—/—	4804 ± 75	4793 ± 22	93	SB	42310	341
BD+09 2870	4721 ± 18	4731 ± 33	4723 ±61 /—/—	4725 ± 80	4724 ± 1	9	—	42310	169
BD-18 5550	4909 ± 51	4900 ± 63	4906 ± 95/ —/ —	5030 ± 76	4981 ± 85	74	—	42310	520
BPS CS 22186−025	5056 ± 20	5065 ± 39	5057 ± 60/ —/ —	5036 ± 41	5042 ± 14	11	—	42310	113
BPS CS 22891−209	4826 ± 27	4808 ± 41	4820 ± 66 / —/ —	4896 ± 132	4835 ± 43	25	—	42310	250
BPS CS 22896−154	5309 ± 26	5312±46	5310 ± 65/ —/ —	5274 ± 53	5288 ± 25	24	—	42310	179
BPS CS 22956−050	5039 ± 21	5028 ± 40	5036 ± 62/ —/ —	4960 ± 187	5028 ± 32	12	—	42310	150
BPS CS 22966−057	5549 ± 23	5542 ± 52	5548 ± 61 / —/ —	5469 ± 146	5536 ± 40	9	—	42310	160
BPS CS 29491−053	4850 ± 20	4834 ± 35	4846 ± 61 / —/ —	4775 ± 135	4834 ± 38	7	—	42310	145
BPS CS 29518−051	5339 ± 20	5341 ± 45	5339 ± 60/ —/ —	5340 ± 91	5339 ± 6	7	—	42310	159
HD 122563	—	—	— / 4635 ± 34/ —	4616 ± 54	4627 ± 13	—	—	19000	660

GESJ17543319-4110487	5105±70	5087 ± 92	5098 ± 113/ —/ —	5129 ± 160	5108±21	95	—	47000	40
GESJ17545552-3803393	4772 ± 84	4725 ±101	4754 ± 124/ —/ —	4717 ± 269	4748 ± 20	104	—	47000	28
GESJ17574658-3847500^⋆	5088 ± 81	5542±112	5251 ± 306/ —/ —	—	—	119	Hα(em)/1.47	47000	27
GESJ18185545-2738118^⋆	4859 ± 98	5015 ± 125	4921 ± 197 / —/ —	—	—	154	Hα(em)/1.21	47000	31
GESJ18215385-3410188	4919 ± 44	4945 ± 62	4928 ± 77 / —/ —	4904 ± 237	4925 ± 10	46	—	47000	72
GESJ18261627-3154272	4965 ± 68	5194±90	5014 ± 149/ —/ —	4827 ± 156	4924 ± 132	103	—	47000	31
GESJ18265160-3159404^⋆	4603 ± 74	4561 ± 88	4586 ± 102/ —/ —	—	—	76	Hα(em)	47000	43
GESJ18361733-2700053	4908 ± 83	4864± 103	4890 ± 135/ —/ —	4789 ± 86	4818±65	117	—	47000	36
GESJ18370372-2806385	4831 ± 64	4836 ± 79	4833 ± 110 / —/ —	5044 ± 211	4878 ± 122	91	—	47000	62
GESJ18374490-2808311	4589 ± 69	4572 ± 82	4582 ± 97/ —/ —	4727 ± 150	4627 ± 99	75	—	47000	23
GESJ01293652-5020327^‡	6278 ± 43	6331 ± 69	6293 ± 69 / —/ —	6343 ± 71	6368 ± 35	8	Hα(em)/SB?	47000	44
GESJ03372526-2724127^⋆	5814±29	5824 ± 56	5816 ± 61 / —/ —	—	—	6	Hα(art)	47000	55
GESJ09475504-1027247^⋆	5403 ± 26	5402 ± 57	5403 ± 64/ —/ —	—	—	22	Hα(art)	47000	112
GESJ10091577-4127155^⋆	5368 ± 56	5348 ± 79	5361 ± 100/ —/ —	—	—	79	Hα(art)	47000	70
GESJ10142785-4052503^⋆	5206 ± 60	5191 ± 80	5201 ± 102/ —/ —	—	—	83	Hα(art)	47000	141
GESJ10580638-1542390	4828 ± 35	4819±57	4826 ± 64 / —/ —	4955 ± 201	4838 ± 53	20	—	47000	53
GESJ12555146-4507342^⋆	5053 ± 38	5066 ± 63	5057 ± 73/ —/ —	—	—	40	Hα(em)	47000	53
GESJ14214860-4408399^⋆	4678 ± 48	4666 ± 64	4674 ± 69 / —/ —	—	—	34	Hα(em)	47000	44
GESJ14410090-4007413	4907 ± 39	4912 ± 59	4908 ± 68 / —/ —	4976 ± 110	4926 ± 43	31	—	47000	99
GESJ15300154-2005148	5644 ± 48	5704 ± 63	5666 ± 98/ —/ —	5826 ± 31	5811±65	66	—	47000	80
GESJ22125747-4539203	5524 ± 23	5522 ± 56	5524 ± 61 /—/—	5417 ± 116	5500 ± 62	9	—	47000	53
GESJ22494718-5001048	6301 ± 41	6322 ± 69	6307 ± 62 / —/ —	6235 ± 230	6302 ± 25	5	—	47000	30

Notes. The second and third columns list temperatures derived from the Gaia colours using the relations of Casagrande et al. (2021); the errors accompanying the values include those induced by log g and [Fe/H] errors. The fourth column lists either $T_{eff}^{phot}, T_{eff}^{int}$ $T_\frame{\frame{\text{eff~}}}^\frame{\frame{\text{phot~}}},T_\frame{\frame{\text{eff~}}}^\frame{\frame{\text{int~}}}$ , or $T_{eff}^{IRFM}$ $T_\frame{\frame{\text{eff~}}}^\frame{\frame{\text{IRFM~}}}$ ; where $T_{eff}^{phot}$ $T_\frame{\frame{\text{eff~}}}^\frame{\frame{\text{phot~}}}$ is the weighted average of the quantities in the first two columns. The corresponding errors are internal and include the influence of the interstellar extinction uncertainty in the budget. $T_{eff}^{int}$ $T_\frame{\frame{\text{eff~}}}^\frame{\frame{\text{int~}}}$ and $T_{eff}^{IRFM}$ $T_\frame{\frame{\text{eff~}}}^\frame{\frame{\text{IRFM~}}}$ (direct measurements, not from calibrated relations) are fundamental determinations. Stars with them do not include T ^phot to avoid potential biases. $T_{eff}^{IRFM}$ $T_\frame{\frame{\text{eff~}}}^\frame{\frame{\text{IRFM~}}}$ and $T_{eff}^{int}$ $T_\frame{\frame{\text{eff~}}}^\frame{\frame{\text{int~}}}$ are provided by Casagrande et al. (2010) and Karovicova et al. (2020), respectively. The fifth column displays T_eff(Hα) along with its internal uncertainty, according to the expansion in Giribaldi et al. (2021) and Giribaldi et al. (2023). Sixth column lists the weighted average of T_eff(Hα) and the temperature in preceding column. The total uncertainty may be obtained by adding the accuracy of the standard scale in quadrature (50 K Giribaldi et al. 2021, 2023); however, we note that this estimate is dominated by the precision of the interferometic measurements (Casagrande et al. 2014; Giribaldi et al. 2021, 2023). The seventh column lists the error in temperature induced by the uncertainty in E(B V). The eighth column lists the comments according to the coding: Spectroscopic binary (SB), emission around the Hα core (Hα(em)), artefact at the Hα profile (Hα(art)), Gaia ruwe value is given when > 1. The two last columns list the nominal spectral resolution and S/N around the Mg line at 5528 Å. Stars indicated with the symbol (⋆) have T_eff determined only with Gaia colour calibrations because of distorted Hα profiles. The star accompanied by the symbol (‡) has unreliable atmospheric parameters, see main text in Sect 3.

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