Table 3
Metallicity comparisons with high-resolution studies.
| Median Δ[Fe/H] ± Std.dev relative to surveys | Median | ||||
|---|---|---|---|---|---|
| Selection | APOGEE | GALAH | Li et al. (2022) | cr([Fe/H])(a) | [Fe/H] source |
| MP+(b) | 0.00 ± 0.16 | 0.06 ± 0.19 | 0.06 | GSP-Spec | |
| −0.01 ± 0.16 | 0.06 ± 0.19 | 0.32 | This work | ||
| (N) | 141 298 | 104050 | |||
| MP+([Fe/H]HR < −1.5) | 0.22 ± 0.36 | 0.22 ± 0.36 | 0.19 ± 0.43 | 0.33 | GSP-Spec |
| 0.02 ± 0.17 | −0.01 ± 0.19 | 0.21 ± 0.29 | 0.18 | This work | |
| (N) | 571 | 324 | 22 | ||
| RMP (c) | −0.00 ± 0.19 | 0.05 ± 0.22 | 0.08 | GSP-Spec | |
| 0.00 ± 0.17 | 0.07 ± 0.20 | 0.30 | This work | ||
| (N) | 174753 | 142535 | |||
| RMP ([Fe/H]HR < −1.5) | 0.23 ± 0.42 | 0.24 ± 0.50 | 1.22 ± 0.90 | 0.35 | GSP-Spec |
| 0.02 ± 0.18 | −0.01 ± 0.20 | 0.22 ± 0.25 | 0.18 | This work | |
| (N) | 654 | 390 | 64 | ||
| eRMP1(d) | −0.00 ± 0.19 | 0.05 ± 0.22 | 0.08 | GSP-Spec | |
| 0.00 ± 0.17 | 0.07 ± 0.20 | 0.30 | This work | ||
| (N) | 175 635 | 142 606 | |||
| eRMP1([Fe/H]HR < −1.5) | 0.22 ± 0.43 | 0.23 ± 0.51 | 1.19 ± 0.89 | 0.35 | GSP-Spec |
| 0.01 ± 0.19 | −0.00 ± 0.21 | 0.23 ± 0.34 | 0.18 | This work | |
| (N) | 678 | 413 | 67 | ||
| eRMP2 (e) | −0.00 ± 0.19 | 0.05 ± 0.22 | 0.08 | GSP-Spec | |
| 0.00 ± 0.17 | 0.07 ± 0.20 | 0.30 | This work | ||
| (N) | 175 667 | 142611 | |||
| eRMP2([Fe/H]HR < −1.5) | 0.20 ± 0.54 | 0.23 ± 0.54 | 0.98 ± 1.06 | 0.36 | GSP-Spec |
| 0.02 ± 0.21 | −0.00 ± 0.22 | 0.24 ± 0.34 | 0.18 | This work | |
| (N) | 704 | 418 | 76 | ||
Notes. The following stars are removed from the comparisons: [Fe/H]GALAH < −1.5 and [Fe/H]Thisstudy > −0.5 in GALAH, and Gaia DR3 4580919415339537280, a relatively hot horizontal branch star that is an outlier in Fig. 8 of Li et al. (2022). (a)The median uncertainty in GSP-Spec or our new metallicity estimates. We also provide uncertainties for stars with [Fe/H] < −1 .5 in the corresponding metallicities. (b)The sample selected according to the quality cuts by Recio-Blanco et al. (2023) combined with the cuts on our photometric stellar parameters. (c)Conditions on GSP-Spec solutions are relaxed from the MP+ sample. More specifically, we remove constraints on the first six digits of the GSP-Spec flags, which are related to vbroad[TGM] and vrad[TGM]. We also include stars with hot Teff,GSP-Spec and high log g (region B in Fig. 4). (d)In addition to the RMP sample, this sample includes stars with KMgiantPar = 1, [M/H]gspspec > −3, and log 
. (e) In addition to the eRMP1 sample, this sample includes stars with KMgiantPar = 1, [M/H]gspspec = −3.51.
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