Table D.2
List of BSSs detected in this study and their properties.
| isochrone method | ||||||||||||||
|---|---|---|---|---|---|---|---|---|---|---|---|---|---|---|
| cluster | type | Gaia source id | Teff,IRFM | Teff | log(age/yr) | M | log (L/L⊙) | logg | Teff, xpp | loggxpp | Me | Mesequence | BP0 | (BP-RP)0 |
| (K) | (K) | (M⊙) | (K) | (mag) | (mag) | |||||||||
| (1) | (2) | (3) | (4) | (5) | (6) | (7) | (8) | (9) | (10) | (11) | (12) | (13) | (14) | (15) |
| NGC2141 | OC | 3341815582307132416 | 6363 ± 82 | 6510 ± 59 | 9.222 ± 0.015 | 1.70 ± 0.01 | 1.040 ± 0.006 | 3.833 ± 0.010 | – | – | 0.17 | lower | 2.237 | 0.597 |
| NGC2141 | OC | 3341815582307133056 | 6391 ± 84 | 6464 ± 79 | 9.222 ± 0.015 | 1.72 ± 0.00 | 1.070 ± 0.003 | 3.800 ± 0.020 | – | – | 0.19 | lower | 2.176 | 0.589 |
| NGC2141 | OC | 3341815681086838272 | 6736 ± 101 | 6855 ± 95 | 9.087 ± 0.077 | 1.56 ± 0.01 | 0.800 ± 0.005 | 4.122 ± 0.025 | – | – | 0.08 | lower | 2.807 | 0.500 |
| ⋮ | ⋮ | ⋮ | ⋮ | ⋮ | ⋮ | ⋮ | ⋮ | ⋮ | ⋮ | ⋮ | ⋮ | ⋮ | ⋮ | ⋮ |
| NGC104 | GC | 4689572883825672192 | 6422 ± 126 | 6567 ± 46 | 9.740 ± 0.027 | 1.01 ± 0.01 | 0.550 ± 0.004 | 4.119 ± 0.015 | 6831 ± 136 | 4.142 ± 0.123 | 0.28 | upper | 3.538 | 0.566 |
| NGC104 | GC | 4689573433581464192 | 6262 ± 109 | 6384 ± 26 | 9.842 ± 0.024 | 0.93 ± 0.01 | 0.350 ± 0.003 | 4.226 ± 0.009 | 6896 ± 166 | 4.216 ± 0.2 | 0.18 | lower | 4.043 | 0.609 |
| NGC104 | GC | 4689574086416430464 | 6669 ± 154 | 6838 ± 35 | 9.505 ± 0.035 | 1.08 ± 0.01 | 0.490 ± 0.002 | 4.271 ± 0.009 | 6652 ± 159 | 4.195 ± 0.142 | 0.37 | upper | 3.651 | 0.505 |
| ⋮ | ⋮ | ⋮ | ⋮ | ⋮ | ⋮ | ⋮ | ⋮ | ⋮ | ⋮ | ⋮ | ⋮ | ⋮ | ⋮ | ⋮ |
Notes. The complete catalog is made available at the CDS. The list of columns presented here is (1) the name of the cluster to which the BSS belong; (2) whether the cluster is classified as an open cluster (OC) or globular cluster (GC); (3) source id of the BSS as per the Gaia DR3; (4) effective temperature of the BSS based on IRFM method; (5) – (9) effective temperature, age, mass, luminosity and surface gravity of the BSS, respectively, estimated using isochrone method; (10) – (11) effective temperature and logg of the BSS estimated from Gaia-XPP spectrum. (12) fractional mass excess of the BSS based compared to MSTO mass; (13) location of the BSS based on mass excess, as mentioned in Figure 9; (14)-(15) BP magnitude and (BP-RP) color in absolute scale.
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