Table 2
Atmospheric parameters for the KEYSTONE sample.
| K2 | IRFM | SPC | |||||||
|---|---|---|---|---|---|---|---|---|---|
| EPIC | Cam. | Kp (mag) | θ (µas) | Teff (K) | Teff (K) | log 𝑔 (cgs; dex) | [Fe/H] (dex) | υ sin i★ (km s−1) | LOS (km s−1) |
| 201623069 | 14 | 8.50 | 151 ± 3 | 6029 ± 40 | 5827 ± 77 | 3.98 ± 0.10 | 0.06 ± 0.10 | 7.07 ± 0.50 | 7.47 ± 0.07 |
| 201644284 | 10 | 8.20 | 217 ± 3 | 5329 ± 30 | 5383 ± 77 | 3.88 ± 0.10 | 0.19 ± 0.10 | 2.82 ± 0.50 | −16.24 ± 0.01 |
| 201725213 | 14 | 10.17 | 93 ± 2 | 5278 ± 37 | 5359 ± 78 | 3.78 ± 0.10 | 0.07 ± 0.10 | 3.61 ± 0.50 | 13.88 ± 0.08 |
| 203530127 | 11 | 7.11 | 259±4 | 6212 ± 45 | 6180 ±77 | 4.05 ± 0.10 | 0.15 ± 0.10 | 8.59 ± 0.50 | −22.22 ± 0.05 |
| 211311380 | 18 | 9.13 | 114±3 | 6339 ± 50 | 6307 ± 77 | 4.31 ± 0.10 | −0.04 ± 0.10 | 7.07 ± 0.50 | 50.70 ± 0.04 |
| 211388537(a) | 18 | 12.29 | 41 ± 1 | 5046 ± 41 | 5021 ± 77 | 3.40 ± 0.10 | −0.06 ± 0.10 | 3.19 ± 0.50 | 34.05 ± 0.07 |
| 211401787 | 18 | 9.71 | 83 ± 2 | 6336 ± 53 | 6213 ±77 | 4.21 ± 0.10 | −0.09 ± 0.10 | 9.26 ± 0.50 | 10.77 ± 0.02 |
| 211403248(a) | 16, 18, A | 12.31 | 41 ± 2 | 5023 ± 38 | 5042 ± 77 | 3.44 ± 0.10 | 0.01 ± 0.10 | 3.29 ± 0.50 | 33.52 ± 0.10 |
| 211405262(a) | 16, 18, A | 12.66 | 35 ± 2 | 5091 ± 39 | 5150 ± 82 | 3.55 ± 0.10 | 0.14 ± 0.10 | 3.47 ± 0.50 | 34.18 ± 0.10 |
| 211409088 | 5, 16,18, A | 12.82 | 5198 ±102 | 3.67 ± 0.14 | 0.27 ± 0.10 | 5.31 ± 0.52 | 33.20 ± 0.15 | ||
| – | 31 ± 2 | 5136 ± 36 | 5160 ± 100(b) | 3.72 ± 0.07(b) | −0.01 ± 0.01(b) | ||||
Notes. The table is available in its entirety in the machine-readable format at the CDS. A portion is shown here for guidance regarding its form and content. The table provides atmospheric parameters for the 173 targets under study, sorted by EPIC ID. “Cam” gives the K2 campaign(s) during which a given target was observed in SC, and indicates which individual campaigns resulted in a detection of oscillations – no detections were made from individual campaigns written in italics. An “A” indicates that the seismic values are based on the combined data from all campaigns. We note that analysis was not performed for individual C5 data, but this data was included if available when combining all data for a given star. “θ” gives the stellar angular diameter from the IRFM in µas. Results from the IRFM are generally based on especially SPC [Fe/H] and E(B – V) as listed in Table 3; “LOS” gives the line-of-sight velocity from the CfA TRES observations, corrected by −0.61 km/s. Deviations from the standard sources mentioned here are stated in the table, see the footnotes. A repeated entry for a given star (in which the EPIC is not indicated again) gives the spectroscopic values adopted from a literature study, and the associated IRFM results, in cases where the quality of the SPC data was deemed too low. (a)Member of M67; (b)Parameters from APOGEE DR16 (Jönsson et al. 2020); (c)Parameters from Luck (2017), uncertainty on [Fe/H] assigned based on spread from GCS (Casagrande et al. 2011); (d)GCS average metallicity (Casagrande et al. 2011); (e)RV from Gaia DR2 (Soubiran et al. 2018); (f)poor 2MASS-EDR3 cross-match;(𝑔)high phot_bp_rp_excess_factor on Gaia photometry; (h)poor 2MASS photometry; (*)SPC has poor quality factor.
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