Table 2.
Basic data for our S star sample.
| CSS | Name | Sp. type | V | K | J | ϖEDR3 ± σϖ | Z5 | EB − V | BCK | Observation date | S/N |
|---|---|---|---|---|---|---|---|---|---|---|---|
| (mas) | (mas) | ||||||||||
| 89 | V1139 Tau | S | 7.90 | 0.97 | 2.27 | 1.79 ± 0.05 | −0.047 | 0.34 | 3.00 | 23 November 2012 | 150 |
| 151 | CSS 151 | S | 10.99 | 4.64 | 5.97 | 0.36 ± 0.03 | −0.053 | 0.27 | 2.91 | 31 July 2017 | 40 |
| 233 | HD 288833 | S3/2 | 9.40 | 4.26 | 5.51 | 0.83 ± 0.02 | −0.038 | 0.31 | 2.84 | 20 August 2012 | 100 |
| 265 | KR CMa | M4S | 8.50 | 1.96 | 3.30 | 1.29 ± 0.03 | −0.030 | 0.11 | 3.01 | 10 April 2011 | 70 |
| 312 | AA Cam | M5S | 7.79 | 1.39 | 2.59 | 2.08 ± 0.05 | −0.024 | 0.13 | 2.84 | 9 April 2011 | 90 |
| 416 | HD 64147 | S5/2.5 | 9.20 | 3.61 | 5.00 | 0.56 ± 0.03 | −0.041 | 0.09 | 2.93 | 27 November 2016 | 40 |
| 454 | CSS 454 | S | 10.39 | 4.93 | 6.13 | 0.40 ± 0.03 | −0.045 | 0.07 | 2.91 | 2 February 2017 | 50 |
| 474 | CD −27°5131 | S4,2 | 9.62 | 2.72 | 4.35 | 0.64 ± 0.03 | −0.031 | 0.14 | 3.01 | 2 April 2010 | 70 |
| 597 | BD −18°2608 | S | 9.58 | 4.01 | 5.27 | 0.71 ± 0.02 | −0.038 | 0.14 | 2.91 | 24 March 2018 | 70 |
| 997 | V812 Oph | S5+/2.5 | 10.58 | 4.00 | 5.22 | 0.64 ± 0.03 | −0.053 | 0.22 | 2.93 | 22 April 2016 | 40 |
| 1070 | V679 Oph | S5/5+ | 8.92 | 2.69 | 4.16 | 1.04 ± 0.03 | −0.049 | 0.37 | 2.83 | 16 March 2018 | 80 |
| 1152 | Vy 12 | S5−/6 | 10.13 | 3.76 | 5.06 | 0.58 ± 0.02 | −0.037 | 0.21 | 2.99 | 18 March 2018 | 80 |
| 1315 | HR Peg | S4+/1+ | 6.36 | 0.94 | 2.15 | 2.14 ± 0.08 | −0.043 | 0.12 | 2.93 | 17 July 2009 | 60 |
Notes. Columns 1 and 2 list different identifiers: CGSS (Stephenson 1984) entry number and HD, BD or other names. Columns 3, 4, 5, and 6 indicate spectral type, V, K and J magnitudes, respectively, extracted from the SIMBAD Astronomical Database (Wenger et al. 2000). Column 7 lists the Gaia EDR3 parallax and its error. Z5 is the five-parameter zero-point correction on the parallax from Lindegren et al. (2021). The reddenning EB − V has been obtained from the Gontcharov (2017) extinction maps. BCK is the bolometric correction in the K band as computed from the MARCS model atmospheres. Columns 10 and 11 document the HERMES observation dates and their signal-to-noise ratio (S/N) around 500 nm.
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