Table 4.
Orbital elements of VELOCE SB1 Cepheids with literature-known orbits (excerpt).
| Cepheid | Ppuls | T0–2.4 M | Data | Porb (d) | e | K (km s−1) | a sin i (au) | fmass | ω (deg) | M1 | rms |
|---|---|---|---|---|---|---|---|---|---|---|---|
| (d) | σPorb | σe | σK | σasini | σfmass | σargperi | M⊙ | (km s−1) | |||
| Update to literature-known SB1s orbits | |||||||||||
| AX Cir | 5.2734 | 54483.59 | V+L | 6284.51 | 0.187 | 10.954 | 6.2167 | 8.1 × 10−1 | 211.34 | 5.0 | 1.76 |
| 33.04 | 12.41 | 0.009 | 0.229 | 0.1311 | 5.1 × 10−2 | 1.21 | |||||
| δ Cep | 5.3663 | 58696.03 | V | 3450.96 | 0.745 | 3.012 | 0.6367 | 2.9 × 10−3 | 242.75 | 5.0 | 0.09 |
| 13.61 | 19.57 | 0.006 | 0.018 | 0.0081 | 9.9 × 10−5 | 0.56 | |||||
| DL Cas | 8.0009 | 58113.85 | V | 684.89 | 0.344 | 16.656 | 0.9846 | 2.7 × 10−1 | 25.92 | 7.1 | 0.30 |
| 1.00 | 0.21 | 0.005 | 0.098 | 0.0061 | 5.0 × 10−3 | 0.60 | |||||
| 57434.67 | V+L | 684.67 | 0.341 | 16.343 | 0.9668 | 2.6 × 10−1 | 29.25 | 1.43 | |||
| 0.99 | 0.06 | 0.004 | 0.102 | 0.0062 | 5.0 × 10−3 | 0.61 | |||||
| FF Aql | 4.4710 | 58253.28 | V | 1433.20 | 0.050 | 4.788 | 0.6300 | 1.6 × 10−2 | 304.87 | 5.8 | 0.14 |
| 35.41 | 5.66 | 0.011 | 0.028 | 0.0045 | 3.0 × 10−4 | 6.55 | |||||
| 58302.23 | V+L | 1431.70 | 0.068 | 4.877 | 0.6403 | 1.7 × 10−2 | 317.41 | 3.68 | |||
| 7.86 | 0.55 | 0.004 | 0.014 | 0.0019 | 1.5 × 10−4 | 2.02 | |||||
| S Mus | 9.6600 | 56663.89 | V | 505.27 | 0.087 | 14.786 | 0.6842 | 1.7 × 10−1 | 197.92 | 6.0 | 0.09 |
| 1.39 | 0.09 | 0.002 | 0.019 | 0.0009 | 6.5 × 10−4 | 0.96 | |||||
| 56152.57 | V+L | 505.16 | 0.081 | 14.777 | 0.6839 | 1.7 × 10−1 | 194.11 | 2.18 | |||
| 2.43 | 0.09 | 0.004 | 0.020 | 0.0009 | 6.8 × 10−4 | 1.75 | |||||
| ... | |||||||||||
Notes. The pulsation period and epoch are retrieved after the RV fitting following the method described in Paper 1. In column 4, “V” denotes when the orbits were strictly fitted with VELOCE data alone, while “V+L” denotes when the orbit was fitted using the combination of vγ residuals from VELOCE and literature datasets (See Section 3.2 for more details). The next columns list the different orbital elements, namely, orbital period (Porb), eccentricity (e), semi-amplitude (K), projected semi-major axis (asini), mass function (fmass), argument of periastron (ω). We estimated the individual Cepheid masses (M1) using period-mass relations based on Geneva stellar evolution models (Ekström et al. 2012), our method was similar to the one described in Anderson et al. (2016a). The last column presents the “rms” (root mean square) of the fit between the Fourier+Keplerian model and the RV data for V orbits and between the keplerian model and epoch residuals for V+L orbits. The full version is available at: https://zenodo.org/records/12818503
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