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Table 2.

CEMP stars that have Gaia radial velocity uncertainties > 1 km s−1, with new binary candidates in bold-face.

Name CEMP G rvGaia σGaia rvlita σlit nlit Ref. Teffb [Fe/H]c Teff, T [Fe/H]T
class (mag) (km s−1) (km s−1) (km s−1) (km s−1) (K) (K)
HE 2155–3750 s 13.1 77.5 4.5 27.7 10.0b 1 1 5000 −2.64 5500 0.0
HE 1305+0007 s 11.9 228.5 3.3 217.8 1.5 1 2 4750 −2.08 4750 −2.0
HE 2123–0329 no 13.1 −217.7 3.1 −219.1 0.4 2 3 4725 −3.22 6500 −1.5
SMSS J1738–1457 no 12.9 43.7 3.1 −26.9 2.0 1 4 4600 −3.58 5700 0.0
HKII 17435–00532 r/s 12.8 39.3 2.4 38.9 0.3 4 5 5200 −2.23 6000 −1.5
CS 30301–015 s 12.8 87.0 1.8 86.6 0.1 18 6 4900 −2.73 6000 −1.5
HE 2319–5228 no 13.0 286.2 1.8 294.3 4.0 2 7 4900 −2.60 6000 −1.5
BS 16077–077 s 11.9 68.3 1.7 ... ... ... ... 5900 −2.05 6000 −1.5
CS 22947–187 s 12.8 −252.3 1.4 −251.9 0.9 2 8,9 5300 −2.58 6000 −1.5
HE 1305+0132 s 12.4 157.0 1.4 ... ... ... ... 4462 −2.45 4500 0.0
CS 22873–128 no 12.8 207.15 1.2 205.5 0.3 2 8,9 4710 −3.32 6000 −1.5

Notes.

(a)

For stars with only one measurement, this is the radial velocity as presented in the literature. For stars with multiple measurements (see column nlit), it is the (weighted) average of the different measurements. Similarly, for the uncertainty, it is either the uncertainty reported in the literature or the (weighted) standard deviation between different literature values.

(b)

As reported in the Yoon et al. (2016) compilation.

(c)

No uncertainty is given in the reference, but since it is a measurement from an intermediate-resolution spectrum, we assume σ = 10 km s−1.

References. (radial velocities) (1) Placco et al. (2011), (2) Goswami et al. (2006), (3) Hollek et al. (2011), (4) Jacobson et al. (2015), (5) Roederer et al. (2008), (6) Hansen et al. (2016a), (7) Beers et al. (2017), (8) Roederer et al. (2014), and (9) McWilliam et al. (1995).

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