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Table B.1.

List of 45 CEMP-no stars with multiple radial velocity measurements.

Name nrv rvw σrv P( χ2) Bin? Teff logg [Fe/H] [C/Fe] A(C) [Ba/Fe] [Mg/C] Ref.
(km s−1) (km s−1) (K)
BD+44°493 61 −150.09 0.63 0.015 1 5430 3.4 −3.83 1.35 5.95 −0.60 −0.89 1
BS 16929–005 21 −50.77 0.66 0.629 1 5229 2.6 −3.34 0.99 6.09 −0.41 −0.70 2
CD–24°17504 2 136.25 0.49 0.227 1 6228 3.9 −3.41 1.10 6.12 < −1.05 −0.76 3
CS 22166–016 9 −210.39 0.77 0.607 1 5250 2.0 −2.40 1.02a 7.05a −0.37 −0.34a 4
CS 22877–001 16 166.25 0.12 0.790 1 4790 1.5 −3.31 1.10 6.67 −0.50 −1.17 5
CS 22878–027 21 −91.28 0.61 0.058 1 6319 4.4 −2.51 0.86a 6.78a < −0.75 −0.97a 2
CS 22949–037 26 −125.74 0.29 0.889 1 4630 1.0 −4.38 1.16 5.97 −0.60 −0.36 5
CS 22957–027 40 −66.87 5.16 < 10−6 2 5220 2.7 −3.19 2.61 7.87 −0.81 −2.55 5
CS 29498–043 26 −32.55 0.60 0.994 1 4440 0.5 −3.87 2.75 7.62 −0.49 −1.54 5
CS 29502–092 35 −67.22 0.51 0.575 1 4820 1.5 −3.30 1.06 6.59 −1.36 −1.18 5
CS 29527–015 6 47.13 0.42 0.988 1 6577 3.9 −3.32 1.18 6.29 −0.68 2
G64–12 33 442.55 1.05 0.009 1 6463 4.3 −3.29 1.07a 6.21a −0.07 −0.59a 6
G64–37 22 81.49 0.95 0.312 1 6570 4.4 −3.11 1.12a 6.44a −0.36 −0.74a 6
G77–61 13 −23.94 11.35 < 10−6 2 4000 5.1 −4.08 2.65 7.00 < +1.00 −2.16 7
HE 0020–1741 10 93.06 0.83 0.001 1 4765 1.6 −4.05 1.40 6.12 −1.11 −0.71 6
HE 0057–5959 3 375.64 1.60 0.143 5257 2.7 −4.08 0.86 5.21 −0.46 −0.35 2
HE 0107–5240 7 44.78 1.91 < 10−6 2 5100 2.2 −5.44 3.97 7.03 < +0.93 −3.77 8
HE 0219–1739 15 107.96 5.09 < 10−6 2 4238 0.5 −3.09 1.90 7.55 < −1.39 9
HE 0405–0526 13 165.66 0.04 1.000 1 5083 3.9 −2.18 0.92 7.17 −0.22 9
HE 0557–4840 22 211.94 0.80 0.965 4900 2.2 −4.73 1.59 5.29 < +0.07 −1.43 10
HE 1012–1540 20 225.84 0.47 0.217 1 5230 2.7 −4.17 2.40 6.67 −0.28 −0.56 5
HE 1133–0555 9 270.70 0.34 0.810 1 5526 1.3 −2.40 2.20 8.31 −0.58 9
HE 1150–0428 27 47.49 8.13 < 10−6 2 5208 2.5 −3.47 2.37 7.35 −0.48 −1.98 2
HE 1201–1512b 13 238.91 2.51 0.016 1 5725 4.7 −3.86 1.14 5.71 < +0.05 −0.86 2
HE 1300–0641 2 68.79 0.11 0.162 1 5308 3.0 −3.14 1.25 6.54 −0.82 −1.23 11
HE 1300+0157 20 74.40 0.70 0.871 1 5529 3.3 −3.75 1.31 5.99 < −0.85 −0.98 2
HE 1302–0954 3 32.56 0.04 0.973 1 5120 2.4 −2.25 1.17 7.37 < −0.53 9
HE 1327–2326 17 64.38 1.30 0.202 1 6180 3.7 −5.71 4.18 6.90 < +1.39 −2.63 12
HE 1410+0213 23 81.12 0.18 0.614 1 5000 2.0 −2.14 1.92 8.21 −0.26 −1.81 13
HE 1506–0113 29 −83.50 11.22 < 10−6 2 5016 2.0 −3.54 1.47 6.38 −0.80 −0.60 2
HE 2139–5432 4 102.18 10.07 < 10−6 2 5416 3.0 −4.02 2.59 7.01 < −0.33 −0.99 2
HE 2142–5656 4 103.70 0.80 0.718 4939 1.9 −2.87 0.95 6.61 −0.63 −0.72 2
HE 2202–4831 3 56.32 0.67 0.797 5331 3.0 −2.78 2.41 8.08 −1.28 −2.31 2
HE 2247–7400 2 5.78 0.59 0.602 4829 1.6 −2.87 0.70 6.58 −0.94 −0.69 2
HE 2318–1621 7 −41.77 0.28 0.218 1 4846 1.4 −3.67 1.04 6.30 −1.61 −1.34 14
SDSS J0140+2344b 8 −198.65 4.54 < 10−6 2 5703 4.7 −4.00 1.13 5.56 < +0.34 −0.81 2
SDSS J0929+0238 26 388.33 10.40 2 5894 4.5 −4.97 3.91a 7.44a < +1.46 −3.56a 15
SDSS J1313–0019 3 255.50 13.50 < 10−6 2? 5200 2.6 −5.00 2.98 6.41 < +0.22 −2.45 16
SDSS J1341+4741 5 −194.68 26.63 < 10−6 2 5450 2.5 −3.20 0.99a 6.22a −0.73 −0.28a 17
SDSS J1422+0031 6 −118.97 6.09 < 10−6 2 5200 2.2 −3.03 1.70 7.11 −1.18 −0.95 18
SDSS J1613+5309 4 0.01 0.89 0.745 5350 2.1 −3.33 2.09 7.21 +0.03 −1.18 18
SDSS J1746+2455 5 78.45 0.54 0.431 5350 2.6 −3.17 1.24 6.51 +0.26 −0.56 2
SDSS J2206–0925 3 14.83 0.90 0.626 5100 2.1 −3.17 0.64a 5.90a −0.85 +0.61a 18
Segue 1–7 4 204.86 0.59 0.580 4960 1.9 −3.52 2.30a 7.21a < −0.96 +0.94a 19
SMSS 0313–6708 34 298.50 0.35 0.592 1 5125 2.3 < −6.50 > 5.39 6.02 −1.20 20

Notes. Columns: star name; number of radial velocity measurements in Table B.2; weighted average of radial velocity measurements in Table B.2; standard deviation of radial velocity measurements in Table B.2; variability criterion P( χ2); binary status (1 = single, 2 = binary, labels as collected by Yoon et al. (2016) and updated in this work); effective temperature; surface gravity; iron abundance; carbon-to-iron ratio; absolute carbon abundance; barium-to-iron ratio, magnesium-to-carbon ratio; literature reference. (a)These carbon abundances have not been corrected for evolutionary status (all other measurements have been, as reported in Yoon et al. 2016). However, all of these stars have logg ≳2.0, where the correction is expected to be small. (b)Of the two provided solutions in the reference, these are the dwarf solutions.

References. (1) Ito et al. (2013), (2) Yong et al. (2013), (3) Jacobson et al. (2015), (4) Giridhar et al. (2001), (5) Roederer et al. (2014), (6) Placco et al. (2016b), (7) Plez & Cohen (2005), (8) Christlieb et al. (2004), (9) H16a, (10) Norris et al. (2007), (11) Barklem et al. (2005), (12) Frebel et al. (2008), (13) Cohen et al. (2013), (14) Placco et al. (2014), (15) Bonifacio et al. (2015) and for magnesium Caffau et al. (2011), (16) Frebel et al. (2015), (17) Bandyopadhyay et al. (2018), (18) Aoki et al. (2013), (19) Norris et al. (2010), (20) Bessell et al. (2015), and for magnesium Keller et al. (2014).

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