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Table 1

Sample of CEMP-no stars monitored for radial-velocity variation.

Stellar ID RA (J2000) Dec (J2000) V BV Ref [Fe/H] [C/Fe] [Ba/Fe] Ref

HE 0020−1741 00:22:44 17:24:28 12.89 0.94 a 4.11 +1.36 <0.67 1
CS 29527−015 * 00:29:11 19:10:07 14.26 0.40 d 3.55 +1.18 <+0.10 10
CS 22166−016 00:58:24 14:47:07 12.75 0.65 b 2.40 +1.02 0.37 4
HE 0219−1739 02:21:41 17:25:37 14.73 1.52 b 3.09 +1.90 <1.39 1
BD+44°493 02:26:50 +44:57:47 9.22 0.67 a 3.83 +1.35 0.60 2
HE 0405−0526 04:07:47 05:18:11 10.72 0.71 a 2.18 +0.92 0.22 1
HE 1012−1540 * 10:14:53 15:55:53 14.04 0.66 a 3.51 +2.22 +0.19 6
HE 1133−0555 11:36:12 +06:11:43 15.43 0.64 b 2.40 +2.20 0.58 1
HE 1150−0428 11:53:07 04:45:03 15.01 0.76 a 3.21 +2.28 0.44 6
HE 1201−1512 12:03:37 15:29:33 13.79 0.55 a 3.92 +1.60 <0.34 3
HE 1300+0157 13:02:56 +01:41:52 14.06 0.48 b 3.49 +1.31 0.74 6
BS 16929−005 13:03:30 +33:51:09 13.61 0.62 b 3.27 +0.99 0.41 3
HE 1300−0641 13:03:34 06:57:21 14.80 0.62 b 3.14 +1.29 0.77 8
HE 1302−0954 13:04:58 10:10:11 13.96 0.79 a 2.25 +1.17 <0.53 1
CS 22877−001 13:13:55 12:11:42 12.16 0.77 b 2.71 +1.00 0.49 5
HE 1327−2326 * 13:30:06 23:41:54 13.53 0.44 b 5.76 +4.26 <+1.46 3
HE 1410+0213 14:13:06 +01:59:21 13.05 1.14 b 2.14 +1.71 0.26 6
HE 1506−0113 15:09:14 01:24:57 14.44 0.64 a 3.54 +1.65 0.80 3
CS 22878−027 16:37:36 +10:22:08 14.41 0.44 c 2.52 +0.86 <0.75 3
CS 29498−043 21:03:52 29:42:50 13.63 1.12 b 3.75 +1.90 0.45 7
CS 29502−092 22:22:36 01:38:24 11.87 0.77 b 2.99 +0.96 1.20 3
HE 2318−1621 23:21:22 16:05:06 12.73 0.68 a 3.67 +1.04 1.61 9
CS 22949−037 23:26:30 02:39:58 14.36 0.79 b 3.93 +1.01 0.77 6
CS 22957−027 23:59:13 03:53:49 13.62 0.80 b 3.06 +2.13 0.96 6

Notes.

(*)

Stars not formally qualifying as CEMP-no stars according to the [Ba/Fe] criterion. However, see discussion of their light-element abundance signatures in Sect. 2.3.

Reference. Photometry: (a) Henden et al. (2015); (b) Beers et al. (2007); (c) Preston et al. (1991); (d) Norris et al. (1999).Abundances: (1) This work; (2) Ito et al. (2013); (3) Yong et al. (2013); (4) Giridhar et al. (2001); (5) Aoki et al. (2002a); (6) Cohen et al. (2013); (7) Aoki et al. (2002c); (8) Barklem et al. (2005); (9) Placco et al. (2014a); (10) Bonifacio et al. (2009) and M. Spite (priv. comm.).

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