TOPoS - II. On the bimodality of carbon abundance in CEMP stars Implications on the early chemical evolution of galaxies

P. Bonifacio; E. Caffau; M. Spite; M. Limongi; A. Chieffi; R. S. Klessen; P. François; P. Molaro; H.-G. Ludwig; S. Zaggia; F. Spite; B. Plez; R. Cayrel; N. Christlieb; P. C. Clark; S. C. O. Glover; F. Hammer; A. Koch; L. Monaco; L. Sbordone; M. Steffen

doi:10.1051/0004-6361/201425266

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Volume 579 (July 2015)

A&A, 579 (2015) A28

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Table 7

Abundances of SDSS J1035+0641.

Atomic lines

Ion	λ	χ	log gf	EW	A(X)	A(X)	A(X)_err	A(X)⊙
	nm	eV		pm	log g = 4.0	log g = 4.4

Li i	6707.761^a	0.00	–0.009	<1.80	<1.1^b	<1.1^b		1.03
Mg i	518.3604	2.72	–0.239	<0.30	<2.47	<2.47		7.54
Ca ii	393.3663	0.00	0.105	syn	1.35	1.53	0.10	6.33
Fe i	382.0425	0.86	0.119	<0.57^c	<1.91	<1.91		7.52
Fe i	382.0425	0.86	0.119	<1.67^d	<2.45	<2.45		7.52
Sr ii	407.7709	0.00	0.167	<0.50	<–1.80	<–1.67		2.92
Ba ii	4554.029	0.00	0.170	<3.30	<–0.49	<–0.38		2.17

Molecular bands

element	molecule		band		A(X)	A(X)		A(X)⊙
					log = 4.0	log = 4.4

C	CH		G-band		6.90	6.70		8.50

Notes.

^(a)

We list the strongest line of the doublet.

^(b)

Derived from the EW and the fitting formula of Sbordone et al. (2010).

^(c)

1σ.

^(d)

3σ.

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