LTE or non-LTE, that is the question - The NLTE chemical evolution of strontium in extremely metal-poor stars

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Volume 551 (March 2013)

A&A, 551 (2013) A57

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Table 3

Stellar parameters and derived Sr abundances ± standard deviation for the selected sample of stars.

Star	π ± σ	T_eff	log g	log g_corr.	[Fe/H]_LTE	[Fe/H]_NLTE	ξ	[Sr/Fe]_LTE	[Sr/Fe]_NLTE	Comment
	[mas]	[K]					km s^-1

HD 3567	9.57 ± 1.38	6035	4.08	4.08	−1.33	−1.29	1.5	−0.03 ± 0.8^x	0.06 ± 0.8^x	[u,H]
HD 19445	25.85 ± 1.14	5982	4.38	4.38	−2.13	−2.10	1.4	0.13 ± 0.8^x	0.16 ± 0.8^x	[u,H]
HD 106038	9.16 ± 1.50	5950	4.33	4.33	−1.48	−1.45	1.1	0.42 ± 0.12	0.45 ± 0.21	[u,H]
HD 121004	16.73 ± 1.35	5711	4.46	4.46	−0.73	−0.71	0.7	0.18 ± 0.04	0.26 ± 0.17	[u,H]
HD 122196	9.77 ± 1.32	6048	3.89	3.89	−1.81	−1.75	1.2	0.24⁽¹⁾	0.19⁽¹⁾	[u,H]
HD 134169	16.80 ± 1.11	5930	3.98	3.98	–	−0.86	1.8	− 0.05 ± 0.14	− 0.06 ± 0.13	[f,s,BG]
HD 140283	17.16 ± 0.68	5777	3.70	3.70	−2.58	−2.38	1.5	− 0.15⁽¹⁾	− 0.37⁽¹⁾	[u,H,B]
HD 148816	24.34 ± 0.90	5880	4.07	4.07	–	−0.78	1.2	− 0.13 ± 0.18	− 0.13 ± 0.17	[f,s,BG]
HD 184448	19.16 ± 0.63	5765	4.16	4.16	–	−0.43	1.2	0.00 ± 0.21	− 0.01 ± 0.21	[f,s,BG]
G 64-12	0.57 ± 2.83	6464	4.30	4.30	−3.24	−3.12	1.5	0.00⁽¹⁾	0.17⁽¹⁾	[u,B]
G 64-37	2.88 ± 3.10	6494	3.82^*	4.23	−3.17	−3.00	1.4	0.08⁽¹⁾	0.17⁽¹⁾	[u,H]
HD 122563	4.22 ± 0.35	4665	1.65	1.65	−2.60	−2.50	1.8	− 0.23 ± 0.8^x	− 0.12 ± 0.8^x	[u,B]
HD 175305	6.18 ± 0.56	5100	2.70	2.70	−1.38	−1.34	1.2	− 0.12 ± 0.32	0.04 ± 0.1	[h,H]

BD-133442	–	6450	4.20	4.42	−2.56	−2.47	1.5	0.30⁽¹⁾	0.21⁽¹⁾	[u,H]
CS 30312-059	–	5021	1.90	2.41	−3.06	−2.89	1.5	0.50⁽¹⁾	0.31⁽¹⁾	[h,H]
CS 31082-001	–	4925	1.51	2.05	−2.81	−2.63	1.4	0.70⁽¹⁾	0.60⁽¹⁾	[h,H]
HD 74462	–	4590	1.84	1.98	−1.48	−1.43	1.1	− 0.25 ± 0.35	− 0.14 ± 0.03	[h,H]
HD 126238	–	4900	1.80	2.02	−1.92	−1.85	1.5	− 0.17 ± 0.24	0.01 ± 0.06	[u,H]
HD 126587	–	4950	1.90	2.36	−3.01	−2.86	1.65	0.23 ± 0.8^x	0.22 ± 0.8^x	[u,H]
HE 0315+0000	–	5050	2.05	2.47	−2.81	−2.67	1.7	0.39⁽¹⁾	0.23⁽¹⁾	[u,H]
HE 1219-0312	–	5100	2.05	2.58	−2.99	−2.81	1.65	0.29⁽¹⁾	0.12⁽¹⁾	[u,H]

Notes.Strontium abundances with superscript (1) are derived only from the 4077 Å Sr ii line. Parameters with subscript have been corrected for NLTE effects. Stars with an “s” have had their abundances derived in SIU.

^(*)

Value from ionisation equilibrium.

^{(B, BG, H)}

Temperature from Bergemann et al. (2012b, B), Bergemann & Gehren (2008, BG), and Hansen et al. (2012, H), respectively. (u,f,h) Observed spectra from: (u) UVES/VLT, (f) FOCES/Calar-Alto Gehren et al. (2004, 2006), (h) HIRES/Keck.

^(x)

Weighted average, which includes an upper limit that was given half weight. The large uncertainty is a reciprocal square root of the summed weights.

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