Table A.4: Data for atomic lines of Fe. The spectral window employed for the line is from $\lambda +{\rm d}\lambda _{\rm blue}$ to $\lambda +{\rm d}\lambda _{\rm red}$ . Lines which are removed in carbon-enhanced stars are marked with asterisks in the wavelength column.
Species $\lambda$ $\chi$ $\log gf$ d $\lambda_{\rm blue}$ d $\lambda_{\rm red}$ Refs.

[Å] [eV] [mÅ] [mÅ]

Fe I *3856.372 0.052 -1.286 -200 400 OWLWB91

Fe I *3859.911 0.000 -0.710 -400 350 OWLWB91

Fe I 3865.523 1.011 -0.950 -250 250 OWLWB91

Fe I *3878.018 0.958 -0.896 -300 100 OWLWB91

Fe I 4005.242 1.557 -0.583 -150 150 OWLWB91

Fe I 4045.812 1.485 0.284 -100 150 OWLWB91

Fe I 4063.594 1.558 0.062 -100 300 OWLWB91

Fe I 4071.738 1.608 -0.008 -100 300 OWLWB91

Fe I 4114.445 2.831 -1.303 -250 250 OWLWB91

Fe I 4132.058 1.608 -0.675 -300 100 OWLWB91

Fe I 4143.868 1.557 -0.511 -200 300 OWLWB91

Fe I *4175.636 2.845 -0.827 -150 300 OWLWB91

Fe I *4187.039 2.449 -0.514 -150 200 OWLWB91

Fe I *4199.095 3.047 0.156 -200 300 OWLWB91

Fe I 4202.029 1.485 -0.689 -200 150 OWLWB91

Fe I 4222.213 2.449 -0.914 -300 200 OWLWB91

Fe I 4227.426 3.332 0.266 -150 150 OWLWB91

Fe I *4233.603 2.482 -0.579 -150 100 OWLWB91

Fe I *4250.120 2.469 -0.380 -100 300 OWLWB91

Fe I 4250.787 1.557 -0.713 -300 300 OWLWB91

Fe I 4260.474 2.400 0.077 -150 200 OWLWB91

Fe I *4271.154 2.449 -0.337 -300 100 OWLWB91

Fe I *4271.761 1.485 -0.173 -150 300 OWLWB91

Fe I 4282.403 2.176 -0.779 -250 150 OWLWB91

Fe I *4325.762 1.608 0.006 -250 100 OWLWB91

Fe I *4375.930 0.000 -3.031 -150 300 OWLWB91

Fe I *4383.545 1.485 0.208 -300 300 OWLWB91

Fe I *4404.750 1.557 -0.147 -250 200 OWLWB91

Fe I *4415.123 1.608 -0.621 -300 200 OWLWB91

Fe I *4430.614 2.223 -1.728 -250 250 OWLWB91

Fe I *4442.339 2.198 -1.228 -300 300 OWLWB91

Fe I 4443.194 2.858 -1.043 -100 250 OWLWB91

Fe I 4447.717 2.223 -1.339 -300 300 OWLWB91

Fe I 4489.739 0.121 -3.899 -300 200 OWLWB91

Fe I 4494.563 2.198 -1.143 -300 300 OWLWB91

Fe I 4528.614 2.176 -0.887 -100 300 OWLWB91

Fe I 4602.941 1.485 -2.208 -300 300 OWLWB91

Fe I *4736.773 3.211 -0.752 -200 200 OWLWB91

Fe I 4872.137 2.882 -0.567 -300 300 OWLWB91

Fe I 4890.755 2.876 -0.394 -350 350 OWLWB91

Fe I 4891.492 2.852 -0.112 -300 300 OWLWB91

Fe I 4918.994 2.845 -0.342 -350 350 OWLWB91

Fe I 4920.503 2.832 0.068 -400 100 OWLWB91

Fe I 4938.814 2.875 -1.077 -300 200 OWLWB91

Fe I 4939.687 0.859 -3.252 -250 300 OWLWB91

Fe II *4178.862 2.583 -2.443 -100 200 SSK04

Fe II 4233.172 2.583 -1.809 -150 200 SSK04

Fe II 4416.828 2.778 -2.540 -240 300 M83

Fe II 4508.289 2.856 -2.318 -300 300 BBKAP91

Fe II 4515.343 2.844 -2.362 -100 300 SSK04

Fe II 4520.224 2.807 -2.550 -200 300 M83

Fe II *4541.524 2.856 -2.990 -100 200 M83

Fe II *4555.893 2.828 -2.250 -150 100 SSK04

Fe II 4583.839 2.807 -1.740 -250 300 SSK04

Fe II 4923.927 2.891 -1.206 -400 400 SSK04

References: BBKAP91 = Biémont et al. (1991), M83 = Moity (1983),
OWLWB91 = O'Brian et al. 1991, SSK04 = Schnabel et al. (2004).

**Table A.4:** Data for atomic lines of Fe. The spectral window employed for the line is from $\lambda +{\rm d}\lambda _{\rm blue}$ to $\lambda +{\rm d}\lambda _{\rm red}$ . Lines which are removed in carbon-enhanced stars are marked with asterisks in the wavelength column.
Species	$\lambda$	$\chi$	$\log gf$	d $\lambda_{\rm blue}$	d $\lambda_{\rm red}$	Refs.
	[Å]	[eV]		[mÅ]	[mÅ]
Fe I	*3856.372	0.052	-1.286	-200	400	OWLWB91
Fe I	*3859.911	0.000	-0.710	-400	350	OWLWB91
Fe I	3865.523	1.011	-0.950	-250	250	OWLWB91
Fe I	*3878.018	0.958	-0.896	-300	100	OWLWB91
Fe I	4005.242	1.557	-0.583	-150	150	OWLWB91
Fe I	4045.812	1.485	0.284	-100	150	OWLWB91
Fe I	4063.594	1.558	0.062	-100	300	OWLWB91
Fe I	4071.738	1.608	-0.008	-100	300	OWLWB91
Fe I	4114.445	2.831	-1.303	-250	250	OWLWB91
Fe I	4132.058	1.608	-0.675	-300	100	OWLWB91
Fe I	4143.868	1.557	-0.511	-200	300	OWLWB91
Fe I	*4175.636	2.845	-0.827	-150	300	OWLWB91
Fe I	*4187.039	2.449	-0.514	-150	200	OWLWB91
Fe I	*4199.095	3.047	0.156	-200	300	OWLWB91
Fe I	4202.029	1.485	-0.689	-200	150	OWLWB91
Fe I	4222.213	2.449	-0.914	-300	200	OWLWB91
Fe I	4227.426	3.332	0.266	-150	150	OWLWB91
Fe I	*4233.603	2.482	-0.579	-150	100	OWLWB91
Fe I	*4250.120	2.469	-0.380	-100	300	OWLWB91
Fe I	4250.787	1.557	-0.713	-300	300	OWLWB91
Fe I	4260.474	2.400	0.077	-150	200	OWLWB91
Fe I	*4271.154	2.449	-0.337	-300	100	OWLWB91
Fe I	*4271.761	1.485	-0.173	-150	300	OWLWB91
Fe I	4282.403	2.176	-0.779	-250	150	OWLWB91
Fe I	*4325.762	1.608	0.006	-250	100	OWLWB91
Fe I	*4375.930	0.000	-3.031	-150	300	OWLWB91
Fe I	*4383.545	1.485	0.208	-300	300	OWLWB91
Fe I	*4404.750	1.557	-0.147	-250	200	OWLWB91
Fe I	*4415.123	1.608	-0.621	-300	200	OWLWB91
Fe I	*4430.614	2.223	-1.728	-250	250	OWLWB91
Fe I	*4442.339	2.198	-1.228	-300	300	OWLWB91
Fe I	4443.194	2.858	-1.043	-100	250	OWLWB91
Fe I	4447.717	2.223	-1.339	-300	300	OWLWB91
Fe I	4489.739	0.121	-3.899	-300	200	OWLWB91
Fe I	4494.563	2.198	-1.143	-300	300	OWLWB91
Fe I	4528.614	2.176	-0.887	-100	300	OWLWB91
Fe I	4602.941	1.485	-2.208	-300	300	OWLWB91
Fe I	*4736.773	3.211	-0.752	-200	200	OWLWB91
Fe I	4872.137	2.882	-0.567	-300	300	OWLWB91
Fe I	4890.755	2.876	-0.394	-350	350	OWLWB91
Fe I	4891.492	2.852	-0.112	-300	300	OWLWB91
Fe I	4918.994	2.845	-0.342	-350	350	OWLWB91
Fe I	4920.503	2.832	0.068	-400	100	OWLWB91
Fe I	4938.814	2.875	-1.077	-300	200	OWLWB91
Fe I	4939.687	0.859	-3.252	-250	300	OWLWB91
Fe II	*4178.862	2.583	-2.443	-100	200	SSK04
Fe II	4233.172	2.583	-1.809	-150	200	SSK04
Fe II	4416.828	2.778	-2.540	-240	300	M83
Fe II	4508.289	2.856	-2.318	-300	300	BBKAP91
Fe II	4515.343	2.844	-2.362	-100	300	SSK04
Fe II	4520.224	2.807	-2.550	-200	300	M83
Fe II	*4541.524	2.856	-2.990	-100	200	M83
Fe II	*4555.893	2.828	-2.250	-150	100	SSK04
Fe II	4583.839	2.807	-1.740	-250	300	SSK04
Fe II	4923.927	2.891	-1.206	-400	400	SSK04

Source LaTeX | All tables | In the text

	1 Introduction
	2 Observations and sample
	3 Automated spectrum analysis
	4 Results
	5 Discussion
	6 Conclusions
	References
	Online Material
	Appendix A: Line list
	Appendix B: Error estimates