On the nature of sn stars - I. A detailed abundance study

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Table 6

Sample of the line by line abundance table.

Lambda	Abund	log gf	Ref	χ ²	Int	AbAccept	Comment

14.01 Si II
3853.66	–4.50	–1.440	LA	0.002441	0.3534	Y
3856.02	–4.57	–0.490	LA	0.006904	0.2570	Y
3862.60	–4.60	–0.740	LA	0.004232	0.2811	Y
4075.45	–4.63	–1.400	SG	0.001527	0.8158	Y
4076.78	–4.59	–1.670	SG	0.000888	0.8748	Y
4128.05	–4.58	0.380	LA	0.004738	0.3695	Y
4130.89	–4.60	0.530	LA	0.002375	0.3549	Y
4673.28	–4.48	–0.710	KX	0.001259	0.9896	Y	Weak and blended with Fe I 4673.2
5041.02	–4.64	0.290	SG	0.001421	0.5269	Y

Si II Avg	–4.59	+/– 0.05 (9)

16.01 S II
4153.07	–4.71	0.620	WS	0.001254	0.8554	Y
4162.66	–4.68	0.780	WS	0.001783	0.8287	Y
4415.34	–2.97	–1.080	KP	0.006496	0.8903	N	No fit
4991.97	–4.60	–0.650	WS	0.000846	0.9455	Y
5014.04	–4.68	0.030	KX	0.002286	0.9011	Y
5032.43	–4.61	0.180	WS	0.000620	0.8455	Y
5212.62	–4.77	0.240	WS	0.001127	0.9439	Y
5320.72	–4.56	0.460	WS	0.001090	0.9052	Y

S II Avg	–4.66	+/– 0.07 (7)

20.01 Ca II
3933.66	–5.59	0.130	WM	0.019829	0.1294	Y	Intense line

Ca II Avg	–5.59	(1)

Notes. The chemical species are identified at the beginning of the line lists using the code “z.i” where z is the atomic number and i the ionization stage. For instance, 14.01 corresponds to Si II. The same code z.i is used to identify elements in the figures of this work.

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