Gas phase atomic metals in the circumstellar envelope of IRC+10216

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Table 1:

Metal lines in the envelope of IRC+10216.
Species	$\lambda_\circ$	f-value	$W_{\lambda}$ ^a	N
	(Å)		(mÅ)	(cm^-2)
Na I	5895.924	0.3180	625	4.6(14)^b
	5889.951	0.6311	625
	3302.368	0.0090	230
Al I	3944.006	0.1134	<44	<2.8(12)
K I	7698.974	0.3393	530	4.6(12)^c
	7664.911	0.6816	635
	4044.143	0.0061	<29
Ca I	4226.728	1.7530	300	1.9(12)
Ca II	3968.468	0.3145	255	7.0(12)
	3933.663	0.6346	390
Ti I	3635.462	0.2229	<49	<1.9(12)
Ti II	3383.768	0.3401	<69	<2.0(12)
Cr I	4289.716	0.0622	37:	1.4(12)^d
	4274.796	0.0839	49:
	4254.332	0.1099	38:
	3605.322	0.2248	27:
	3593.482	0.2897	62:
	3578.683	0.3663	<62
Mn I	4034.483	0.0257	<33	<3.1(12)
	4033.062	0.0402	<33
	4030.753	0.0565	<33
Fe I	3859.911	0.0217	225	8.8(13)^e
	3824.444	0.0048	80
	3719.934	0.0412	197
	3440.606	0.0236	170
Sr II	4077.709	0.7010	<28	<2.7(11)

Notes. ^(a) Upper limits are 3 $\sigma$ . ^(b) D-lines are saturated, N based on the 3302 Å line. ^(c) Based on the 7699, 7665 Å doublet. ^(d) Indicates 2-3 $\sigma$ features; N based on weighted mean. ^(e) Based on the 3860, 3720 Å lines which have better S/N.

Source LaTeX | All tables | In the text

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