Oxygen lines in solar granulation - II. Centre-to-limb variation, NLTE line formation, blends, and the solar oxygen abundance

T. M. D. Pereira; M. Asplund; D. Kiselman

doi:10.1051/0004-6361/200912840

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Volume 508 / No 3 (December IV 2009)

A&A, 508 3 (2009) 1403-1416

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Table 2:

Lines studied in the present work and their parameters.
Atomic species	$\lambda$ [nm]	$\log gf$	$E_{{\rm low}}$ [eV]	$W_{\mu=1}$ [pm]^a
Fe I	615.1618^d	-3.299^c	2.18^c	4.95
Si I	615.5693^b	-2.252^b	5.62^b	0.61
Ca I	615.6023^b	-2.497^b	2.52^b	0.92
Fe I	615.7728^d	-1.260^b	4.08^c	6.45
O I	615.8186^c	-1.841^c	10.74^c	0.63
Fe I	615.9378^d	-1.970^b	4.61^b	1.21
Fe I	629.0965^b	-0.774^b	4.73^b	7.06
Fe I	629.7792^c	-2.740^c	2.22^c	7.54
[O I]	630.0304^c	-9.717^e	0.00^c	0.45
Sc II	630.0698^b	-1.887^b	1.51^b	0.59
O I	777.1944^c	0.369^c	9.15^c	8.48
O I	777.4166^c	0.223^c	9.15^c	7.44
O I	777.5390^c	0.002^c	9.15^c	5.90
Fe I	778.0557^b	0.029^b	4.47^b	14.81

^a Equivalent widths at disk-centre measured from our observations. ^b VALD database (Kupka et al. 2000; Piskunov et al. 1995). ^c NIST database (Ralchenko et al. 2009). ^d Nave et al. (1994). ^e Storey & Zeippen (2000).

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