Chemical evolution of the Galactic bulge as traced by microlensed dwarf and subgiant stars - Detailed abundance analysis of OGLE-2008-BLG-209S

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Volume 499 / No 3 (June I 2009)

A&A, 499 3 (2009) 737-753

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Table 2:

Equivalent widths and elemental abundances based on method 1^a.
					Sun			OGLE-2008-BLG-209S			OGLE-2006-BLG-265S			MOA-2006-BLG-099S			OGLE-2007-BLG-349S
element		wavelength	$\log gf$	$\chi_{\rm l}$	$W_{\rm\lambda,\odot}$	$\log \epsilon (X)_{\odot}$	flag	$W_{\rm\lambda}$	$\log \epsilon (X)$	[X/H]	$W_{\rm\lambda}$	$\log \epsilon (X)$	[X/H]	$W_{\rm\lambda}$	$\log \epsilon (X)$	[X/H]	$W_{\rm\lambda}$	$\log \epsilon (X)$	[X/H]
Al	1	5557.063	-2.21	3.14	10.4	6.44	-	17.1	6.45	0.01	39.9	7.04	0.60	29.4	7.00	0.56	37.9	6.89	0.45
Al	1	6696.023	-1.62	3.14	44.9	6.62	-	47.9	6.45	-0.17	87.8	7.09	0.47	58.8	6.84	0.23	89.5	7.03	0.41

^a For each line we give the $\log gf$ value, lower excitation potential ( $\chi_{\rm l}$ ), measured equivalent widths ( $W_{\rm\lambda}$ ), derived absolute abundance ( $\log \epsilon (X)$ ), abundance normalised to the Sun (on a line-by-line basis) ([X/H]). The ``flag'' for the Sun indicates that a line has not been measured in the solar spectrum and that the abundance given (and used in the normalisation) for that line is the average abundance based on all the other lines, that could be measured in the solar spectrum, of the same species. The full table is only available in electronic form at the CDS.

Source LaTeX | All tables | In the text

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