Abundances in bulge stars from high-resolution, near-IR spectra - I. The CNO elements observed during the science verification of CRIRES at VLT

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Volume 496 / No 3 (March IV 2009)

A&A, 496 3 (2009) 701-712

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Table 4:

Abundances for Arcturus and the three bulge giants relative to the Sun, where ${\rm [X/Fe]} = \{ {\rm \log\varepsilon(X)} - {\rm \log\varepsilon(Fe)\}_{star}} - \{ {\rm \log\varepsilon(X) } - {\rm \log\varepsilon(Fe)\}_\odot }$ .
Star	Ref. Star	[C/Fe]	[N/Fe]	[C+N/Fe]	[O/Fe]	[Ti/Fe]	[Si/Fe]	[S/Fe]	[Cr/Fe]	[Ni/Fe]	[Fe/H]
Arcturus	this work^a	0.15	0.37	0.20	0.60	0.16	0.30	0.24	0.00	0.03	-0.50
	Fulbright et al.^b	-	-	-	0.51	0.16	0.34	-	-	-	-0.50
Arp 4203	this work^a	-0.54	1.15	0.48	0.30	0.21	0.45	0.31	-0.14	0.12	-1.25
	Fulbright et al.^b	-	-	-	0.14	0.26	0.52	-	-	-	-1.25
Arp 4329	this work^a	-0.09	0.33	0.03	0.49	0.21	0.50	0.51	0.00	0.06	-0.90
	Fulbright et al.^b	-	-	-	0.40	0.18	0.49	-	-	-	-0.90
Arp 1322	this work^a	-0.25	0.53	0.05	0.18	0.08	0.20	0.38	0.18	0.00	-0.17^c
	Fulbright et al.^b	-	-	-	0.37	0.05	0.11	-	-	-	-0.23

^a We have used the following solar abundances: ${\rm\log\varepsilon(C)=8.41}$ , ${\rm\log\varepsilon(N)=7.80}$ , ${\rm\log\varepsilon(O)=8.66}$ , ${\rm\log\varepsilon(Fe)=7.50}$ , ${\rm\log\varepsilon(Ti)=5.02}$ , ${\rm\log\varepsilon(Si)=7.55}$ , ${\rm\log\varepsilon(S)=7.20}$ , ${\rm\log\varepsilon(Cr)= 5.67}$ , and ${\rm\log\varepsilon(Ni)=6.25}$ .
^b Fulbright et al. used the following solar abundances: ${\rm\log\varepsilon(O)=8.69}$ , ${\rm\log\varepsilon(Fe)=7.45}$ , ${\rm\log\varepsilon(Ti)=4.92}$ , and ${\rm\log\varepsilon(Si)=7.54}$ . For the sake of comparison we have scaled their values to the solar values we have used.
^c The [Fe/H] from this work is determined from Fe I lines in the CRIRES wavelength region, but not used as the metallicity in the models.

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