Two distinct halo populations in the solar neighborhood - Evidence from stellar abundance ratios and kinematics

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Volume 511 (February 2010)

A&A, 511 (2010) L10

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Issue		A&A Volume 511, February 2010


Article Number		L10
Number of page(s)		9
Section		Letters
DOI		https://doi.org/10.1051/0004-6361/200913877
Published online		16 March 2010

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$\begin{figure} \par\resizebox{8.8cm}{!}{\includegraphics{13877fig5.eps}} \end{figure}$	Figure 5: [Si/Fe], [Ca/Fe], and [Ti/Fe] as a function of [Fe/H]. The same symbols as in Fig. 1 are used.
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$\begin{figure} \par\resizebox{8.8cm}{!}{\includegraphics{13877fig6.eps}} \end{figure}$	Figure 6: [Na/Fe], [Cr/Fe], and [Ni/Fe] as a function of [Fe/H]. The same symbols as in Fig. 1 are used.
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$\begin{figure} \par\resizebox{8.8cm}{!}{\includegraphics{13877fig7.eps}} \end{figure}$

Figure 7:

UVES spectra of two stars with nearly the same atmospheric parameters $T_{\rm eff}$ , log g, and [Fe/H]. The spectrum of the low- $\alpha$ star HD 22879 ( $T_{\rm eff}$ = 5597 K, log g = 4.55, [Fe/H] = -0.91, [ $\alpha$ /Fe] = 0.12) is shown with a red line and that of the high- $\alpha$ star HD 22879 ( $T_{\rm eff}$ = 5624 K, log g = 4.37, [Fe/H] = -0.93, [ $\alpha$ /Fe] = 0.31) with a green line. The Fe lines have the same strength in the two spectra, but the Na, Mg, Si, and Ni lines are significantly weaker in the spectrum of the low- $\alpha$ star.

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$\begin{figure} \par\resizebox{8.8cm}{!}{\includegraphics{13877fig8.eps}} \end{figure}$	Figure 8: $W_{\rm LSR}$ versus $U_{\rm LSR}$ for stars with $\mbox{\rm [Fe/H]}> -1.4$ . The same symbols as in Fig. 3 are used.
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Table 1: UVES spectra acquired from the ESO/ST-ECF Science Archive.

Table 2: Stars observed with the NOT/FIES spectrograph.

Table 3: Atmospheric parameters, abundance ratios, and space velocities for stars with VLT/UVES spectra.

Table 4: Atmospheric parameters, abundance ratios, and space velocities for stars with NOT/FIES spectra.

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