Rubidium, zirconium, and lithium production in intermediate-mass asymptotic giant branch stars

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Volume 540 (April 2012)

A&A, 540 (2012) A44

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Table 1

Ranges of the observed Rb and Zr abundances in AGB stars in the Galaxy and in the Magellanic Clouds.

	Putative low-mass AGB stars		Putative intermediate-mass AGB stars
	Galaxy	Magellanic Clouds^a	Galaxy	Magellanic Clouds

[Rb/Fe^b]	−0.3– + 0.9	(−1.2– + 0.4)	+0.4– + 2.5	+1.7– + 5.0
[Zr^c/Fe^b]	−0.3– + 1.4	(−0.3– + 0.70)	0^d	0^d
[Rb/Zr]	<0	(<0)	>0	>0
[Fe^b/H]	−1.3– + 0.1	(−0.70– − 0.37^e)	set to 0^e	set to −0.3^e and −0.7^e

	Lambert et al. (1995)	Plez et al. (1993)	García-Hernández et al. (2006)	García-Hernández et al. (2009)
	Abia et al. (2001)	García-Hernández et al. (2009)	García-Hernández et al. (2007)

Notes.

^(a)

As discussed in the text, these stars have high Li abundances and may represent a link between low-mass and intermediate-mass AGB stars in the Magellanic Clouds.

^(b)

In some of the reported studies the average of Fe and Ni, M, is used instead of Fe.

^(c)

In Lambert et al. (1995) [s/M] is reported as the average of several s-process elements. We use this value as an indicator of the [Zr/Fe] ratio for stars from this study.

^(d)

The observational uncertainties allow for an upper limit of +0.5 and of +0.3 for Galactic and Magellanic Clouds intermediate-mass AGB stars, respectively.

^(e)

In the studies by Garcia-Hernandez et al., the metallicity of each star is not reported and the Rb and Zr abundances are derived using model atmospheres for the average abundances [M/H] set to 0, −0.3, and −0.7 in the Galaxy, Large and Small Magellanic Clouds, respectively.

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