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Erratum
This article is an erratum for: [this article]

Issue
A&A
Volume 500, Number 3, June IV 2009
Page(s) 1025 - 1025
Section Extragalactic astronomy
DOI https://doi.org/10.1051/0004-6361/200809366e
Published online 29 April 2009

Erratum

AGB stars as tracers of metallicity and mean age across M 33

M.-R. L. Cioni1,2 - M. Irwin3 - A. M. N. Ferguson1 - A. McConnachie4 - B. C. Conn5 - A. Huxor1,6 - R. Ibata7 - G. Lewis8 - N. Tanvir9


1 - SUPA, School of Physics, University of Edinburgh, IfA, Blackford Hill, Edinburgh EH9 3HJ, UK
2 - Centre for Astrophysics Research, University of Hertfordshire, Hatfield AL10 9AB, UK
3 - Institute of Astronomy, University of Cambridge, Madingley Road, Cambridge CB3 0HA, UK
4 - Deptartment of Physics & Astronomy, University of Victoria, PO Box 3055, STN CSC, Victoria, BC, V8W 3P6 Canada
5 - European Southern Observatory, Alonso de Cordova 3107, Vitacura, Santiago, Chile
6 - Department of Physics, University of Bristol, Tyndall Avenue, Bristol BS8 1TL, UK
7 - Observatoire de Strasbourg, 11 rue de l'Université, 67000 Strasbourg, France
8 - Institute of Astronomy, School of Physics, A29, University of Sydney, NSW 2006, Australia
9 - Department of Physics and Astronomy, University of Leicester, Leicester LE1 7RH, UK

A&A 487, 131-146 (2008), DOI: 10.1051/0004-6361:200809366

Key words: galaxies: individual: M 33 - stars: late-type - galaxies: stellar content - galaxy: abundances - galaxies: structure - errata, addenda


The surface distribution of the C/M ratio across M 33 is shown in Fig. 1, while Fig. 2 shows the map corresponding to twice a lower resolution. These figures substitute Figs. 10 and 11 in the published version of the paper that show, instead, the distribution of the M/C ratio across the galaxy. The new figures show more clearly that regions with higher C/M ratio and lower [Fe/H] abundance occupy the outer part of the galaxy and delineate a metal-poor ring.

 \begin{figure}
\resizebox{8.5cm}{!}{\includegraphics{09366efig1a.ps}}\par\resizebox{8.5cm}{!}{\includegraphics{09366efig1b.ps}}
\end{figure} Figure 1:

Distribution of the C/M ratio across M 33. C-rich and O-rich AGB stars above the tip of the RGB have been selected using slanted lines ( top) or vertical lines (bottom). Darker regions correspond to higher ratios. Contours are at: 0.2, 0.6, 1.2, 1.6, 2.0, and 2.4 in the top panel, and at 0.15, 0.35 and 0.55 in the bottom panel.

Open with DEXTER

 \begin{figure}
\resizebox{8.8cm}{!}{\includegraphics{09366efig2.ps}}
\end{figure} Figure 2:

The same as the bottom panel of Fig. 1 but using bins of  $2.4^{\prime }$. Contours are at: 0.28, 0.38, 0.48, and 0.68.

Open with DEXTER


All Figures

  \begin{figure}
\resizebox{8.5cm}{!}{\includegraphics{09366efig1a.ps}}\par\resizebox{8.5cm}{!}{\includegraphics{09366efig1b.ps}}
\end{figure} Figure 1:

Distribution of the C/M ratio across M 33. C-rich and O-rich AGB stars above the tip of the RGB have been selected using slanted lines ( top) or vertical lines (bottom). Darker regions correspond to higher ratios. Contours are at: 0.2, 0.6, 1.2, 1.6, 2.0, and 2.4 in the top panel, and at 0.15, 0.35 and 0.55 in the bottom panel.

Open with DEXTER
In the text

  \begin{figure}
\resizebox{8.8cm}{!}{\includegraphics{09366efig2.ps}}
\end{figure} Figure 2:

The same as the bottom panel of Fig. 1 but using bins of  $2.4^{\prime }$. Contours are at: 0.28, 0.38, 0.48, and 0.68.

Open with DEXTER
In the text


Copyright ESO 2009

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