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.
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 |
Figure 2: The same as the bottom panel of Fig. 1 but using bins of . Contours are at: 0.28, 0.38, 0.48, and 0.68. |
|
Open with DEXTER |
All Figures
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 |
Figure 2: The same as the bottom panel of Fig. 1 but using bins of . 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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