| Issue |
A&A
Volume 567, July 2014
|
|
|---|---|---|
| Article Number | C1 | |
| Number of page(s) | 1 | |
| Section | Cosmology (including clusters of galaxies) | |
| DOI | https://doi.org/10.1051/0004-6361/201321929e | |
| Published online | 17 July 2014 | |
The galaxy population of the complex cluster system Abell 3921 (Corrigendum)
1
Institute for Astro- and Particle Physics, University of
Innsbruck, Technikerstr.
25/8, 6020
Innsbruck, Austria
e-mail: florian.pranger@uibk.ac.at
2
Laboratoire Lagrange, UMR7293, Université de Nice Sophia
Antipolis, CNRS, Observatoire de la Côte d’Azur, 06300
Nice,
France
3
Dipartimento di Fisica, Università degli Studi di
Torino, via P. Giuria
1, 10125
Torino, Italy ;
Istituto Nazionale di Fisica Nucleare (INFN), Sezione di
Torino, via P. Giuria
1, 10125
Torino,
Italy
4
School of Physics, University of Sydney, NSW,
2006
Sydney,
Australia
5
Leiden Observatory, Leiden University,
2300 RA
Leiden, The
Netherlands
Key words: galaxies: clusters: general / galaxies: clusters: individual: Abell 3921 / galaxies: distances and redshifts / galaxies: evolution / cosmology: observations / errata, addenda
This is an erratum to the paper entitled “The galaxy population of the complex cluster system Abell 3921” published in A&A. An error was made in computing SFRs following Kennicutt (1992). We used R-band instead of B-band luminosities, which led to an underestimation of SFRs by a factor of ~2−3. Formula (1) in the original paper should read ![\begin{equation} {\it SFR}(M_{\odot}\,{\rm yr}^{-1})\simeq 2.7 \times 10^{-12} \frac{L_{B}}{L_{B}(\odot)} EW([{\rm OII}]) E({\rm H}\alpha). \label{eq:sfr} \end{equation}](/articles/aa/full_html/2014/07/aa21929e-13/aa21929e-13-eq46.png)
(1)Since we do not have B-band imaging for the galaxies in the area of Abell 3921, the B-band luminosities used for the corrected SFR values shown in Fig. 1 and Table 1 were calculated after transforming apparent R-band to apparent B-band magnitudes. For this transformation we used synthetic photometry based on the SED classification described in the original paper. We tested this approach with a sample of galaxies at similar redshifts, for which both B- and R-band imaging is available, and find that systematic errors are negligible (<0.1 M⊙/yr).
All results and conclusions in the original paper remain unchanged.
 |
Fig. 1 Median star formation rate (corrected) for objects with detectable [OII] emission line (compare to Fig. 10 in the original paper). The thin error bars represent the standard deviation within each data bin. The corresponding data for the subsamples of components A and B are listed in Table 1. |
Median star formation rates (corrected) in subclusters A and B (compare to Table 3 in the original paper).
References
- Kennicutt, Jr., R. C. 1992, ApJ, 388, 310 [NASA ADS] [CrossRef] [Google Scholar]
© ESO, 2014
All Tables
Median star formation rates (corrected) in subclusters A and B (compare to Table 3 in the original paper).
All Figures
|
Fig. 1 Median star formation rate (corrected) for objects with detectable [OII] emission line (compare to Fig. 10 in the original paper). The thin error bars represent the standard deviation within each data bin. The corresponding data for the subsamples of components A and B are listed in Table 1. |
| In the text | |
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