| Issue |
A&A
Volume 556, August 2013
|
|
|---|---|---|
| Article Number | C4 | |
| Number of page(s) | 2 | |
| Section | Extragalactic astronomy | |
| DOI | https://doi.org/10.1051/0004-6361/201321268e | |
| Published online | 08 August 2013 | |
Morphology with light profile fitting of confirmed cluster galaxies at z = 0.84 (Corrigendum)
1
Departamento de AstronomíaUniversidad de Concepción,
Casilla 160-C
Concepcion,
Chile
e-mail: jnantais@astro-udec.cl
2
GEPI, Paris Observatory, CNRS, University of
Paris-Diderot, 5 place Jules
Janssen, 92195
Meudon,
France
3
Australian Astronomical Observatory, PO Box 296, Epping
NSW
1710,
Australia
4
ESO, Karl-Schwarzchild Strasse 2, 85748
Garching,
Germany
5
Department of Physics, University of California,
Davis, One Shields Avenue,
Davis, CA
95616,
USA
Key words: galaxies: clusters: general / galaxies: clusters: individual: RX J0152.7-1357 / galaxies: evolution / errata, addenda
In Nantais et al. (2013), Galaxy 682 of RXJ0152.7-1357 was incorrectly assigned to the high-density regions rather than the low-density regions of the cluster. This galaxy is classified as peculiar, of the subtype resembling a lenticular galaxy but not meeting our lenticular criteria for Sérsic index and/or bulge-to-total ratio. Reassigning this galaxy to the low-density regions makes a few minor changes in the counts of early-type and peculiar/compact/merging fractions. The correct values are reflected in the figures and tables below. The new results do not affect the major qualitative results of the paper, but they may be of interest to readers comparing the results of the paper to other similar studies.
Galaxy type fractions by morphology (corrected Table 2).
The correct fraction of galaxies in the low-density regions with E/S0 morphologies is now 27%, or 17 out of 63 galaxies. The peculiar, compact, and merger fraction in the low-density regions is 54% (34 out of 63 galaxies). In the high-density regions, the adjusted E/S0 fraction in the high-density regions is 83% (19 out of 23 galaxies), and the adjusted peculiar/compact/merger fraction in the high-density regions is 17% (4 out of 23 galaxies). Since Galaxy 682 is of low stellar mass, it is also now excluded from the low-mass/high-density atypical sample in Sect. 4.2 of the paper. There are now 24 low-mass galaxies in the high- and intermediate- density regions, 50% of which are E/S0 and 38% of which are peculiar, compact, or merging.
 |
Fig. 1 Corrected version of Fig. 7: galaxy type fraction vs. environmental density region (HDMD = high dark-matter density, IDMD = intermediate dark-matter density, LDMD = low dark-matter density) for J0152.7 cluster galaxies. Error bars in galaxy type fractions are from Poisson counting statistics. |
 |
Fig. 2 Corrected version of Fig. 11: galaxy type fraction vs. logarithm of mean sample mass for two samples of J0152.7 cluster galaxies that are atypical in the light of the correlation of galaxy mass with environment. Low-mass galaxies in regions of high to intermediate density are shown on the left, and high-mass galaxies in the low-density outskirts are shown on the right. Error bars in galaxy type fractions are from Poisson counting statistics. |
References
- Nantais, J. B., Flores, H., Demarco, R., et al. 2013, A&A, 555, A5 [NASA ADS] [CrossRef] [EDP Sciences] [Google Scholar]
© ESO, 2013
All Tables
All Figures
|
Fig. 1 Corrected version of Fig. 7: galaxy type fraction vs. environmental density region (HDMD = high dark-matter density, IDMD = intermediate dark-matter density, LDMD = low dark-matter density) for J0152.7 cluster galaxies. Error bars in galaxy type fractions are from Poisson counting statistics. |
| In the text | |
|
Fig. 2 Corrected version of Fig. 11: galaxy type fraction vs. logarithm of mean sample mass for two samples of J0152.7 cluster galaxies that are atypical in the light of the correlation of galaxy mass with environment. Low-mass galaxies in regions of high to intermediate density are shown on the left, and high-mass galaxies in the low-density outskirts are shown on the right. Error bars in galaxy type fractions are from Poisson counting statistics. |
| In the text | |
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