EDP Sciences
Open Access
Erratum
This article is an erratum for: [this article]

Issue
A&A
Volume 623, March 2019
Article Number C2
Number of page(s) 2
Section Galactic structure, stellar clusters and populations
DOI https://doi.org/10.1051/0004-6361/201834020e
Published online 19 March 2019

Due to an unfortunate error in the computation of distance between clusters, Tables 4 and 5, and Fig. 12 in Sect. 3.3 of the original paper contain incorrect values. Here we present the updated tables and figure.

Table 4 gives the list of cluster pairs that differ by less than 100 pc in distance and 5 km s−1 in velocity in our high-quality sample. The closest pair includes ASCC 16 and ASCC 21, which are separated by ∼13 pc, with a velocity difference of 4.5 km s−1. RSG 7 and RSG 8, as well as ASCC 16 and ASCC 19, are also close pairs separated by ∼24 pc, with velocity differences of 2.3 km s−1 and 3.6 km s−1 respectively, thus good candidates to be physically related. Several possibly larger complexes may be found in that table, formed by clusters that appear more than one time. Table 5 gives a list of candidates binaries from the literature. The most famous binary cluster formed by h and χ Persei (NGC 869 and NGC 884, Messow & Schorr 1913) appears to have a separation of 19.5 pc. An excellent candidate binary is the pair Collinder 394 and NGC 6716, which lie at a distance of ∼11 pc from each other. IC 2602 and Platais 8 are also close from each other (∼35 pc) and they are possibly physically related, owing to their common age in DAML and similar velocity (also reported in Table 4). The other pairs in Table 5 have much larger separation and they are more likely to result from a chance alignment than that they are a physical binary system.

Table 4.

Pairs of OCs differing by less than 100 pc in their Galactic position and 5 km s−1 in velocity in the high-quality sample.

Table 5.

Separation in space and velocity of binary candidates from the literature, computed from our mean parameters for 861 OCs.

thumbnail Fig. 12.

Histogram of the distance between nearest neighbours in the high-quality sample (upper panel) and the same in velocity (lower panel).

Open with DEXTER

References


© C. Soubiran et al. 2019

Licence Creative Commons
Open Access article, published by EDP Sciences, under the terms of the Creative Commons Attribution License (http://creativecommons.org/licenses/by/4.0), which permits unrestricted use, distribution, and reproduction in any medium, provided the original work is properly cited.

All Tables

Table 4.

Pairs of OCs differing by less than 100 pc in their Galactic position and 5 km s−1 in velocity in the high-quality sample.

Table 5.

Separation in space and velocity of binary candidates from the literature, computed from our mean parameters for 861 OCs.

All Figures

thumbnail Fig. 12.

Histogram of the distance between nearest neighbours in the high-quality sample (upper panel) and the same in velocity (lower panel).

Open with DEXTER
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