2010
DOI: 10.1051/0004-6361/200913741
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A revisit to the region of Collinder 132 using Carte du Ciel and Astrographic Catalogue plates

Abstract: Aims. Based on stellar positions and proper motions, we aim to re-analyse the region of the controversial open cluster Collinder 132. Methods. We have developed a model which analyses the proper motion distribution and the stellar density to find moving groups. The astrometric data were obtained from four Carte du Ciel (CdC) and one Astrogaphic Catalogue (AC) plates of the Córdoba Astronomical Observatory collection (Argentina). Results.We detected an open cluster from the field stars and calculated the mean p… Show more

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Cited by 6 publications
(9 citation statements)
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“…This means that if Φ a represents the spatial function distribution of all stars in the region belonging to the association and Φ f represents the spatial distribution of all non-member stars present in the same region (see Sect. 4.1 of Orellana et al 2010), then…”
Section: Cen Ob1mentioning
confidence: 95%
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“…This means that if Φ a represents the spatial function distribution of all stars in the region belonging to the association and Φ f represents the spatial distribution of all non-member stars present in the same region (see Sect. 4.1 of Orellana et al 2010), then…”
Section: Cen Ob1mentioning
confidence: 95%
“…Firstly, the technique of Orellana et al (2010) was applied to the Hipparcos Catalogue, i.e. down to a visual (V) magnitude ranging from 7.3 to 9.0 (depending on spectral type), on a circular area of radius 7…”
Section: Cen Ob1mentioning
confidence: 99%
See 1 more Smart Citation
“…Therefore, a selection based on proper motion is the most reliable method for the separation of the association from field stars. We analysed this over-density using the model proposed by Orellana et al (2010). In their paper they proposed for the first time, a standardised way to identify the members of an association.…”
Section: Cen Ob1mentioning
confidence: 99%
“…Figure 4b shows the 86 association members. Further adjustment was made by applying the Orellana et al (2010) model by eliminating from the initial group of 299 stars the 213 that are not distance members. The new parameters are N 3 = 52, μ xa = −4.78 ± 0.10 mas yr −1 , μ ya = −0.93 ± 0.10 mas yr −1 , σ a = 1.05 ± 0.14 mas yr −1 , and for the field stars N 4 = 609, μ a xf = −5.58 ± 0.62 mas yr −1 , μ a yf = −2.02 ± 0.43 mas yr −1 , σ a xf = 6.59 ± 0.27 mas yr −1 and σ a yf = 7.57 ± 0.31 mas yr −1 .…”
Section: Cen Ob1mentioning
confidence: 99%