Characterization of open cluster remnants

Pavani, Daniela Borges; Bica, E.

doi:10.1051/0004-6361:20066240

Cited by 40 publications

(44 citation statements)

References 44 publications

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“…These are marked as follows in the DAML02 catalog: 145 were discovered in the infrared but are visible in the DSS images, 50 are considered doubtful based on the DSS images inspection, 5 are non-existent NGC (RNGC, Sulentic 1973), 32 were not found in the DSS images inspection, 2 are cluster remnants (Pavani & Bica 2007), and 9 are possible clusters. In the sample of clusters with unpublished mean proper motions, 373 objects have estimations of distance and age, of which 23 are within 1 kpc from the Sun and 17 are younger than 12 Myr.…”

Section: Statistics and General Commentsmentioning

confidence: 99%

Proper motions of the optically visible open clusters based on the UCAC4 catalog

Dias

Monteiro

Caetano

et al. 2014

A&A

174

207

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We present a catalog of mean proper motions and membership probabilities of individual stars for optically visible open clusters, which have been determined using data from the UCAC4 catalog in a homogeneous way. The mean proper motion of the cluster and the membership probabilities of the stars in the region of each cluster were determined by applying the statistical method in a modified fashion. In this study, we applied a global optimization procedure to fit the observed distribution of proper motions with two overlapping normal bivariate frequency functions, which also take the individual proper motion errors into account. For 724 clusters, this is the first determination of proper motion, and for the whole sample, we present results with a much larger number of identified astrometric member stars. Furthermore, it was possible to estimate the mean radial velocity of 364 clusters (102 unpublished so far) with the stellar membership using published radial velocity catalogs. These results provide an increase of 30% and 19% in the sample of open clusters with a determined mean absolute proper motion and mean radial velocity, respectively.

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Section: Statistics and General Commentsmentioning

confidence: 99%

Proper motions of the optically visible open clusters based on the UCAC4 catalog

Dias

Monteiro

Caetano

et al. 2014

A&A

174

207

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“…Assigning a probability to a detected spatial overdensity of being a true stellar cluster rather than a random field stars overdensity, is particularly useful in the study of open cluster remnants (Pavani & Bica 2007), and, in general, for OCs poorly populated and not easily distinguishable from their surroundings. This probability can be evaluated with the kde.test statistical function provided by the ks package 9 (Duong 2007).…”

Section: Real Cluster Probabilitymentioning

confidence: 99%

ASteCA: Automated Stellar Cluster Analysis

Perren

Vazquez

Piatti

2015

A&A

112

121

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We present the Automated Stellar Cluster Analysis package (ASteCA), a suit of tools designed to fully automate the standard tests applied on stellar clusters to determine their basic parameters. The set of functions included in the code make use of positional and photometric data to obtain precise and objective values for a given cluster's center coordinates, radius, luminosity function and integrated color magnitude, as well as characterizing through a statistical estimator its probability of being a true physical cluster rather than a random overdensity of field stars. ASteCA incorporates a Bayesian field star decontamination algorithm capable of assigning membership probabilities using photometric data alone. An isochrone fitting process based on the generation of synthetic clusters from theoretical isochrones and selection of the best fit through a genetic algorithm is also present, which allows ASteCA to provide accurate estimates for a cluster's metallicity, age, extinction and distance values along with its uncertainties. To validate the code we applied it on a large set of over 400 synthetic The results show that ASteCA is able to recover cluster parameters with an acceptable precision even for those clusters affected by substantial field star contamination. ASteCA is written in Python and is made available as an open source code which can be downloaded ready to be used from its official site.

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“…These aggregates are results of the dynamical evolution of open clusters during their lifetimes within the tidal field of the Milky Way. Furthermore, it is rather difficult to distinguish them from moving groups and stellar associations (Pavani & Bica 2007).…”

Section: Introductionmentioning

confidence: 99%

BVRIphotometry of NGC 3231, NGC 7055, and NGC 7127

Paunzen

Hermansson²,

Holmstrom³

2012

A&A

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Context. Open clusters are often used as tracers for the formation and evolution of the Milky Way. But they can also be used to study distinct "local stellar populations" and all kind of stellar groups. All these studies crucially depend on their unambiguous detection and classification separating them from the fore-and background field population. Aims. Still more than one third of the catalogued galactic open clusters are unstudied to date. We have chosen three northern open cluster fields, namely NGC 3231, NGC 7055, and NGC 7127 which have been never studied before to shed more light on their true nature.Methods. We present Johnson-Cousins BVRI photometry down to V ≈ 19 mag. After the transformation to the standard systems, colour-magnitude diagrams were generated. These diagrams were used to fit solar abundant isochrones to determine the distance modulus, reddening and apparent age of the main sequences. Results. As reported before, a significant plate-dependent distortion of the UCAC3 compared to the PPMXL within all three star fields was found. No correlation of this distortion with the apparent magnitude of the objects was detected. From the analysis of the colour-magnitude diagrams and the available proper motions we conclude that NGC 7055 and NGC 7127 are young, real, open clusters with ages of about 10 and 100 Myr, respectively. They are located in a distance of about 3300 as well as 5700 pc from the Sun. NGC 3231, on the other hand, is probably a high galactic latitude open cluster remnant.

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Characterization of open cluster remnants

Cited by 40 publications

References 44 publications

Proper motions of the optically visible open clusters based on the UCAC4 catalog

Proper motions of the optically visible open clusters based on the UCAC4 catalog

ASteCA: Automated Stellar Cluster Analysis

BVRIphotometry of NGC 3231, NGC 7055, and NGC 7127

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