Global survey of star clusters in the Milky Way II. The catalogue of basic parameters

By N. Kharchenko, A. Piskunov, E. Schilbach, S. Röser, R. Scholz. 2013

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Context. Although they are the main constituents of the Galactic disk population, for half of the open clusters in the Milky Way reported in the literature nothing is known except the raw position and an approximate size. Aims. The main goal of this study is to determine a full set of uniform spatial, structural, kinematic, and astrophysical param eters for as many known open clusters as possible. Methods. On the basis of stellar data from PPMXL and 2MASS, we used a dedicated data-processing pipeline to determine kinematic and photometric membership probabilities for stars in a cluster region. Results. For an input list of 3784 targets from the literature, we confi rm that 3006 are real objects, the vast majority of them are open clusters, but associations and globular clusters are also p resent. For each confirmed object we determined the exact pos ition of the cluster centre, the apparent size, proper motion, distance , colour excess, and age. For about 1500 clusters, these basic astrophysical parameters have been determined for the first time. For the bu lk of the clusters we also derived the tidal radius. We estimated additionally average radial velocities for more than 30% of the confirmed clusters. The present sample (called MWSC) reaches both the central parts of the Milky Way and its outer regions. It is almost complete up to 1.8 kpc from the Sun and also covers neighbouring spiral arms. However, for a small subset of the oldest open clusters (log t & 9) we found some evidence of incompleteness within about 1 kpc from the Sun.

Subfields: Astronomy and Astrophysics

View Paper: https://www.semanticscholar.org/paper/17e726af7ca915fedfa9046ff0676710b20eb6e2

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Citations in the corpus

Proper motions and dynamics of the Milky Way globular cluster system fromGaiaDR2 (2018, result): “…Chemel et al. (2018) still demonstrate a rather good correlation with the Gaia measurements (2nd and 3rd columns in Figure 2), however, the one from Kharchenko et al. (2013) bears almost no resemblance to the space-based measurements, with differences exceeding MNRAS 000, 000–000 (0000) 5 mas/yr…”
BANYAN. XI. The BANYAN Σ Multivariate Bayesian Algorithm to Identify Members of Young Associations with 150 pc (2018, background): “…U > 0 km s−1 THA Z > −20 pc U < 12.5 km s−1 −4 km s−1 < W < 2 km s−1 THOR U < −25 km s−1 USCO U > 10 km s−1 The χ1 For association (XFOR; also called Alessi 13) was identified by Dias et al. (2002), and Kharchenko et al. (2013) estimated an age of ∼ 525 Myr based on the main-sequence turnoff.”
On the metallicity of open clusters. III. Homogenised sample (2015, methodology): “Furthermore, we included two global parameter studies (Bukowiecki et al. 2011; Kharchenko et al. 2013), both using 2MASS photometry (Skrutskie et al. 2006) and isochrone fitting.”
The Search for Spatial Extension in High-latitude Sources Detected by the Fermi Large Area Telescope (2018, background): “5+3525 is located near NGC1579, an SFR at a distance of 700pc(Kharchenko et al. 2013).”
A New Distortion Solution for NIRC2 on the Keck II Telescope (2016, background): “The predicted velocity dispersion is 0.066 mas/yr in the plane of the sky given the measured lineof-sight velocity dispersion (5.6 km s−1; Kimmig et al. 2015) and distance of 17.8 kpc (Kharchenko et al. 2013).”
Clusters and mirages: cataloguing stellar aggregates in the Milky Way (2019, methodology): “Kos et al. (2018), using Gaia DR2 data supplemented with radial velocities from high-resolution spectroscopy, remark that not a single pair of stars among the proposed members of Carraro (2002) and Kharchenko et al. (2013) have matching parameters.”
A self-consistent, absolute isochronal age scale for young moving groups in the solar neighbourhood (2015, unknown): “Kharchenko et al. (2013) recovered the cluster and estimated it to to be at 95 pc, with mean proper motion µα, µδ ' +10.0,−32.2 mas yr−1 (±0.8 mas yr−1), a core radius of ∼ 1.6 pc, and an isochronal age of 32 Myr.”
Milky Way Satellite Census. I. The Observational Selection Function for Milky Way Satellites in DES Y3 and Pan-STARRS DR1 (2019, background): “…bright stars (Hoffleit & Jaschek 1991), Milky Way globular clusters (Harris 1996, 2010 edition), open clusters (WEBDA)9, and nearby galaxies that are resolved into 9 https://webda.physics.muni.cz individual stars (Corwin 2004; Nilson 1973; Webbink 1985; Kharchenko et al. 2013; Bica et al. 2008).”
A Gaia DR2 view of the open cluster population in the Milky Way (2018, background): “Although claims have been made that the sample of known OCs might be complete out to distances of 1.8 kpc (Kharchenko et al. 2013; Joshi et al. 2016; Yen et al. 2018), it is likely that there are still some objects to be found in the solar neighbourhood, in particular old OCs, as pointed out by…”
EIGHT ULTRA-FAINT GALAXY CANDIDATES DISCOVERED IN YEAR TWO OF THE DARK ENERGY SURVEY (2015, methodology): “The resulting list of seeds was matched against catalogs of known Local Group galaxies (McConnachie 2012) and star clusters (Harris 1996, 2010 edition; Kharchenko et al. 2013).”
THE RADIAL VELOCITY EXPERIMENT (RAVE): FIFTH DATA RELEASE (2013, methodology): “The open cluster properties come from the Milky Way global survey of star clusters (Kharchenko et al. 2013) and the globular cluster properties come from the Harris catalog (Harris 1996, 2010 update).”
EIGHT NEW MILKY WAY COMPANIONS DISCOVERED IN FIRST-YEAR DARK ENERGY SURVEY DATA (2015, methodology): “The resulting seed list was compared against catalogs of known star clusters (Harris 1996, 2010 edition; Kharchenko et al. 2013) and Milky Way satellite galaxies (McConnachie 2012a) as well as catalogs of other astrophysical objects that can produce false positives, such as large nearby galaxies…”
A Catalog of Newly Identified Star Clusters in Gaia DR2 (2019, background): “B19 made use of infrared photometry, and discovered several hundreds of new OC candidates in addition to those found by Kharchenko et al. (2013).”
Untangling the Galaxy. I. Local Structure and Star Formation History of the Milky Way (2019, methodology): “The CNN was trained on the cluster populations from Cantat-Gaudin et al. (2018), with the age and extinction labels from Kharchenko et al. (2013), with the combination of the Gaia, 2MASS, and WISE photometry which were obtained from the cross match tables (Marrese et al. 2019).”
Painting a portrait of the Galactic disc with its stellar clusters (2020, methodology): “Another widely-cited study by Kharchenko et al. (2013) presents an automated characterisation of the cluster population (known at the time), which was performed with all-sky 2MASS photometry (Skrutskie et al. 2006).”