58 open clusters investigated with UBVRI and<i>Gaia</i>eDR3 data

Dias, W. S.; Monteiro, H.; Caetano, Thiago Costa; Hickel, G. R.; Alves, G; Sacchi, M; Lépine, J. R. D.; Amarinho, N.

doi:10.1093/mnras/stac718

Cited by 6 publications

(5 citation statements)

References 88 publications

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“…In addition, we also compared the proper-motion dispersions of our new OCs with those of CG20. Figure 13 shows the distribution of OC candidates identified in the study have similar smaller dispersions to the known OCs, which show the characteristics of a real cluster (CG20; Dias et al 2022). Figure 10.…”

Section: Pd Parallax and Proper-motion Dispersionsmentioning

confidence: 59%

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Identifying 46 New Open Cluster Candidates in Gaia EDR3 Using a Hybrid pyUPMASK and Random Forest Method

Chi

Wei

Wang

et al. 2023

ApJS

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Open clusters (OCs) are regarded as tracers to understand stellar evolution theory and validate stellar models. In this study, we presented a robust approach to identifying OCs. A hybrid method consisting of pyUPMASK and the random forest (RF) algorithm is first used to remove field stars and determine more reliable members. An identification model based on the RF algorithm built based on 3714 OC samples from Gaia DR2 and EDR3 is then applied to identify OC candidates. The OC candidates are obtained after isochrone fitting, advanced stellar population synthesis model fitting, and visual inspection. Using the proposed approach, we revisited 868 candidates and preliminarily clustered them by the friends-of-friends algorithm in Gaia EDR3. Excluding OCs that have already been reported, we focused on the remaining 300 unknown candidates. From high to low fitting quality, these unrevealed candidates were further classified into Class A (59), Class B (21), and Class C (220). As a result, 46 new reliable OC candidates among Classes A and B are identified after visual inspection.

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Section: Pd Parallax and Proper-motion Dispersionsmentioning

confidence: 59%

“…pyUPMASK is a Python package for UPMASK (Krone-Martins & Moitinho 2014) used to estimate the membership probability of each input star. pyUPMASK has been widely used in the determination of member stars of OCs based on astrometric parameters (Cantat-Gaudin et al 2019;He et al 2022b;Bai et al 2022;Dias et al 2022).…”

Section: Member Star Determination Methodsmentioning

confidence: 99%

Identifying 46 New Open Cluster Candidates in Gaia EDR3 Using a Hybrid pyUPMASK and Random Forest Method

Chi

Wei

Wang

et al. 2023

ApJS

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“…PyUPMASK is a Python package for Unsupervised Photometric Membership Assignment in Stellar Clusters (UP-MASK) Krone-Martins & Moitinho (2014) used to estimate the membership probability of each input star. PyUP-MASK has been widely used in the determination of member stars of OC based on astrometric parameters (Cantat-Gaudin et al 2019;He et al 2022d;Bai et al 2022;Dias et al 2022). The membership probability of stars is iteratively calculated by…”

Section: Member Star Determinationmentioning

confidence: 99%

Blind Search of The Solar Neighborhood Galactic Disk within 5kpc: 1,179 new Star clusters found in Gaia DR3

Chi¹,

Wang²,

Wang³

et al. 2023

Preprint

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Studying open clusters (OCs) is essential for a comprehensive understanding of the structure and evolution of the Milky Way. Many previous studies have systematically searched for OCs near the solar system within 1.2 kpc or 20 degrees of galactic latitude. However, few studies searched for OCs at higher galactic latitudes and deeper distances. In this study, based on a hybrid unsupervised clustering algorithm (Friends-of-Friends and pyUPMASK) and a binary classification algorithm (Random Forest), we extended the search region (i.e., galactic latitude |b| ≥ 20 • ) and performed a fine-grained blind search of Galactic clusters in Gaia DR3. After cross-matching, the newly discovered cluster candidates are fitted using isochrone fitting to estimate the main physical parameters (age and metallicity) of these clusters. These cluster candidates were then checked using manual visual inspection. Their statistical properties were compared with previously exposed cluster catalogs as well. In the end, we found 1,179 new clusters with considerable confidence within 5kpc.

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“…In the past few years, the Gaia mission has provided highprecision photometry, proper motions, and parallaxes of nearly 2 billion stars in the Milky Way (Gaia Collaboration 2018, 2021, Gaia DR2 andDR3). This exquisite dataset has allowed accurate separations to be obtained between the bulk of the OC members and the background and foreground stars (e.g., Cantat-Gaudin et al 2018Bossini et al 2019;Dias et al 2022).…”

Section: Introductionmentioning

confidence: 99%

Photometric binaries, mass functions, and structural parameters of 78 Galactic open clusters

Cordoni

Milone

Marino

et al. 2023

A&A

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Context. Binary stars play a crucial role in our understanding of the formation and evolution of star clusters and their stellar populations. Aims. We use Gaia Data Release 3 to homogeneously analyze 78 Galactic open clusters and the unresolved binary systems they host, each composed of two main sequence (MS) stars. Methods. We first investigated the structural parameters of these clusters, such as the core radius and the central density, and determined the cluster mass function (MF) and total mass by interpolating the density profile of each cluster. We measured the fraction of binaries with a large mass ratio and the fraction of blue straggler stars (BSSs), and finally investigated possible connections between the populations of binary stars and BSSs with the main parameters of the host cluster. Results. Remarkably, we find that the MFs of 78 analyzed open clusters follow a similar trend and are well reproduced by two single power-law functions, with a change in slope around masses of 1 M⊙. The fraction of binary stars ranges from ∼15% to more than ∼60% without significant correlation with the mass and the age of the host cluster. Moreover, we detect hints of a correlation between the total fraction of binary stars and the central density of the host cluster. We compared the fraction of binary stars with that of BSSs, finding that clusters with high and low central density exhibit different trends. The fraction of binaries does not significantly change with the mass of the primary star and the mass ratio. The radial distribution of binary stars depends on cluster age. The binaries of clusters younger than ∼800 Myr typically show a flat radial distribution, with some hints of a double peak. In contrast, the binaries of the remaining clusters are more centrally concentrated than the single stars, which is similar to what is observed in globular clusters.

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58 open clusters investigated with UBVRI andGaiaeDR3 data

Cited by 6 publications

References 88 publications

Identifying 46 New Open Cluster Candidates in Gaia EDR3 Using a Hybrid pyUPMASK and Random Forest Method

Identifying 46 New Open Cluster Candidates in Gaia EDR3 Using a Hybrid pyUPMASK and Random Forest Method

Blind Search of The Solar Neighborhood Galactic Disk within 5kpc: 1,179 new Star clusters found in Gaia DR3

Photometric binaries, mass functions, and structural parameters of 78 Galactic open clusters

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