A catalogue of 74 new open clusters found in Gaia Data-Release 2

He, Zhihong; Xu, Ye; Hao, Chao-Jie; Wu, Zhenyu; Li, Jingjing

doi:10.1088/1674-4527/21/4/93

Cited by 45 publications

(54 citation statements)

References 45 publications

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“…Since the publication of Gaia DR2 (Brown et al, 2018), on the one hand, the parameters of known OCs have been updated (Cantat-Gaudin et al, 2018;Soubiran et al, 2018;Bossini et al, 2019;Monteiro and Dias, 2019;Dias et al, 2021;Tarricq et al, 2021). On the other hand, a large number of new OCs and candidates have been identified (e.g., see Castro-Ginard et al, 2018;Cantat-Gaudin et al, 2019;Castro-Ginard et al, 2019;Sim et al, 2019;Liu and Pang, 2019;Hao et al, 2020;Castro-Ginard et al, 2020;Ferreira et al, 2020;He et al, 2021a;Hunt and Reffert, 2021;Ferreira et al, 2021). With OCs, the nearby spiral arms were studied by Cantat-Gaudin et al ( 2018 2021) compiled a catalogue of more than 3,700 OCs from the references above, and re-calculated the parameters (parallaxes, mean proper motions, radial velocities) based on the latest Gaia EDR3 (Brown et al, 2021).…”

Section: Young Open Clustersmentioning

confidence: 99%

The Spiral Structure in the Solar Neighborhood

Hou

2021

Front. Astron. Space Sci.

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The spiral structure in the solar neighborhood is an important issue in astronomy. In the past few years, there has been significant progress in observation. The distances for a large number of good spiral tracers, i.e., giant molecular clouds, high-mass star-formation region masers, HII regions, O-type stars, and young open clusters, have been accurately estimated, making it possible to depict the detailed properties of nearby spiral arms. In this work, we first give an overview about the research status for the Galaxy’s spiral structure based on different types of tracers. Then the objects with distance uncertainties better than 15% and <0.5 kpc are collected and combined together to depict the spiral structure in the solar neighborhood. Five segments related with the Perseus, Local, Sagittarius-Carina, Scutum-Centaurus, and Norma arms are traced. With the large dataset, the parameters of the nearby arm segments are fitted and updated. Besides the dominant spiral arms, some substructures probably related to arm spurs or feathers are also noticed and discussed.

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Section: Young Open Clustersmentioning

confidence: 99%

The Spiral Structure in the Solar Neighborhood

Hou

2021

Front. Astron. Space Sci.

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“…A new era comes as more and more new open clusters (e.g. Cantat-Gaudin et al 2018Castro-Ginard et al 2018, 2020Sim et al 2019;Liu & Pang 2019;Ferreira et al 2020;He et al 2021), large scale co-eval relic filaments (Jerabkova et al 2019;Beccari et al 2020) and extended stellar streams (Kounkel & Covey 2019) have been discovered recently using Gaia. With the Gaia data, for the first time, it has become possible to extract tidal tails of open star clusters, a challenging task due to the difficulty to distinguish tail stars from the Galactic field population (e.g.…”

Section: Introductionmentioning

confidence: 99%

The impact of massive stars and black holes on the fate of open star clusters and their tidal streams

Wang,

Jerabkova

2021

Preprint

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Context. To investigate how the content of massive OB stars affects the long-term evolution of young open clusters and their tidal streams, and how such an effect influences the constraint of initial conditions by looking at the present-day observations. Aims. OB stars are typically in binaries, have a strong wind mass loss during the first few Myr, and many become black holes. These affect the dynamical evolution of an open star cluster and impact its dissolution in a given Galactic potential. We investigate the correlation between the mass of OB stars and the observational properties of open clusters. Hyades-like star clusters are well represented in the Solar neighborhood and thus allow comparisons with observational data. Methods. We perform a large number of star-by-star numerical N-body simulations of Hyades-like star clusters by using the highperformance N-body code petar combined with galpy. Results. We find that OB stars and black holes have a major effect on star cluster evolution. Star clusters with the same initial conditions, but a different initial content of OB stars, follow very different evolutionary paths. Thus, the initial total mass and radius of an observed star cluster cannot be unambiguously determined unless the initial content of OB stars is known. We show that the stellar counts in the corresponding tidal tails, that can be identified in the Gaia data, help to resolve this issues. We thus emphasise the importance of exploring not only star-clusters, but also their corresponding tidal tails. These findings are relevant for studies of the formation of massive stars.

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“…With the advent of the ESA's Gaia space mission (Gaia Collaboration et al 2016), its second data release (DR2, Gaia Collaboration et al 2018) and, more recently, the Early Data Release 3 (EDR3, Gaia Collaboration et al 2021), astronomers have an homogeneous source of data with unprecedented astrometric precision and accuracy that have allowed to increase the census of known OCs and to improve the determinations of their properties. In the last years, the number of papers using data from Gaia and different techniques (from simple visual inspection to supervised or unsupervised machine learning techniques) and reporting the discovery of new OCs has increased notoriously (Castro-Ginard et al 2018;Cantat-Gaudin et al 2019;Ferreira et al 2019;Liu and Pang 2019;Sim et al 2019;Castro-Ginard et al 2020;Casado 2021;He et al 2021;Ferreira et al 2021;Hunt and Reffert 2021;Xiang et al 2021). An important requirement to be able to carry out reliable studies of the Galactic cluster population is that OC parameters are derived in a homogeneous manner.…”

Section: Introductionmentioning

confidence: 99%

Study of the open cluster Alessi-Teutsch 9 (ASCC 10) using multiband photometry and Gaia EDR3

Sanchez,

Lopez-Martinez,

Ocando

et al. 2021

Preprint

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There is a growing interest in the automated characterization of open clusters using data from the Gaia mission. This work evidences the importance of choosing an appropriate sampling radius (the radius of the circular region around the cluster used to extract the data) and the usefulness of additional multiband photometry in order to achieve accurate results. We address this issue using as a case study the cluster Alessi-Teutsch 9. The optimal sampling is determined by counting the number of assigned members at different sampling radii. By using this strategy with data from Gaia EDR3 and with observed photometry in 12 bands spanning the optical range from 3000 to 10000 Å, approximately, we are able to obtain reliable members and to determine the properties of the cluster. The spatial distribution of stars show a two-component structure with a central core of radius ∼ 12 − 13 arcmin and an outer halo extending out to 35 arcmin. With the derived cluster distance (654 pc) we obtain that the number density of stars is ≃ 0.06 star/pc 3 , making Alessi-Teutsch 9 one of the less dense known open clusters. The short relaxation time reveals that it is a dynamically relaxed and gravitationally bound system.

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A catalogue of 74 new open clusters found in Gaia Data-Release 2

Cited by 45 publications

References 45 publications

The Spiral Structure in the Solar Neighborhood

The Spiral Structure in the Solar Neighborhood

The impact of massive stars and black holes on the fate of open star clusters and their tidal streams

Study of the open cluster Alessi-Teutsch 9 (ASCC 10) using multiband photometry and Gaia EDR3

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