Wide- and contact-binary formation in substructured young stellar clusters

Dorval, Julien; Boily, C. M.; Moraux, E.; Roos, O.

doi:10.1093/mnras/stw2880

Cited by 10 publications

(10 citation statements)

References 73 publications

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“…Figure 1 shows the initial, intermediate, and final steps for one of our models. More details and further examples are given in Dorval et al (2016Dorval et al ( , 2017.…”

Section: Gravity-driven Fragmentation Modellingmentioning

confidence: 99%

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Assessing membership projection errors in star forming regions

Roland

Boily

Cambrésy

2020

A&A

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Context. Young stellar clusters harbour complex spatial structures emerging from the star formation process. Identifying stellar overdensities is a key step in better constraining how these structures are formed. The high accuracy of distances derived from Gaia DR2 parallaxes still do not allow us to locate individual stars within clusters of ≈1 pc in size with certainty. Aims. In this work, we explore how such uncertainty on distance estimates can lead to the misidentification of membership of subclusters selected by the minimum spanning tree (MST) algorithm. Our goal is to assess how this impacts their estimated properties. Methods. Using N-body simulations, we build gravity-driven fragmentation models that self-consistently reproduce the early stellar configurations of a star forming region. Stellar groups are then identified both in two and three dimensions by the MST algorithm, representing respectively an inaccurate and an ideal identification. We compare the properties derived for these resulting groups in order to assess the systematic bias introduced by projection and incompleteness. Results. We show that in such fragmented configurations, the dynamical mass of groups identified in projection is systematically underestimated compared to those of groups identified in 3D. This systematic error is statistically of 50% for more than half of the groups and reaches 100% in a quarter of them. Adding incompleteness further increases this bias. Conclusions. These results challenge our ability to accurately identify sub-clusters in most nearby star forming regions where distance estimate uncertainties are comparable to the size of the region. New clump-finding methods need to tackle this issue in order to better define the dynamical state of these substructures.

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“…Figure 1 shows the initial, intermediate, and final steps for one of our models. More details and further examples are given in Dorval et al (2016Dorval et al ( , 2017.…”

Section: Gravity-driven Fragmentation Modellingmentioning

confidence: 99%

“…This method is an efficient way to build fragmented initial conditions self-consistently using only N-body modelling. It allows the user to explore a large number of fragmented configurations and test our understanding of the dynamical processes in action (see also Dorval et al 2017).…”

Section: Introductionmentioning

confidence: 99%

Assessing membership projection errors in star forming regions

Roland

Boily

Cambrésy

2020

A&A

Self Cite

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show abstract

“…Figure 1 shows the initial, intermediate, and final steps for one of our models. More details and further examples are given in Dorval et al (2016) and Dorval et al (2017).…”

Section: Gravity-driven Fragmentation Modellingmentioning

confidence: 99%

Assessing membership projection errors in star forming regions

Roland,

Boily,

Cambrésy

2020

Preprint

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Context. Young stellar clusters harbour complex spatial structures emerging from the star formation process. Identifying stellar overdensities is a key step in better constraining how these structures are formed. The high accuracy of distances derived from Gaia DR2 parallaxes still do not allow us to locate individual stars within clusters of ≈ 1 pc in size with certainty. Aims. In this work, we explore how such uncertainty on distance estimates can lead to the misidentification of membership of subclusters selected by the minimum spanning tree (MST) algorithm. Our goal is to assess how this impacts their estimated properties. Methods. Using N-body simulations, we build gravity-driven fragmentation (GDF) models that self-consistently reproduce the early stellar configurations of a star forming region. Stellar groups are then identified both in two and three dimensions by the MST algorithm, representing respectively an inaccurate and an ideal identification. We compare the properties derived for these resulting groups in order to assess the systematic bias introduced by projection and incompleteness. Results. We show that in such fragmented configurations, the dynamical mass of groups identified in projection is systematically underestimated compared to those of groups identified in 3D. This systematic error is statistically of 50% for more than half of the groups and reaches 100% in a quarter of them. Adding incompleteness further increases this bias. Conclusions. These results challenge our ability to accurately identify sub-clusters in most nearby star forming regions where distance estimate uncertainties are comparable to the size of the region. New clump-finding methods need to tackle this issue in order to better define the dynamical state of these substructures.

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“…The binary destruction rate in small clusters is faster than in more massive ones. In principle, the observed binary fraction of young star clusters can therefore offer a possible tool to distinguish between the two cluster formation scenarios mentioned above (Dorval et al 2017).…”

Section: Young Star Clustersmentioning

confidence: 99%

A MODEST review

et al. 2018

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We present an account of the state of the art in the fields explored by the research community invested in "Modeling and Observing DEnse STellar systems". For this purpose, we take as a basis the activities of the MODEST-17 conference, which was held at Charles University, Prague, in September 2017. Reviewed topics include recent advances in fundamental stellar dynamics, numerical methods for the solution of the gravitational N-body problem, formation and evolution of young and old star clusters and galactic nuclei, their elusive stellar populations, planetary systems, and exotic compact objects, with timely attention to black holes of different classes of mass and their role as sources of gravitational waves.Such a breadth of topics reflects the growing role played by collisional stellar dynamics in numerous areas of modern astrophysics. Indeed, in the next decade many revolutionary instruments will enable the derivation of positions and velocities of individual stars in the Milky Way and its satellites, and will detect signals from a range of astrophysical sources in different portions of the electromagnetic and gravitational spectrum, with an unprecedented sensitivity. On the one hand, this wealth of data will allow us to address a number of long-standing open questions in star cluster studies; on the other hand, many unexpected properties of these systems will come to light, stimulating further progress of our understanding of their formation and evolution.

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Wide- and contact-binary formation in substructured young stellar clusters

Cited by 10 publications

References 73 publications

Assessing membership projection errors in star forming regions

Assessing membership projection errors in star forming regions

Assessing membership projection errors in star forming regions

A MODEST review

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