Diagnosing the Stellar Population and Tidal Structure of the Blanco 1 Star Cluster

Zhang, Yu; Tang, Shih-Yun; Chen, Wen-Ping; Pang, Xiaoying; Liu, J. Z.

doi:10.3847/1538-4357/ab63d4

Cited by 53 publications

(56 citation statements)

References 64 publications

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“…Eight of them are part of our sample : Coma Berenices, Ruprecht 147, Praesepe, Blanco 1, NGC 752, NGC 7092, NGC 2516 and Platais 9. Our study identifies tidal tails for Coma Berenices, Blanco 1, NGC 752, NGC 7092 and NGC 2516 previously found respectively by Tang et al (2019), Zhang et al (2020), Bhattacharya et al (2021) and Meingast et al (2021). We found the same orientations as these authors.…”

Section: Discussionsupporting

confidence: 89%

“…For NGC 2682 we identify many halo stars, confirming previous findings of Carrera et al (2019). In the case of Blanco 1, a tidal tail already reported by Zhang et al (2020) is also detected by our method in addition to halo stars. We detect vast coronae around a significant number of clusters, similarly to Meingast et al (2021) who performed a 3D analysis on ten prominent and nearby clusters.…”

Section: New Membershipssupporting

confidence: 90%

“…, Meingast & Alves (2019) and Jerabkova et al (2021) characterized the tidal tails of the Hyades at large spatial scale with different methods. The tidal tails of Coma Berenices, Ruprecht 147, Praesepe, Blanco 1, NGC 2506 and NGC 752 were discovered successively by Tang et al (2019), Yeh et al (2019), , Zhang et al (2020), Gao (2020) and Bhattacharya et al (2021). Meingast et al (2021) studied ten nearby (located closer than 500 pc), prominent and young OCs and identified around almost all of them an extended population of stars, referred as a corona.…”

Section: Introductionmentioning

confidence: 99%

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Structural parameters of 389 local Open Clusters

Tarricq,

Soubiran,

Casamiquela

et al. 2021

Preprint

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Context. The distribution of member stars in the surroundings of an open cluster can shed light on the process of its formation, evolution and dissolution. The analysis of structural parameters of open clusters as a function of their age and position in the Galaxy brings constraints on theoretical models of cluster evolution. The Gaia catalogue is very appropriate to find members of open clusters at large distance from their centers. Aims. We aim at revisiting the membership lists of open clusters from the solar vicinity, in particular by extending these membership lists to the peripheral areas thanks to Gaia EDR3. We then take advantage of these new lists of members to study the morphological properties and the mass segregation levels of the clusters. Methods. We used the clustering algorithm HDBSCAN on Gaia parallaxes and proper motions to systematically look for members up to 50 pc from the cluster centers. We fitted a King's function on the radial density profile of these clusters and a Gaussian Mixture Model on their two dimensional distribution of members to study their shape. We also evaluated the degree of mass segregation of the clusters and the correlations of these parameters with the age and Galactic position of the clusters. Results. Our methodology performs well on 389 clusters out of the 467 selected ones, including several recently discovered clusters that were poorly studied until now. We report the detection of vast coronae around almost all the clusters and report the detection of 71 open clusters with tidal tails, multiplying by more than four the number of such structures identified. We find the size of the cores to be on average smaller for old clusters than for young ones. Also, the overall size of the clusters seems to slightly increase with age while the fraction of stars in the halo seems to decrease. As expected the mass segregation is more pronounced in the oldest clusters but a clear trend with age is not seen. Conclusions. Open Clusters are more extended than previously expected, regardless of their age. The decrease in the proportion of stars populating the clusters halos highlights the different cluster evaporation processes and the short timescales they need to affect the clusters. Reported parameters like cluster sizes or mass segregation levels all depend on cluster ages but can not be described as single functions of time.

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Section: Discussionsupporting

confidence: 89%

Section: New Membershipssupporting

confidence: 90%

Section: Introductionmentioning

confidence: 99%

See 1 more Smart Citation

Structural parameters of 389 local Open Clusters

Tarricq,

Soubiran,

Casamiquela

et al. 2021

Preprint

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“…Here we estimated the radius of the cluster main body as the distance r with the highest density contrast, calculated as the ratio between the number of stars inside r to the number of stars in an annulus of interior radius r and equal area. We refer to some detailed studies of open clusters with well-known tidal tails: Hyades ), Praesepe , Coma Berenices (Tang et al 2019), and Blanco 1 (Zhang et al 2020), among others. Furthermore, cluster binary stars have so far been observed to be more centrally concentrated than single MS stars because of mass segregation that is caused by the dynamics internal evolution driven by two-body relaxation (Reino et al 2018;Gao 2018;Cohen et al 2020), even though open clusters have also been subject of tidal effects due to the gravitational potential of the Milky Way (Piatti & Mackey 2018;Piatti et al 2019b).…”

Section: Analysis and Discussionmentioning

confidence: 99%

Binary star sequence in the outskirts of the disrupting Galactic open cluster UBC 274

Piatti

2020

A&A

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We report the identification of a numerous binary star population in the recently discovered ∼3 Gyr old open cluster UBC 274. It becomes visible when the cluster color-magnitude diagram is corrected by differential reddening and spans mass ratio (q) values from 0.5 up to 1.0. Its stellar density radial profile and cumulative distribution as a function of the distance from the cluster center reveal that it extends out to the observed boundaries of the tidal tails of the cluster (about six times the cluster radius) following a spatial distribution indistinguishable from that of cluster main-sequence (MS) stars. Furthermore, binary stars with q values lower or higher than 0.75 do not show any spatial distribution difference either. From Gaia DR2 astrometric and kinematics data we computed Galactic coordinates and space velocities with respect to the cluster center and mean cluster space velocity, respectively. We found that cluster members located throughout the tidal tails move relatively fast, regardless of whether they are a single or binary star. The projection of their motions onto the Galactic plane resembles that of a rotating solid body, while the motions along the radial direction from the Galactic center and perpendicular to the Galactic plane suggest that the cluster is being disrupted. The similarity of the spatial distributions and kinematic patterns of cluster MS and binary stars reveals that UBC 274 is facing an intense process of disruption that has apparently swept out any signature of internal dynamic evolution, such as mass segregation driven by two-body relaxation.

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“…Meingast et al (2021) described the nearby extended spatial distribution of stars that co-move with their clusters but are not bound to them. After the release of the Gaia DR2 catalogue, tidal tails have been found around four nearby (<300 pc) OCs, namely Blanco 1 (≈100 Myr, Zhang et al 2020), the Hyades (≈600−700 Myr; Douglas et al 2019;Gossage et al 2018;Reino et al 2018;Lodieu 2020;Gaia Collaboration 2018b), Coma Berenices (≈750 Myr; Tang et al 2019;Fürnkranz et al 2019), and Praesepe (≈800 Myr; .…”

Section: Introductionmentioning

confidence: 99%

The 800 pc long tidal tails of the Hyades star cluster

Jeřabková

Boffin

Beccari

et al. 2021

A&A

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The tidal tails of stellar clusters provide an important tool for studying the birth conditions of the clusters and their evolution, coupling, and interaction with the Galactic potential. The Gaia satellite, with its high-quality astrometric data, opened this field of study, allowing us to observe large-scale tidal tails. Theoretical models of tidal-tail formation and evolution are available. However, the exact appearance of tidal features as seen in the Gaia catalogue has not yet been studied. Here we present the N-body evolution of a Hyades-like stellar cluster with backward-integrated initial conditions on a realistic 3D orbit in the Milky Way galaxy computed within the AMUSE framework. For the first time, we explore the effect of the initial cluster rotation and the presence of lumps in the Galactic potential on the formation and evolution of tidal tails. For all of our simulations we present Gaia observables and derived parameters in the convergent point (CP) diagram. We show that the tidal tails are not naturally clustered in any coordinate system and that they can span up to 40 km s−1 relative to the cluster centre in proper motions for a cluster age of 600–700 Myr. Models with initial rotation result in significant differences in the cluster mass loss and follow different angular momentum time evolution. Thus the orientation of the tidal tails relative to the motion vector of the cluster and the current cluster angular momentum constrain the initial rotation of the cluster. We highlight the use of the standard CP method in searches for co-moving groups and introduce a new compact CP (CCP) method that accounts for internal kinematics based on an assumed model. Using the CCP method, we are able to recover candidate members of the Hyades tidal tails in the Gaia Data Release 2 and early Data Release 3 (eDR3) reaching a total extent of almost 1 kpc. We confirm the previously noted asymmetry in the detected tidal tails. In the eDR3 data we recovered spatial overdensities in the leading and trailing tails that are kinematically consistent with being epicyclic overdensities and thus would present candidates for the first such detection in an open star cluster. We show that the epicyclic overdensities are able to provide constraints not only on the cluster properties, but also on the Galactic potential. Finally, based on N-body simulations, a close encounter with a massive Galactic lump can explain the observed asymmetry in the tidal tails of the Hyades.

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Diagnosing the Stellar Population and Tidal Structure of the Blanco 1 Star Cluster

Cited by 53 publications

References 64 publications

Structural parameters of 389 local Open Clusters

Structural parameters of 389 local Open Clusters

Binary star sequence in the outskirts of the disrupting Galactic open cluster UBC 274

The 800 pc long tidal tails of the Hyades star cluster

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