The Relation of the Alpha Persei Star Cluster with the Nearby Stellar Stream

Nikiforova, V. V.; Kulesh, M. V.; Seleznev, A. F.; Carraro, G.

doi:10.3847/1538-3881/aba753

Cited by 11 publications

(6 citation statements)

References 32 publications

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“…Given the cluster has an age of log(t) = 8.803, it is unlikely that this elongated feature is associated with the remnants of a filament. However, it is possible that this feature belongs to a stream associated with Alessi 6, as was found for Coma Berenices (Tang et al 2019) and Alpha Persei (Nikiforova et al 2020).…”

Section: Notes On Individual Clustersmentioning

confidence: 78%

“…The Pleiades has only short tidal tails discovered (Ye et al 2021) with possibility of longer tails being uncovered. Alpha Persei's tidal tails were only identified by Nikiforova et al (2020) as photometric overdensities against the forground and background sources, and the tail members were not identified from kinematic measurements. We thus continue to include Alpha Persei and the Pleiades in our study.…”

Section: Cluster Selectionmentioning

confidence: 99%

“…• Alpha Persei: Nikiforova et al (2020) identified tidal tails in Alpha Persei from stellar overdensities, but were not able to determine members for the tails. In this work, we are also unable to identify the tail members and detect just the cluster corona, same as Lodieu et al (2019).…”

Section: Notes On Individual Clustersmentioning

confidence: 99%

“…Reliable astrometry (proper motion and parallax) from Gaia Data Release 2 (Gaia DR2; Gaia Collaboration et al 2018) and recently Gaia Early Data Release 3 (Gaia EDR3; Gaia Collaboration et al 2021) has allowed for improved field-star decontamination of many nearby open clusters, resulting in the recent discovery of a many open clusters with extended stellar coronae (e.g. Carrera et al 2019;Meingast et al 2021;Tarricq et al 2022), as well as 13 of those with tidal tails -Hyades: ; Meingast & Alves (2019); Jerabkova et al (2021); Coma Berenices: ★ E-mail: souradeep@iucaa.in Tang et al (2019); Ruprecht 147: Yeh et al (2019); Praesepe: ; NGC 2506: Gao (2020b); Blanco 1: Zhang et al (2020); M 67: Gao (2020a); UBC 274: Castro-Ginard et al (2020); Alpha Persei: Nikiforova et al (2020); NGC 2516, NGC 6633: Pang et al (2021); NGC 752: Bhattacharya et al (2021a); Pleiades: Li et al (2021). Tarricq et al (2022) recently carried out a systematic search for tidal tails in open clusters by identifying elongated features in the 2D projected spatial distribution of cluster members identified from Gaia EDR3 data.…”

Section: Introductionmentioning

confidence: 99%

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A $Gaia$ EDR3 search for tidal tails in disintegrating open clusters

Bhattacharya¹,

Rao²,

Agarwal³

et al. 2022

Preprint

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We carry out a search for tidal tails in a sample of open clusters with known relatively elongated morphology. We identify the member stars of these clusters from the precise astrometric and deep photometric data from Gaia Early Data Release 3 using the robust membership determination algorithm, ML-MOC. We identify 46 open clusters having a stellar corona beyond the tidal radius, 20 of which exhibit extended tails aligned with the cluster orbit direction in galactocentric coordinates. Notably we find NGC 6940 (at a distance of ∼ 1 kpc) is the furthest open cluster exhibiting tidal tails that are ∼ 50 pc from its center, while also identifying ∼ 40 pc long tidal tails for the nearby Pleiades. Using the minimum spanning tree length for the most massive stars relative to all cluster members, we obtain the mass segregation ratio (𝜆 MSR ) profiles as a function of the number of massive stars in each cluster. From these profiles, we can classify the open clusters into four classes based on the degree of mass segregation experienced by the clusters. We find that clusters in the most mass segregated classes are the oldest on average and have the flattest mass function slope. Of the 46 open clusters studied in this work, 41 exhibit some degree of mass segregation. Furthermore, we estimate the initial masses (M i ) of these open clusters finding that some of them, having M i 10 4 M , could be the dissolving remnants of Young Massive Clusters.

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Section: Notes On Individual Clustersmentioning

confidence: 78%

Section: Cluster Selectionmentioning

confidence: 99%

Section: Notes On Individual Clustersmentioning

confidence: 99%

Section: Introductionmentioning

confidence: 99%

See 2 more Smart Citations

A $Gaia$ EDR3 search for tidal tails in disintegrating open clusters

Bhattacharya¹,

Rao²,

Agarwal³

et al. 2022

Preprint

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“…A number of young OCs have been detected with tail-like structures, including IC 2391, IC 2602, NGC 2451A, NGC 2547 (Meingast et al 2021) and NGC 2232, NGC 2451B (Pang et al 2021) (NGC 2547 has been analyzed in both Meingast et al 2021 andPang et al 2021). In addition, more and more relatively elder OCs have been revealed with tidal tails, such as Hyades Jerabkova et al 2021); NGC 6774 (Yeh et al 2019;Pang et al 2021); Coma Berenices (Fürnkranz et al 2019;Tang et al 2019); Praesepe ; NGC 2682 (Carrera et al 2019;; Blanco 1 (Zhang et al 2020;Meingast et al 2021;Pang et al 2021); newly discovered OC UBC 274 (Castro-Ginard et al 2020); NGC 2506 ); α Per (Nikiforova et al 2020;Meingast et al 2021); Platais 9, Messier 39 (Meingast et al 2021); NGC 6633 (Pang et al 2021); NGC 2516 (Meingast et al 2021;Pang et al 2021); NGC 752 (Bhattacharya et al 2021).…”

Section: Introductionmentioning

confidence: 99%

Extended Tidal Tails of IC 4756 detected by {\it Gaia} EDR3

Ye,

Zhao,

Zhang

et al. 2021

Preprint

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We report the discovery of emerged tidal tails around open cluster IC 4756 (∼ 1 Gyr) based on 644 members identified from Gaia EDR3. Three-dimensional spatial positions, two-dimensional tangential velocities (x, y, z, κ • µ * α /̟, κ • µ δ /̟) are utilized to determine the co-moving member candidates of IC 4756. Using a Bayesian method, we correct the distance for each cluster member. Two tidal tails extend up to 180 pc and display a S-shape in X ′ Y ′ space (Cartesian coordinates focused on cluster center). A clean sequence of our members in Color-Absolute-Magnitude Diagram (CAMD) indicates the coeval population and matches perfectly with the PARSEC isochrone with age from Bossini et al. (2019). Mass segregation is detected in this cluster as well. Finally, we derive the tidal radius and core radius of IC 4756 about 12.13 pc and 4.33 ± 0.75 pc, respectively.

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Lithium depletion boundary, stellar associations, andGaia

Galindo-Guil

Barrado

Bouy

et al. 2022

A&A

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Context. Stellar ages are key to improving our understanding of different astrophysical phenomena. However, many techniques to estimate stellar ages are highly model-dependent. The lithium depletion boundary (LDB), based on the presence or absence of lithium in low-mass stars, can be used to derive ages in stellar associations of between 20 and 500 Ma. Aims. The purpose of this work is to revise former LDB ages in stellar associations in a consistent way, taking advantage of the homogeneous Gaia parallaxes as well as bolometric luminosity estimations that do not rely on monochromatic bolometric corrections. Methods. We studied nine open clusters and three moving groups characterised by a previous determination of the LDB age. We gathered all the available information from our data and the literature: membership, distances, photometric data, reddening, metallicity, and surface gravity. We re-assigned membership and calculated bolometric luminosities and effective temperatures using distances derived from Gaia DR2 and multi-wavelength photometry for individual objects around the former LDB. We located the LDB using a homogeneous method for all the stellar associations. Finally, we estimated the age by comparing it with different evolutionary models. Results. We located the LDB for the twelve stellar associations and derived their ages using several theoretical evolutionary models. We compared the LDB ages among them, along with data obtained with other techniques, such as isochrone fitting, ultimately finding some discrepancies among the various approaches. Finally, we remark that the 32 Ori MG is likely to be composed of at least two populations of different ages. Conclusions.Key words. open clusters and associations: general -stars: fundamental parameters, low-mass stars, brown dwarfs 1 We use the term stellar association to refer both to open clusters and moving groups. A moving group is a stream of stars with common age and motion through the Milky Way and with no overdensity of stars discernible in any region (Zuckerman & Song 2004). An open cluster is a group of gravitationally bound stars that shows a clear concentration above the surrounding stellar background

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The Relation of the Alpha Persei Star Cluster with the Nearby Stellar Stream

Cited by 11 publications

References 32 publications

A $Gaia$ EDR3 search for tidal tails in disintegrating open clusters

A $Gaia$ EDR3 search for tidal tails in disintegrating open clusters

Extended Tidal Tails of IC 4756 detected by {\it Gaia} EDR3

Lithium depletion boundary, stellar associations, andGaia

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