Tidal tails in the disintegrating open cluster NGC 752

Bhattacharya, Souradeep; Agarwal, Manan; Rao, Khushboo K.; Vaidya, Kaushar

doi:10.48550/arxiv.2105.06108

Cited by 1 publication

(2 citation statements)

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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%

“…, 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: 98%

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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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