Open cluster kinematics with <i>Gaia</i> DR2

Soubiran, C.; Cantat-Gaudin, T.; Romero-Gómez, M.; Casamiquela, L.; Jordi, C.; Vallenari, A.; Antoja, T.; Balaguer-Núñez, L.; Bossini, D.; Bragaglia, A.; Carrera, R.; Castro-Ginard, A.; Figueras, F.; Heiter, U.; Katz, David; Krone-Martins, A.; Campion, J.-F. Le; Moitinho, A.; Sordo, R.

doi:10.1051/0004-6361/201834020

Cited by 185 publications

(236 citation statements)

References 61 publications

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“…The extra-tidal features we observe in M67 would thus be quite a natural result of disk shocking. This is to be confirmed quantitatively with dedicated N-body models in an upcoming paper (Pasquato et al 2019, in preparation Soubiran et al (2018). Blue arrows show the direction to the observer.…”

Section: Physical Interpretationsupporting

confidence: 53%

Extended halo of NGC 2682 (M 67) from Gaia DR2

Carrera

Pasquato

Vallenari

et al. 2019

A&A

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Context. NGC 2682 is a nearby open cluster, approximately 3.5 Gyr old. Dynamically, most open clusters should dissolve on shorter timescales, of ≈ 1 Gyr. Having survived until now, NGC 2682 was likely much more massive in the past, and is bound to have an interesting dynamical history. Aims. We investigate the spatial distribution of NGC 2682 stars to constrain its dynamical evolution, especially focusing on the marginally bound stars in the cluster outskirts. Methods. We use Gaia DR2 data to identify NGC 2682 members up to a distance of ∼150 pc (10 degrees). Two methods (Clusterix and UPMASK) are applied to this end. We estimate distances to obtain three-dimensional stellar positions using a Bayesian approach to parallax inversion, with an appropriate prior for star clusters. We calculate the orbit of NGC 2682 using the GRAVPOT16 software. Results. The cluster extends up to 200 ′ (50 pc) which implies that its size is at least twice as previously believed. This exceeds the cluster Hill sphere based on the Galactic potential at the distance of NGC 2682. Conclusions. The extra-tidal stars in NGC 2682 may originate from external perturbations such as disk shocking or dynamical evaporation from two-body relaxation. The former origin is plausible given the orbit of NGC 2682, which crossed the Galactic disk ≈ 40 Myr ago.

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Section: Physical Interpretationsupporting

confidence: 53%

Extended halo of NGC 2682 (M 67) from Gaia DR2

Carrera

Pasquato

Vallenari

et al. 2019

A&A

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“…The second data release of the Gaia mission (Prusti et al 2016;Brown et al 2018) has revolutionized our view of the Milky Way Galaxy. Among its many results, it has proven very useful for investigating purported stellar clusters, in many cases confirming their existence (e.g., Simpson et al 2017b;Soubiran et al 2018;Cantat-Gaudin et al 2018), but in some cases showing they are not real physical associations (e.g., Kos et al 2018). The precise proper motions are especially helpful in the Milky Way bulge, where imaging surveys are hampered by the large and differential reddening and extinction, resulting in clusters hidden from easy view.…”

Section: Introductionmentioning

confidence: 99%

The retrograde orbit of the globular cluster FSR1758 revealed with Gaia DR2

Simpson

2019

Monthly Notices of the Royal Astronomical Society

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We report the first radial velocity measurements of the recently identified globular cluster FSR1758. From the two member stars with radial velocities from the Gaia Radial Velocity Spectrograph reported in Gaia DR2, we find FSR1758 has a radial velocity of 227 ± 1km s −1 . We also find potential extra-tidal star lost from the cluster in the surrounding 1 deg. Combined with Gaia proper motions and photometric distance estimates, this shows that FSR1758 is on a relatively retrograde, radial orbit with an pericentre of 3.8 +0.9 −0.9 kpc, an apocentre of 16 +8 −5 kpc, and eccentricity of 0.62 +0.05 −0.04 . Although it is currently at a Galactocentric distance of 3.8 +0.9 −0.9 kpc -at the edge of the bulge -it is an intruder from the halo. We investigate whether a reported 'halo' of stars around FSR1758 is related to the cluster, and find that most of these stars are likely foreground dwarf stars. We conclude that FSR1758 is not a dwarf galaxy, but rather a globular cluster.

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“…From this sample we check those with radial velocities from Gaia DR2 (88 stars) and use it only to calculate a median radial velocity with a sigma clipping, resulting in v rad = 34.5 ± 2.0 km s −1 from 84 stars. Soubiran et al (2018) find a v rad = 33.80±1.06 km s −1 from 64 member stars.…”

Section: Ngc 2682 (M 67)mentioning

confidence: 81%

“…Clusterix 2.0 allows the user to modify h at will, although the system proposes by default a value computed by means of Silverman's rule (Silverman 1986):…”

Section: Raw Normalised and Scaled Frequency Functionsmentioning

confidence: 99%

“…The determination of the mean properties of open clusters (like radial velocity or metallicity) requires prior knowledge of their member stars to optimise the costly process of obtaining and reducing high resolution spectroscopic data on a large scale. Some information is already available mainly for radial velocity (Soubiran et al 2018;Carrera et al 2019a). Moreover, knowing the membership probability of the stars in the cluster area helps to select member stars on photometric diagrams, to determine the age of the cluster by isochrone fitting (e.g.…”

Section: Introductionmentioning

confidence: 99%

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Clusterix 2.0: a virtual observatory tool to estimate cluster membership probability

Balaguer-Núñez

Fresno

Solano

et al. 2020

Monthly Notices of the Royal Astronomical Society

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Clusterix 2.0 is a web-based, Virtual Observatory-compliant, interactive tool for the determination of membership probabilities in stellar clusters based on proper motion data using a fully non-parametric method. In the area occupied by the cluster, the frequency function is made up of two contributions: cluster and field stars. The tool performs an empirical determination of the frequency functions from the Vector-Point Diagram without relying in any previous assumption about their profiles. Clusterix 2.0 allows to search in an interactive way the appropriate spatial areas until an optimal separation of the two populations is obtained. Several parameters can be adjusted to make the calculation computationally feasible without interfering in the quality of the results. The system offers the possibility to query different catalogues, such as Gaia, or upload the user own data. The results of the membership determination can be sent via SAMP to VO tools like TopCat.We apply Clusterix 2.0 to several open clusters with different properties and environments to show the capabilities of the tool: an area of five degrees around NGC 2682 (M 67), an old, well known cluster; a young cluster NGC 2516 with a striking elongate structure extended up to four degrees; NGC 1750 & NGC 1758, a pair of partly overlapping clusters; in the area of NGC 1817 we confirm a little-known cluster, Juchert 23; and in an area with many clusters we disentangle the existence of two overlapping clusters where only one was previously known: Ruprecht 26 and the new, Clusterix 1.

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Open cluster kinematics with Gaia DR2

Cited by 185 publications

References 61 publications

Extended halo of NGC 2682 (M 67) from Gaia DR2

Extended halo of NGC 2682 (M 67) from Gaia DR2

The retrograde orbit of the globular cluster FSR1758 revealed with Gaia DR2

Clusterix 2.0: a virtual observatory tool to estimate cluster membership probability

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