Spectroscopic signatures of extratidal stars around the globular clusters NGC 6656 (M 22), NGC 3201, and NGC 1851 from RAVE

Kunder, Andrea; Bono, G.; Piffl, Tilmann; Steinmetz, Matthias; Grebel, Eva K.; Anguiano, Borja; Freeman, K. C.; Kordopatis, G.; Zwitter, T.; Scholz, R. D.; Gibson, Brad K.; Bland-Hawthorn, Joss; Seabroke, G. M.; Boeche, C.; Siebert, A.; Wyse, Rosemary F. Ġ.; Bienaymé, O.; Navarro, Julio F.; Siviero, A.; Minchev, Ivan; Parker, Quentin A.; Reid, Warren A.; Gilmore, G.; Munari, U.; Helmi, Amina

doi:10.1051/0004-6361/201424113

Cited by 48 publications

(45 citation statements)

References 120 publications

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“…This is borne out by observations: Ness et al (2013) found a population of stars in their ARGOS study of the bulge that had properties consistent with NGC 6656, which could be extratidal stars from the cluster. Kunder et al (2014) also found a candidate extratidal star of NGC 6656 in RAVE data.…”

Section: Ngc 6656 (M 22)mentioning

confidence: 78%

Tycho-Gaia Astrometric Solution Parallaxes and Proper Motions for Five Galactic Globular Clusters

Watkins

Marel

2017

ApJ

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We present a pilot study of Galactic globular cluster (GC) proper motion (PM) determinations using Gaia data. We search for GC stars in the Tycho-Gaia Astrometric Solution (TGAS) catalogue from Gaia Data Release 1 (DR1), and identify five members of NGC 104 (47 Tucanae), one member of NGC 5272 (M 3), five members of NGC 6121 (M 4), seven members of NGC 6397, and two members of NGC 6656 (M 22). By taking a weighted average of member stars, fully accounting for the correlations between parameters, we estimate the parallax (and, hence, distance) and PM of the GCs. This provides a homogeneous PM study of multiple GCs based on an astrometric catalogue with small and well-controlled systematic errors and yields random PM errors similar to existing measurements. Detailed comparison to the available Hubble Space Telescope (HST) measurements generally shows excellent agreement, validating the astrometric quality of both TGAS and HST. By contrast, comparison to ground-based measurements shows that some of those must have systematic errors exceeding the random errors. Our parallax estimates have uncertainties an order of magnitude larger than previous studies, but nevertheless imply distances consistent with previous estimates. By combining our PM measurements with literature positions, distances, and radial velocities, we measure Galactocentric space motions for the clusters and find that these also agree well with previous analyses. Our analysis provides a framework for determining more accurate distances and PMs of Galactic GCs using future Gaia data releases. This will provide crucial constraints on the near end of the cosmic distance ladder and provide accurate GC orbital histories.

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Section: Ngc 6656 (M 22)mentioning

confidence: 78%

Tycho-Gaia Astrometric Solution Parallaxes and Proper Motions for Five Galactic Globular Clusters

Watkins

Marel

2017

ApJ

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“…Other six globular clusters have also been associated to the same progenitor, namely: FSR 1758, IC 4499, NGC 3201, 5466, 6101 and 7006. As far as we are aware, 4 of them with previous studies of their external structures have been found to have extra-tidal features : FSR 1758: Barbá et al (2019); NGC 3202: Kunder et al (2014);NGC 5466, and NGC 7006: Jordi & Grebel (2010).…”

Section: Introductionmentioning

confidence: 78%

Pal 13: its moderately extended low-density halo and its accretion history

Piatti

Fernández-Trincado

2020

A&A

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We present results on the basis of Dark Energy Camera Legacy Survey (DECaLS) DR8 astrometric and photometric data sets of the Milky Way globular cluster Pal 13. Because of its relative small size and mass, there has not been yet a general consensus about the existence of extra-tidal structures around it. While some previous results claim for the absence of such features, others have shown that the cluster is under the effects of tidal stripping. From DECaLS g, r magnitudes of stars placed along the cluster Main Sequence in the color-magnitude diagram -previously corrected by interstellar reddening-, we built the cluster stellar density map. The resulting density map shows nearly smooth contours around Pal 13 out to ≈ 1.6 times the most recent estimate of its Jacobi radius, derived by taking into account its variation along its orbital motion. This outcome favors the presence of stars escaping the cluster, a phenomenon frequently seen in globular clusters that have crossed the Milky Way disc a comparable large number of times. Particularly, the orbital high eccentricity and large inclination angle of this accreted globular cluster could have been responsible for the relatively large amount of cluster mass lost.

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“…More recently a group of RAVE stars with radial velocities and chemical abundances consistent with stars observed from ω Centauri cluster has been detected by (Kunder et al 2014). As mentioned by Meza et al (2005), the presence of nearby stars with odd kinematics and chemistry, suggests an extra-Galactic origin for them, possibly what they call "tidal relics".…”

Section: Introductionmentioning

confidence: 85%

RAVE stars tidally stripped or ejected from theωCentauri globular cluster

Fernández-Trincado

Robin

Vieira³

et al. 2015

A&A

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Using six-dimensional phase-space information from the Fourth Data release of the RAdial Velocity Experiment (RAVE) over the range of Galactic longitude 240• < l < 360• and V LSR < −239 km s −1 , we computed orbits for 329 RAVE stars that were originally selected as chemically and kinematically related to ω Centauri. The orbits were integrated in a Milky-Way-like axisymmetric Galactic potential, ignoring the effects of the dynamical evolution of ω Centauri due to the tidal effects of the Galaxy disk on the cluster along time. We also ignored secular changes in the Milky Way potential over time. In a Monte Carlo scheme, and under the assumption that the stars may have been ejected with velocities greater than the escape velocity (V rel > V esc,0 ) from the cluster, we identified 15 stars as having close encounters with ω Centauri: (i) 8 stars with relative velocities V rel < 200 km s −1 may have been ejected ∼200 Myr ago from ω Centauri; (ii) another group of 7 stars were identified with high relative velocity V rel > 200 km s −1 during close encounters, and it seems unlikely that they were ejected from ω Centauri. We also confirm the link between J131340.4-484714 as a potential member of ω Centauri, and probably ejected ∼2.0 Myr ago, with a relative velocity V rel ∼ 80 km s −1 .

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Spectroscopic signatures of extratidal stars around the globular clusters NGC 6656 (M 22), NGC 3201, and NGC 1851 from RAVE

Cited by 48 publications

References 120 publications

Tycho-Gaia Astrometric Solution Parallaxes and Proper Motions for Five Galactic Globular Clusters

Tycho-Gaia Astrometric Solution Parallaxes and Proper Motions for Five Galactic Globular Clusters

Pal 13: its moderately extended low-density halo and its accretion history

RAVE stars tidally stripped or ejected from theωCentauri globular cluster

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