On the structure of tidal tails

Küpper, Andreas H. W.; Macleod, Andrew; Heggie, Douglas C.

doi:10.1111/j.1365-2966.2008.13323.x

Cited by 130 publications

(197 citation statements)

References 23 publications

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“…4. This kinematic process, described and studied in a number of papers (Küpper et al 2008;Just et al 2009;Kupper et al 2010Kupper et al , 2012Lane et al 2012), is applied here for the first time to reproduce observed stellar streams, including both the position and the intensity of the observed stellar inhomogeneities. Also the absence of overdensities in the trailing tail at distances greater than 4 • -5 • is simply because we have integrated Pal 5's orbit for the last ∼3 Gyr.…”

Section: Resultsmentioning

confidence: 99%

“…When analyzing a set of simulations of GCs orbiting in a triaxial potential, Capuzzo-Dolcetta et al (2005) and proposed an alternative explanation, suggesting for the first time that the clumps observed in their simulations were instead kinematic effects, related to a local deceleration in the motion of stars along the tails. Küpper et al (2008), Just et al (2009), and more recently Küpper et al (2010Küpper et al ( , 2012 and Lane et al (2012) show that these kinematic effects and local decelerations correspond to "epicyclic cusps", where stars escaping from the cluster slow down in their epicyclic motion, as seen in the cluster reference frame. Because stars cross the tidal boundary with similar position and velocities, the location of such epicyclic cusps is similar for most escapers, generating visible overdensities.…”

Section: Introductionmentioning

confidence: 99%

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Clumpy streams in a smooth dark halo: the case of Palomar 5

Mastrobuono-Battisti

Matteo

Montuori

et al. 2012

A&A

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By means of direct N-body simulations and simplified numerical models, we study the formation and characteristics of the tidal tails around Palomar 5, along its orbit in the Milky Way potential. Unlike previous findings, we are able to reproduce the substructures observed in the stellar streams of this cluster, without including any lumpiness in the dark matter halo. We show that overdensities similar to those observed in Palomar 5 can be reproduced by the epicyclic motion of stars along its tails, i.e. a simple local accumulation of orbits of stars that escaped from the cluster with very similar positions and velocities. This process is able to form stellar clumps at distances of several kiloparsecs from the cluster, so it is not a phenomenon confined to the inner part of Palomar 5's tails, as previously suggested. Our models can reproduce the density contrast between the clumps and the surrounding tails found in the observed streams, without including any lumpiness in the dark halo, suggesting new upper limits on its granularity.

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Section: Resultsmentioning

confidence: 99%

Section: Introductionmentioning

confidence: 99%

Clumpy streams in a smooth dark halo: the case of Palomar 5

Mastrobuono-Battisti

Matteo

Montuori

et al. 2012

A&A

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“…In the case of star clusters, escaping orbits form so-called tidal tails (Odenkirchen et al 2003;Di Matteo et al 2005;Küpper et al 2008;Just et al 2009;Ernst 2009;Küpper et al 2010;Berentzen & Athanassoula 2012). Based on the similarity of the correspondig effective potentials, we would like to point out here the striking similarity between spiral arms of barred spiral galaxies and star cluster tidal tails and mention the hypothesis that the spiral arms of barred spiral galaxies such as NGC 1300 are the equivalent of such star cluster tidal tails forming in an effective potential similar to that of Eqn.…”

Section: Spiral Armsmentioning

confidence: 99%

“…In such a way we simulate a real N -body simulation of such a system: The density of particles will be highest where the velocity is lowest. Similarly, clumps form in tidal tails of star clusters at positions where the velocity of the escaping particles is lowest (Küpper et al 2008).…”

Section: Spiral Armsmentioning

confidence: 99%

Fractal basins of escape and the formation of spiral arms in a galactic potential with a bar

Ernst¹,

Peters²

2014

Monthly Notices of the Royal Astronomical Society

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We investigate the dynamics in the close vicinity of and within the critical area in a 2D effective galactic potential with a bar of Zotos. We have calculated Poincaré surfaces of section and the basins of escape. In both the Poincaré surfaces of section and the basins of escape we find numerical evidence for the existence of a separatrix which hinders orbits from escaping out of the bar region. We present numerical evidence for the similarity between spiral arms of barred spiral galaxies and tidal tails of star clusters.

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“…The clumps are not self-gravitating systems. Küpper et al (2008) showed that the clumps are a result of epicyclic motion of the stars lost by the cluster. Just et al (2009) investigated the formation of the clumps and discussed their observability.…”

Section: Introductionmentioning

confidence: 99%

Search for extratidal features around 17 globular clusters in the Sloan Digital Sky Survey

Jordi

Grebel

2010

A&A

110

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Context. The dynamical evolution of a single globular cluster and also of the entire Galactic globular cluster system has been studied theoretically in detail. In particular, simulations show how the "lost" stars are distributed in tidal tails emerging from the clusters. Aims. We investigate the distribution of Galactic globular cluster stars on the sky to identify such features as tidal tails. The Sloan Digital Sky Survey provides consistent photometry of a large part of the sky to study the projected two-dimensional structure of the 17 globular clusters in its survey area. Methods. We used a color-magnitude weighted counting algorithm to map (potential) cluster member stars on the sky. Results. We recover the already known tidal tails of Pal 5 and NGC 5466. For NGC 4147 we find a two-arm morphology. Possible indications of tidal tails are also seen around NGC 5053 and NGC 7078, confirming earlier suggestions. Moreover, we find potential tails around NGC 5904 and Pal 14. Especially for Palomar clusters other than Pal 5, deeper data are needed to confirm or to rule out the existence of tails. For many of the remaining clusters in our sample we observe a pronounced extratidal halo, which is particularly large for NGC 7006 and Pal 1. In some cases, the extratidal halos may be associated with the stream of the Sagittarius dwarf spheroidal galaxy (e.g., NGC 4147, NGC 5024, NGC 5053).

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On the structure of tidal tails

Cited by 130 publications

References 23 publications

Clumpy streams in a smooth dark halo: the case of Palomar 5

Clumpy streams in a smooth dark halo: the case of Palomar 5

Fractal basins of escape and the formation of spiral arms in a galactic potential with a bar

Search for extratidal features around 17 globular clusters in the Sloan Digital Sky Survey

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