Planetary dynamics in stellar clusters

In addition to their effect on the true abundance of clusters as a function of mass and redshift, cosmological parameters also affect the cluster observables through their in fluence

The minimum binary fraction of this cluster ( ∼ 14%) differs to the average fraction measured on the nearby clusters (∼ 44%). In order to better constrain this discrepancy, an

Surprisingly, it was already shown from microSQUID measurements performed on single Co clusters embedded in a Nb matrix that even if the CoNb shell is not magnetic, the Co

Results: In the present work, five clusters have been studied: a cluster of thirteen genes characterized by an F-box domain localized on chromosome 9, a cluster of six genes related

A single-burst model with formation redshift of 3, calibrated on the CMR of the nearby Coma cluster, provides a good fit to the red sequence observed over the full redshift

Cluster passive ETGs are on average larger at z ∼ 1 and present a less steep evolution than field galaxies at fixed stellar mass.. We notice that the Newman