Aims. Our goal is to provide a wide ultracool companion frequency for metal-poor halo stars for the first time. Methods. We selected nearby halo stars with...
HST Astrometry in the 30 Doradus Region. II. Runaway Stars from New Proper Motions in the Large Magellanic Cloud
We present a catalog of relative proper motions for 368,787 stars in the 30 Doradus region of the Large Magellanic Cloud (LMC), based on a dedicated two-epoch...
Hubble Space Telescope Observations of an Outer Field in Omega Centauri: A Definitive Helium Abundance
We revisit the problem of the split main sequence (MS) of the globular cluster ω Centauri, and report the results of two-epoch Hubble Space Telescope...
Low-mass stars and brown dwarfs in Praesepe (Baker+, 2010)
Presented are the results of a large and deep optical-near-infrared multi-epoch survey of the Praesepe open star cluster using data from the UKIRT Infrared Deep...
Mass function of IC4665 from UKIDSS-GCS (Lodieu+, 2011)
Knowledge of the mass function in open clusters constitutes one way to constrain the formation of low-mass stars and brown dwarfs along with the knowledge of...
Origin of the Proper Motions of Emerging Bipolar Magnetic Regions
We have performed numerical simulations of the rise of magnetic flux tubes through the convection zone. We find that the observed proper motions of pores and...
Proper Motions and Orbits of Distant Local Group Dwarf Galaxies from a Combination of Gaia and Hubble Data
We have determined the proper motions (PMs) of 12 dwarf galaxies in the Local Group (LG), ranging from the outer Milky Way (MW) halo to the edge of the LG. We...
Proper motions of field L and T dwarfs (Jameson+, 2008)
In order to measure proper motions for known L and T dwarfs we observed 142 L and T dwarfs from the DwarfArchive (detailed in Table 1, see http://spider.ipac...
Search and characterization of T-type planetary mass candidates in the σ Orionis cluster
Context. The proper characterization of the least massive population of the young σ Orionis star cluster is required to understand the form of the cluster mass...