We explore a sample of 148 solar-like stars to search for a possible correlation between the slopes of the abundance trends versus condensation temperature (known as the Tc slope) with stellar parameters and Galactic orbital parameters in order to understand the nature of the peculiar chemical signatures of these stars and the possible connection

On 2010 August 20, an energetic disturbance triggered large-amplitude longitudinal oscillations in a nearby filament. The triggering mechanism appears to be episodic jets connecting the energetic event with the filament threads. In the present work, we analyze this periodic motion in a large fraction of the filament to characterize the underlying

Context. Gravity modifies the spectral features of young brown dwarfs (BDs). A proper characterization of these objects is crucial for the identification of the least massive and latest-type objects in star-forming regions, and to explain the origin(s) of the peculiar spectrophotometric properties of young directly imaged extrasolar planets and BD

The association of a star with the different galactic components determines on a first order its velocity within the Galaxy. This stellar motion influences the structure and dynamics of the ejected Asymptotic Giant Branch (AGB) envelope as the stellar mass loss interacts with the local interstellar medium (ISM). We have explore the effects that

Spectroscopic data of two relatively [O III]-luminous -PNe have been obtained with the 10.4-m Gran Telescopio Canarias. M174 and M2496 are each ˜1 degree from the center of M31 along opposite sides of its minor axis. The ensemble of these two distant PNe plus 16 similarly luminous outer-disk PNe published earlier (Kwitter et al. 2012 & 2013) forms

The Balloon-borne Large Aperture Submillimeter Telescope for Polarimetry (BLASTPol) was created by adding polarimetric capability to the BLAST experiment that was flown in 2003, 2005, and 2006. BLASTPol inherited BLAST's 1.8 m primary and its Herschel/SPIRE heritage focal plane that allows simultaneous observation at 250, 350, and 500 μm. We flew