With the use of N-body calculations, the numbers and properties of escaping stars from low-N (N= 100 and 1000) young embedded star clusters prior to gas...
ESO Very Large Telescope Optical Spectroscopy of BL Lacertae Objects. I. New Redshifts
We report redshift measurements for 12 BL Lacertae objects from a program aimed at obtaining high signal-to-noise ratio (up to ~500) optical spectroscopy of a...
ESO Very Large Telescope Optical Spectroscopy of BL Lacertae Objects. II. New Redshifts, Featureless Objects, and Classification Assessments
We report on ESO Very Large Telescope optical spectroscopy of 42 BL Lacertae objects of unknown redshift. Nuclear emission lines were observed in 12 objects...
ESPRESSO at VLT. On-sky performance and first results
Context. ESPRESSO is the new high-resolution spectrograph of ESO's Very Large Telescope (VLT). It was designed for ultra-high radial-velocity (RV) precision and...
ESPRESSO high-resolution transmission spectroscopy of WASP-76 b
Aims: We report on ESPRESSO high-resolution transmission spectroscopic observations of two primary transits of the highly irradiated, ultra-hot Jupiter-sized...
ESPRESSO highlights the binary nature of the ultra-metal-poor giant HE 0107-5240
Context. The vast majority of the known stars of ultra low metallicity ([Fe/H] < -4.5) are known to be enhanced in carbon, and belong to the "low-carbon band"...
ESPRESSO mass determination of TOI-263b: an extreme inhabitant of the brown dwarf desert
The TESS mission has reported a wealth of new planetary systems around bright and nearby stars amenable for detailed characterizations of planet properties and...
ESPRESSO observations of HE 0107−5240 and other CEMP-no stars with [Fe/H] ≤ -4.5
Context. HE 0107−5240 is a hyper metal-poor star with [Fe/H] = −5.39, one of the lowest-metallicity stars known. Its stellar atmosphere is enhanced in carbon...
ESPRESSO reveals blueshifted neutral iron emission lines on the dayside of WASP-76 b
Context. Ultra hot Jupiters (gas giants with T eq > 2000 K) are intriguing exoplanets due to the extreme physics and chemistry present in their atmospheres...