We present outburst spectroscopy of GX 339-4 that may reveal the motion of its elusive companion star. N III lines exhibit sharp emission components moving over...
Dynamical evidence for a black hole in the X-ray transient QZ VUL (=GS 2000+25)
We report the first spectroscopic detection of the secondary star in the X-ray transient QZ Vul (=GS 2000+25). Cross-correlation of individual spectra against K...
Dynamical evolution of globular cluster systems in clusters of galaxies - I. The case of NGC 1404 in the Fornax cluster
We investigate, via numerical simulations, the tidal stripping and accretion of globular clusters (GCs). In particular, we focus on creating models that...
Dynamical evolution of two associated galactic bars
We study the dynamical interactions of mass systems in equilibrium under their own gravity that mutually exert and experience gravitational forces. The method...
Dynamical mass of the white dwarf in XY Ari: a test for intermediate polar X-ray spectral models
We present a dynamical study of the eclipsing intermediate polar XY Ari based on time-resolved near-infrared spectroscopy obtained with the EMIR spectrograph on...
Dynamical masses and non-homology of massive elliptical galaxies grown by dry mergers
We study whether dry merger-driven size growth of massive elliptical galaxies depends on their initial structural concentration, and analyse the validity of the...
Dynamical masses of a nova-like variable on the edge of the period gap
We present the first dynamical determination of the binary parameters of an eclipsing SW Sextantis star in the 3-4 h orbital period range during a low state. We...
Dynamical Masses of the Binary Brown Dwarf GJ 569 Bab
We have obtained new images and high-resolution (R~22,400) near-infrared (1.2400-1.2575 μm) spectra of each component of the brown dwarf binary GJ 569 Bab using...
Dynamical masses of two young transiting sub-Neptunes orbiting HD 63433
Context. Although the number of exoplanets reported in the literature exceeds 5000 so far, only a few dozen of them are young planets (≤900 Myr). However, a...