Context. Recent studies show that barred galaxies have a light deficit, called a dark gap (DG), in the direction of the bar minor axis with respect to the major...
Evolution of dust temperature of galaxies through cosmic time as seen by Herschel
We study the dust properties of galaxies in the redshift range 0.1 ~ 5 × 1010Lsolar appears to be 2-5K colder than that of AKARI-selected local galaxies with...
Evolution of galaxy scaling relations in clusters at 0.5 < z < 1.5
Aims: We present new gas kinematic observations with the OSIRIS instrument at the GTC for galaxies in the Cl1604 cluster system at z ∼ 0.9. These observations...
Evolution of galaxy stellar masses and star formation rates in the EAGLE simulations
We investigate the evolution of galaxy masses and star formation rates in the Evolution and Assembly of Galaxies and their Environment (EAGLE) simulations...
Evolution of Stellar Bars in Live Axisymmetric Halos: Recurrent Buckling and Secular Growth
Evolution of stellar bars in disk galaxies is accompanied by dynamical instabilities and secular changes. Following the vertical buckling instability, the bars...
Evolution of Stellar Population: Environments vs galaxy interactions
Several authors have studied the dependence of galaxy properties on environment in order to understand which mechanisms operate in the galaxy evolution...
Evolution of structure in late-type spiral galaxies. I. Ionized gas kinematics in NGC 628
Aims:We study two dimensional Fabry-Perot interferometric observations of the nearby face-on late-type spiral galaxy, NGC 628, in order to analyse the ionized...
Evolution of Super Star Cluster Winds with Strong Cooling
We study the evolution of super star cluster winds driven by stellar winds and supernova explosions. Time-dependent rates at which mass and energy are deposited...
Evolution of the anti-truncated stellar profiles of S0 galaxies since z = 0.6 in the SHARDS survey. I. Sample and methods
Context. The controversy about the origin of the structure of early-type S0-E/S0 galaxies may be due to the difficulty of comparing surface brightness profiles...