Active Galactic Nuclei at kiloparsec scales and their cosmological
... Besides being among the brightest objects in the universe, AGN are further characterised by being strong emitters at any range of the electromagnetic spectrum. The power of these sources is based on the availability of material in their immediate surroundings, host galaxy, and/or circumgalactic medi ...
... Besides being among the brightest objects in the universe, AGN are further characterised by being strong emitters at any range of the electromagnetic spectrum. The power of these sources is based on the availability of material in their immediate surroundings, host galaxy, and/or circumgalactic medi ...
Mnassa Report 2005 - (UCT)
... previously for this galaxy and will be analysed in detail, in combination with the GALEV models (see galaxy transformation at intermediate redshift below), to determine the star-formation history of this peculiar galaxy. To further our understanding of the Great Attractor (GA), Woudt and Kraan-Korte ...
... previously for this galaxy and will be analysed in detail, in combination with the GALEV models (see galaxy transformation at intermediate redshift below), to determine the star-formation history of this peculiar galaxy. To further our understanding of the Great Attractor (GA), Woudt and Kraan-Korte ...
The Milky Way and Andromeda galaxies in a constrained
... Despite the recent progress, the Aquila code comparison project (Scannapieco et al. 2012) showed that, even when the formation history of a halo is fully specified, different models predict the formation of a galaxy with different gas fractions, morphologies, stellar masses and angular momentum conten ...
... Despite the recent progress, the Aquila code comparison project (Scannapieco et al. 2012) showed that, even when the formation history of a halo is fully specified, different models predict the formation of a galaxy with different gas fractions, morphologies, stellar masses and angular momentum conten ...
REVIEWS 18 years of science with the Hubble Space Telescope Julianne J. Dalcanton
... reducing the uncertainties in Cepheid-based distances. Although this period–luminosity relationship may potentially vary with the metallicity of the galaxy2, with appropriate corrections it can reliably be used for many massive spiral galaxies. Previously, climbing from reliable parallax measurement ...
... reducing the uncertainties in Cepheid-based distances. Although this period–luminosity relationship may potentially vary with the metallicity of the galaxy2, with appropriate corrections it can reliably be used for many massive spiral galaxies. Previously, climbing from reliable parallax measurement ...
STAR CLUSTERS M. Ramella e G. Iafrate INAF – Astronomical
... M45 can be clearly seen also by naked eye. When we look at these clusters on the sky, we observe a variety of densities and sizes, but it is important to remember that these differences may be only apparent since they depend on the different distances from us of the objects. This is a common situati ...
... M45 can be clearly seen also by naked eye. When we look at these clusters on the sky, we observe a variety of densities and sizes, but it is important to remember that these differences may be only apparent since they depend on the different distances from us of the objects. This is a common situati ...
N-body Simulations and Galaxy Formation
... and, later on, Negroponte & White (1983) were among the first who performed self-consistent merger simulations of disk galaxies. However, the resolution of these simulations was very low and the number of particles representing each galaxy did not exceed 500. The situation changed with the advent of ...
... and, later on, Negroponte & White (1983) were among the first who performed self-consistent merger simulations of disk galaxies. However, the resolution of these simulations was very low and the number of particles representing each galaxy did not exceed 500. The situation changed with the advent of ...
Weak gravitational lensing
While the presence of any mass bends the path of light passing near it, this effect rarely produces the giant arcs and multiple images associated with strong gravitational lensing. Most lines of sight in the universe are thoroughly in the weak lensing regime, in which the deflection is impossible to detect in a single background source. However, even in these cases, the presence of the foreground mass can be detected, by way of a systematic alignment of background sources around the lensing mass. Weak gravitational lensing is thus an intrinsically statistical measurement, but it provides a way to measure the masses of astronomical objects without requiring assumptions about their composition or dynamical state.