Dark matter distribution and indirect detection in dwarf spheroidal
... Median value + Cls are not affected by the parametrisation Independent on sample size ...
... Median value + Cls are not affected by the parametrisation Independent on sample size ...
The Milky Way galaxy Contents Summary
... Galaxies vary enormously in size from objects that contain only 100 000 stars, to ones with hundreds of billions of stars. The smaller galaxies are much more numerous than the larger ones, but not by a sufficient factor to compensate for their lower luminosities. So most of the luminosity in the Uni ...
... Galaxies vary enormously in size from objects that contain only 100 000 stars, to ones with hundreds of billions of stars. The smaller galaxies are much more numerous than the larger ones, but not by a sufficient factor to compensate for their lower luminosities. So most of the luminosity in the Uni ...
and galaxies
... 50 parsecs and contain up to 106 solar masses. Inside the GMCs are more hot and dense cores with dimensions of 0.05-1 parsec, T~100-200K and densities of 107-109 /cm3. 1000s of GMC are known in our galaxy, mostly in the spiral arms ...
... 50 parsecs and contain up to 106 solar masses. Inside the GMCs are more hot and dense cores with dimensions of 0.05-1 parsec, T~100-200K and densities of 107-109 /cm3. 1000s of GMC are known in our galaxy, mostly in the spiral arms ...
Euclid - at www.arxiv.org.
... leading position to address a most fascinating question that may revolutionise physics. Primary Science Objectives: Our understanding of cosmology is that of the Universe evolving from a homogeneous state after the Big Bang to a hierarchical assembly of galaxies, clusters and superclusters at our ep ...
... leading position to address a most fascinating question that may revolutionise physics. Primary Science Objectives: Our understanding of cosmology is that of the Universe evolving from a homogeneous state after the Big Bang to a hierarchical assembly of galaxies, clusters and superclusters at our ep ...
Objective Classification of Galaxy Spectra using the Information Bottleneck Method
... galaxies into classes. These classes are obtained such that they maximally preserve the original information between the galaxies and their spectra. The end goal of galaxy classification is a better understanding of the physical origin of different populations and how they relate to one another. In ...
... galaxies into classes. These classes are obtained such that they maximally preserve the original information between the galaxies and their spectra. The end goal of galaxy classification is a better understanding of the physical origin of different populations and how they relate to one another. In ...
PRESENT-DAY CLUSTER FORMATION
... full content and extent of the Trapezium cluster have become apparent only with the advent of infrared array photographs, which have shown that it contains more than 500 stars in a highly centrally concentrated and approximately symmetrical distribution centered on the Trapezium (McCaughrean 1989; M ...
... full content and extent of the Trapezium cluster have become apparent only with the advent of infrared array photographs, which have shown that it contains more than 500 stars in a highly centrally concentrated and approximately symmetrical distribution centered on the Trapezium (McCaughrean 1989; M ...
Head–tail Galaxies: beacons of high
... believed to be formed via ram pressure in the cases where the host galaxy has a peculiar velocity of the order of 600 km s−1 and is embedded in a hot, dense plasma (Venkatesan et al. 1994), and wide-angle tailed galaxies (WATs) believed to be the result of ‘cluster weather’ (Klamer et al. 2004). NAT ...
... believed to be formed via ram pressure in the cases where the host galaxy has a peculiar velocity of the order of 600 km s−1 and is embedded in a hot, dense plasma (Venkatesan et al. 1994), and wide-angle tailed galaxies (WATs) believed to be the result of ‘cluster weather’ (Klamer et al. 2004). NAT ...
cast-of-characters
... (as they appear) [The Unknown Thief #2] - Believed to be the mastermind behind a series of thefts, this villain always seems to be a step ahead of the game. Stealing some of Megacorp’s latest gadgets and weaponry and transits, it is still unknown what these things will be used for. What is known abo ...
... (as they appear) [The Unknown Thief #2] - Believed to be the mastermind behind a series of thefts, this villain always seems to be a step ahead of the game. Stealing some of Megacorp’s latest gadgets and weaponry and transits, it is still unknown what these things will be used for. What is known abo ...
Stellar interactions in dense and sparse star clusters
... et al. 2005; Moeckel & Bally 2006, 2007b; Kley et al. 2008), only a few numerical studies have directly investigated the effect of stellar encounters on circumstellar discs in a dense cluster environment (Scally & Clarke 2001; Adams et al. 2006). It has been shown only recently by numerical simulatio ...
... et al. 2005; Moeckel & Bally 2006, 2007b; Kley et al. 2008), only a few numerical studies have directly investigated the effect of stellar encounters on circumstellar discs in a dense cluster environment (Scally & Clarke 2001; Adams et al. 2006). It has been shown only recently by numerical simulatio ...
THE DISRUPTION OF STELLAR CLUSTERS CONTAINING
... is part of the collapsing core, we add its mass to a growing central point mass and remove it from the simulation. This central point mass is then used only during the calculation of the cluster gravitational potential. We determine whether a star is part of the collapsing core by monitoring its orb ...
... is part of the collapsing core, we add its mass to a growing central point mass and remove it from the simulation. This central point mass is then used only during the calculation of the cluster gravitational potential. We determine whether a star is part of the collapsing core by monitoring its orb ...
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.