The star formation history of galaxies in 3D: CALIFA perspective
... One step to understand how galaxies form and evolve is classifying galaxies and studying their properties. Most of the massive galaxies in the near Universe are E, S0 and spirals (Blanton & Moustakas 2009), following well the Hubble tuning-fork diagram. The bulge fraction seems to be one of the main ...
... One step to understand how galaxies form and evolve is classifying galaxies and studying their properties. Most of the massive galaxies in the near Universe are E, S0 and spirals (Blanton & Moustakas 2009), following well the Hubble tuning-fork diagram. The bulge fraction seems to be one of the main ...
Dust and Molecules in Early Galaxies
... Consider a protogalactic cloud of M ~ 1011 Msun. Since the radius R is a few kpc in this case, we have its column density ...
... Consider a protogalactic cloud of M ~ 1011 Msun. Since the radius R is a few kpc in this case, we have its column density ...
MAPPING THE GALAXY DISTRIBUTION AT LARGE DISTANCES1
... tangential direction (at z 1 0.18, 0.29, 0.31). The typical diameter of voids as defined by the spacing between sharp structures appears to be in the range 120 –50 h 21 Mpc. These maps closely resemble the expected structure from an underlying distribution dominated by voids and walls of galaxies as ...
... tangential direction (at z 1 0.18, 0.29, 0.31). The typical diameter of voids as defined by the spacing between sharp structures appears to be in the range 120 –50 h 21 Mpc. These maps closely resemble the expected structure from an underlying distribution dominated by voids and walls of galaxies as ...
Cosmology with objects from the Hamburg Quasar Surveys
... which accurate abundances can be obtained only with knowledge of the spectral energy distribution (SED) of the ionizing background. Consequently, one has to admit that the metallicity of the largest part of the baryons is at present not known. The direct measurement of the SED is possible only in ab ...
... which accurate abundances can be obtained only with knowledge of the spectral energy distribution (SED) of the ionizing background. Consequently, one has to admit that the metallicity of the largest part of the baryons is at present not known. The direct measurement of the SED is possible only in ab ...
THE EVOLUTION OF BIAS ABSTRACT Bias in the
... the degree of biasing decreases at larger expansion factors, but they do not quantify the effect. There has been no study to date of the evolution of the three-point correlation function or the bispectrum for such a tagged subset. It is important to separate a physical bias at the time of galaxy for ...
... the degree of biasing decreases at larger expansion factors, but they do not quantify the effect. There has been no study to date of the evolution of the three-point correlation function or the bispectrum for such a tagged subset. It is important to separate a physical bias at the time of galaxy for ...
Discovery of the host galaxy of HDF850. 1, the brightest sub
... redshift than these identified sources. The strongest hint of this comes from the fact that these now identified SCUBA sources have been detected in the radio at S1.4GHz > 50 µJy, whereas HDF850.1 has evaded radio detection at the level of S1.4GHz < 23 µJy (3-σ). The radio investigation of HDF850.1 ...
... redshift than these identified sources. The strongest hint of this comes from the fact that these now identified SCUBA sources have been detected in the radio at S1.4GHz > 50 µJy, whereas HDF850.1 has evaded radio detection at the level of S1.4GHz < 23 µJy (3-σ). The radio investigation of HDF850.1 ...
SOME CONSTRAINTS ON GALAXY EVOLUTION IMPOSED BY
... somewhat mitigated by the fact that the young stellar populations in disk galaxies fade as they evolve. As a result, the specific globular cluster frequency, i.e. the number of clusters per unit luminosity, will increase with time. However, this effect is partly compensated for by the apparent brigh ...
... somewhat mitigated by the fact that the young stellar populations in disk galaxies fade as they evolve. As a result, the specific globular cluster frequency, i.e. the number of clusters per unit luminosity, will increase with time. However, this effect is partly compensated for by the apparent brigh ...
Galaxies and the Universe
... If you enjoy science fiction, you might have read about explorers traveling through the galaxy. On their way, they visit planets around other stars and encounter strange alien beings. Although this type of space exploration is futuristic, it is possible to explore galaxies today. Using a variety of ...
... If you enjoy science fiction, you might have read about explorers traveling through the galaxy. On their way, they visit planets around other stars and encounter strange alien beings. Although this type of space exploration is futuristic, it is possible to explore galaxies today. Using a variety 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.