The Evolution of the Mass-Size relation to z = 3.5 in the GOODS
... in narrow mass bins for all galaxies from CDF-S. The UV bright galaxies are in general larger than normal field galaxies at the same mass. ...
... in narrow mass bins for all galaxies from CDF-S. The UV bright galaxies are in general larger than normal field galaxies at the same mass. ...
Transverse and Longitudinal Correlation Functions in the
... photoionised Intergalactic Medium distributed as expected in a CDM model explains the statistical properties of individual QSO absorption spectra very well. Most of the baryons are located in filaments and sheets which are only overdense by factors of a few and produce absorption in the column densi ...
... photoionised Intergalactic Medium distributed as expected in a CDM model explains the statistical properties of individual QSO absorption spectra very well. Most of the baryons are located in filaments and sheets which are only overdense by factors of a few and produce absorption in the column densi ...
the discovery of a massive cluster of red supergiants with glimpse
... in the diffuse emission, possibly a cavity sculpted by the winds and energetic photons from young massive stars. Infrared dark clouds (IRDCs) and dark filaments appear superimposed on the bright diffuse background at many locations across this field, indicating the presence of opaque, cold clouds in ...
... in the diffuse emission, possibly a cavity sculpted by the winds and energetic photons from young massive stars. Infrared dark clouds (IRDCs) and dark filaments appear superimposed on the bright diffuse background at many locations across this field, indicating the presence of opaque, cold clouds in ...
PPT presentation
... We have a “toy-model” to make predictions of the M/L trend in the LCDM framework, to be compared with future PNe observations AND other dynamical tracers (GCs, Xrays, lensing). Thanks to the PN.S statistical samples of PN radial velocities are reaching the precision which will allow to discriminate ...
... We have a “toy-model” to make predictions of the M/L trend in the LCDM framework, to be compared with future PNe observations AND other dynamical tracers (GCs, Xrays, lensing). Thanks to the PN.S statistical samples of PN radial velocities are reaching the precision which will allow to discriminate ...
three-body dynamics with gravitational wave emission
... that can be produced with roughly solar metallicity stellar evolution (Fryer & Kalogera 2001). The ULXs are thought to be powered by black holes because many are variable, but they cannot be powered by supermassive black holes or they would have sunk to the center of their host galaxies because of d ...
... that can be produced with roughly solar metallicity stellar evolution (Fryer & Kalogera 2001). The ULXs are thought to be powered by black holes because many are variable, but they cannot be powered by supermassive black holes or they would have sunk to the center of their host galaxies because of d ...
Properties of simulated Milky Way-mass galaxies in loose group and
... A rich literature exists comparing simulated field disk galaxies with observations of the Milky Way (e.g. Brook et al. 2004; Scannapieco et al. 2005; Sánchez-Blázquez et al. 2009; Kobayashi & Nakasato 2011; House et al. 2011; Guedes et al. 2011). The purpose of our work here is to determine whether ...
... A rich literature exists comparing simulated field disk galaxies with observations of the Milky Way (e.g. Brook et al. 2004; Scannapieco et al. 2005; Sánchez-Blázquez et al. 2009; Kobayashi & Nakasato 2011; House et al. 2011; Guedes et al. 2011). The purpose of our work here is to determine whether ...
A fundamental metallicity relation for galaxies at z = 0.84–1.47 from
... allows for the placement of up to 400 1.2 arcsec diameter fibres within a 30 arcmin diameter circular field of view and the light ...
... allows for the placement of up to 400 1.2 arcsec diameter fibres within a 30 arcmin diameter circular field of view and the light ...
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.