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 ...
Summary - X-ray Astronomy Group at ISAS
... • angular resolution • sensitivity XMM/Chandra are ideally suited for • extending previous studies to fainter, higher redshift, higher – and lower luminosity systems • detailed studies of many bright low redshift objects. • critical progress in the temporal/spectral domain Combined with other facili ...
... • angular resolution • sensitivity XMM/Chandra are ideally suited for • extending previous studies to fainter, higher redshift, higher – and lower luminosity systems • detailed studies of many bright low redshift objects. • critical progress in the temporal/spectral domain Combined with other facili ...
SN Ia host galaxy properties and the dust extinction
... underlying AV distribution, but rather to explore how the observed distribution relates to host galaxy observables to ascertain which host galaxy property should have priority in future SN Ia surveys. The SDSS-SN fits used in this analysis made use of a particular extinction distribution as a prior, ...
... underlying AV distribution, but rather to explore how the observed distribution relates to host galaxy observables to ascertain which host galaxy property should have priority in future SN Ia surveys. The SDSS-SN fits used in this analysis made use of a particular extinction distribution as a prior, ...
Lyman Break Galaxies at z~ 5: Luminosity Function
... well as the rest-frame photometric data points of LBGs at z ∼ 3 in the HDF-N (Papovich et al. 2001). The model spectra reasonably cover the UV colors of the LBGs at z ∼ 3. The adoption of the dust extinction is rather arbitrary to reproduce the redder colors of LBGs. The interpretation is, however, ...
... well as the rest-frame photometric data points of LBGs at z ∼ 3 in the HDF-N (Papovich et al. 2001). The model spectra reasonably cover the UV colors of the LBGs at z ∼ 3. The adoption of the dust extinction is rather arbitrary to reproduce the redder colors of LBGs. The interpretation is, however, ...
A re-examination of galactic conformity and a comparison with semi
... of the effect and how it changes as a function of the mass of the central galaxy. Conformity extends over a central galaxy stellar mass range spanning two orders of magnitude. The scale dependence and the precise nature of the effect depend on the mass of the central. In central galaxies with masses ...
... of the effect and how it changes as a function of the mass of the central galaxy. Conformity extends over a central galaxy stellar mass range spanning two orders of magnitude. The scale dependence and the precise nature of the effect depend on the mass of the central. In central galaxies with masses ...
Feedback in low-mass galaxies in the early Universe
... the evolution of galaxies during the peak epoch of star formation, with a variety of important consequences for the properties of galaxies and the intergalactic medium. These consequences include the shape of the relationship between the heavy-element content of galaxies and their mass; in both loca ...
... the evolution of galaxies during the peak epoch of star formation, with a variety of important consequences for the properties of galaxies and the intergalactic medium. These consequences include the shape of the relationship between the heavy-element content of galaxies and their mass; in both loca ...
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.