The Balloon-borne Large Aperture Submillimeter Telescope
... arrays being developed for Herschel. The combination of northern and southern hemisphere LDB flights, providing the first surveys at 250, 350 and 500 µm, will significantly extend the wavelength range, sensitivity, and area of existing ground-based extragalactic and galactic surveys. Compared to the pi ...
... arrays being developed for Herschel. The combination of northern and southern hemisphere LDB flights, providing the first surveys at 250, 350 and 500 µm, will significantly extend the wavelength range, sensitivity, and area of existing ground-based extragalactic and galactic surveys. Compared to the pi ...
The VLT LEGA-C Spectroscopic Survey: The Physics of Galaxies at
... typically well over 5 Gyr and it is difficult to resolve star formation histories from integrated spectra. Now LEGA-C is obtaining spectra of similar quality for ∼3200 K-band selected galaxies in the redshift range 0.6 < z < 1.0, at a look-back time of 6 − 8 Gyr. LEGA-C is a 4-year, 128-night Public ...
... typically well over 5 Gyr and it is difficult to resolve star formation histories from integrated spectra. Now LEGA-C is obtaining spectra of similar quality for ∼3200 K-band selected galaxies in the redshift range 0.6 < z < 1.0, at a look-back time of 6 − 8 Gyr. LEGA-C is a 4-year, 128-night Public ...
Document
... and disk thickness along the line of the sight cause confusion of gas with smaller velocities than the terminal one, which often results in a lower rotation velocity in the former two methods. Problems : ET method is ill-defined when applied to the innermost part of a PV diagram. This is a consequ ...
... and disk thickness along the line of the sight cause confusion of gas with smaller velocities than the terminal one, which often results in a lower rotation velocity in the former two methods. Problems : ET method is ill-defined when applied to the innermost part of a PV diagram. This is a consequ ...
DEDUCING THE LIFETIME OF SHORT GAMMA
... Sky Survey (SDSS). The Bell et al. catalog provides welldefined samples of galaxies of different spectral types as defined by either the light concentration or the color of galaxies. In Figure 1, we show the stellar MF, φ, multiplied by the stellar mass, Mstar , for galaxies of different spectral ty ...
... Sky Survey (SDSS). The Bell et al. catalog provides welldefined samples of galaxies of different spectral types as defined by either the light concentration or the color of galaxies. In Figure 1, we show the stellar MF, φ, multiplied by the stellar mass, Mstar , for galaxies of different spectral ty ...
Dark Matter Capture in the first stars
... continues for a longer time Are there still some dark stars around today? ...
... continues for a longer time Are there still some dark stars around today? ...
Instrument Proposal Document
... When observing in scanning mode, it takes several hours to complete scans and as such, the observations are susceptible to changes in seeing and transparency between individual frames. The result is that the profile of the scanned line will be biased, unless the scan is rapid enough so that it can t ...
... When observing in scanning mode, it takes several hours to complete scans and as such, the observations are susceptible to changes in seeing and transparency between individual frames. The result is that the profile of the scanned line will be biased, unless the scan is rapid enough so that it can t ...
Open access
... the source, suggesting that the blend is likely to be the lens. Although we find planetary signals for none of events, we provide exclusion diagrams showing the confidence levels excluding the existence of a planet as a function of the separation and mass ratio. ...
... the source, suggesting that the blend is likely to be the lens. Although we find planetary signals for none of events, we provide exclusion diagrams showing the confidence levels excluding the existence of a planet as a function of the separation and mass ratio. ...
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.