On the Plausibility of an Upper Bound Uncertainty Principle
... the reading Nyambuya (2014b), where it has been argued that photons may very well be massive with this mass being so small that it would require much more sensitive measurements than presently obtaining if we are to detect it. If photons are massive, this would cause some problems with the Standard ...
... the reading Nyambuya (2014b), where it has been argued that photons may very well be massive with this mass being so small that it would require much more sensitive measurements than presently obtaining if we are to detect it. If photons are massive, this would cause some problems with the Standard ...
Environment and self-regulation in galaxy formation
... per cent of all objects, at least 20 indices were included in the fit. The average errors in log(age), metallicity, and [α/Fe] ratio are 0.10 dex, 0.07 dex, and 0.06 dex, respectively. The error distributions are well approximated by Gaussian functions with standard deviations of 0.04, 0.02, and 0.0 ...
... per cent of all objects, at least 20 indices were included in the fit. The average errors in log(age), metallicity, and [α/Fe] ratio are 0.10 dex, 0.07 dex, and 0.06 dex, respectively. The error distributions are well approximated by Gaussian functions with standard deviations of 0.04, 0.02, and 0.0 ...
Lyman Break Galaxies at z~ 5: Luminosity Function
... choose the sky area including the Hubble Deep Field-North (HDF-N; Williams et al. 1996), because there is plenty of information of galaxies with a wide redshift range (0 < z < 6). This database is quite powerful to examine our method for searching for galaxies at z ∼ 5 and to obtain a reliable sampl ...
... choose the sky area including the Hubble Deep Field-North (HDF-N; Williams et al. 1996), because there is plenty of information of galaxies with a wide redshift range (0 < z < 6). This database is quite powerful to examine our method for searching for galaxies at z ∼ 5 and to obtain a reliable sampl ...
Inverse Square Law
... From everyday experience, it is obvious that light sources appear to become brighter as you move closer to them. The apparent brightness of the source is related to its distance. However, moving a light source twice as close to you does not make it twice as bright. In this lab, we will examine this ...
... From everyday experience, it is obvious that light sources appear to become brighter as you move closer to them. The apparent brightness of the source is related to its distance. However, moving a light source twice as close to you does not make it twice as bright. In this lab, we will examine this ...
Extragalactic Globular Cluster Systems
... The globular clusters that were once within the merging protogalaxies are so dense that they survive intact and will orbit freely within the Galaxy. The surviving protogalaxies may be the precursors of the old satellite galaxies, some of which host old globular clusters such as Fornax, whose morphol ...
... The globular clusters that were once within the merging protogalaxies are so dense that they survive intact and will orbit freely within the Galaxy. The surviving protogalaxies may be the precursors of the old satellite galaxies, some of which host old globular clusters such as Fornax, whose morphol ...
Einstein, Black Holes and Gravity Waves, oh my! (x)
... • If I have a star, or black hole, just sitting in space then other things know where it is because of the curvature of space-time • If its just sitting there (or moving with a constant velocity) space-time isn’t changing • If it accelerates, then this information is passed through space-time at the ...
... • If I have a star, or black hole, just sitting in space then other things know where it is because of the curvature of space-time • If its just sitting there (or moving with a constant velocity) space-time isn’t changing • If it accelerates, then this information is passed through space-time at the ...
The Void Probability Function and Related Statistics
... for the reduced volume-averaged N-point correlation function SN’s roughly constant with scale Good agreement for S3 and S4 in different redshift catalogs But different amplitudes from 2D and 3D measurement (damping of clustering in z space, Lahav et al. 1993) ...
... for the reduced volume-averaged N-point correlation function SN’s roughly constant with scale Good agreement for S3 and S4 in different redshift catalogs But different amplitudes from 2D and 3D measurement (damping of clustering in z space, Lahav et al. 1993) ...
