Galaxy’s Approximate Luminosity Probability and Linear Statistic Analysis of Luminosity Graph

Cluster Merger Variance and the Luminosity Gap Statistic

The presence of multiple luminous galaxies in clusters can be explained by the finite time over which a galaxy sinks to the center of the cluster and merges with the the central galaxy. The simplest measurable statistic to quantify the dynamical age of a system of galaxies is the luminosity (magnitude) gap, which is the difference in photometric magnitude between the two most luminous galaxies....

Luminosity * †

where v+(v−) is the common velocity of all the particles in bunch +(−). Eq. (1) is a relativistic invariant, has dimensions of 1/area, and is valid for arbitrary velocities v±. (Generalization to the case when the velocity distributions are not homogeneous is given in Ref. 2.) For a storage ring collider with bunch spacing sB , bunches collide periodically with frequency fc = βc/sB . For a line...

Preserving high multibunch luminosity in linear colliders

An analytic theory of cumulative multibunch beam breakup in linear colliders is developed. Included is a linear variation of transverse focusing across the bunch train as might be applied, e.g., by chirping the radio frequency power sources or by using radio frequency quadrupole magnets. The focusing variation saturates the exponential growth of the beam breakup and establishes an algebraic dec...

ATTAINING HIGH LUMINOSITY IN LINEAR efe- COLLIDERS*

Evolution of Galaxy Luminosity Function and Luminosity Function by Density

Using galaxy sample observed by the BATC large-field multi-color sky survey and galaxy data of SDSS in the overlapped fields, we study the dependence of the restframe r-band galaxy luminosity function on redshift and on large-scale environment. The large-scale environment is defined by isodensity contour with density contrast δρ/ρ. The data set is a composite sample of 69,671 galaxies with reds...