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Large surface arrays of current cosmic ray experiments measure the signals of electromagnetic or muonic components or their combination. The correction to the zenith angle (the attenuation curve) has to be taken into account before the signal is converted to the shower energy. Either Monte Carlo simulations or indirect estimation using collected data (Constant Intensity Cut method) can be used. However, the assumptions of composition or isotropy used for the determination of the attenuation curve can still influence the final physics results such as the energy spectrum, or modify anisotropy searches and composition analysis. Using simplified Toy Monte Carlo with an output from CORSIKA simulations we try to find several examples of what kind of effects can be caused by the methods of inferring the attenuation curve. Surface arrays of different sensitivities to electromagnetic and muonic components were considered.
Modern cosmic ray experiments consisting of large array of particle detectors measure the signals of electromagnetic or muon components or their combination. The correction for an amount of atmosphere passed is applied to the surface detector signal
We investigate -- as an alternative to usual Monte Carlo Renormalization Group methods -- the feasibility of extracting QCD beta-functions directly from a lattice analysis of correlations between the action and Wilson loops. We test this correlation
We compile a sample of about 157,000 spaxels from the Mapping Nearby Galaxies at the Apache Point Observatory survey to derive the average dust attenuation curve for subgalactic star-forming regions of local star-forming galaxies (SFGs) in the optica
As a science verification study of the newly released AKARI/FIS Faint Source Catalog ver.1, this paper discusses the different levels of dust attenuation toward stellar light and nebular emission lines within local star-forming galaxies at 0.02<z<0.1
Since its launch in 2008, the Fermi Large Area Telescope (LAT) has detected over 200 -ray pulsars above 100 MeV. This population of pulsars is characterised by a rich diversity of light curve morphologies. Researchers have been using both the radio a