Next: Inspection of results Up: *fit* - Fit Data Previous: Verbose Mode . If the number of net counts for a source is less than it is impractical to fit the data in all 34 energy bits. However, if the flux is required, then a fit must be performed first. ... Fit will then calculate the normalization of the model and xflux can be used to determine the flux and luminosity of the source from the best fit model. xs> fit rebin=yes . ...
The LCDM paradigm: successes and challenges on scales of galaxies Anatoly Klypin (NMSU) LCDM · · · · DM profiles, concentrations, .. Clustering of galaxies: P(k) and correlation functions Satellites: abundance, number-density profiles Galaxies and Dark Matter: abundances Dwarfs. ... Springel et al 2008. ... Klypin et al 2010. ... Observations - LCDM: just enough Magellanic Clouds Observations LCDM Vmax > 50 km/s Busha et al 2010 Dark matter profiles: standard LCDM Aquarius simulation. ...
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Ссылки http://mavr.sao.ru/Doc-k8/Science/seminar/Klypin/LCDMissues.pdf -- 2705.2 Кб -- 11.06.2013
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Ссылки http://www.sao.ru/Doc-k8/Science/seminar/Klypin/LCDMissues.pdf -- 2705.2 Кб -- 11.06.2013
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Ссылки http://jet.sao.ru/hq/seminar/optic/Klypin/LCDMissues.pdf -- 2705.2 Кб -- 01.07.2011 Похожие документы
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