Neutrinos y materia oscura

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Neutrinos y materia oscura. REDFAE. Desarrollo de detectores. Desarrollar estudios detallados de prototipos de detectores de materia oscura con objetivo a largo plazo y de frontera. A desarrollarse en Mxico Busqueda sistemtica del sitio subterrneo (~ Industria minera). - PowerPoint PPT Presentation

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  • Neutrinos y materia oscuraREDFAE

  • Desarrollo de detectores Desarrollar estudios detallados de prototipos de detectores de materia oscura con objetivo a largo plazo y de frontera. A desarrollarse en MxicoBusqueda sistemtica del sitio subterrneo (~ Industria minera)

  • Desarrollo de detectoresDesarrollar prototipos de detectores de neutrinos para salvaguardas (~ CFE)Buscar la conexin con colaboraciones internacionales

  • Evidence for Dark Matter

    Flat Rotation curves of Galaxies. Rubin and W.K. Ford (1970) What you see is not what you get.Modified Newtonian Dynamics (Moglim 1983)Modified Gravity such as Scalar tensor vector gravity theory (Moffat 2006)Alternative Explanationsvc ~ r 1/2Local density : 0.3 GeV/cm3

  • Evidence for Dark Matter Lambda-Cold Dark Matter (concordance) model explains cosmic microwave background observations (WMAP), as well as large scale structure observations (Sloan Digital Sky Survey) and supernovae Ia data of the accelerating expansion of the universe. The Composition of the Universe

  • WIMP DETECTIONIndirect DetectionSuperK, AMANDA, ICECUBE, GLASTSearch for neutrinos, gamma rays, radio waves, antiprotons, positrons in earth- or space-based experimentsDirect and indirect methods are complementary techniques along with a possible discovery at the LHC

  • WIMP DETECTIONDirect Detection of halo particles in terrestrial detectors CDMS-II, ZEPLIN Edelweiss, DAMA, GENIUS, etc

  • Current direct detection experimentsEvent-by-eventStatisticalNone

  • Deteccin de materia oscura

  • COUPP

  • COUPP

  • Busqueda del sitio

  • Fsica de neutrinos

  • Neutrinos solares

  • Double Chooz

  • ProyectoAngraen Rio

  • Desarrollo de detectores Desarrollar estudios detallados de prototipos de detectores de materia oscura con objetivo a largo plazo y de frontera. A desarrollarse en MxicoBusqueda sistemtica del sitio subterrneo (~ Industria minera)

  • Desarrollo de detectoresDesarrollar prototipos de detectores de neutrinos para salvaguardas (~ CFE)Buscar la conexin con colaboraciones internacionales

    The first evidence for the existence of Dark Matter comes from the observation of galaxies rotation curves. The visible objects (stars) cannot possibly account for the observed speeds distribution, which naturally lead to the idea of a non-visible dark matter component.

    Lastly, the latest cosmological background measurements, notably by WMAP last year, give the most drastic constraints. Within an apparently flat universe, baryonic matter only amounts to about 5% of the total mass, while the total matter contribution is around 30%, thus leaving at least 85% of non-baryonic matter so far unaccounted for, and therefore supposed to be very weakly interacting.

    Taking into account all those parameters has lead to a number of experiments, set in various underground sites all over the world. In this table are reported the most notable or representative of them, which have given results or are still running. For ease of view they are sorted by way of nuclear versus electronic recoil discrimination capabilities.The first generation experiments used only one way of measure, be it Heat, Ionization, or Light. However, this lead to very little to no background discrimination capabilities. HDMS or IGEX Ge diodes, or CUORICINO TeO2 crystals, are examples of detectors which cant discriminate nuclear from electronic recoils events. DAMA Sodium Iodide crystals, or ZEPLIN Liquid Xenon setups only allow a limited and statistical discrimination.Next generation detectors aiming to obtain an energy spectrum almost all include two channels of measure. This is the case with the Heat and Ionization or Heat and Light bolometers, and the new LXe detectors with Light and ionization measurement.Well now go through the most notable and representative experimentsBe careful with the comparison of experiments, we must use the same prescriptions as Lewin and Smith (example for the halo parameters, the form factor, )

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