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The XENIA mission and the missing barions

The XENIA mission and the missing barions. Luigi Piro , C . Kouveliotou , J.W. den Herder , T. Ohashi, D. Hartmann , D. Burrows and the WHIM team :

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The XENIA mission and the missing barions

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  1. The XENIA mission and the missingbarions Luigi Piro, C. Kouveliotou, J.W. den Herder, T. Ohashi, D. Hartmann, D. Burrows and the WHIM team: E. Branchini, Y Takei, E. Ursino, M. Galeazzi, F. Nicastro, L. Amati, A. Corsi, J. Kaastra, F. Paerels, M.Viel, L. Moscardini, M. Roncarelli

  2. StructureFormation HOW ? Most of the baryon of the Universe are locked in large scale, low density structures visible only in X-rays z High resolution spectroscopy and spatial resolution, wide field in emission 10 1 GRB as cosmological beacons: fast reaction, high res. absorption spectroscopy 0 Structure size Stars Galaxies Clusters Filaments

  3. XENIA: Mission and Payload HARI: High AngularResolutionImager 1000cm2@1keV 0.3-8 keV CCD Field=1.4° ang.res=10” constant • Low bkg: LEO • equatorial • Autonomous fast pointing in 60 s • 2 tons • TRL4 • DecadalSurvey • medium size CRIS: CryogenicImagingSpectrometer 1000cm2@0.5keV 0.1-3 keV TES DE<2.5eV Field=1.0°ang.res=3’ TED: TransientEvent Detector ¼ of the sky, 3’ localization 8-200keV

  4. Exploring a newregionof the Cosmicweb Cluster @ Virial r. Hot (clusters) WHIM Branchiniet al 2009 Star forming Cold Diffuse

  5. Tomography of the Universe: the X-ray forest from the Cosmic Web with GRBs From 150 GRBs with afterglow Fluence>2 10-6 cgs ~200s OVII-OVIII filaments in 5 years

  6. 3D mapping of the Cosmic Web Model, Dz=0.02 @z=0.22 Detected, OVII+OVIII in emission, 5 s, 1 Ms 5x5° Down tooverdensitiesof30

  7. WHIM Angular Correlation • Xenia HARI • Remove 50% brightpixels (dominatedby hot dense gas phase) + 2000 AGN + foreground • Galeazzi talk, Ursino & Branchini, Nicastroet al

  8. Summary • Xenia unique capabilities wrt WHIM : fast reaction to GRB, high spectral resolution with wide field of view • probe at least 200 filaments in absorption by exploiting bright GRB afterglows • Afterglow decay allows follow up observation of the same filament region in emission, providing a unique abs+emission measurement • Deep wide field (5x5) spectroscopy in emission: tomography of the WHIM up to z=0.5 (about 104 OVII+OVIII line measurements) • Wide Field High Angular resolution: • ACF of the WHIM • Proposal to ASTRO2010 as medium size mission • More info: http://sms.msfc.nasa.gov/xenia/

  9. Back up slides

  10. Absorption

  11. WHIM in emission • Spectrumfrom a 2.6’x2.6’ bin in 1 MsbyXenia CRIS

  12. Whim in emissionprobedbyXenia • Blacklineis the gas modeldistribution, Blu is the gas acessedbyXenia in 100 ksec, red in 1Ms, allowingaccesstolower density WHIM regions

  13. Numberofemissionlinedetections

  14. 0.1 ph cm-2 s-1 sr-1 gives 50 linephotons in a 2.5x2.5’ pixel ofXenia/CRIS in 1Ms

  15. Tracing clusters at virial radius

  16. Spectroscopy: fast reaction and wide field • Linespectroscopymeritfactorforvariablesources = S/N for EW=1eV for a typical GRB afterglow

  17. Observingprogramme

  18. Xeniawill trace the cosmichistoryofbaryons • Gamma-Ray Bursts • Evolution of massive star formation using GRBs to trace their explosions back to z > 8) • Measure the metals in the host galaxies of GRBs and the explosive enrichment in their close environment out to z>8 • ClustersofGalaxies • Trace the evolution and physics of clusters out to their formation epoch (z>1) • Measure the thermodynamical and chemical properties of a fair sample out to the virial radius • CosmicWeb • Detect the largest reservoir of baryons from z~1 to the present time by measuring densities ~30 times smaller

  19. CRIS • Mirror: 2/4 reflection • TESmicrocalorimeter

  20. HARI • Mirror: Polynomial profile with constant PSF • CCD

  21. TED • 2 CodedMask / CZT detectors

  22. Angular Correlation Remove 50% brightest pixels Normalized to Total Flux

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