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Résumé (très partiel) des confs d’été « astro »

Résumé (très partiel) des confs d’été « astro ». IRFU/SPP 27 septembre 2010. Résumé (très partiel) des confs d’été « astro ». Ondes gravitationnelles : non couvertes Cosmo : pas de nouveaux faits marquants, cf. Moriond Cosmo 2010. IRFU/SPP 27 septembre 2010. Rayons cosmiques.

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Résumé (très partiel) des confs d’été « astro »

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  1. Résumé (très partiel) des confs d’été « astro » IRFU/SPP 27 septembre 2010

  2. Résumé (très partiel) des confs d’été « astro » • Ondes gravitationnelles : non couvertes • Cosmo : pas de nouveaux faits marquants, cf. Moriond Cosmo 2010 IRFU/SPP 27 septembre 2010

  3. Rayons cosmiques

  4. Fermi electron spectrum: low energy part Significance of deviations from the mean rate. • No significant anisotropy is observed in the CR electron flux. • The results can rule out dominance of a very bright nearby source. • Analyse en cours 1 year of data Spectrum from 7 GeV up to 1 TeV Compatible wit a power law of index -3.08 +/- 0.05 Johnson, ICHEP 2010

  5. Arrival directions of ~TeV protons MILAGRO ARGO-YBJ Single layer of resistive plate counters water Cherenkov detector Two regions of excess 15.0  and 12.7 (7 yr data taking) 584 days Hot spots observed in both Milagro and ARGO with high significance Harder spectrum (flattering) Nearby CR accelerator … with non-standard diffusion parameters! No compelling explanation found yet Open issue! Talk Omodei ICHEP 2010

  6. Auger’s sky (E>5x1019 eV)Evolution of degree of correlation After publication in 11/2007, correlation degree dropped from 69% to 38% 0.3% probability to find such a correlation from an isotropic distribution Kampert, ICHEP 2010

  7. UHECR composition Compositions between HiRes and Auger do not seem to agree… HIRES and AUGER are seeing different sky? Modifications of cross sections at highest energies? Increasing p-Air X-section could bring down Xmax RMS of Xmax large.. Farrar, ICHEP 2010

  8. Matière Noire

  9. Résultats de Xenon 100et WIMP “basse masse” (1) Talk Sadoulet Blois 2010 Xe double phase Run préliminaire : 11 jours, volume actif 40kg Pas d’indication en faveur des événements CoGeNT? tout dépend de la calibration de L_eff …

  10. Résultats de Xenon 100et WIMP “basse masse” (2) t Systematique importante à basse energie Talk Sachuman IDM 2010 Normalisation de Leff: +/- 30% CoGeNT pourrait ne pas être exclu Xe coll. prend une moyenne ponderee pour Leff

  11. CRESST : evts à basse energie • CaWO4 crystals: scintillation/heat • threshold 10 keV • ~400 kgd For small WIMP mass, only O recoils above threshold 32 events in the O band Expected bck ~9 (neutrons+alpha+gamma leakage) Compatible with a ~10 GeV WIMP Waiting for details on background rejection… Talk Seidel IDM 2010

  12. Comment abaisser le seuil pour Xenon ? PRELIMINARY Talk Sorensen IDM 2010 Donnees de Xenon 10 Seuil limité par le premier signal de scintillation Utilisation de S2 seulement : seuil~1keVr ~pas de pouvoir de rejet

  13. Limites d’exclusion été 2010:spin-independent cross section x 2 Talk Armengaud IDM 2010 Edelweiss II 2009: 144 kg.day Edelweiss II prel. : ~300 kg.day (Apr 09 – May 10) - 3 evts pres du seuil - ~ 5 x 10-8 pb New prototype FIDs now working at LSM

  14. Limites d’exclusion été 2010:spin-dependent cross section Talk Danninger TeVPA 2010 DM searches towards the Sun IceCube DeepCore (6 additional lines) 20 GeV energy threshold Competitive SD limits wrt direct detection

  15. Fermi : search for DM spectral lines Energy resolution : 10% at 100 GeV Example fit for a 40 GeV line 95% CL upper limits bck signal 11 months of data ROI: b>10 and 20x20 around GC Galactic plane and point sources excluded Sources removed for b > 10  No line detection NO line Talk Conrad IDM 2010

  16. Galactic Halo Dark Matter Limits (|b|>10) from Fermi unpublished PRELIMINARY Halo size CR source distribution from Case&Battacharya 98 The diffuse flux from the Galactic halo can be used to set limits on dark matter annihilation. • Relies on differences in the angular and spectral distributions of the diffuse production from cosmic rays versus dark matter. • Still very preliminary. The constraints are very sensitive to the choice of the Galactic diffuse model. Investigations are still in progress of the dependence of the result on our astrophysical models of the Galaxy (e.g the CR source distribution, halo height, diffusion coef. etc.). R.P. Johnson

  17. Dwarf galaxies FERMI HESS Sculptor dwarf (Preliminary) Excluded (95% CL) Observed by Fermi Fermi limit Observed by HESS Johnson’s talk Glicenstein’s talk o Canis Major Talk Omodei ICHEP 2010

  18. Fermi : Cosmological Dark Matter The isotropic extragalactic contribution have be interpreted in terms of limits on cosmological dark matter [Dark matter annihilation in all halos at all red-shifts should contribute] Models of absorption by EBL DM structure evolution scenarios DM could supply all the photons in a given bin Assuming a power-law model for astrophysical background R.P. Johnson JCAP04 (2010) 014

  19. Astro neutrinos: diffuse nmflux Upper limits on diffuse neutrino emission E2F(E)90%= 4.7×10-8 GeV cm-2 s-1 sr-1 20 TeV<E<2.5 PeV Energy estimator= Repetition (R) of integration gate on the same Optical Module Rejection of downward going atmospheric muons (using measured zenith angle, track quality parameter, number of hits) Separation of the atmospheric n background from signal using the energy estimator R Talk Spurio ICHEP 2010

  20. Gamma-rays

  21. Galactic Diffuse Emission The first Fermi-LAT publication on the galactic diffuse spectrum is in disagreement with the EGRET spectrum. In particular, there is no obvious “GeV excess” with respect to standard models of the diffuse production from cosmic rays. R.P. Johnson

  22. Fermi isotropic gamma-ray background • Some inconsistency with previous measurements by EGRET. • Higher energy reach. 1 year Femi LAT data, |b|> 10deg. Derivation of the isotropic gamma-ray flux (believed to be primarly extragalactic) by reducing and understanding the residual CR background. Guaranteed contribution: unresolved extragalactic sources: blazars, star forming and star burst galaxies,... Spectrum featureless Consistent with powerlaw : -2.41

  23. Fermi gamma-ray haze Gamma-ray overdensity in the inner Galaxy Spectrum consistent with a the IC emission of a hard population of electrons on interstellar radiation Morphology : elongated in b with respect to l DM? It doesn’t look like.. Local source of electrons? Talk Dobler TeVPA 2010

  24. Fermi gamma-ray haze Recap: after known foregrounds are subtracted, an excess appears in the residual maps within the inner ~20 around the Galactic Center [GeV-TeV electrons emit hard synchrotron in the frequency range of WMAP] “WMAP haze” 22 GHz Gamma-ray overdensity in the inner Galaxy May be the IC counterpart to the WMAP haze Similar spatial morphology to the WMAP haze supporting the synchrotron interpretation of the microwave signal Talk Dobler TeVPA 2010

  25. Fermi AGN stacking • Official Fermi statement : PSF broader than expected at high energy • Corrections underway to fix the MC issue • “in-flight” PSF released soon 170 AGN (>4.1s) stacked (improved statistics!) Expected photon maps from P6_v3 IRF (pre-launched estimate) Excess! But… Talk Ando TeVPA 2010

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