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● canonical disclaimer ● some general remarks ● selected topics

VULCANO 2008 – CONCLUDING REMARKS. ● canonical disclaimer ● some general remarks ● selected topics. ● UHECRs ● DM ● GRBs. ● nomination for the conference hit ● acknowledgements.

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● canonical disclaimer ● some general remarks ● selected topics

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  1. VULCANO 2008 – CONCLUDING REMARKS ● canonical disclaimer ● some general remarks ● selected topics ● UHECRs ● DM ● GRBs ● nomination for the conference hit ● acknowledgements

  2. As every year, the selection, based on personal impressions, will be arbitrary and unfair

  3. quotation from my Vulcano 2007 concluding remarks: ● we had an excellent conference ●we heard a lot of excellent talks ● some talks were clearly missing e.g. ●status of HST & JWST ●highlights of SWIFT (I hope that organizers of Vulcano 2008 will rectify this deficiency) AND THEY DID !

  4. UHECRs Big news from AUGER!

  5. ●Correlations of UHECR events with AGNs! If events > 57 EeV with |b|>12o are considered, then 19 out of 21 are correlated (5 expected) ●GZK cut off confirmed ! ●Composition of UHECRs: neither p nor Fe

  6. courtesy A. Letessier-Selvon

  7. (De Roeck, 2008)

  8. courtesy A. Letessier-Selvon GZK cut off Maximum signal occurs @ same energy where the flux is reduced by 50% with respect to an extrapolated power law

  9. CONCLUSIONS (A. Letessier-Selvon) It is just the beginning…. • Anisotropy of UHECR has been established at > 99% CL for the parameters E~60 EeV, D~100 Mpc, ~4º • Nature of the correlation provides evidences for the ‘GZK’ effect and the hypothesis that the CR are dominantly protons from AGN within our ‘GZK’ horizon • Sources could be other than AGN as long as they have similar spatial distributions • Increased statistics (+Auger North) will allow source identification as well as measurements of MF along the line of sight and maybe some surprises….

  10. GOOD NEWS: Dark matter exists ! Beautiful talks by: ●Sergio Colafrancesco ●many others

  11. gazeta wyborcza, 9.01.2007

  12. Gravitinos Neutralinos Sneutrinos Axinos Q-balls Split-SUSY DM candidates “Fuzzy” CDM Lower possible end of CDM Bosons with M10-22 eV Chaplygin Gas DM-DE common origin P = - A / r Non-thermal production m eV < Maxion < m eV Experimental limits Axions Neutrinos Warm DM 0.0005 < Wn h2< 0.0076 Massive neutrinos acceptable Sterile n with mn  10-100 keV Light (MeV) DM Spin = 0 supersymmetric particle 1 MeV < MLDM < 4 MeV Elusive: only e± 511 keV line SUSY DM Dark Matter Kaluza-Klein excitations L-KK (r-parity) particle: stable MKK 1 TeV Extra dimension Branons String theory brane fluctuations Mbranon > 100 GeV Mirror Matter Ordinary matter in mirror world Dissipative & complex chemics WIMPzillas Produced at the end of Inflation M > 1013 GeV MWIMP PBHs BHs @ quark-hadron transition MPBH Mhorizon(T=102MeV) > M

  13. POPULAR DM CANDIDATES

  14. DM induced astro-particle signals Heating Bremss.-ICS UV/X-rays SZE sub-mm c-c annihilation cc annihilation Synchrotron Radio g-rays Neutrinos

  15. Covering the whole e.m. spectrum cc annihilation products ICS SZ Effect ICS Brem.+ICS Brem.+ICS+p0 Synchrotron

  16. DM annihilation in cosmic structures Galaxies (Optical) Diffuse gas (X-rays) Relativistic particles (Radio halos/relics) Cluster No gas (No X-rays) No rel. particles (No radio emission) Stars (Optical) dSph Galaxy

  17. SZE in DM halos SZth • A structure with: • Hot gas • Warm gas • Rel. Plasma • DM • Distant & Vr SZwarm SZkin SZrel SZDM

  18. SZE in pure DM halos • A structure with: • DM • Nearby (Vr ≈ 0) SZDM Dwarf Spheroidal gal.

  19. 1ES0657-556

  20. ●It is fascinating that we could map so well so many possibilities and that we may expect to obtain significant astrophysical constraints on DM particles

  21. The signal from DAMA (significant annual modulation) is very exciting But, if interpreted as due to DM annihilation (model dependent) it seems to be too strong comparing with other astrophysical constraints We have to be patient! [Vulcano 2006] The last statement remains true atVulcano 2008

  22. GRBs We live in a SWIFT era Beautiful talks by: ●Lorenzo Amati ●Guido Chincarini ● many others

  23. ●collimation ●cosmology & GRBs ●giant flares of distant magnetars

  24. How strong is the collimation ? 10-6 (DF, AD) or 10-2÷ 10-3 (common wisdom) This translates into the frequency of the events (and also their energetics): is the fraction of SNe that are accompanied by GRBs≥ 10-1 or rather ~10-3? New SWIFT data indicate that light curves breaks are not achromatic → common wisdom has a problem

  25. Collimation ●no evidence of achromatic breaks in light curves ! (they are chromatic or absent) ●Amati relation is alive and well (now based on 70 GRBs) But ● Amati relation,corrected for beaming is no longer shown (too few GRBs with achromatic breaks – only ~ 10) ●There were people in this room (D. Fargione, A. Dar), who never believed achromatic breaks interpretation and advocated much stronger collimation (10-7÷ 10-6)

  26. Amati et al. (2002) analyzed a sample of 12 BeppoSAX events with known redshift • we found evidence of a strong correlation between Ep,i and Eiso, highly significant (r = 0.949, chance prob. 0.005%) despite the low number of GRBs included in the sample Ep,i= kEiso (0.52+/-0.06) Amati et al. , A&A, 2002

  27. analysis of an updated sample of long GRBs/XRFs with firm estimates of z and Ep,i (41 events) gives a chance probability for the Ep,i-Eiso correlation of ~10-15 and a slope of 0.57+/-0.02 • the scatter of the data around the best fit power-law can be fitted with a Gaussian with s(logEp,i) ~ 0.2 (~0.15 extra-poissonian) • confirmed by the most recent analysis (more than 70 events, Ghirlanda et al. 2008, Amati et al. 2008) • only firm outlier the local peculiar GRB 980425 (GRB 031203 debated) ● ● ● Amati et al. 2008

  28. Recent Swift detection of an X-ray transient associated with SN 2008D at z = 0.0064, showing a light curve and duration similar to GRB 060218 • Peak energy limits and energetics consistent with a very-low energy extension of the Ep,i-Eiso correlation • Evidence that this transient may be a very soft and weak GRB (XRF 080109), thus confirming the existence of a population of sub-energetic GRB ? courtesy L. Amati ● Modjaz et al., ApJ, 2008 Li, MNRAS, 2008

  29. courtesy L. Amati • Standardizing GRB with 3-parameters spectrum-energy correlations • the Ep,i-Eiso correlation becomes tighter when adding a third observable: jet opening angle (qjet -> Eg = [1-cos(qjet)]*Eiso (Ghirlanda et al. 2004) or “high signal time” T0.45 (Firmani et al. 2006) • the logarithmic dispersion of these correlations is very low: can they be used to standardize GRB ? • jet angle inferred from break time in optical afterglow decay, while Ep,i-Eiso-T0.45 correlation based on prompt emission properties only

  30. courtesy L. Amati • Collimated or isotropic ? • lack of jet breaks in several Swift X-ray afterglow light curves, in some cases, evidence of achromatic break • challenging evidences for Jet interpretation of break in afterglow light curves or due to present inadequate sampling of optical light curves w/r to X-ray ones and to lack of satisfactory modeling of jets ?

  31. Collimated or isotropic ? ●Unusual burst GRB080319B ●Possible interpretation: double jet (G. Chincarini) inner jet:opening angle≈ 0.4o outer jet:opening angle ≈ 8o The collimation factor for inner jet is~ 2x10-6 !!!

  32. ●cosmology & GRBs

  33. What can be obtained with 150 GRB with known z and Ep and complementarity with other probes (SN Ia, CMB) • complementary to SN Ia: extension to much higher z even when considering the future sample of SNAP (z < 1.7), cross check of results with different probes Ghirlanda, Ghisellini et al. 2005, 2006,2007 courtesy L. Amati

  34. SHORT GRBs ●Large part (majority ?) of short GRBs are compact objects mergers ● Some of them must be giant outbursts of distant magnetars Events such as Dec. 27, 2004 outburst of SGR 1806-20 (Eburst=3x1046 erg) must happen in nearby galaxies (they occur at a rate of ~ 0.1/yr in our Galaxy) If they occur within ~ 100 Mpc, they have to be classified as short GRBs

  35. Candidates for giant outburst of distant magnetars (seen as short GRBs) GRB 051103 (in M81) Eburst=7x1046 erg GRB 070201 (in M31)Eburst=6x1046 erg

  36. GRB051103 – A POSSIBLE EXTRAGALACTIC MAGNETAR FLARE (EMF) M82 Swift BAT 15-150 keV Not imaged M81 IPN Error Ellipse

  37. GRB070201 – ANOTHER EMF? M31 IPN Error Box Eburst=6x1046 erg

  38. My nomination to the conference hit goes this year to Auger (early results) !

  39. In 2009 a silver jubilee ! (25 anniversary of the start of „Multifrequency …” workshop!) SEE YOU AT VULCANO!

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