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Massimo Persic INAF+INFN - Trieste

Bologna, 19.03.2009. Massimo Persic INAF+INFN - Trieste. MAGIC1 highlights. Nell’ultimo anno:. … grazie a E thr = 50 GeV. Scoperta la sorgente VHE- g più lontana : 3C 279 (z=0.54). Scoperta emissione pulsata a E>25 GeV da Crab pulsar, misurato il cutoff.

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Massimo Persic INAF+INFN - Trieste

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  1. Bologna, 19.03.2009 Massimo Persic INAF+INFN - Trieste MAGIC1 highlights

  2. Nell’ultimo anno: … grazie a Ethr = 50 GeV Scoperta la sorgente VHE-gpiùlontana: 3C 279 (z=0.54). Scopertaemissionepulsata a E>25 GeVda Crab pulsar, misuratoil cutoff. ELIV > 0.03 MPlda flare di Mk501. Prima osservazionesimultanea broadband HE-VHE diblazar. Misuraprofondadiannichilazionedi neutralinodagalassia con più alto M/L. Ma … mancato GRB brillante!!

  3. Publication rate

  4. Galactic highlights

  5. Crab nebula & pulsar

  6. Synchrotron emission IC emission B~0.4 mG: not an effective IC emitter!

  7. Crab pulsar: detection First detection of pulsed emission at >25 GeV. Searches going on for ~35 years!! EGRET + MAGIC: pl * exp [–E/16.3 GeV)] pl *exp [–(E/20.7 GeV)2] • at least for Crab pulsar, • polar cap scenario challenged More psr obs’s: ms pulsars?

  8. Sistemi doppi

  9. Extragalactic highlights

  10. TeVBlazars TeV blazars: highly variable, NT emission Most are HBL (high-peaked BL Lacs) Emission: leptonic Spectral Energy Distribution SSC model parameters: Plasma blob:R, B, dj Electron pop:n0, a1, a2, Ebr, Emin, Emax EBL: uEBL(z)

  11. Mrk 421

  12. Target-of-Opportunity (ToO) obs’s:  high states • trigger in other l (g: AGILE, Fermi; x: Swift, Suzaku; optical: KVA) • simultaneous mwl observations: • evolution of emitting particle population • emergy-dependent evolution in time • Monitoring obs’s:  low states • in several l • check quiet emission of blazar • properties of steady-state particle spectrum • emergy-dependent evolution in time

  13. Limitless possibility for • IACT follow-up?

  14. TeV detections: current status • 1. Mrk 421 z=0.031 Whipple 1992 • 2. Mrk 501 z=0.034 Whipple 1996 • 3. PKS 2344+514 z=0.044 Whipple 1998 • 4. Mrk 180 z=0.045 MAGIC 2006 • 5. 1ES 1959+650 z=0.047 7Tel.Array 1999 • 6. BL Lacertae z=0.069 MAGIC 2007 • 7. PKS 0548-322 z=0.069 HESS 2007 • 8. PKS 2005-489 z=0.071 HESS 2005 • 9. RGB 0152+017 z=0.080 HESS 2007 • 10. W Comae z=0.102 VERITAS 2008 • 11. PKS 2155-304 z=0.116 Mark VI 1999 • 12. 1ES 1426+428 z=0.129 Whipple 2002 • 13. 1ES 0806+524 z=0.138 VERITAS 2008 • 14. 1ES 0229+200 z=0.139 HESS 2006 • 15. H 2356-309 z=0.165 HESS 2006 • 16. 1ES 1218+304 z=0.182 MAGIC 2006 • 17. 1ES 1101-232 z=0.186 HESS 2006 • 18. 1ES 0347-121 z=0.188 HESS 2007 • 19. 1ES 1011+496 z=0.212 MAGIC 2007 • 20. PG 1553+113 z>0.25? HESS/MAGIC 2006 • 21. 3C 279 z=0.536 MAGIC 2007 • 22. S5 0716+714 z= ? MAGIC 2008 • 23. M 87 z=0.044 HEGRA 2003 • 3C66/A z=.... VERITAS 2008 • 3C66/B z=0.021 MAGIC 2009

  15. IBL Hauser & Dwek 2001 Cross section (differ.): Stecker+ 2006 Optical depth: TeV g: E soft g: e E ~ 1TeV  sggmax for e~0.5 eV (~2mm, K-band) Heitler 1960 x=1+cosq Slkkkàkàk-lkn Stecker 1999 IBL absorption

  16. IBL(e,z) Stecker + 2006 Cosmological g-ray horizon:  t(Eg,z) = 1 (Fazio & Stecker 1970) w. active evolution t(Eg,z) t(Eg,z)=1 Stecker + 2006 Stecker + 2006

  17. … round the corner ?? MAGIC is ideal to follow-up GRBs (fast repositioning, low Ethr) GCN Network member GRB alert active since 04/2005 MAGIC data-taking GRB-alarm from SWIFT GRBs Whipple, HESS also on track … high z! intrinsic TeV src’s?

  18. GRBs Intrinsically: Nearby: z=0.937 Brightest ever observed in optical Exceedingly high isotropic-equivalent in soft g-rays 080319B  missed obs of “naked-eye” GRB Swift/BAT could have observed it out to z=4.9 1m-class telescope could observe out to z=17 Missed by AGILE (Earth screening) and by MAGIC (almost dawn) next BIG ONE awaited

  19. >1 TeV 1. The Galactic Center VLA Sgr A MAGIC no variability, yr-min scale Gal. Eq. Detected: Cangaroo 2003 Confirmed: HESS 2004 Confirmed: MAGIC 2005 consistent with Sgr A* to 6’’ and slightly extended Diffuse GP emission revealed by subtracting strong sources Correlation with molecular gas CRs interacting with MCs GC source coincident w. Sgr A* MAGIC vs HESS agreement ! Subtracted image slope = 2.2 Contours of CS emission (molecular tracer) GC signal: unlikely to be DM

  20. Targets: Draco, Willman-I, Segue gals.

  21. DRACO dSph high M/L>200 d~80 kpc 2. DRACO dSph Milky Way surrounded by small, faint companion galaxies Northern source  MAGIC ok !! • dSph’s very DM-dominated objects. • Distances,M/L ratios16<D/kpc<250 kpc, 30<M/L<300

  22. d~80 kpc Bergström & Hooper 2006 Draco dSph: modeling total DM annihil. rate <sAv>, mc: WIMP annihil. cross section, mass g-ray flux Ng: g-rays / annihil. cusped profile upper limit cored profile g-ray flux rs = 7 – 0.2 kpc r0 = 107 – 109 Mž kpc-3 r02 rs3 = 0.03 – 6 Mž2 kpc-3

  23. _ bb t t t+t- _ min. cored W+W- GLAST 1-yr exp. max. cusped MAGIC 40-h exp. ZZ Bergström & Hooper 2006 IACT neutralino detection: <sAv> ³ 10-25 cm3s-1 Stoehr + 2003

  24. Draco dSph obs’d MAGIC arXiv:0711.2574 7.8 hr May 2007 m0 > 2 TeV … Wc < (WDM+2dWDM)WMAP=0.113 m0 > 2 TeV … Wc < (WDM-2dWDM)WMAP=0.09751 m0£ 2 TeV … Wc < (WDM+2dWDM)WMAP=0.113 m0£ 2 TeV … Wc< (WDM-2dWDM)WMAP=0.09751

  25. Probing Quantum Gravity

  26. Mrk 501: Jul 9, 2005

  27. … into the future …

  28. Thanks!

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