Massimo Persic INAF/INFN-Trieste MAGIC Collaboration GeV-TeV prospects & results Issues :  Origin & diffusion properties of Galactic CRs: Main accelerators: SNRs? Diffusion: measure it?  Galaxies: massive SFR  AGNs: variability, SED, EBL  GRBs: SED, emission  pulsars: emission region  Clusters of galaxies: NT side of structure formation  Galaxy halos: DM Massimo Persic INAF-INFN Trieste MAGIC Collaboration

SNR shell  particle acceleration Resolved shell in VHE-  -rays  -rays from leptonic or hadronic channels? SNR RX J Aharonian Berezhko & Völk 2006 H.E.S.S. 3EG J B=100  G hadronic channel favored leptonic channel fav’d

Leptonic: E e ~ 20 (E  ) 1/2 TeV ~ 110 TeV … but KN sets on..  ~100 TeV Hadronic: E p ~ E  / 0.15 ~ 30 / 0.15 TeV ~ ~ 200 TeV... but: is SN statistics enough to fit CR energy density?

HESS J Hadronic: 2M  of target gas, exp-cutoff proton distrib:  =2.1, E c =100 TeV, n p =6cm -3, L(0.4  6 TeV)=2.5E+34erg/s Leptonic: B=10mG, exp-cutoff electron distrib:  =2.0, E c =20TeV D = 4 kpc ??? MAGIC AGILE Fermi LAT VHE  -rays: hadronic or leptonic ? Albert IACT GeV data  solve TeV spectral degeneracy  CRp normalization ABBA

 index  ~  (strong shock)  little variation across SNR Aharonian GeV+TeV  spatially resolved spectroscopy  young SNRs (t<t cool (p,e)): CRp spectrum  = 1+2  + b  measure  ( p ) as a function of p  = p b … b~0.6 ? from B/CNO ratio from VHE from radio

Galaxies Arp 220 Integrated view of VHE em. from massive SF: acceleration, diffusion, energy loss

F(>0.1 TeV) ~ ~ 2 x cm -2 s -1 F(>100 MeV) ~ ~ cm -2 s -1 MAGIC or VERITAS: hundreds of hours Fermi LAT: first-year scan M82: most promising candidate MP, Rephaeli & Arieli 2008 diffusion-loss eq. solved

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?

Active Galactic Nuclei IACT Fermi AGILE

Mrk 421

MAGIC 3C454.3 z=0.859 Jul/Aug & Nov/Dec 2007 AGILE trigger (S+E)SC model Ghisellini+ 2007

PG (?) AGILE MAGIC Fermi March/April 2008 First ever simultaneous HE+VHE  -ray obs of a blazar! p r e l i m i n a r y

Target-of-Opportunity (ToO) obs’s:  high states trigger in other  (  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 check quiet emission of blazar properties of steady-state particle spectrum –emergy-dependent evolution in time

 Limitless possibility for IACT follow-up?

Cross section ( differ.): Optical depth: TeV  : E soft  :  E ~ 1TeV    max for  ~0.5 eV (~2  m, K -band) Heitler 1960 Stecker+ 2006EBL IBL absorption Slkkkàkàk-lkn Stecker 1999 Hauser & Dwek 2001 x=1+cos 

Franceschini et al. 2008

Measuring EBL(z). Tools : sources with sound modeling & minimum number of parameters  BLLacs !? (l.o.s. orientation, jet-only emission, single-zone SSC). 1) Based on GeV data, set up a list of BLLacs whose predicted VHE flux is detectable with IACTs. Populate redshift space (out to z ~ 1) as closely as possible. 2) For each BLLac source, obtain simultaneous well-sampled mwl SEDs (at optical, X-ray, HE, and VHE frequencies) corresponding to different source states (low, high). This amounts to having several SEDs at each given z. Since in such SEDs the Compton peak typically occurs in the EBL-unaffected region 100 GeV) is known and can be assumed to represent the intrinsic VHE source spectrum. Contrasting it with data (measured between photon energies E 1 and E 2 ), we obtain n EBL (z) at redshift z and in the energy interval between, locally at redshift z, 0.5/[E 2 (1+ z )] eV and 0.5/[E 1 (1+ z )] eV. 3) Repeating procedure (2) with different SEDs (i.e.: different sources, or same source in different emission states) at the same z, in principle we should obtain consistent determinations of the EBL. In practice, we will reduce the statistic error affecting each determination of n EBL ( z ). 4) Selecting BLLac objects progressively farther away, we will measure EBL at different z. By repeating steps (2),(3) we will in principle obtain measures of n EBL (z) -- out to z ~1.

Gamma-Ray Bursts (GRBs)  Most energetic explosions since Big Bang (10 54 erg if isotropic)  Astrophysical setting unknown (hypernova?)  Emission mechanism unknown (hadronic vs leptonic, beaming, size of emitting region, role of environment, … … )  Cosmological distances (z >> 1) but... missed naked-eye GRB B (z=0.937 ) Gggg HE+VHE data crucial to constrain/unveil emission mechanism(s) HESS MAGIC ST

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

Galaxy Clusters

Targets: Draco, Willman-I, Segue gals.

2. DRACO dSph Milky Way surrounded by small, faint companion galaxies - dSph’s  very DM-dominated objects. - Distances, M/L ratios 16<D/kpc<250 kpc, 30<M/L<300 DRACO dSph high M/L>200 d~80 kpc Northern source  MAGIC ok !!

Draco dSph: modeling cusped profile cored profile total DM annihil. rate N  :  -rays / annihil.  - ray flux  A v>, m  : WIMP annihil. cross section, mass d~80 kpc r s = 7 – 0.2 kpc  0 = 10 7 – 10 9 M  kpc -3  0 2 r s 3 = 0.03 – 6 M  2 kpc -3 Bergström & Hooper 2006 upper limit

MAGIC 40-h exp. Fermi 1-yr exp. IACT neutralino detection:  cm 3 s -1 Bergström & Hooper 2006 max. cusped min. cored +-+- W+W-W+W- ZZ bb t _ _ Stoehr unid’d GeV sky brightness fluct’s to be followed up a TeV energies

Draco dSph obs’d MAGIC arXiv: hr May 2007 m 0 > 2 TeV …   < (  DM  DM ) WMAP = m 0 > 2 TeV …   < (  DM  DM ) WMAP =  m 0  2 TeV …   < (  DM  DM ) WMAP =0.113 m 0  2 TeV …    (  DM  DM ) WMAP =

Probing Quantum Gravity

Mrk 501: Jul 9, 2005

GeV+TeV: wide spectral coverage to observe Galactic-environment phenomena useful to solve long-standing issues about CRs. SNRs, molecular clouds  HE+VHE emission mechanism, energy-dependent diffusion. GRBs, star-forming galaxies  SFR(z) Galaxy clusters  NT side of structure formation Pulsars  measure magnetosph. emission cutoff AGNs  solve (S+E)SC model of AGNs measure EBL(z) probe short-time variability as function of E simultaneous mwl monitoring of low-state ToO obs’s of high states DM halos  depending on m , decay channels, central density, distance Outlook

Thanks!