Massimo PersicINAF/INFN-Trieste

MAGIC Collaboration

GeV-TeV prospects & resultsIssues: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 PersicINAF-INFN TriesteMAGIC Collaboration

SNR shell particle accelerationResolved shell in VHE--rays -rays from leptonic or hadronic

channels?

SNR RX J1713.7-3946

Aharonian+ 2006

Berezhko & Völk 2006

H.E.S.S.

3EG J1714-3857

B=100Ghadronic channel favored

leptonic channel fav’d

Leptonic: Ee ~ 20 (E )1/2 TeV ~ 110 TeV … but KN sets on .. ~100 TeV Hadronic: Ep ~ E/ 0.15 ~ 30 / 0.15 TeV ~ ~ 200 TeV

... but: is SN statistics enough to fit CR energy density?

HESS J1813-178

Hadronic: 2M of target gas, exp-cutoff proton distrib: =2.1, E

c=100 TeV,

np=6cm -3, L(0.46 TeV)=2.5E+34erg/s

Leptonic: B=10mG, exp-cutoff electron distrib: =2.0, Ec=20TeV

D = 4 kpc

???MAGIC

AGILEFermi LAT

VHE -rays: hadronic or leptonic ?

Albert+ 2006

IACT

GeV data solve TeV spectral degeneracy CRp normalization

ABBA

index ~ (strong shock)little variation across SNR

Aharonian + 2006

GeV+TeV spatially resolved spectroscopy young SNRs (t<tcool (p,e)):CRp spectrum = 1+2 + b

measure (p) as a function of p

= p b … b~0.6 ?

from B/CNO ratiofrom VHE from radio

GalaxieGalaxiess

Arp 220

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

F(>0.1 TeV) ~~ 2 x10-12 cm-2s-1

F(>100 MeV) ~~ 10-8 cm-2s-1

MAGIC or VERITAS:hundreds of hours

Fermi LAT: first-year scan

M82: most promising candidate

MP, Rephaeli & Arieli 2008diffusion-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 challengedMore psr obs’s: ms pulsars?

Active Galactic Nuclei

IACTFermi AGILE

Mrk 421Mrk 421

MAGIC MAGIC

3C454.3z=0.859

Jul/Aug & Nov/Dec 2007

AGILE trigger(S+E)SC modelGhisellini+ 2007

PG 1553+113(?)

AGILEMAGIC

Fermi

March/April 2008

First ever simultaneousHE+VHE -ray obs of a blazar!

p

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i

m

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• 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:

eeEBLHE TeV : Esoft : E ~ 1TeV

max for ~0.5 eV (~2m, K-band)

Heitler 1960

Stecker+ 2006

EBEBLL

IBL absorption

Slkkkàkàk-lknStecker 1999

Hauser & Dwek 2001

x=1+cos

Franceschiniet 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 <100GeV, using HE data the SSC model can be closed with substantially no EBL-induced bias. Hence, the SSC model in the VHE region (>100 GeV) is known and can be assumed to represent the intrinsic VHE source spectrum. Contrasting it with data (measured between photon energies E1 and E2), we obtain nEBL(z) at redshift z and in the energy interval between, locally at redshift z, 0.5/[E2(1+z)] eV and 0.5/[E1(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 nEBL(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 nEBL(z) -- out to z ~1.

Gamma-Ray Bursts (GRBs)Most energetic explosions since Big Bang (1054 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 080319B (z=0.937)

Gggg

HE+VHE data crucial to constrain/unveil emission mechanism(s)

----------------------------

HESS

MAGIC

MAGIC ST

GRBs 080319B missed obs of “naked-eye” GRB

Intrinsically:Nearby: z=0.937Brightest ever observed in opticalExceedingly high isotropic-equivalent in soft -rays

Swift/BAT could have observed it out to z=4.91m-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 dSph2. 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 dSphhigh

M/L>200d~80 kpc

Northern source MAGIC ok !!

Draco dSph: modeling

cusped profile

cored profile

total DM annihil. rate

N: -rays / annihil.-ray flux

-ray flux

Av>, m: WIMP annihil. cross section, mass

d~80 kpc

rs = 7 – 0.2 kpc0 = 107 – 109 Mž kpc-3

02 rs

3 = 0.03 – 6 Mž2 kpc-3

Bergström & Hooper 2006

upper limit

MAGIC40-h exp.

Fermi1-yr exp.

IACT neutralino detection: <Av> 10-25 cm3s-1

Bergström & Hooper 2006

max. cusped

min. cored+-

W+W-

ZZ

bbt t

__

Stoehr + 2003unid’d GeV sky brightness fluct’sto be followed up a TeV energies

Draco dSph obs’d MAGIC arXiv:0711.2574

7.8 hrMay 2007

m0 > 2 TeV … < (DMDM)WMAP=0.113m0 > 2 TeV … < (DMDM)WMAP=

m0 2 TeV … < (DMDM)WMAP=0.113m0 2 TeV … (DMDM)WMAP=0.09751

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!