indirect dark matter search with magic

Indirect Dark MatterSearch with MAGIC

Adrian Biland, ETHZMAGIC-Collaboration

DSU07, 06.06.07Minneapolis

2 biland@phys.ethz.ch Adrian Biland: Indirect Dark Matter Search with MAGIC; DSU07, Minneapolis, 06.06.2007

MMajor ajor AAtmospheric tmospheric GGamma-rayamma-rayIImaging maging CCherenkov Telescopeherenkov Telescope

~150 Physicists,~150 Physicists, 21 Institutes,21 Institutes, 9 Countries9 CountriesIFAE Barcelona, UAB Barcelona, U Barcelona,IFAE Barcelona, UAB Barcelona, U Barcelona,Humboldt U Berlin,Humboldt U Berlin, IAC IAC CanariasCanarias, UC Davis,, UC Davis,U Dortmund, IAA Granada, INAF Italy,U Dortmund, IAA Granada, INAF Italy,U U LodzLodz, UCM Madrid,, UCM Madrid, MPI MPI MünchenMünchen,,U/INFN Padua, U Siena/INFN Pisa,U/INFN Padua, U Siena/INFN Pisa,INR Sofia,INR Sofia, Tuorla Tuorla Observatory,Observatory,U U Udine/INFN Udine/INFN Trieste,Trieste,U U WürzburgWürzburg,,Yerevan Phys.Inst.,Yerevan Phys.Inst.,DESY DESY ZeuthenZeuthen,,ETH ZurichETH Zurich

Start ofStart of construction: 2001construction: 2001Inauguration: Inauguration: October October 2003 2003StartStart regular data taking: Sept. 2004 regular data taking: Sept. 2004

Roque Roque de de los Muchachoslos Muchachos, Canary Islands, 2200m a.s.l., Canary Islands, 2200m a.s.l.

Original Goal of VHE Astronomy

Identify source(s) ofcharged cosmic ray particles

CR source

CR: existence known since 1912, but origin not (yet) understood..

Cherenkov Telescope PrincipleCherenkov Telescope Principle

- VHE VHE !! hits the hits theatmosphereatmosphere

- produces extend.- produces extend.air-showerair-shower

- shower particles- shower particlesemit emit cherenkovcherenkovlightlight => light pool => light pool

-- telescope catchestelescope catchescherenkov cherenkov lightlight

(eff. area: "105 m2

vs. 1 m2 satellites)

Cherenkov TelescopeCherenkov Telescope ProblemsProblems

-- all kinds ofall kinds ofbackground lightbackground light

-- atmosphericatmosphericconditionsconditions

Cherenkov TelescopeCherenkov Telescope ProblemsProblems

-- all kinds ofall kinds ofbackground lightbackground light

-- atmosphericatmosphericconditionsconditions

-- much moremuch moreabundantabundant showersshowersfrom chargedfrom chargedcosmic rays !!!cosmic rays !!!

(Background dominated, vs. BG-free satellites)

Imaging TechniqueImaging Technique

do not seedo not seelaterallateraldistributiondistribution on ground,on ground,

but see thebut see theprojectionprojectionof (part of)of (part of)showershower

!! candidate candidate

hadron hadron showershower

Imaging TechniqueImaging Technique

electromagnetic and electromagnetic and hadronichadronicshowers have different showers have different shapesshapes ===> ===>using ausing a high resolution Camerahigh resolution Cameraallows to distinguish allows to distinguish (statistically)(statistically)

between between !!- and- and hadron-showershadron-showers

Works excellent > 100 Works excellent > 100 GeVGeVbut very difficult < 100 but very difficult < 100 GeVGeV

MAGIC TelescopeMAGIC Telescope

Mirror:Mirror:17m (234m17m (234m22), ), f/d=1f/d=1parabolic shapeparabolic shapeformed from 964 0.5x0.5mformed from 964 0.5x0.5m22

spherical Al-mirrorsspherical Al-mirrors

Camera:Camera:576 high QE 576 high QE PMTsPMTs,,FoV FoV = 3.5= 3.5°°,,300 MHz FADC300 MHz FADCanalog analog fibre fibre readout ;readout ;

ObsObs. time:. time: ~1000 h/yr dark~1000 h/yr dark ++ 500 h/yr 500 h/yr ‘‘moonmoon’’

17m17m

2 GHz2 GHz

MAGIC TelescopeMAGIC TelescopeFast Repositioning:Fast Repositioning:to keep total weight low,to keep total weight low,use use space frame made ofspace frame made ofcarbon carbon fibre fibre epoxy tubesepoxy tubesvery strong,very strong, but but not very rigidnot very rigid ==>==>AActive ctive MMirror irror CControl:ontrol:494 stepping motors to494 stepping motors tocorrect for gravitationalcorrect for gravitationaldeformations ==>PSF 0.1deformations ==>PSF 0.1oo

MAGIC PerformanceMAGIC Performance

Actual performance reached:Actual performance reached:(for small zenith angles)(for small zenith angles)-- energy threshold energy threshold (trigger)(trigger): : ~50 ~50 GeVGeV-- energy resolution:energy resolution: 30% 30% (100GeV)(100GeV), 20% , 20% (1TeV)(1TeV)-- flux sensitivity flux sensitivity (5(5##)):: 2.5% of Crab flux in 50h2.5% of Crab flux in 50h

-- angular resolution: angular resolution: ~0.1~0.1°°-- determination of source position determination of source position ((pointlikepointlike)): : 22’’-- repositioning: repositioning: <40s<40s (with(with reduced motor power)reduced motor power) (~20s(~20s with full motor power possible)with full motor power possible)

1(2)x17m

4x12m (1x28m) 4x10m

Some Physics ObjectivesSome Physics Objectives

SNRsSNRs

Pulsars/PWNsPulsars/PWNsDark MatterDark Matter !!-ray-ray horizonhorizon

GRBsGRBsAGNsAGNs

X-ray BinariesX-ray Binaries

Galacti

Extragalactic

Fundamental/CosmologyFundamental/Cosmology

Published SourcesMAGIC catalog was authorized by IAU: “MAGIC JHHMM+DDMM”

Crab Crab SgrASgrA*? *? HESS J1813HESS J1813 HESS J1834 HESS J1834 LSI+61 303LSI+61 303 New SourceNew Source

Mrk421 Mrk421 Mrk501 Mrk501 1ES2344 1ES2344 Mrk180Mrk180 1ES1959 1ES1959 BL-Lac.BL-Lac. 1ES1218 PG 15531ES1218 PG 1553z=z=00.030 .030 0.034 0.034 0.044 0.044 0.0450.045 0.047 0.047 0.0690.069 0.1820.182 >0.25 ?>0.25 ? FastestFastest New New SrcSrc. . New ClassNew Class New New SrcSrc.. New New SrcSrc.. FlareFlare

Galactic:Galactic:

AGN:AGN:

+ several upper limits+ several upper limits + 3 new sources+ 3 new sources not yet publishednot yet published

Fundamental Physics hasFundamental Physics hasto compete withto compete with highlyhighly successful successful astro astro programprogram

DMDM approved approved ‘‘key projectkey project’’

Extragalactic:Extragalactic: Markarian501 (AGN)Markarian501 (AGN)

AGN jets have sizes >105 Ly

observer

But VHE flares on few minutes ==> small emission regions ?Energy dep. arrival time !!? Intrinsic?? Quantum Gravity?? ...

250-600 GeV

600-1200 GeV

1200-10000 GeV

4min bins

submitted to submitted to ApJApJ,, astro-ph astro-ph 07020080702008

fastest fluctuationfastest fluctuation

everever observedobserved @VHE@VHE

Mrk501

~similar

‘‘StandardStandard’’ Origins Origins of of VHE-!

VHE photons do have non-thermic origin(s)

distinguish hadronic vs.leptonic ‘acceleration’: => shape of spectrum; Multi-wavelength

Do p or e- act asseed particles?

energy E

$0decay

Synchr.$-

!! (TeV)

p+ (>>TeV)

matter

Inverse Compton

! (TeV)

e- (TeV) Synchrotron! (eV-keV)

! (eV)

VHE-! from e.g. %0-annihilation

X0 does not directly couple to ! ( else not ‘dark’) ==>

E! !100 GeV

Some important processes to produce VHE !:

q-jets produce much more !, but " result in higher energy !

Where to look for CDM ?

Galactic Center expected to be best candidate

Measurement from HESS, confirmed by MAGICproof VHE dominated by unknown other source

color:MAGIC

white: HESSgreen: VLA 20cm

GC: bright; not accessible by MAGIC; strong foreground signalall other potential ‘classical’ sources: ~100 less DM signal

Andromeda/Virgo: prob.additional foreground signal (like GC) Minihalos: no idea where to point at (need scanning)

J. Buckley,2007

Dwarf Galaxies (DRACO)

predicted cross-sect.for possible SUSYparameters

line: 50h MAGIC==>need looong time

boosting the flux by‘clumpy’ substructuresby factor <10? >1000?

corecore oror cusp cusp (0.1(0.1oo))

m0 < 2TeV

m0 > 2TeV

m0 > 2TeV rescaled for

relic density

Other Idea

Instead of observing known candidates,go for the dark...

CDM clumps could have high VHE flux,but very dim/invisible at long wavelengths(e.g. IMBH [Bertone et al. 2005])

e.g. unidentified EGRET sources with hardspectrum could be good candidates...(and soon unidentified AGILE & GLAST sources)

GLAST MAGICGLAST MAGICAGILE AGILE H.E.S.S.,H.E.S.S., VERITASVERITAS

Satellites measure position and spectrumin GeV range,

Telescopes search for cutoff energy

find several sources, universal spectrum = smoking gun ?!?

Outlook MAGICOutlook MAGIC

-- MAGIC data-takingMAGIC data-taking (and analysis) going (and analysis) going onon

-- construction of 2ndconstruction of 2nd telescope startedtelescope started (same size; some improvements)(same size; some improvements)

==> stereo observations ==> stereo observations gain factor >2 sensitivitygain factor >2 sensitivity (goal: start operation mid 2008) (goal: start operation mid 2008)

-- also:also: HESS (HESS-II), HESS (HESS-II), VERITASVERITAS

MAGICMAGIC (17m) (17m)

MAGIC-IIMAGIC-II (17m) (17m)

and beyond MAGIC

Goal: factor ~10 sensitivity extended Energy range==> HESS/MAGIC combined working groups

1 year

100GeV--10TeV:‘just build more telescopes’(must reduce price/telescope)

extended Energy:need some R&D ...

CTA Physics‘Guaranteed’ Physics in 100GeV-10TeV domain: - ~1000 galactic sources (SNR, Plerions, Binaries, ...) - many AGNs - surprises ....

+ Cosmology and Fundamental Questions: Pop-III stars, Cold Dark Matter, Quantum Gravity, ...

+ chemical composition of charged CR (up to knee ???)

HESS/MAGIC/VERITAS: run as Experiment/Collaboration private data, collab. publications

CTA: run as Observatory: guest observers (+core program) data become public domain ???!!!???

CTA fits into Future Multi-Wavelengthand Multi-Messenger Environment

importantimportantfor CDM...for CDM...

CTA Status

pan-european project ~150M! ?!

APPEC: high priority project on ‘preliminary road map’ESFRI: promising ‘emerging project’ (not yet on roadmap)

FP7: - LoI in preparation - first public meeting 1.&2. March 2007 in Paris (several MAGIC/HESS meetings since Feb. 2006) >300 physicists claimed interest to contribute http://www.mpi-hd.mpg.de/hfm/CTA - request for FP7 design study submitted (May 2)

comparable study/project exists also in the US: ‘AGIS’

ConclusionConclusion

very interesting time for VHE-Astronomyvery interesting time for VHE-Astronomy(and important for indirect CDM searches) ...(and important for indirect CDM searches) ...

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