Abelardo Moralejo, INFN Padova on behalf of the MAGIC ...

MAGIC-II

Abelardo Moralejo, INFN Padova on behalf of the MAGIC collaboration

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The MAGIC collaboration

Collaboration: > 100 physicists, 18 institutes, 11Collaboration: > 100 physicists, 18 institutes, 11

countries:countries:Barcelona IFAE, Barcelona UAB, HU Berlin, CrimeanBarcelona IFAE, Barcelona UAB, HU Berlin, Crimean

Observatory, U.C. Davis, U. Dortmund, U. Lodz, UCM Madrid,Observatory, U.C. Davis, U. Dortmund, U. Lodz, UCM Madrid,

INR Moscow, MPI MINR Moscow, MPI Müünchen, INFN/ U. Padua, INFN/ U.nchen, INFN/ U. Padua, INFN/ U.

Siena, U. Sofia, Tuorla Observatory, Yerevan Phys. Institute,Siena, U. Sofia, Tuorla Observatory, Yerevan Phys. Institute,

INFN/ U. Udine, U. WINFN/ U. Udine, U. Wüürzburg, ETH Zrzburg, ETH Züürichrich

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MAGIC I status

Commissioning ended Aug 2004, first physics results

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Ongoing upgrade of MAGIC I DAQGoal: 2 GSample / s signal sampling (better timing, less NSBnoise). Prototype already tested, system currently in production

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MAGIC-IMAGIC-I MAGIC-IIMAGIC-II

MAGIC II fi second 17 m ∅ telescope

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Design parameters of MAGIC-II

• Second telescope is basically an “improved clone”• Clone:

–Carbon fiber structure and drive system–Control system (central control, camera control)–Optical transmission of analog signals

• (possible) Improvements:–Higher QE camera (better PMTs / HPDs)–Faster, higher resolution FADCs (0.3 ’ 2.5 Gsamples/s)–Improved active mirror control (IR lasers)–1 m2 mirror elements (simpler mechanics)

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Signal sampling: DRS chip

• “Domino Ring Sampler” developed by Stefan Ritt(Paul Scherrer institute) for the m Æ g experiment

• 2.5 GSamples / s (less integrated NSB noise, bettertiming), ≥ 10 bit effective resolution

• DAQ for MAGIC-II in development (Univ. Siena,Padova), prototype already tested on MAGIC-I

Less NSB noise integrated, better timing

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Design of MAGIC-II cameraHigher QE classical PMTs 817 or 919 inner pixels?

>40% peak QE reachablewith PMT “milky coating”

36 %

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HPD camera: mid - term solution

GaAsP photocathode

R9792U-40 18mm GaAsP HPD by HamamatsuOngoing tests and developments @ MPI Munich

Open issues: lifetime,gain(T) dependence…

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Long-term option? SiPM for TESLAby Dolgoshein et al. MEPhI, development @ MPI Munich

1 mm

1 mm

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The stereo principle

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MC simulation (45% peak QE assumed)

Stronger backgroundsuppression thanksnot only to angularresolution:

• Better image shapeparameters (multiplesampling of light pool)

• Estimate of impactparameter

Eg peak ≈ 40 GeV

Eg peak ≈ 40 GeV

dNg/dE µ E-2.6, q = 20º

single

stereo

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Discrimination of Hadrons

Many image parameters can be combined in a single“hadronness” through the Random Forest method (Breiman& Cutler). Here: q2 and Alpha included in RF

single stereo

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Discrimination of Hadrons

Cut: hadronness < X; Q = eg eh is a measure of thebackground suppression power (e ≡ efficiencies)

single

stereo

Qmax ~ 6.4

Qmax ~ 3.7

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MC simulation (45% peak QE assumed)

Eg peak ≈ 180 GeVsingle

Eg peak ≈ 180 GeVstereo

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Flux sensitivity for point-like sources

stereo

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Separation of telescopes

Not critical!

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Location of second telescope

Chosen locationallows for 2 moretelescopes

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Angular resolution

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prelim

inary

Energy resolution (RF estimation)SI

NG

LEST

EREO

4 bins of reconstructed energy; point source location known

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Physics goals

Cold DarkCold DarkMatterMatter

Quantum GravityQuantum Gravityeffectseffects

SNRsSNRs

PulsarsPulsarsGRBsGRBs

AGNsAGNs

cosmologicalcosmologicalgg-Ray Horizon-Ray Horizon

Same as for MAGIC I,but easier to achieve

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Time schedule for MAGIC II

• Telescope structureready to be installed byfall 2005, most otherparts in developmentstage

• GLAST will be launchedin January 2007.

• Goal: MAGIC-II end 2006or beginning 2007