STATUS OF THE MAGIC TELESCOPE

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STATUS OF THE MAGIC TELESCOPE
Eckart Lorenz
OVERVIEW SOME GENERAL INFORMATIONS
BASIC MAGIC PARAMETERS PLANS FOR FIRST
MAGIC PHYSICS TECHNICAL ELEMENTS
STATUS APRIL 2003 THE NEXT STEPS
SUMMARY
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The MAGIC Collaboration (14 INSTITUTIONS, 74
PHYSICISTS) Institut de Física d'Altes Energies,
Barcelona Oscar Blanch, Juan Cortina, Eva
Domingo, Enrique Fernández, Jose Flix, Markus
Gaug, Javi López, Manel Martínez Universitat
Autònoma de BarcelonaCarmen Baixeras, Carles
Domingo, Lluis Font, Raul Orduna, Alejandro
Sánchez, Andreu Torres   Crimean Astrophysical
Observatory Arnold Stepanian   University of
California, Davis Daniel Ferenc, Alvin Laille  
Division of Experimental Physics, University of
Lodz Maria Giller, Piotr Jacon, Dorota
Sobczynska, Tadeusz Wibig   Universidad
Complutense, Madrid Luis José Contreras,
Victoria Fonseca, Marcos López, Emma Oña, Raquel
Reyes   Max-Planck-Institut für Physik,
MünchenRudolf K. Bock, José Antonio Coarasa,
Markus Garczarczyk, Jurgen Gebauer, Florian
Goebel, Eckart Lorenz, Keiichi Maze, Razmick
Mirzoyan, David Paneque, Nadia Tonello, Vincenzo
Vitale, Robert Wagner, Wolfgang Wittek  
Dipartimento di Fisica, Università di
Padova Laura Alciati, Denis Bastieri, Ciro
Bigongiari, Nicola Galante, Mosè Mariotti,
Abelardo Moralejo, Donatella Pascoli, Luigi
Peruzzo, Antonio Saggion, Villi Scalzotto  
Space Research Unit, Potchefstroom University 
Okkie C. de Jager Fachbereich Physik,
Universität-GH Siegen Thomas Hengstebeck,
Nikolaj Pavel, Ralf Stiehler, Serguei Volkov  
Dipartimento di Fisica, Università di
Siena Mario Meucci, Riccardo Paoletti, R.Pegna,
A.Piccioli, Antonio Stamerra, Nicola Turini
Tuorla Observatory, Pikkiö Aimo Sillanpää, Leo
Takalo   Universität WürzburgThomas Bretz,
Eduardo Colombo, Tanja Kneiske, Karl Mannheim,
Martin Merck   Yerevan Physics Institute, Cosmic
Ray Division, Yerevan Ashot Chilingarian New
Candidate a group from the ETH Zurich
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THE MAGIC TELESCOPE (Major Atmospheric
Gamma Imaging Cherenkov Telescope) A NEW
TECHNOLOGY GROUND-BASED 17 m DIAMETER IMAGING
CHERENKOV TELESCOPE LOCATED ON LA PALMA 28.8 N,
17.8 W, 2225 m asl (at old HEGRA site) LOW
THRESHOLD 30 GeV (phase I, classical pmts)
12-15 GeV (phase
II, high QE pmt)
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LOW THRESHOLD HIGH SENSITIVITY POSITIONING UP TO
90 ZA FAST POSITIONING, GRBs OPERATION DURING
MOONLIGHT
PHYSICS GOALS AGN STUDIES, g HORIZON SEARCH
FOR GRBs,needs fast alert PULSAR STUDIES SNRs
(small FOV limits) unidentified EGRET
sources NEW PHYSICS (QUANTUM G,)
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NOVEL COMPONENTS LOW WEIGHT CF SPACE FRAME
CONSTRUCTION, 5 TONS
OK
LIGHT WEIGHT ALL-ALU MIRRORS, DIAMOND
TURNED, INTERNAL HEATING OK 99 m2 INSTALLED
LAST YEAR, 15 IN APRIL, 100 IN JUNE ACTIVE
MIRROR CONTROL, FULL TEST STILL MISSING
(OK) PROBLEM
WITH A DEFECT ALLEGRO DRIVE CHIP FOR STEPPING
MOTORS HEMISPHERICAL PMTS WITH 6 STAGES,
IMPROVED QE CAN WORK IN THE PRESENCE OF
MOONSHINE
OK FAST PMT SIGNAL
TRANSMISSION IN ANALOG MODE BY OPTICAL FIBERS
DYN. RANGE 60 dB BW 230 MHZ


OK 300 MHZ F-ADC WITH HIGH, LOW
RANGE SWITCHING,
(OK) 2/3 IN LA PALMA, REST IN
MAY LEVEL 0,1 AND 2 TRIGGER READY (NOT ALL
OPTIONS TESTED) OK
1 KHZ DATA RATE, PROOF STILL MISSING
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FLYING IN OF MIRROR SUPPORT SPACEFRAME, CAMERA
SUPPORT THETA DRIVE RING COMBINED WEIGHT 8.5 TONS
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TELESCOPE MECHANICS
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TELESCOPE MECHANICS
TELESCOPE MECHANICS LESS PROBLEMS THAN
EXPECTED CF TUBES HAVE HIGHER DAMPING THAN
STEEL OR ALU. TESTED DISTORTIONS AS PREDICTED
(FINITE ELEMENT SIMULATIONS VERY USEFULL)
TELESCOPE SURVIVED FIRST STRONG STORM (100
miles/h GUSTS WITHOUT PROBLEMS) THE SINGLE
CAMERA MAST SOLUTION WITH STEEL CABLE OK
AND VERY STABLE. CAMERA SAGS BY 1 cm (AS
PREDICTED) A DESIGN GOAL AND A TECHNICAL
CHALLENGE TELESCOPE SHOULD BE REPOSITIONED
WITHIN 20 SEC. TO ANY POINT ON THE SKY FOR GRB
STUDIES. GOAL NEARLY ACHIEVED 20 SEC. FOR
180 IN DECLINATION (OK) 30 SEC. FOR 180 IN
AZIMUTH. STEERING SOFTWARE STILL NOT
OPTIMIZED, SOME POWER LIMITATIONS.
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MIRROR
THE MIRROR 17 m DIAMETER, 234 m2 TESSALETED,
PARABOLIC PROFILE ISOCHRONOUS D t lt 0.25
nsec 934 SMALL MIRRORS 49.5x 49.5 cm2, All raw
blanks made, 900 mirrrors diamond turned 150 m2
assembled of installed mirrors 99
115 220 234
Nov 02 April 03 June 03
??
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MIRROR
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MIRROR
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MIRROR
Mirrors quartz coated
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MIRROR
TEST SURFACE ROUGHNESS OF DIAMOND TURNED MIRRORS
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MIRROR
INSTALLATION OF MIRROR PANELS
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MIRROR
Status mirror installation Nov 2002
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ACTIVE MIRROR CONTROL
Principle of avtive mirror Control (AMC)
PC SERVO AMPS
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TEST ACTIVE MIRROR CONTROL IMAGE OF A LIGHT SPOT
935m AWAY 30 OF 99 MIRRORS FOCUSSED IMAGES ON
CAMERA COVERAGE
0.1
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TEST ACTIVE MIRROR CONTROL PHOTO OF CAMERA COVER
WITH MOON IMAGE, 30 OUT OF 99 MIRRORS FOCUSSED
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TEST ACTIVE MIRROR CONTROL
PHOTOGRAPH OF THE LASER POINTERS
REFLECTION ON CAMERA COVER, IN 2 MIRRORS
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CAMERA
CAMERA 4 DIAMETER 394 PIXELS 0.1, 180
PIXELS 0.2 6 DYNODE , HEMISPHERICAL CATHODE
PMTS, GAIN 2x104 FAST PREAMP -gt OPERATION
DURING MOONSHINE POSSIBLE SPECIAL GEOMETRY
WINSTON CONES IN CENTRAL REGION OFTEN PHOTON
TRAJECTORY PASSES 2x CATHODE SPECIAL TREATMENT
OF CATHODE WINDOW WITH LAQUER LOADED WITH WLS,
FROSTED SURFACE -gt QE INCREASE BY 30 (-gt 300
m2 mirror of classical type) NEXT LINING
WINSTON CONES WITH 98 REFLECTIVITY FOIL -gt GAIN
13-20 CAMERA TESTED AND INSTALLED ON
TELESCOPE IN LATE NOVEMBER
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CAMERA
A METHOD TO INCREAS E THE QECOAT WINDOW WITH A
LAQUER LOADED WITH WLS AND USING A FAST
EVAPORATING SOLVENT -gt FORMS FROSTED
WINDOW SURFACE LAYER
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CAMERA
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CAMERA
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CAMERA
AREA RATIO OF Winston Cone/PMT1.91
PM GAIN 10 000 PM type 9116A NOTE NON-NEGL.
SENSITIVITY TO NSB LIGHT SCATTERED FROM GROUNG
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PHOTOGRAPH OF CAMEREA, PMT SIDE, WITHOUT WINSTON
CONE PLATE
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CAMERA
PHOTO OF CAMERA, COVER CLOSED
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CONNECTION BETWEEN CAMERA AND DAQ
MAGIC USES OPTICAL FIBERS FOR THE ANALOG SIGNAL
TRANSFER FROM CAMERA PMTS TO THE 100 M AWAY
COUNTING HOUSE PROS LOW WEIGHT OF CAMERA
(OSCILLATIONS REDUCED) REDUCED
ELECTRONICS IN CAMERA -gt LESS DOWNTIME DUE TO
DEFECTS LOW POWER CONSUMPTION IN
CAMERA EASIER TO MODIFY ELECTRONICS
(TRIGGER) EASIER TO IMPLEMENT
TRIGGER FOR MULTITELESCOPESYSTEM CONS NEW
PRINCIPLE, NO EXPERIENCE EXTRA
COSTS USE OF VCSELS AS LIGHT EMITTER (CAN DRIVE
TO 200 MA PULSE CURRENT FOR LOW DUTY CYCLE. HIGH
BANDWIDTH (gt 1 GHZ POSSIBLE, NOW 230 MHZ BW) NO
ATTENUATION OVER 165 M LENGTH ACHIEVED DYNAMIC
RANGE 800 (LINEAR), gt 1000 WITH SOME
NONLINEARITY WE ARE WORKING ON NEXT GENERATION
MONOMODE VCSELS. -gt HIGHER STABILITY, LOWER
NOISE, LOWER POWER
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CONNECTION CAMERA -gt COUNTING HOUSE
FAST PM SIGNAL TRANSMISSION BY OPTICAL FIBER
SYSTEM WORKING IN ANALOG MODE
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CONNECTION CAMERA -gt COUNTING HOUSE
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CALIBRATIONS
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LIGHT PULSER SIGNAL, OUTPUT OF FADC (1 channel
3.3 nsec) 50 pe, LP signalwidth 3 nsec, signal
integrated at FADC input, t 5 nsec
CALIBRATIONS
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CALIBRATIONS
FIRST LIGHT PULSER TEST OF A CAMERA SEXTANT, 8
pixels missing
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MORE ON STATUS FIRST TEST RUNS WITH 100 m2
MIRROR ONGOING (MAINLY CAMERA TESTS BECAUSE
DEFECT AMC CHIP FOR STEPPERS) COMPLETION OF
NEARLY FULL MIRROR JUNE 2003 MIRRORS AT PART OF
THE OUTER RIM LATER PHYSICS RUNS SHOULD BEGIN IN
MID 2003 COUNTING HOUSE LATE JUNE/JULY 2003 -gt
SERIOUS INSTALLATION PROBLEMS OF
ELECTRONICS SOME FUNDING FLOW PROBLEMS
(CUTS) ALSO DIFFICULTIES TO LINK DIFFERENT
ELEMENTS THE LAST 5 PROBLEM INAUGURATION
PLANNED FOR OCTOBER 2003
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COSTS, FUNDING CURRENT PRICE OF TELESCOPE 4.5 M
(including counting house) MAINLY FUNDED BY
ITALY, SPAIN, GERMANY( 50) THE GENERAL
FUNDING OF ALL COLLABORATION PARTNERS STARTED NOV
2000
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A SUMMARY OF THE PHYSICS PROGRAM, OVERVIEW
SEARCH FOR YOUNG SUPERNOVA REMNANTS (SNR)
considered as the sources of the galactic CRs
STUDY OF PLERIONS fundamental pulsar tests.
Polar cap vs. outer gap models DIFFUSE g
EMISSION FROM THE GALACTIC DISK information
about the gas and dust density in the galactic
plane STUDY OF ACTIVE GALACTIC NUCLEI AGN
studies, Black Hole studies, test of the EBL
(IR), -gt info about star formation in early
universe, contribution to the Dark Matter
puzzle POSSIBLE STUDY OF GAMMA RAY BUSTS
(GRB) energy spectra, light curve. Needs fast
slewing detectors fast alert from
satellites SEARCH FOR POSSIBLE g EMISSION FROM
TOPOLOGICAL DEFECTS very difficult, either
isotropic flux or slightly peaked in direction
SEARCH FOR THE LIGHTEST SUPERSYM. PARTICLES gs
would be generated in annihilation processes,
which might occur near center of our galaxy
TEST OF QUANTUM GRAVITYEFFECTS by means of
study of time delays(energy dep.) in variable
sources (AGNs, GRBs)
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SENSITIVITY OF DIFFERENT g RAY DETECTORS
SENSITIVITY OF DIFFERENT g RAY DETECTORS
EGRET
GLAST
PHASE 2
HEGRA SYS.
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CURRENT TELESCOPE SIMULATIONS PREDICT FOR PHASE
I threshold (peak of differential
spectrum) will be slightly below 30 GeV
partly due to improved Winston cones and QE of
PMTs telescope quite sensitive to g showers
below 20 GeV -gt important for GRB and
Pulsar studies -gt dedicated trigger initial
sensitivity not as high as originally predicted
mainly due to misidentified hadrons, muons
seem to be less problematic (hard numbers
missing) for better g/h serparation and
better MC predictions we need real data for the
simulations also we have not yet explored
all tools for g/h separation
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HEGRA
A WARNING THE THRESHOLD OF IACTS HAS A STRONG
ZENITH ANGLE DEPENDENCE
CANGAROOIII
MAGIC PHASE I
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THE FUTURE AFTER MAGIC I (AFTER DEMONSTRATION
THAT THE NEW COMPONENTS OF MAGIC WORK) ADD 1
(2) MORE TELESCOPES AT THE SAME SITE
OBSERVATION OF MORE THAN ONE SOURCE IN PARALLEL
STEREO OBSERVATIONS CONFLICT OF INTEREST
MORE SOURCES vs. HIGHER PRECISION A) a slightly
improved CLONE of 17 m diameter (cost 2.8-4 M,
2-2.5 years construction time) B)
Intensify developments of a CAMERA with high QE
red-extended PMTs to lower threshold to
12 GeV, increase sensitivity below 50 GeV if
development successful-gt exchange camera (cost
1.6-3 M) C) alternative under discussion
instead of 17 m clone build a larger telescope
(25-30 m diameter) with high QE camera and
operate together with MAGIC I gt 5-6 years
construction / funding constraints INTENSE
DISCUSSIONS IN COLLABORATION
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DEVELOPMENTS FOR HIGH QE CAMERA HYBRID PMT
PHOTOGRAPH OF TEST UNITS
SMALL HAPD FOR TESTS OF THE AD PERFORMANCE
TEST UNIT FOR 18 MM GLASS WINDOW WITH GaAsP
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DEVELOPMENTS FOR HIGH QE CAMERA HYBRID PMT
of prototype Hybrid PMT
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CONCLUSIONS
MAGIC INSTALLATION PROCEEDS WELL, TO BE COMPLETED
2003 1 YEAR BEHIND ORIGINAL PLANS, BUT
FUNDING WAS DELAYED BY 2 YEARS ALL NEW
TECHNOLOGY ELEMENTS WORK AS EXPECTED HARD
FIELD TESTS STILL MISSING RAPID REPOSITIONING
GOAL 20 SEC FOR ANY POSITION ON SKY 20 SEC.
ACHIEVED IN DECLINATION, IN AZIMUTH STILL 30 SEC.
MAGIC FULLY OPERATIONAL FOR PHYSICS IN 2003
(IF NO LATE SURPRISES) WE EXPECT A PHASE I
THRESHOLD CLOSE BELOW 30 GEV, BUT SENSITIVITY
WILL BE BELOW PREDICTIONS IN THE RUN-IN PHASE
MAGIC ALONE FOR LOW THRESHOLD OBSERVATIONS ON THE
NORTHERN HEMISPHERE FOR SOME YEARS
POTENTIAL TO FIND A FEW 100 NEW SOURCES
PLANNING FOR 2.(3.) LARGE TELESCOPE STARTED TO
CONVERT TELESCOPE COMPLEX INTO A GAMMA-RAY
OBSERVATORY
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DEVELOPMENTS FOR HIGH QE CAMERA HYBRID PMT
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