MAGICAlessandro De Angelis

July 2006

• Performance & results• Plans for Cycle 2• The second telescope

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Grantecan

MAGIC and its Control House

Telescopio Nazionale Galileo

MAGIC

La Palma, IAC28° North, 18° West

MAGIC

The MAGIC site

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MAGIC

17 m

17 m

Refl. surface:Refl. surface:236 m236 m22, F/1, 17 m , F/1, 17 m

– – 964 heated mirrors on 247 panels964 heated mirrors on 247 panels– – Lasers+mechanisms for AMCLasers+mechanisms for AMC

CameraCamera::~ 1 m ~ 1 m , 3.5°FoV, 3.5°FoV576 PMT (QE576 PMT (QEMAXMAX ~ 30%) ~ 30%)

AnalogicalAnalogicalTransmissionTransmission(optical fiber)(optical fiber)

2-level Trigger:2-level Trigger:1º level: coincidence 1º level: coincidence 2º level: pattern recognition2º level: pattern recognition300 MHz DAQ300 MHz DAQ

Rapid pointingRapid pointing – – Carbon fiber structureCarbon fiber structure – – Active Mirror ControlActive Mirror Control 20÷30 seconds20÷30 seconds

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After upgrade of the optics in July 2004

the telescope is in its final shape

~300Hz shower ratesEth ~40GeV

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the Active Mirror Control laser beams

Photo by R. Wagner

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Photograph of the 576-pixel imaging camera of MAGIC-I.In the central part one can see the 396 high resolution pixelsof 0.1° size. Those are surrounded by 180 pixels of 0.2°.

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Performance

Angular resolutionAngular resolution0.08° @ 1 TeV0.08° @ 1 TeV

0.1° @ 200 GeV0.1° @ 200 GeVEnergy resolutionEnergy resolution

20% @ 1 TeV20% @ 1 TeV30% @ 100 GeV30% @ 100 GeV

10-14

10-13

10-12

10-11

10 100 1000 104 105

E x

F(>

E) [

TeV

/cm2 s]

E [GeV]

Crab

10% Crab

1% Crab

GLAST

MAGIC

HESS

E.F(>E) [TeV/cm2s]

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Cycle1 (Feb 2005-Apr 2006)• Statistics of physics runs for Cycle1:

– 1070 hours dark time out of 1714, plus 150 h “good technical runs”, and 212 hours moon

• Moon time increasing to an asymptotical value ~1/3– ~100 hours ToO (with some important results)

• will increase with the increased number of collaborations– Suzaku, Swift, GLAST, AGILE, …

• All data analyzed– Papers published or submitted for all positive

signals, but 6 (Crab, Mkn501, x, y, z)• 2 GRB observations during the primary burst• MAGIC Catalog opened (MAGIC Jxxx-yyy)

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Cycle2• From period 42, starting on May 14, 2006, to period

54, ending on May 29, 2007• 840 dark time hours recommended for observation

time in Class A, plus a maximum (?) of 236h for ToO – 46% to AGN– 28% to Galactic Sources– 9% to Pulsars– 14% to DM, including M87+ Special projects (neutrinos, …)

GRB fully accepted (36h ToO) – going towards a further improvement of the response time

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MAGIC scientific papers in 2006I: AGNs

1. “Observation of VHE emission from the AGN 1ES1959+650 with MAGIC”, ApJ 639 (2006) 761.

2. “Discovery of VHE -ray emission from 1ES1218+30.4”, ApJ Lett. 642 (2006) 119.

3. “Observations of Mkn 421 with MAGIC”, astro-ph/0603478, accepted for publication in ApJ.

4. “Detection of VHE radiation from the BL Lac PG 1553+113 with the MAGIC telescope”, astro-ph/0606161, subm. to ApJ-Lett.

5. “Discovery of VHE g-rays from Markarian 180 triggered by an optical outburst”, astro-ph/0606630, subm. to ApJ Lett.

PG1553:source at z~0.3detected at 9

1ES1218 (z=0.18)New Source

PG 1553 (New source )

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MAGIC scientific papers in 2006 II: SNRs and QSR 6. “MAGIC observations

of VHE -rays from HESS J1813-178”, ApJ Lett. 637 (2006) 41.

7. “Observation of VHE radiation from HESS J1834-087/W41 with MAGIC”, ApJ Lett. 643 (2006) 53.

8. “Variable Very High Energy Gamma-Ray Emission from the QSR LS I+61 303”, Science, May 2006.

Index –2.5 ± 0.2

90 cm VLA (green) + MAGIC (bck) + 12CO (black)

Source is Extended!

First QSR at VHE (up to 5 TeV)Hint of periodicity over 6T

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MAGIC scientific papers in 2006 - III

9. “Flux upper limit of -ray emission by GRB050713a from MAGIC”, ApJ Lett. 641 (2006)

10. “Observation of rays from the Galactic Center with MAGIC”, ApJ Lett. 638 (2006) 101.

+ 7 additional publications in the pipeline (including 3 new sources)

GRB050713aGRB050904 (in prompt phase)

And response timeIMPROVING!

Galactic Center

2min resolutionLight curve

Mkn501 giant flareBins of 2 min

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ExtragalacticSource Redshift Spectral Index Type Detection (>5) ConfimationM87 0.004 2.9 FR I HESSMkn 421 0.031 2.2 BL Lac Whipple ManyMkn 501 0.034 2.4 BL Lac Whipple Many1ES 2344+514 0.044 2.9 BL Lac Whipple HEGRA,MAGIC1ES 1959+650 0.047 2.4 BL Lac Tel. Array ManyPKS 2005-489 0.071 4.0 BL Lac HESSPKS 2155-304 0.116 3.3 BL Lac Mark VI HESSH1426+428 0.129 3.3 BL Lac Whipple ManyH2356-309 0.165 3.1 BL Lac HESS1ES 1218+304 0.182 3.0 BL Lac MAGIC1ES 1101-232 0.186 2.9 BL Lac HESSPG 1553 >0.25 4.0 BL Lac MAGIC

BL Lac objects

1.5

2.0

2.5

3.0

3.5

4.0

4.5

0 0.1 0.2 0.3 0.4Redshift Parameter z

Spec

tral I

ndex

PKS2005 PG1553

New Sources

At least a handle on EBL, but also the possibility of accessing cosmological constants (Martinez et al.) could become reality soon (maybe including X-ray obs.)

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The threshold• We are publishing with a

threshold of 70 GeV • We detect significant

signal above 40 GeV• Understanding our

efficiency towards the goal of 40 GeV. A special task force (UHU) has been set up; preliminary physics results at 50 GeV.– Substantial improvement

on DM studies and determination of cosmological constants

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The second telescope

• Structure finished in December 2005 (in schedule)• Essentially a clone of the 1st telescope, but improved

– Mirrors– Camera– Electronics

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Mirrors: 1m2 layout • Very similar to the half-size mirrors of MAGIC I

Central hole for the laser housing

Mirror box + honeycomb

Front plate

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3 large mirrors already installed in Oct 05

winter has passed… and we manage the technique!

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Conclusions• MAGIC is close to the design performance for 1

telescope – Threshold of 70 GeV for physics analysis; close to

understand down to 50 GeV, and signal from 40 GeV• MAGIC is delivering very good physics results

– In 2006, 7 papers published (one in Science) and 3 submitted, with 4 new sources; 6 papers in the pipeline, with 2-3 additional new sources

• Cycle 2: important commitment to test more fundamental physics (DM, Lorentz violation, …)

• Second telescope in construction– New 1m2 mirrors successfully tested on the 1st telescope