How to use MAGIC for MW campaigns

Alessandro De AngelisUniversity of Udine, INFN and INAF

• MAGIC as it is• Rules for MW with MAGIC• Some results• The next future

Chicago, August 2007

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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

ReflRefl. . surfacesurface::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, 3.5°°FoVFoV576 PMT (QE576 PMT (QEMAXMAX ~ 30%)~ 30%)

AnalogicalAnalogicalTransmissionTransmission((opticaloptical fiberfiber))

22--level Trigger:level Trigger:11ºº levellevel: : coincidencecoincidence22ºº level: pattern recognitionlevel: pattern recognition300 300 MHzMHz DAQDAQ

RapidRapid pointingpointing–– Carbon fiber structureCarbon fiber structure–– Active Mirror ControlActive Mirror Control

⇒⇒ 2020÷÷30 30 secondsseconds

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After upgrade of theoptics in July 2004

And of electronics in April 2006

the telescope is in itsfinal shape

~300Hz shower ratesEth ~40GeV

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the Active Mirror Control laser beams

Photo by R. Wagner

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MAGIC Sensitivity

Large dish => low threshold

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Performance (measured on Crab)

min) 2~in 5(h1

28

σ

σ tceSignifican =

• We are publishing with a threshold of 60 GeV– and still a reasonable

efficiency • We detect significant

signal above 40 GeV– trigger threshold

• Understanding our efficiency towards the goal of 50 GeV.

50h)in @5σ Crab %5.2(

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Should be good for AGN detection…

e+

e-

γEBLγVHE

IACT

Extragalactic Background Lightblazar

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Extragalactic VHE-sources

New HBL 1ES1011+496 z ~ 0.212arXiv:0706.4435

Big progress in AGN studyfrom z < 0.2 to z = 0.538

MAGICFSRQ0.5383C 279

MAGICHBL4.0 0.2121ES 1011+496

HESSHBL0.1881ES 0347-121

HESSHBL2.9 0.1861ES 1101-232

VERITASMAGICHBL3.0 0.1821ES 1218+304

HESSHBL3.1 0.165H 2356-309

HESSHBL0.1391ES 0229+200

HEGRAWhippleHBL3.3 0.1291ES 1426+428

HESSDurhamHBL3.3 0.116PKS 2155-304

HESS/MAGICHBL4.0 >0.09PG 1553

HESSHBL4.0 0.071PKS 2005-489

MAGICLBL3.6 0.069BL Lac

HESSHBL0.069PKS 0548-322

many7TAHBL2.4 0.0471ES 1959+650

MAGICHBL3.3 0.045Mkn 180

MAGICWhippleHBL2.9 0.0441ES 2344+514

manyWhippleHBL2.4 0.034Mkn 501

manyWhippleHBL2.2 0.031Mkn 421

HESSHEGRAFR-I2.9 0.004M 87

ObservationDiscoveryTypeSp.zSource

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GRBs and MAGIC

• MAGIC is the right instrument, due to its fast movement & lowthreshold– MAGIC is in the GCN Network– GRB alert active since Apr 2005

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GRB-alarm from SWIFTGRBGRB--alarm from SWIFTalarm from SWIFTMAGIC data-takingMAGIC dataMAGIC data--takingtaking

We are on the track!

GRB observation with MAGIC: GRB050713a ApJApJ Letters 641, L9 (2006)Letters 641, L9 (2006)

No VHE No VHE γγ emission from emission from GRB positively detectedGRB positively detectedyet...yet...(all other observed GRB very (all other observed GRB very short or at very high z)short or at very high z)

MAGIC

SWIFT

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12+1ES1011, +3C279 (unpublished) (B. De Lotto)

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13(B. De Lotto)

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MAGIC Cycle 1+2• From Apr 2005 to May 2007• ~2000 dark time hours for observation, plus

~200h for ToO– 46% to AGN– 28% to Galactic Sources– 9% to Pulsars– 14% to DM, including M87+ Special projects (τ neutrinos, …)

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MAGIC Cycle3• From June 2007 to May 2008• Deadline expired on Apr 30

– But consideration of new projects in November

• 10% of the time open to external proposals

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Conclusions on MAGIC• MAGIC reached the design performance for 1

telescope – Threshold of 60 GeV for physics analysis; hope to

understand down to 50 GeV, and signal from 40 GeV

• MAGIC is delivering very good physics results– >20 papers published or submitted, with 6 new

sources; more in the pipeline– And the second telescope will see the first light

soon…• Schedule is not published in an official way,

but…

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Multiwavelength: Normal procedure - I

• Every year, AoO open to Guest Observations & Multiwavelength campaigns

• Discussed in the Physics Committee, which tries to identify an internal PI– The internal PI should interact with the external PI in order to

guarantee that the proposal contains all information needed for a correct evaluation

– A suggestion for the internal PI could be attached to the proposal

– People from the collaboration can volunteer to be PI• In general discussed case-by-case, but special

agreements with AGILE and in progress with GLAST

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MAGIC’s Multiwavelength Policy

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MAGIC’s Multiwavelength Policy

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co-authorships are, of course, welcome

plus the external authors, in block if they like

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Some MW results• Many successful ToOs, for example

• 3C279 at z ~ 0.54• 1ES1011• Mkn180• Bl Lac (thanks Gino)• GRBs (the July 05 went into a MW publication w/ Swift)• …

– For one event, we gave the trigger• A big flare on Mkn501, Jul 05 – we do have a monitoring program…

– Several programs are “agreed ToOs” (w/ Integral, optical)• a few real MW (Lindfors, Saggion, Pian, Persic, …)

• 3C454.3 (thanks Dave, Toni, …)• 1ES1959 (w/ Integral) • Mkn421, Mkn501 (keV/TeV correlations)

– Some going on• LSI +61 303 (TeV, X, radio)• …

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Mkn 421 (z=0.030)

• Dec 2004 – Apr 2005 ZA < 30º• 25.6 h, over 7000 excess events• Energy threshold: 150 GeV

TeV-X-ray-correlation

Astro-ph/0603478

TeV

X-ray

optical

LightcurveTeV

X-ray

optical

Clear correlation X-ray γ-ray

(C. Bigongiari)

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Mkn 501 (z=0.034)

Preliminary !VHE

X-rays

Optical

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Mkn 501 (z=0.034)

VHE

X-rays

Optical

Preliminary !

•Observed for 23h in June – July 2005

•Detected at 85 σ level (14k exc. events)

•Analysis threshold 150 GeV

Flare on Jun 29th shows

very fast variability (~4 min) !

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Clear hardening of the spectrum with increasing flux level !

Differential photon spectra fitted with power law:

Low : Flux (E>150 GeV) < 0.5 Crab 12 daysMedium : 0.5 Crab < Flux < 1.0 Crab 8 daysHigh : Flux > 1.0 Crab 2 days (Flare nights excluded)

Mkn 501 (z=0.034)

Preliminary !

Preliminary !

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VHE detection of 3C 279 with MAGIC

• Observation of 3C 279– In the period of January - April 2006– Observation of 9.5hrs in 10 nights– Zenith angle range was between 32 and 40 degrees

relatively high threshold of 120GeV

• Analysis– 4 independent analyses have been done

• Standard analysis and standard quality cut• Relative time image cleaning (lower threshold)• All results are consistent each other

– 6.1 sigma at 80 - 220GeV, and 5.1 sigma above 220GeV

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Sky-map and alpha ploton 23rd Feb 2006

80-220 GeV

E> 220 GeV

PreliminaryPreliminary

Sky map around 3C279Sky map around 3C279

PreliminaryPreliminary

PreliminaryPreliminary

PreliminaryPreliminary

PreliminaryPreliminary

(M. Teshima)

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3C279 VHE gamma-ray light curve

PreliminaryPreliminary

Optical light curveKVA

MAGIC

3C279 was active in optical in 20062~3 times brighter than 2005.

We did not see any apparent correlation between optical and VHE gamma-rays.

PreliminaryPreliminary

(M. Teshima)

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The second MAGIC telescope

News: Electronics, mirrors

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Mirrors: 1m2 layout • 2 technologies:

– INFN (50%) very similar to the half-size mirrors of MAGIC I– INAF (50%) new technology from Brera and MediaLario

Central hole for the laser housing

Mirror box + honeycomb

Front plate

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3 large INFN mirrors already installed in Oct 05

winter has passed… and we manage the technique!

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Mould and panel produced in Medialario Tech.

Aluminum master 1040 x 1040 mm

Front and rear of a produced segment

Size = 985 x 985 mm Weight = 7.5 kg

Nominal radius= 35 m

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Calendar (tentative)

• 3 Medialario mirrors under test in La Palma since December ‘06

• May ’07 Starting mass production first mirrors (INFN)

• October ‘07 First batch installation ?• Mar ’08 Reflector completed ?

• Inauguration on September 21st, 2008

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Performance of MAGIC 2

ARGO

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Conclusions

• MAGIC is working according to the expected performance for 1 telescope– And 2nd telescope operating soon

• We are open to MW observations, and somehow the thing has still to develop organically– Organization

• We should improve our communication– Signature policy