recent highlights of magic razmik mirzoyan on behalf of the magic collaboration max-planck-institute...

Recent Highlights of MAGIC

Razmik MirzoyanOn behalf of the MAGIC

CollaborationMax-Planck-Institute for Physics

Munich, Germany

Razmik Mirzoyan: Recents Highlights of MAGIC

2

Today‘s VHE -g ray Sources in the Sky

Thursday 5th September 2013, YerPhI, Yerevan

~150 Established Sources

http://tevcat.uchicago.edu/


3

The Two 17m Ø MAGIC Telescopes



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System of 2 MAGICs: the main parameters

• Energy threshold (trigger): ~ 50 GeV• Energy threshold in “Sum-Trigger” modus: 25-30 GeV• Energy resolution: 20 % @ 100 GeV; < 15 % @ 1TeV• Angular resolution: 0.1° @ 100 GeV; 0.05° @ 1 TeV• Sensitivity: 7/1000 of Crab Nebula in 50h observations• Light-weight construction, only ~70 T • Fast re-positioning to any coordinates in the sky: 20s/180°• Electro-optical design optimized and set to provide ~2.5ns

FWHM pulses• Data digitized by using 2GSample/s DRS4 chips• Producing ~ 1 TB data per observation nightThursday 5th September 2013, YerPhI, Yerevan


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~170 Collaborating Astro-Physicists from 9 CountriesBulgaria SofiaCroatia Consortium (Zagreb, +…)Finland Consortium (Tuorla, +…)Germany DESY Zeuthen, U. Dortmund,

MPI Munich, U. WürzburgJapan Consortium (Kyoto, +…)Italy INFN & U. Padova, INFN Pisa &

U. Siena, INFN Como/Milano Bicocca, INFN Udine/Trieste & U. Udine,

INAF (Consortium: Rome, +…)Poland LodzSpain U. Barcelona, UAB Barcelona,

IEEC-CSIC Barcelona, IFAE Barcelona, IAA Granada, IAC Tenerife, U. Complutense Madrid, CIEMAT Madrid

Switzerland ETH ZurichThursday 5th September 2013, YerPhI, Yerevan


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The Main Telescopes of the “Roque de los Muchachos” European Northern Observatory


ORM is located on the Canary island of La Palma, at a height of 2200-2400 m a.s.l.


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Beginnings of MAGIC• In mid 1994, still when building the HEGRA telescopes, we

understand that the threshold of an IACT depends inversely on the mirror area (and NOT as square root from the inverse area). That meant one can build very large size telescopes of ~200m² mirror area (~15-20m Ø) providing ~20-times lower threshold of ~50GeV (HEGRA: ~10m², threshold ~1TeV)

• The pioneering work of building the 17m Ø MAGIC was a difficult task, we need to invest plenty of time and efforts

• Other colleagues from HEGRA followed the path of proven technologies (steming from HEGRA and from 10m Ø Whipple). They built H.E.S.S..

• Now, slightly over 10 years after HEGRA, one can say that both decisions were very successful and very much justified!



8

MAGIC technological novelties

• It was impossible to simply up-scale the ~4.2m diameter HEGRA telescopes to the aimed 17m diameter MAGIC

• For successful „invasion“ into <100GeV domain we needed to develop and test quite some number of new technologies– AMC system, all-Al diamond milled mirrors– Light-weight mechanical mount from reinforced CF– Fast repositioning to arbitrary position in the sky (for

„catching“ GRBs)– Super-bialkali PMTs, low gain, VCSELs for optical analog

signal transport, 2GSample/s FADC, sealed, T° controlled camera, ultra-fast electro-optical design of the telescope,…



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Fast Rotation of MAGIC to„catch“ GRB



10

Recently MAGIC reported plenty of results

• Despite the fact that in the last 2 years MAGIC was under upgrade for about 1.5 years long, and only partially in test operation, we made a rich harvest of new results

• MAGIC discovered 20 out of 58 known extra-galactic sources



11Thursday 5th September 2013, YerPhI, Yerevan

IC 310: Unexpected Discovery in the Perseus Cluster of Galaxies

IC 310: detected ≥ 30GeV by Fermi/LAT (Neronov et al. 2010) & ≥ 260GeV by MAGIC (Aleksic et al. 2010)

• Flux and spectral variability in X-ray

• Day-scale variability in VHE, no spectral variability

• Hard spectrum in HE and VHE 2nd hump ≥ 1TeV

• Original head-tail classification not supported

• VLBI reports parsec-scale blazar-like structures; q ≤ 38°

MWL campaign in Nov. 2012 to Feb 2013



VHE Flare of IC 310 on Nov. 12-13 2012

• 28.5 s in 3.5h for E ≥ 250GeV; • Light curve ≥ 300 GeV• Low flux measured after the flare with no significant variations• Variability on a time scale of a few minutes



Mkn-421: Broadband SED Characterization and Modeling on 1-Day Timescales

A two-zone SSC model with a quiescent and flaring blob describes the SED better than the (commonly used) one-zone SSC model



The very low X-ray and VHE activity of Mrk421

• Synchrotron and IC peaks shift to low energies by factor ~10• NuSTAR exquisite characterization of the tail of the synch. bump



Unprecedented flaring activity of Mrk421 during April 2013

• Large flare lasting many days, with VHE gamma-ray fluxes ≥ 11 Crab• Excellent multi-instrument coverage, including strictly simultaneous

observations with Swift and NuSTAR.

• Unprecedented opportunity to test theoretical models• MWL data is currently being analyzed


16

New Source: MS 1221.8+2452 discovered in May 2013


• Blazar • z = 0.218• Discovered in the night April 30th – May 1st • 6.3s in 4h• High synchrotron peaked BL Lac• XBL (X-ray selected BL Lac)• 2.3% Crab ≥ 100GeV• continued observing together with SWIFT

Discovery of Very High Energy Gamma-Ray Emission from MS1221.8+2452 with the MAGIC telescopesATel #5038Juan Cortina (IFAE Barcelona) on behalf of the MAGIC collaboration on 2 May 2013; 19:25 UTCredential Certification: Juan Cortina ([email protected])Subjects: Gamma Ray, TeV, VHE, Request for Observations, AGN, Blazar, TransientThe MAGIC collaboration reports the discovery of very high energy (VHE; E>100 GeV) gamma-ray emission from MS1221.8+2452 (12h24m24.2s +24d36m24s, J2000.0).

mailto:[email protected]





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New Source: H1722+119 discovered in May 2013


• A highly polarised BL Lac• Listed in Costamante & Ghisellini 2002• from Fermi 2nd catalogue• red shift lower limit ≥ 0.17• Simultaneous optical, X-ray, and Fermi LAT data• Measured on May 17-22• ~6.5s in 10h

See ATel #5080

These observations were triggered by the optical high state observed by the Tuorla blazar monitoring program, like many other MAGIC discoveries in the past

Preliminary


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W51

W51A & W51B: star forming regions, W51C medium-age (~30kyr) SNR @ ~5.5 Kpc. Possible PWN CXO J192318.5+1403035 maybe associated with W51C (Koo et al 2005)

The SNR appears to be interacting with W51B (Koo et al. 1997, Green et al. 1997)

High Cosmic Ray ionization, ~100xISM value (Ceccarelli et al. 2011)

MAGIC stereo data taken in 2010 and 2011 (53h), 11 σ signal

0.4º



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The morphology cartoon of W51


J.Krause thesis



W51 as seen by MAGIC

Skymaps: 0.3 < E < 1 TeV

Skymaps: E > 1 TeV


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W51: SNR W51C interacts with molecular clouds in W51BThe broad-band spectral energy distribution can be explained only (1-zone) with a hadronic model. This implies proton acceleration ≥ 50TeV. This result, together with the morphology of the source, tentatively suggests that we are observing ongoing acceleration of ions in the interaction zone between the supernova remnant and the cloud.


Aleksic, et al, 1012


22

Unidentified source HESS J1857+026

• HESS discovery 2008• Crab-like spectrum,

~0.15 C.U.• Extention: 0.11°x0.08°• Distance: 9 kpc (factor

2-3 uncertain)• Age: 21 kyr• PWN candidate: PSR

J1856+0245 detected• Vela-like pulsar nearby• Spin-down luminosity

4.6 x 1036 erg/s



23

MAGIC measurements


• Data taken in 2010• ~ 30h effective observations• ~ 12s detection• Extention (≥ 300GeV): (0.20 ± 0.03stat ± 0.02sys)• Power law spectrum• in 0.4° integration radiusG = 2.24 ± 0.07stat ± 0.15sys (80 GeV – 20 TeV)• Position compatible with H.E.S.S. & Fermi/LAT• Spectral measurements bridging Fermi/Lat and H.E.S.S

Recent results by Fermi/LAT• Spectral slope -1.5 (< 100GeV)• Point-like (> 10GeV)• Leptonic requires low B-field• Also hadronic model possible


24

Morphology from MAGIC measurements


300 – 1000 GeV > 1000 GeV


25

Parameters of resolved regions


Lack of emission between pulsar and MAGIC J1857.6+0297 cast doubt on a common PWN scenario


26

New source: MAGIC J1857.6+0297


For E ≥ 1TeV• 2 spatially separated emission regions, strong signal from each • MAGIC J1857.2+0263 likely the PWN of the pulsar J1856+02245

• MAGIC J1857.6+0297 lies in the vicinity of an HII region, the position of the TeV emission coincides with the possible gas cavity


27

VHE spectrum of the Crab Nebula and of the Pulsar


• MAGIC & VERITAS measured the spectrum of the Crab pulsar stretching till energies as high as 400GeV!• The Crab Nebula spectrum is measured in 50GeV – 50TeV range by MAGIC• But we are learning more and the story is continueing

Crab pulsar: P1 + P2

Aleksic, et al, 2012


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Cartoon of a pulsar



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New data shows much narrower pulsed peaks


In a high statistics data we can see many details, like for example, that the peaks P1 and P2 are very narrowThis could be important for the pulsar theory

recent, preliminary data


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MAGIC Upgrade

• Started upgrade the MAGIC telescope in mid summer 2011• Successfully finished in November 2012• The aim was to use the same cameras, the same readout,

providing stable operation for the next 5-7 years• Decrease dead-time down to 1%, enlarge trigger area of M1

and overlap of 2 telescopes, provide lower by ~(10%) threshold • M-I has got the next built-in in MPP camera (576 -> 1039 pixels)• Both telescopes are readout by using 2GSample/s DRS4 chips• New receiver boards, new trigger• Fully-automatic Sum-Trigger will be implemented in Sept. 2013• We expect a trigger threshold of 25-30GeV with SUM-Trigger Thursday 5th September 2013, YerPhI, Yerevan

Talk by D. Mazin, 1071, GA-IN01


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MAGIC-1 obtained the new 1039 pixel camera



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Next 5-7 years

• Planning to have smooth operation for the next 5-7 years• Software improvements should help to further enhance the

current sensitivity• Next serious improvement of sensitivity is planned to happen

with the installation of SUM-Trigger (fall 2013; currently under construction); threshold ~ 20-30 GeV

• Performance of MAGIC was never as good as it is now• Successful source hunting and deep observation of diverse

source types entered in its most sensitive phase


recent highlights of magic razmik mirzoyan on behalf of the magic collaboration max-planck-institute...

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