Recent Highlights of MAGIC Razmik Mirzoyan On behalf of the MAGIC Collaboration Max-Planck-Institute for Physics Munich, Germany

Today‘s VHE  ray Sources in the Sky Thursday 5th September 2013, YerPhI, Yerevan Razmik Mirzoyan: Recents Highlights of MAGIC 2 ~150 Established Sources

The Two 17m Ø MAGIC Telescopes Thursday 5th September 2013, YerPhI, Yerevan Razmik Mirzoyan: Recents Highlights of MAGIC 3

System of 2 MAGICs: the main parameters Energy threshold (trigger): ~ 50 GeV Energy threshold in “Sum-Trigger” modus: GeV Energy resolution: GeV; < 15 1TeV Angular resolution: 100 GeV; 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 night Thursday 5th September 2013, YerPhI, Yerevan Razmik Mirzoyan: Recents Highlights of MAGIC 4

~170 Collaborating Astro-Physicists from 9 Countries BulgariaSofia CroatiaConsortium (Zagreb, +…) FinlandConsortium (Tuorla, +…) Germany DESY Zeuthen, U. Dortmund, MPI Munich, U. Würzburg JapanConsortium (Kyoto, +…) ItalyINFN & U. Padova, INFN Pisa & U. Siena, INFN Como/Milano Bicocca, INFN Udine/Trieste & U. Udine, INAF (Consortium: Rome, +…) PolandLodz SpainU. Barcelona, UAB Barcelona, IEEC-CSIC Barcelona, IFAE Barcelona, IAA Granada, IAC Tenerife, U. Complutense Madrid, CIEMAT Madrid Switzerland ETH Zurich Thursday 5th September 2013, YerPhI, Yerevan Razmik Mirzoyan: Recents Highlights of MAGIC 5

The Main Telescopes of the “Roque de los Muchachos” European Northern Observatory Thursday 5th September 2013, YerPhI, Yerevan Razmik Mirzoyan: Recents Highlights of MAGIC ORM is located on the Canary island of La Palma, at a height of m a.s.l. 6

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! Thursday 5th September 2013, YerPhI, Yerevan 7 Razmik Mirzoyan: Recents Highlights of MAGIC

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,… Thursday 5th September 2013, YerPhI, Yerevan Razmik Mirzoyan: Recents Highlights of MAGIC 8

Fast Rotation of MAGIC to„catch“ GRB Thursday 5th September 2013, YerPhI, Yerevan Razmik Mirzoyan: Recents Highlights of MAGIC 9

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 Thursday 5th September 2013, YerPhI, Yerevan Razmik Mirzoyan: Recents Highlights of MAGIC 10

Thursday 5th September 2013, YerPhI, Yerevan Razmik Mirzoyan: Recents Highlights of MAGIC 11 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  2 nd hump ≥ 1TeV Original head-tail classification not supported VLBI reports parsec-scale blazar-like structures;  ≤ 38°  MWL campaign in Nov to Feb 2013

Thursday 5th September 2013, YerPhI, Yerevan Razmik Mirzoyan: Recents Highlights of MAGIC 12 VHE Flare of IC 310 on Nov  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

Thursday 5th September 2013, YerPhI, Yerevan Razmik Mirzoyan: Recents Highlights of MAGIC 13 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

Thursday 5th September 2013, YerPhI, Yerevan Razmik Mirzoyan: Recents Highlights of MAGIC 14 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

Thursday 5th September 2013, YerPhI, Yerevan Razmik Mirzoyan: Recents Highlights of MAGIC 15 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

New Source: MS discovered in May 2013 Thursday 5th September 2013, YerPhI, Yerevan Razmik Mirzoyan: Recents Highlights of MAGIC 16 Blazar z = Discovered in the night April 30th – May 1st 6.3  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 MS with the MAGIC telescopes ATel #5038 Juan Cortina (IFAE Barcelona) on behalf of the MAGIC collaboration Juan Cortina (IFAE Barcelona) on behalf of the MAGIC collaboration on 2 May 2013; 19:25 UT Credential Certification: Juan Cortina Subjects: Gamma Ray, TeV, VHE, Request for Observations, AGN, Blazar, Transient The MAGIC collaboration reports the discovery of very high energy ( VHE; E>100 GeV) gamma-ray emission from MS (12h24m24.2s +24d36m24s, J2000.0).

New Source: H discovered in May 2013 Thursday 5th September 2013, YerPhI, Yerevan Razmik Mirzoyan: Recents Highlights of MAGIC 17 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 ~6.5  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

W51 W51A & W51B: star forming regions, W51C medium-age (~30kyr) ~5.5 Kpc. Possible PWN CXO J 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 Thursday 5th September 2013, YerPhI, Yerevan 18 Razmik Mirzoyan: Recents Highlights of MAGIC

The morphology cartoon of W51 Thursday 5th September 2013, YerPhI, Yerevan Razmik Mirzoyan: Recents Highlights of MAGIC 19 J.Krause thesis

Thursday 5th September 2013, YerPhI, Yerevan Razmik Mirzoyan: Recents Highlights of MAGIC W51 as seen by MAGIC Skymaps: 0.3 < E < 1 TeV 20 Skymaps: E > 1 TeV

W51: SNR W51C interacts with molecular clouds in W51B The 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. Thursday 5th September 2013, YerPhI, Yerevan 21 Razmik Mirzoyan: Recents Highlights of MAGIC Aleksic, et al, 1012

Unidentified source HESS J 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 J detected Vela-like pulsar nearby Spin-down luminosity 4.6 x erg/s Thursday 5th September 2013, YerPhI, Yerevan Razmik Mirzoyan: Recents Highlights of MAGIC 22

MAGIC measurements Thursday 5th September 2013, YerPhI, Yerevan Razmik Mirzoyan: Recents Highlights of MAGIC 23 Data taken in 2010 ~ 30h effective observations ~ 12  detection Extention (≥ 300GeV): (0.20 ± 0.03 stat ± 0.02 sys ) Power law spectrum in 0.4° integration radius  = 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

Morphology from MAGIC measurements Thursday 5th September 2013, YerPhI, Yerevan Razmik Mirzoyan: Recents Highlights of MAGIC – 1000 GeV > 1000 GeV

Parameters of resolved regions Thursday 5th September 2013, YerPhI, Yerevan Razmik Mirzoyan: Recents Highlights of MAGIC 25 Lack of emission between pulsar and MAGIC J cast doubt on a common PWN scenario

New source: MAGIC J Thursday 5th September 2013, YerPhI, Yerevan Razmik Mirzoyan: Recents Highlights of MAGIC 26 For E ≥ 1TeV 2 spatially separated emission regions, strong signal from each MAGIC J likely the PWN of the pulsar J MAGIC J lies in the vicinity of an HII region, the position of the TeV emission coincides with the possible gas cavity

VHE spectrum of the Crab Nebula and of the Pulsar Thursday 5th September 2013, YerPhI, Yerevan Razmik Mirzoyan: Recents Highlights of MAGIC 27 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

Cartoon of a pulsar Thursday 5th September 2013, YerPhI, Yerevan Razmik Mirzoyan: Recents Highlights of MAGIC 28

New data shows much narrower pulsed peaks Thursday 5th September 2013, YerPhI, Yerevan Razmik Mirzoyan: Recents Highlights of MAGIC 29 In a high statistics data we can see many details, like for example, that the peaks P1 and P2 are very narrow This could be important for the pulsar theory recent, preliminary data

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 We expect a trigger threshold of 25-30GeV with SUM-Trigger Thursday 5th September 2013, YerPhI, Yerevan Razmik Mirzoyan: Recents Highlights of MAGIC 30 Talk by D. Mazin, 1071, GA-IN01

MAGIC-1 obtained the new 1039 pixel camera Thursday 5th September 2013, YerPhI, Yerevan Razmik Mirzoyan: Recents Highlights of MAGIC 31

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 ~ 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 Thursday 5th September 2013, YerPhI, Yerevan Razmik Mirzoyan: Recents Highlights of MAGIC 32