NewScientist Magazine, issue 2620 Finally, a MAGIC test for string theory? 08 September 2007 Zeeya Merali

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1 BEING 4 minutes late doesn't usually cause physicists around the world to fizz with excitement - but it's a different matter if the latecomer is a photon, and its tardiness could indicate a breakdown of relativity on cosmic scales. What's more, this delay could provide us with our first hints of quantum gravity at work, and thus be a unique way of testing string theory. NewScientist Magazine, issue 2620 Finally, a MAGIC test for string theory? 08 September 2007 Zeeya Merali

2 MAGIC Gamma-Ray Observatory Test of relativity breakdown and Quantum Gravity Daniel Ferenc (UC Davis), for the MAGIC Collaboration Dario Hrupec, IRB CROATEA Cosmic Ray Observatory At The Eastern Adriatic

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4 Daniel Ferenc of U.C. Davis on the MAGIC team writes: "There have been attempts to observe time lags in gamma flares and in gamma-ray bursts, but we have never seen something like this... We should keep in mind that the effect may still be inherent to the process of the emission of gamma rays in the source, although not very likely. We are rapidly learning about such emission processes in AGNs from new data collected by MAGIC, HESS, VERITAS, and CANGAROO, in coincidence with x-ray and optical measurements, and will know more soon."

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9 KVANTNE FLUKTUACIJE QUANTUM FOAM - na kratkoj prostorno-vremenskoj skali [2] MODELI: non-critical string theory [3], loop quantum gravity [4], string theory [5], double special relativity [6] and an effective field theory approach [7]. [2] G. Amelino-Camelia, J. R. Ellis, N. E. Mavromatos and D. V. Nanopoulos, Int. J.Mod. Phys. A 12 (1997) 607 [arxiv:hep-th/ ]. [3] J. R. Ellis, N. E. Mavromatos and D. V. Nanopoulos, Phys. Lett. B 293 (1992)37 [arxiv:hepth/ ]; For reviews see: J. R. Ellis, N. E. Mavromatos and D. V. Nanopoulos, Erice Subnucl. Phys. Series, Vol (World Sci. 1994) [arxiv:hep-th/ ]; J. Chaos, Solitons and Fractals, Vol. 10 (1999) 345 (eds. C. Castro and M.S. El Naschie, Elsevier Science, Pergamon 1999) [arxiv:hep-th/ ]. [4] R. Gambini and J. Pullin, Phys. Rev. D 59 (1999) [arxiv:gr-qc/ ]; J. Alfaro, H. A. Morales-Tecotl and L. F. Urrutia, Phys. Rev. D 65 (2002) [arxiv:hepth/ ]. [5] V. A. Kostelecky and S. Samuel, Phys. Rev. D 39 (1989) 683. [6] G. Amelino-Camelia, Int. J. Mod. Phys. D 11 (2002) 35 [arxiv:gr-qc/ ]. [7] R. C. Myers and M. Pospelov, Phys. Rev. Lett. 90 (2003) [arxiv:hep-ph/ ].

10 SIRENJE SVJETLOSTI kroz KVANTNU PJENU Quantum Gravity Netrivijalna disperzijska relacija u vacuumu [*] Narusenje relativisticke teorije Brzina svjetlosti: c(e) c 0 (1 (E/M) n ) Index loma vacuuma 1 (E/M QGn ) n, n = 1, 2 E = energija fotona, c 0 = niskoenergetska brzina svjetlosti M = masena skala za kvantno-gravitacijske efekte TEST mjerenje funkcije c(e) [*] G. Amelino-Camelia, J. Ellis, N. Mavromatos, D. Nanopoulos and S. Sarkar, Nature 393 (1998) 763.

11 TEST mjerenje c(e) IZVOR VISOKENERGIJSKIH FOTONA: DALEK (astronomski, kozmoloski) JAK (astrofizicki akcelerator) BRZO VARIJABILAN (kratak bljesak) Mjerenje c(e) c 0 (1 (E/M) n ) KONKRETNI ASTROFIZICKI IZVORI: Pulsari Aktvne galakticke jezgre (AGN) Gamma-ray bursts (GRB) MAGIC Observatory Prije MAGICa M > to GeV Ref. [9,10, 11, 12, 13, 14] & Laboratorijski testovi [15]

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13 MAGIC Observatory MAGIC-2 (under construction) MAGIC-1

14 La Palma, Canary Islands 28 North, 18 West

15 MAGIC-1 Telescope Inauguration, October (Photo-W. Ko)

16 MAGIC Collaboration SUOSNIVACI (Founders) 1994/95 IFAE Barcelona, UAB Barcelona, DT Barcelona, Humboldt U. Berlin, UC Davis, U. Lodz, UC Madrid, MPI München, INFN / U. Padova, U. Potchefstrom, INFN / U. Siena, Tuorla Observatory, INFN / U. Udine, U. Würzburg, Yerevan Physics Inst., ETH Zürich Academy of Sciences, Bulgaria Rudjer Boskovic Institute, Croatia

17 CRO MAGIC-1 Telescope Inauguration, October (Photo-W. Ko)

18 GALACTIC SOURCES

19 VARIABLE EMISSION from LS I PERIASTRON PERIASTRON + 1/3 Fig. 3. Map of gamma-rays measured by MAGIC

20 GAMMA-RAY BURSTS

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22 DARK MATTER Publication Coming Soon

23 EXTRAGALACTIC SOURCES

24 Extragalactic VHE-sources (19) Source Redshift Sp. Types Discovery Observation M FR-I HEGRA HESS Mkn HBL Whipple many Mkn HBL Whipple many 1ES HBL Whipple MAGIC Mkn HBL MAGIC 1ES HBL 7TA many PKS HBL HESS BL Lac LBL MAGIC PKS HBL HESS PKS HBL Durham many 1ES HBL Whipple HEGRA 1ES HBL HESS H HBL HESS 1ES HBL MAGIC VERITAS 1ES HBL HESS 1ES HBL HESS 1ES HBL MAGIC 3C x LBL MAGIC PG 1553? 4.0 HBL HESS/MAGIC

25 E = GeV E = TeV

26 P t [min] P t [min]

27 P t [min] P ( ) P 1 P t [min] ( ) P 1 P t [min] t [min]

28 P t [min] P Maksimalna korelacija uz pretpostavku: t = 4 minute ( ) P 1 P t [min] ( ) P 1 P t [min] t [min]

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30 M QG1 M QG 2 M M M M M M n ( ) 0 1 E c E = c, n = 1,2 M QGn QG1 = (0.30 ± 0.10) QG1 > GeV QG1 = (0.47 ± 0.13) QG 2 = (0.61 ± 0.14) QG 2 > GeV QG 2 = (0.57 ± 0.19) 10 95% C.L. GeV 95% C.L. GeV METHOD 1 METHOD 2 METHOD 2 METHOD 2

31 CRO MAGIC-1 Telescope Inauguration, October (Photo-W. Ko)

32 CROATEA Cosmic Ray Observatory At The Eastern Adriatic

33 DUBROVNIK KUNA Dubrovnik International Airport

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35 POZIV NA SURADNJU Pojedinci i institucije Studenti Srednje skole (!) CROATEA Kontakt: Daniel Ferenc FERENC@physics.ucdavis.edu Dario Hrupec, IRB Zagreb Ivica Puljak, Zeljko Antunoic, Nikola Godinovic, Split

36 It was also pointed out that one powerful way to probe this possibility may be provided by distant astrophysical sources of energetic photons that exhibit significant and rapid variations in time, such as gamma-ray bursters (GRBs) [8]. The possibility of an energy-dependent velocity of light: [8] G. Amelino-Camelia, J. Ellis, N. Mavromatos, D. Nanopoulos and S. Sarkar, Nature 393 (1998) 763. [9] S.D. Biller et al., Phys. Rev. Lett. 83 (1999) [10] B.E. Schafer, Phys. Rev. Lett. 82 (1999) [11] S. E. Boggs, C. B. Wunderer, K. Hurley and W. Coburn, Astrophys. J. 611 (2004) L77 [arxiv:astroph/ ]. [12] P. Kaaret, arxiv:astro-ph/ [13] T. Jacobson, S. Liberati and D. Mattingly, Phys. Rev. D 66 (2002) [arxiv:hep-ph/ ]. [14] J. Alfaro and G. Palma, Phys. Rev. D 67 (2003) [arxiv:hep-th/ ]; F. W. Stecker and S. L. Glashow, Astropart. Phys. 16 (2001) 97 [arxiv:astro-ph/ ]; S. R. Coleman and S. L. Glashow, Phys. Rev. D 59 (1999) [arxiv:hep-ph/ ]; R. J. Protheroe and H. Meyer, Phys. Lett. B 493 (2000) 1[arXiv:astro-ph/ ]; G. Amelino-Camelia and T. Piran, Phys. Rev. D 64 (2001) [arxiv:astroph/ ]; G. Amelino-Camelia, New J. Phys. 6, 188 (2004) [arxiv:gr-qc/ ]; T. J. Konopka and S. A. Major, New J. Phys. 4 (2002) 57 [arxiv:hep-ph/ ]; F. W. Stecker, New Astron. Rev. 48 (2004) 437 [arxiv:astro-ph/ ]; F. W. Stecker, Astropart. Phys. 20 (2003) 85 [arxiv:astro-ph/ ]; [15] V. A. Kostelecky and M. Mewes, Phys. Rev. D 66 (2002) [arxiv:hep-ph/ ]. [16] J. R. Ellis, N. E. Mavromatos, D. V. Nanopoulos and A. S. Sakharov, Astron. Astro-phys. 402 (2003) 409 [arxiv:astro-ph/ ].15 The propagation of light through this space-time foam might exhibit a non-trivial dispersion relation in vacuo [8], corresponding to Lorentz violation via an energy-dependent velocity of light.

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38 [8] G. Amelino-Camelia, J. Ellis, N. Mavromatos, D. Nanopoulos and S. Sarkar, Nature 393 (1998) 763. [9] S.D. Biller et al., Phys. Rev. Lett. 83 (1999) [10] B.E. Schafer, Phys. Rev. Lett. 82 (1999) [11] S. E. Boggs, C. B. Wunderer, K. Hurley and W. Coburn, Astrophys. J. 611 (2004) L77 [arxiv:astroph/ ]. [12] P. Kaaret, arxiv:astro-ph/ [13] T. Jacobson, S. Liberati and D. Mattingly, Phys. Rev. D 66 (2002) [arxiv:hep-ph/ ]. [14] J. Alfaro and G. Palma, Phys. Rev. D 67 (2003) [arxiv:hep-th/ ]; F. W. Stecker and S. L. Glashow, Astropart. Phys. 16 (2001) 97 [arxiv:astro-ph/ ]; S. R. Coleman and S. L. Glashow, Phys. Rev. D 59 (1999) [arxiv:hep-ph/ ]; R. J. Protheroe and H. Meyer, Phys. Lett. B 493 (2000) 1[arXiv:astro-ph/ ]; G. Amelino-Camelia and T. Piran, Phys. Rev. D 64 (2001) [arxiv:astroph/ ]; G. Amelino-Camelia, New J. Phys. 6, 188 (2004) [arxiv:gr-qc/ ]; T. J. Konopka and S. A. Major, New J. Phys. 4 (2002) 57 [arxiv:hep-ph/ ]; F. W. Stecker, New Astron. Rev. 48 (2004) 437 [arxiv:astro-ph/ ]; F. W. Stecker, Astropart. Phys. 20 (2003) 85 [arxiv:astro-ph/ ]; [15] V. A. Kostelecky and M. Mewes, Phys. Rev. D 66 (2002) [arxiv:hep-ph/ ]. [16] J. R. Ellis, N. E. Mavromatos, D. V. Nanopoulos and A. S. Sakharov, Astron. Astro-phys. 402 (2003) 409 [arxiv:astro-ph/ ].15

39 Observation of VHE Gamma Radiation from HESS J /W41 with the MAGIC Telescope J. Albert et al., ApJ Letters 643, L53 (2006); astro-ph/

40 MAGIC observations of very high energy gamma-rays from HESS J J. Albert et al., ApJ Letters 637, L41 (2006); astro-ph/

41 Discovery of VHE gamma-ray emission from 1ES J. Albert et al., ApJ Letters 642, L119 (2006); astro-ph/

42 Discovery of Very High Energy Gamma-Rays from Markarian~180 Triggered by an Optical Outburst J.Albert et al,.submitted to ApJ Letters in June 2006; astro-ph/

43 Detection of VHE radiation from the BL Lac PG with the MAGIC telescope J.Albert et al., astro-ph/ , submitted to ApJ Letters, May 2006; astro-ph/

44 Observations of Mkn~421 with the MAGIC Telescope J. Albert et al,. submitted to ApJ 2006; astro-ph/

45 Observation of VHE gamma-ray emission from the Active Galactic Nucleus 1ES using the MAGIC telecope E. Aliu et al., Astrophys.J.639: ,2006; astro-ph/

46 MOTIVATION 1. High Sensitivity for the very important energy interval ~30(10) GeV < E < 100 GeV 1-Year Observation Time!!! The extinction interval for many sources that have been observed at lower energies (EGRET) and are invisible at high energies (ground-based 50 IACTs) Hours Gamma-ray horizon extended at low energies (like GZK): - AGN studies per se, and - EBL (IR) background studies, galaxy and star formation Pulsar studies require very low threshold 2. Counterparts of Gamma Ray Bursts at higher energies 3. Transient and Periodical sources in general, like AGNs and microquasars