DOCSLIB.ORG

Recent MAGIC Observations of Active Galactic Nuclei: Studies in the E>50 Gev Region

Total Page：16

File Type：pdf, Size：1020Kb

Download full-text PDF Read full-text
Recent MAGIC Observations of Active Galactic Nuclei: Studies in the E>50 Gev Region Recent MAGIC Observations of Active Galactic Nuclei: Studies in the E>50 GeV Region Robert Wagner on behalf of the MAGIC Collaboration Max-Planck-Institut für Physik & Excellence Cluster “Universe” R. M. Wagner: MAGIC AGN Observaons Munich,Fermi andGermany Jansky | St. Michaels, MD | 2011-11-12 MAGIC Coll, Astropart. Phys. subm. arXiv:1108.1477 The MAGIC Telescopes Carmona+ (MAGIC Coll), Proc ICRC 2011, arXiv:1110.0947 • Two-dish stereoscopic Cherenkov telescope, 17 m diameter each • Located at the European Northern Observatory, Instituto Astrofísica de Canarias on the Canary Island of La Palma, Spain • Currently upgrade of readout, of MAGIC-1 camera in 2012 • 150 physicists • 23 institutes Roque de los Muchachos observatory, 2200 m a.s.l. Click to edit Master tle style MAGIC-1 MAGIC-2 R. M. Wagner: MAGIC AGN Observaons Fermi and Jansky | St. Michaels, MD | 2011-11-12 MAGIC Coll, Astropart. Phys. subm. arXiv:1108.1477 The MAGIC Telescopes Carmona+ (MAGIC Coll), Proc ICRC 2011, arXiv:1110.0947 • Two-dish stereoscopic Cherenkov telescope, 17 m diameter each • Located at the European Northern Observatory, Instituto Astrofísica de Canarias on the Canary Island of La Palma, Spain • Currently upgrade of readout, of MAGIC-1 camera in 2012 • 150 physicists • Substantially lower energy threshold than other installations: • 23 institutes • 50-60 GeV nominal Roque de los Muchachos observatory, • 25 GeV pulsar (“sum”) trigger 2200 m a.s.l. • ClickSensitivity to: 0.75% edit Crab Master in 50 h tle style • Angular resolution: <0.07° • Energy resolution: 15-20% • Enhanced duty cycle (by 20%) thanks to moonlight & twilight observations Britzger, RMW+09 MAGIC-1 MAGIC-2 R. M. Wagner: MAGIC AGN Observaons Fermi and Jansky | St. Michaels, MD | 2011-11-12 Some Key Features Fast repositioning (below 1 minute) ➙ sensitivity to transients: GRB Low energy threshold (50-60 GeV, 25 GeV in sum-trigger mode) – Overlap with Fermi-LAT – Deep universe MAGIC Coll, Astropart. Phys. subm. arXiv:1108.1477 MAGIC I achieved Click to edit Master tle style MAGIC II achieved (dashed: MC expect.) R. M. Wagner: MAGIC AGN Observaons Fermi and Jansky | St. Michaels, MD | 2011-11-12 Low Threshold: Overlap with Fermi-LAT (IC peak, cross-calibration) 10-9 ] -1 SMA s Abdo+11 -2 VLBA_core(BP143) VLBA(BP143) 10-10 VLBA(BK150) Metsahovi [erg cm i Noto F i VLBA_core(MOJAVE) 10-11 VLBA(MOJAVE) FERMI MAGIC OVRO RATAN Medicina Swift/UVOT MAGIC Click10-12 toEffelsberg edit MasterROVOR tle styleFermi NewMexicoSkies Swift/BAT MITSuME RXTE/PCA GRT Swift/XRT -13 10 GASP WIRO OAGH Most complete SED for Mkn 421 ever 10-14 1010 1012 1014 1016 1018 1020 1022 1024 1026 1028 …and, by the way, access to pulsars cutoffs, e.g., Crab i [Hz] R. M. Wagner: MAGIC AGN Observaons Fermi and Jansky | St. Michaels, MD | 2011-11-12 The Extragalactic TeV Sky Click to edit Master tle style http://www.mpp.mpg.de/∼rwagner/sources/ approx. 50 VHE γ-ray sources, mostly blazars Relativistically beamed gamma-ray emission R. M. Wagner: MAGIC AGN Observaons 5 Fermi and Jansky | St. Michaels, MD | 2011-11-12 Beyond blazars… New generation IACTs have established new classes of VHE active galaxies different than BL Lacs… Radio galaxies M87, Cen A, starburst galaxies M82, NGC 253, Perseus cluster galaxies IC310, NGC 1275 Starbursts 2 discovered — none yet by MAGIC BL Lacs No central source, probably global still the vast majority: emission of all CR in galaxy approx. 45 discovered — 17 by MAGIC Extensive studies Click to edit Master tle style FSRQ 3 discovered — 2 by MAGIC Different physics: intense radiation fields. Radiogalaxies Very distant: useful to study EBL 4 discovered — 2 by MAGIC Study emission in jet: they are nearby (can be resolved in other wavelengths) and jets not aligned with line of sight. May be sources of UHECRs? R. M. Wagner: MAGIC AGN Observaons 6 Fermi and Jansky | St. Michaels, MD | 2011-11-12 Radiogalaxies: M87 Science 325 (2009) 444 Very close (17 Mpc) Flare at VHE Very well characterized in other frequencies. M87 was the first radiogalaxy discovered a VHE (HEGRA/HESS) and has been extensively studied VHE Gamma-Rays by HESS, VERITAS & MAGIC. X-Rays In 2008, using all 3 experiments and simultaneous radio VLBI: ClickVHE emission to edit came Master from very tle style Brightening of radio core Radio close to the central BH (a few Schwarzschild radii, Science 325 (2009) 444 Rs~100 A.U.). R. M. Wagner: MAGIC AGN Observaons 7 Fermi and Jansky | St. Michaels, MD | 2011-11-12 VERITAS/MAGIC/HESS/ Very dense sampling: Walker+/Harris+ ApJ subm. 21 observations in Radiogalaxies: M87 Harris+ ApJ subm. 15 days. Rise in 1.7 days, Further cooperation of the 3 experiments decay in 0.6 days and multiwavelength add essential information… but may be complicating the picture! Results submitted to ApJ: In total, 3 flares at VHE: 2005, 2008 and 2010. Flare in 2010 showed exponential rise and decay. Not so clear for the others. 2nd flare was followed by a radio brightening of the core Science 325 (2009) 444. The others not. ClickIn 2008 and to 2010, edit VHE simultaneousMaster to increasetle instyle X-rays. Unclear in 2005. Do all flares come from the same emission site? How are they produced? R. M. Wagner: MAGIC AGN Observaons 8 Fermi and Jansky | St. Michaels, MD | 2011-11-12 VERITAS/MAGIC/HESS/ Very dense sampling: Walker+/Harris+ ApJ subm. 21 observations in Radiogalaxies: M87 Harris+ ApJ subm. 15 days. Rise in 1.7 days, Further cooperation of the 3 experiments decay in 0.6 days and multiwavelength add essential information… but may be complicating the picture! Results submitted to ApJ: In total, 3 flares at VHE: 2005, 2008 and 2010. Flare in 2010 showed exponential rise and decay. Not so clear for the others. 2nd flare was followed by a radio brightening of the core Science 325 (2009) 444. The others not. ClickIn 2008 and to 2010, edit VHE simultaneousMaster to increasetle instyle X-rays. Unclear in 2005. Do all flares come from the same emission site? How are they produced? Recently, MAGIC studied only low state: MAGIC: low spectral index consistent with high state state 2005-7 emission, pointing to the same emission mechanism. MAGIC A&A subm. R. M. Wagner: MAGIC AGN Observaons 8 Fermi and Jansky | St. Michaels, MD | 2011-11-12 MAGIC Coll., ApJL 723 (2010) L207 Hildebrand+ ICRC 2011 Radiogalaxies: IC 310, NGC 1275 MAGIC Coll. MAGIC has discovered 2 radiogalaxies: IC 310 and NGC 1275, both in the Perseus cluster Click to edit Master tle style R. M. Wagner: MAGIC AGN Observaons Fermi and Jansky | St. Michaels, MD | 2011-11-12 MAGIC Coll., ApJL 723 (2010) L207 Hildebrand+ ICRC 2011 Radiogalaxies: IC 310, NGC 1275 MAGIC Coll. MAGIC has discovered 2 radiogalaxies: IC 310 and NGC 1275, both in the Perseus cluster Detected during enhanced activity seen in Fermi-LAT. Very steep spectrum Γ=-4.0±0.4. Detection only possible thanks to stereo threshold and sensitivity Click to edit Master tle style Diff spectrum NGC 1275 Hildebrand+ (MAGIC) ICRC 2011 from August 2010 to Feb 2011 46 h of observations 3% Crab nebula (E>100 GeV) 5.2 standard deviations R. M. Wagner: MAGIC AGN Observaons Fermi and Jansky | St. Michaels, MD | 2011-11-12 MAGIC Coll., ApJL 723 (2010) L207 Hildebrand+ ICRC 2011 Radiogalaxies: IC 310, NGC 1275 MAGIC Coll. MAGIC has discovered 2 radiogalaxies: IC 310 and NGC 1275, both in the Perseus cluster Detected during enhanced activity seen in Fermi-LAT. Very steep spectrum Γ=-4.0±0.4. Detection only possible thanks to stereo threshold and sensitivity Click to edit Master tle style Diff spectrum NGC 1275 “Head-tail” radiogalaxy. Hildebrand+ (MAGIC) ICRC 2011 Very hard spectrum: from August 2010 to Feb 2011 Γ=2.00±0.14 SED 46 h of observations 3% Crab nebula (E>100 GeV) IC 310 5.2 standard deviations MAGIC Coll., ApJL 723 (2010) L207 R. M. Wagner: MAGIC AGN Observaons Fermi and Jansky | St. Michaels, MD | 2011-11-12 Radio Galaxy IC 310 MAGIC Coll., ApJL 723 (2010) L207 Belongs to Perseus cluster Fermi-LAT MAGIC 7.6 sigma significance from 20.6 hrs stereo 2.5% Crab nebula flux -2 Radio galaxy at z=0.019 E from 2GeV to 7TeV 22×/5× further away than Cen A, M87 must be intrinsically much more luminous (could also be weakly beamed blazar) Mechanism? ClickClose toto black edit hole Master tle style at shocks with cluster medium? Variability excludes CR/medium interaction very hard spectrum: probably IC scattering off IR photons, difficult in SSC R. M. Wagner: MAGIC AGN Observaons 10 Fermi and Jansky | St. Michaels, MD | 2011-11-12 MAGIC Collab. A&A 530 (2011) A4 Quasars: 3C 279 & PKS 1222+21 ApJL 730 (2011) L8 3C 279 (z=0.536) is the farthest VHE Primack et al. (2005) Stecker et al. (2006) Mkn 501 source, discovered by MAGIC in 2006. 10 Kneiske et al. (2002) modified • Spectrum for such a far source Universe Opaque to Gamma Rays H 1426+428 allowed to place strong constraints 1 1ES 0229+200 1ES 1ES1101-232 0347-121 on Extragalactic Background Light. Gamma-Ray Energy [TeV] 1ES 1011+496 3C 279 = 1 τ -1 10 MAGIC Energy Thresholdexcluded Universe Transparent to Gamma Rays -2 10 0 0 .1 0.2 0 .3 0.4 0 .5 0.6 0 .7 Redshift z Click to edit Master tle Sciencestyle 320 (2008) 1752 R. M. Wagner: MAGIC AGN Observaons 11 Fermi and Jansky | St. Michaels, MD | 2011-11-12 MAGIC Collab. A&A 530 (2011) A4 Quasars: 3C 279 & PKS 1222+21 ApJL 730 (2011) L8 3C 279 (z=0.536) is the farthest VHE Primack et al.
Load more

Recommended publications
  • Active Galactic Nuclei: a Brief Introduction
    Active Galactic Nuclei: a brief introduction Manel Errando Washington University in St. Louis The discovery of quasars 3C 273: The first AGN z=0.158 2 <latexit sha1_base64="4D0JDPO4VKf1BWj0/SwyHGTHSAM=">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</latexit> <latexit sha1_base64="H7Rv+ZHksM7/70841dw/vasasCQ=">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</latexit> The power source of quasars • The luminosity (L) of quasars, i.e. how bright they are, can be as high as Lquasar ~ 1012 Lsun ~ 1040 W. • The energy source of quasars is accretion power: - Nuclear fusion: 2 11 1 ∆E =0.007 mc =6 10 W s g−
    [Show full text]
  • The Cherenkov Telescope Array Observatory Comes of Age
    The Organisation DOI: 10.18727/0722-6691/5194 The Cherenkov Telescope Array Observatory Comes of Age Federico Ferrini 1 Conceived around a decade ago by a the detection of a clear signal from Wolfgang Wild 1, 2 group of scientists, we are now on the the Crab nebula above 1 TeV with the cusp of constructing the largest observa- Whipple 10-m imaging atmospheric tory to study the gamma-ray Universe. Cherenkov telescope (IACT). Since then, 1 CTAO, Heidelberg (DE) and Bologna (IT) Here we present a short look back at the the instrumentation for, and techniques 2 ESO evolution and recent matu ration of the of, astronomy with IACTs have evolved CTA project, as well as an outline of our to the extent that a flourishing new scien- expectations for the near future. A com- tific discipline has been established, with The Cherenkov Telescope Array (CTA) is prehensive introduction to CTA, including the detection of more than 150 sources the next-generation ground-based the detection technique, its history, the and a major impact in astrophysics — observatory for gamma-ray astronomy extraordinary improvements with respect and, more widely, in physics. The current at very high energies. With up to 120 to previous experimental facilities, and the major arrays of IACTs (the High Energy telescopes on two sites, CTA will be the scientific objectives has been provided by Stereoscopic System [H.E.S.S.], the world’s largest and most sensitive Werner Hofmann, Spokesperson of the Major Atmospheric Gamma Imaging high-energy gamma-ray observatory CTA Consortium (Hofmann, 2017). Cherenkov Telescope [MAGIC], and the covering the entire sky.
    [Show full text]
  • MAGIC Observations of the Diffuse Γ-Ray Emission in the Vicinity of the Galactic Center? MAGIC Collaboration: V
    A&A 642, A190 (2020) Astronomy https://doi.org/10.1051/0004-6361/201936896 & c MAGIC Collaboration 2020 Astrophysics MAGIC observations of the diffuse γ-ray emission in the vicinity of the Galactic center? MAGIC Collaboration: V. A. Acciari1,2, S. Ansoldi3,24, L. A. Antonelli4, A. Arbet Engels5, D. Baack6, A. Babic´7, B. Banerjee8, U. Barres de Almeida9, J. A. Barrio10, J. Becerra González1,2, W. Bednarek11, L. Bellizzi12, E. Bernardini13,17, A. Berti14, J. Besenrieder15, W. Bhattacharyya13, C. Bigongiari4, A. Biland5, O. Blanch16, G. Bonnoli12, Ž. Bošnjak7, G. Busetto17, R. Carosi18, G. Ceribella15, Y. Chai15, A. Chilingaryan19, S. Cikota7, S. M. Colak16, U. Colin15, E. Colombo1,2, J. L. Contreras10, J. Cortina20, S. Covino4, V. D’Elia4, P. Da Vela18, F. Dazzi4, A. De Angelis17, B. De Lotto3, M. Delfino16,27, J. Delgado16,27, D. Depaoli14, F. Di Pierro14, L. Di Venere14, E. Do Souto Espiñeira16, D. Dominis Prester7, A. Donini3, D. Dorner21, M. Doro17, D. Elsaesser6, V. Fallah Ramazani22, A. Fattorini6, A. Fernández-Barral17, G. Ferrara4, D. Fidalgo10, L. Foffano17, M. V. Fonseca10, L. Font23, C. Fruck15;??, S. Fukami24, R. J. García López1,2, M. Garczarczyk13, S. Gasparyan19, M. Gaug23, N. Giglietto14, F. Giordano14, N. Godinovic´7, D. Green15, D. Guberman16, D. Hadasch24, A. Hahn15, J. Herrera1,2, J. Hoang10, D. Hrupec7, M. Hütten15, T. Inada24, S. Inoue24, K. Ishio15, Y. Iwamura24;??, L. Jouvin16, D. Kerszberg16, H. Kubo24, J. Kushida24, A. Lamastra4, D. Lelas7, F. Leone4, E. Lindfors22, S. Lombardi4, F. Longo3,28, M. López10, R. López-Coto17, A. López-Oramas1,2, S. Loporchio14, B. Machado de Oliveira Fraga9, C.
    [Show full text]
  • Antimatter Gravity and the Universe Dragan Hajdukovic
    Antimatter gravity and the Universe Dragan Hajdukovic To cite this version: Dragan Hajdukovic. Antimatter gravity and the Universe. Modern Physics Letters A, World Scientific Publishing, 2019, 10.1142/S0217732320300013. hal-02106808v3 HAL Id: hal-02106808 https://hal.archives-ouvertes.fr/hal-02106808v3 Submitted on 21 Nov 2019 HAL is a multi-disciplinary open access L’archive ouverte pluridisciplinaire HAL, est archive for the deposit and dissemination of sci- destinée au dépôt et à la diffusion de documents entific research documents, whether they are pub- scientifiques de niveau recherche, publiés ou non, lished or not. The documents may come from émanant des établissements d’enseignement et de teaching and research institutions in France or recherche français ou étrangers, des laboratoires abroad, or from public or private research centers. publics ou privés. 1 Brief Review Antimatter gravity and the Universe Dragan Slavkov Hajdukovic Institute of Physics, Astrophysics and Cosmology Crnogorskih junaka 172, Cetinje, Montenegro [email protected] Abstract: The aim of this brief review is twofold. First, we give an overview of the unprecedented experimental efforts to measure the gravitational acceleration of antimatter; with antihydrogen, in three competing experiments at CERN (AEGIS, ALPHA and GBAR), and with muonium and positronium in other laboratories in the world. Second, we present the 21st Century’s attempts to develop a new model of the Universe with the assumed gravitational repulsion between matter and antimatter; so far, three radically different and incompatible theoretical paradigms have been proposed. Two of these 3 models, Dirac-Milne Cosmology (that incorporates CPT violation) and the Lattice Universe (based on CPT symmetry), assume a symmetric Universe composed of equal amounts of matter and antimatter, with antimatter somehow “hidden” in cosmic voids; this hypothesis produced encouraging preliminary results.
    [Show full text]
  • Very High Energy Gamma Ray Observations with the MAGIC Telescope (A Biased Selection)
    Very High Energy Gamma Ray Observations with the MAGIC Telescope (a biased selection) Nepomuk Otte for the MAGIC collaboration • Imaging air shower Cherenkov technique – The MAGIC telescope • Observation of the AGN 3c279 • Observation of Neutron Stars with MAGIC • The Crab nebula and Pulsar (young pulsar) [astro-ph/0705.3244] • PSR B1951+32 (middle aged pulsar) [astro-ph/0702077] • PSR B1957+20 (millisecond pulsar) • LS I 61+303 [Science 2006] • Where to go next? A. Nepomuk Otte Max-Planck-Institut für Physik / Humboldt Universität Berlin 2 The non-thermal universe in VHE gamma-rays SNRs Pulsars Micro quasars AGNs and PWN X-ray binaries GRBs Origin of Space-time cosmic rays Dark matter & relativity Cosmology A. Nepomuk Otte Max-Planck-Institut für Physik / Humboldt Universität Berlin 3 VHE gamma-ray sources status ICRC 2007 71 known sources detections from ground Rowell A. Nepomuk Otte Max-Planck-Institut für Physik / Humboldt Universität Berlin 4 Imaging Air Cherenkov Technique Cherenkov light image of particle shower Gamma in telescope camera ray Particle ~ 10 km • fast light flash (nanoseconds) shower • 100 photons per m² (1 TeV Gamma Ray) t h g o li ~ 1 v o k n e r e h C reconstruct: ~ 120 m arrival direction, energy reject hadron background A. Nepomuk Otte Max-Planck-Institut für Physik / Humboldt Universität Berlin 5 CurrentCurrent generationgeneration CherenkovCherenkov telescopestelescopes MAGIC Veritas MAGIC (Germany, Spain, Italy) VERITAS 1 telescope 17 meters Ø (USA & England) 4 (7) telescopes Montosa 10 meters Ø Canyon, Roque de Arizona los Muchachos, Canary Islands CANGAROO III Cangaroo(Australia III & Japan) 4 telescopes 10 meters Ø H.E.S.S.
    [Show full text]
  • Pos(ICRC2021)788
    ICRC 2021 THE ASTROPARTICLE PHYSICS CONFERENCE ONLINE ICRC 2021Berlin | Germany THE ASTROPARTICLE PHYSICS CONFERENCE th Berlin37 International| Germany Cosmic Ray Conference 12–23 July 2021 Very-high-energy gamma-ray emission from GRB 201216C detected by MAGIC Satoshi Fukami,0,∗ Alessio Berti,1 Serena Loporchio,2 Yusuke Suda,3 Lara Nava,4 PoS(ICRC2021)788 Koji Noda,0 Željka Bošnjak, 5 Katsuaki Asano0 and Francesco Longo6,ℎ on behalf of the MAGIC Collaboration† 0Institute for Cosmic Ray Research, The University of Tokyo, Kashiwanoha 5-1-5, Kashiwa, Japan 1Max Planck Institut for Physics,Föhringer Ring 6, Munich, Germany 2INFN MAGIC Group: INFN Sezione di Bari and Dipartimento Interateneo di Fisica dell’Università e del Politecnico di Bari, I-70125, Bari, Italy 3Physics Program, Graduate School of Advanced Science and Engineering, Hiroshima University, 739-8526 Hiroshima, Japan 4National Institute for Astrophysics (INAF), Street number, Merate, Italy 5 Faculty of Electrical Engineering and Computing, University of Zagreb, Zagreb, Croatia 6University of Trieste, Department of Physics, via Valerio 2, Trieste, Italy ℎINFN, Sezione di Trieste, via Valerio 2, Trieste, Italy E-mail: [email protected] Gamma-ray bursts (GRBs) are the most energetic phenomena in the Universe. Many aspects of GRB physics are still under debate, such as the origin of their gamma-ray emission above the GeV energy range. In 2019, MAGIC detected TeV gamma rays from the long GRB 190114C, whose emission can be well explained by synchrotron-self Compton emission by relativistic electrons. However, it is still unclear whether such a process is common in GRBs, given the reduced number of GRBs detected until now at the very high energies (VHE).
    [Show full text]
  • The Cherenkov Telescope Array Science Goals and Current Status
    EPJ Web of Conferences 209, 01038 (2019) https://doi.org/10.1051/epjconf /201920901038 RICAP-18 1 The Cherenkov Telescope Array 2 Science Goals and Current Status 1,a 2,b 3 The CTA Consortium , represented by Rene A. Ong 1 4 See https://www.cta-observatory.org/consortium_authors/authors_2018_09.html 2 5 Department of Physics and Astronomy, University of California, Los Angeles CA, 90095, USA 6 7 Abstract. The Cherenkov Telescope Array (CTA) is the major ground-based gamma-ray 8 observatory planned for the next decade and beyond. Consisting of two large atmospheric 9 Cherenkov telescope arrays (one in the southern hemisphere and one in the northern 10 hemisphere), CTA will have superior angular resolution, a much wider energy range, and 11 approximately an order of magnitude improvement in sensitivity, as compared to existing 12 instruments. The CTA science programme will be rich and diverse, covering cosmic 13 particle acceleration, the astrophysics of extreme environments, and physics frontiers 14 beyond the Standard Model. This paper outlines the science goals for CTA and covers 15 the current status of the project. 16 1 Introduction 17 The field of very high-energy gamma-ray (VHE, E > 20 GeV) astronomy has come of age in recent 18 years, due to a wealth of information from both ground-based and space-borne telescopes. Prior to 19 2000, the general expectation for the field was to detect the accelerators of the high-energy cosmic 20 rays, most likely supernova remnants (SNRs). However, the reality over the last two decades has 21 been the discovery of an astonishing variety of VHE gamma-ray sources, both within the Milky Way, 22 e.g.
    [Show full text]
  • The Future of Gamma-Ray Astronomy Jürgen Knödlseder
    The future of gamma-ray astronomy Jürgen Knödlseder To cite this version: Jürgen Knödlseder. The future of gamma-ray astronomy. Comptes rendus Physique, Gamma-ray astronomy, Volume 2, 17 (6), pp.663-678, 2016, 10.1016/j.crhy.2016.04.008. hal-01381811 HAL Id: hal-01381811 https://hal.archives-ouvertes.fr/hal-01381811 Submitted on 28 Apr 2020 HAL is a multi-disciplinary open access L’archive ouverte pluridisciplinaire HAL, est archive for the deposit and dissemination of sci- destinée au dépôt et à la diffusion de documents entific research documents, whether they are pub- scientifiques de niveau recherche, publiés ou non, lished or not. The documents may come from émanant des établissements d’enseignement et de teaching and research institutions in France or recherche français ou étrangers, des laboratoires abroad, or from public or private research centers. publics ou privés. Astrophysics The future of gamma-ray astronomy J¨urgenKn¨odlseder IRAP, 9 avenue du Colonel Roche 31028 Toulouse Cedex 4, France Received *****; accepted after revision +++++ Abstract The field of gamma-ray astronomy has experienced impressive progress over the last decade. Thanks to the advent of a new generation of imaging air Cherenkov telescopes (H.E.S.S., MAGIC, VERITAS) and thanks to the launch of the Fermi-LAT satellite, several thousand gamma-ray sources are known today, revealing an unexpected ubiquity of particle acceleration processes in the Universe. Major scientific challenges are still ahead, such as the identification of the nature of Dark Matter, the discovery and understanding of the sources of cosmic rays, or the comprehension of the particle acceleration processes that are at work in the various objects.
    [Show full text]
  • An Interacting Molecular Cloud Scenario for Production of Gamma
    An interacting molecular cloud scenario for production of gamma-rays and neutrinos from MAGIC J1835−069, and MAGIC J1837−073 Prabir Banik∗ and Arunava Bhadra† High Energy and Cosmic Ray Research Centre, University of North Bengal, Siliguri 734013, India Recently the MAGIC telescope observed three TeV gamma-ray extended sources in the galactic plane in the neighborhood of radio SNR G24.7+0.6. Among them, the PWN HESS J1837−069 was detected earlier by the HESS observatory during its first galactic plane survey. The other two sources, MAGIC J1835−069 and MAGIC J1837−073 are detected for the first time at such high energies. Here we shall show that the observed gamma-rays from the SNR G24.7+0.6 and the HESS J1837−069 can be explained in terms of hadronic interactions of the PWN/SNR accelerated cosmic rays with the ambient matter. We shall further demonstrate that the observed gamma-rays from the MAGIC J1837−073 can be interpreted through hadronic interactions of runaway cosmic- rays from PWN HESS J1837−069 with the molecular cloud at the location of MAGIC J1837−073. No such association has been found between MAGIC J1835−069 and SNR G24.7+0.6 or PWN HESS J1837−069. We have examined the maximum energy attainable by cosmic-ray particles in the SNR G24.7+0.6/ PWN HESS J1837−069 and the possibility of their detection with future gamma-ray telescopes. The study of TeV neutrino emissions from the stated sources suggests that the HESS J1837−069 should be detected by IceCube Gen-2 neutrino telescope in a few years of observation.
    [Show full text]
  • MAGIC Multiwavelength Observations: Policy, and Some
    MAGIC multiwavelength observations: policy, and some recent results Alessandro De Angelis Universit`adi Udine, INFN and INAF, Italy, and IST, Lisboa, Portugal on behalf of the MAGIC Collaboration Email: [email protected] Abstract— MAGIC, 17 meters of diameter, is the world’s largest single dish Imaging Atmospheric Cherenkov Telescope, and reaches in the analysis the lowest energy threshold (60 GeV) among the VHE gamma detectors. Completed in September 2004, MAGIC started full operation with its first cycle of data taking in February 2005. MAGIC observations in the galaxy cover, among others, supernova remnants, the Galactic Center and binary systems. The low threshold makes of MAGIC the IACT looking deepest in the Universe: the record of extragalactic sources detected includes Active Galactic Nuclei (AGN) at z > 0.2. Here we discuss the present performance of MAGIC and the policy for the use of MAGIC data in multiwavelength campaigns. After a review of some recent highlights from MW studies, including the discovery of the most distant source ever detected (the AGN 3C279 at z ≃ 0.54), we present the expected performance of MAGIC after the inauguration of the second telescope, scheduled for September 21st, 2008. Multiwavelength studies are a key for the study of emission mechanisms from galactic and extragalactic sources, and Very-High Energy photon detectors are becoming crucial as the GLAST era approaches. Fig. 1. The MAGIC telescope in August 2004. I. INTRODUCTION The Major Atmospheric Gamma Imaging Cherenkov (MAGIC) telescope [1] is located on the Canary Island of related to fundamental physics (search for dark matter, study of La Palma and is the largest Imaging Atmospheric Cherenkov anomalous dispersion relations for photons such as predicted Telescope (IACT) worldwide.
    [Show full text]
  • Science Case for a Wide Field-Of-View Very-High-Energy Gamma-Ray Observatory in the Southern Hemisphere
    Science Case for a Wide Field-of-View Very-High-Energy Gamma-Ray Observatory in the Southern Hemisphere A. Albert1, R. Alfaro2 H. Ashkar3, C. Alvarez4,4 J.Alvarez´ 5, J.C. Arteaga-Vel´azquez5, H. A. Ayala Solares6, R. Arceo4, J.A. Bellido7, S. BenZvi8, T. Bretz9, C.A. Brisbois10, A.M. Brown11, F. Brun3, K.S. Caballero-Mora4, A. Carosi12, A. Carrami~nana13, S. Casanova14;15, P.M. Chadwick11, G. Cotter16, S. Couti~no De Le´on13, P. Cristofari17;18, S. Dasso19;20, E. de la Fuente21, B.L. Dingus1,23 P. Desiati22, F. de O. Salles23, V. de Souza24, D. Dorner25, J. C. D´ıaz-V´elez21;22, J.A. Garc´ıa-Gonz´alez2, M. A. DuVernois22, G. Di Sciascio26, K. Engel27, H. Fleischhack10, N. Fraija28, S. Funk29, J-F. Glicenstein3, J. Gonzalez,30 M. M. Gonz´alez28, J. A. Goodman27, J. P. Harding1, A. Haungs31, J. Hinton15, B. Hona10, D. Hoyos32;33, P. Huentemeyer10, A. Iriarte34, A. Jardin-Blicq15, V. Joshi15, S. Kaufmann11, K. Kawata35, S. Kunwar15, J. Lefaucheur3, J.-P. Lenain36, K. Link31, R. L´opez-Coto37, V. Marandon15, M. Mariotti38, J. Mart´ınez-Castro39, H. Mart´ınez-Huerta24, M. Mostaf´a6, A. Nayerhoda14, L. Nellen32, E. de O~naWilhelmi40;41, R.D. Parsons15, B. Patricelli42;43, A. Pichel19, Q. Piel12, E. Prandini38, E. Pueschel41, S. Procureur3, A. Reisenegger44;45, C. Rivi`ere27, J. Rodriguez2;46, A. C. Rovero19, G. Rowell7, E. L. Ruiz-Velasco15, A. Sandoval2, M. Santander47, T. Sako35, T. K. Sako35, K. Satalecka41, H. Schoorlemmer15;?, F. Sch¨ussler3;?, M. Seglar-Arroyo3, A.
    [Show full text]
  • Letter of Intent: Antimatter Gravity Experiment (AGE) at Fermilab
    Version 2.0 February 6, 2009 Letter of Intent: Antimatter Gravity Experiment (AGE) at Fermilab Alex D. Cronin University of Arizona, Tucson, Arizona 85721, USA Thomas J. Phillips∗ Duke University, Durham, North Carolina 27708, USA Mark Fischler, Alan Hahn, James T. Volk, G.P. Yeh Fermilab, Batavia, Illinois 60510, USA Rod G. Greaves First Point Scientific, Agoura Hills, California 91301, USA Stephen D. Howe, Gerald P. Jackson, Raymond Lewis, Joseph M. Zlotnicki Hbar Technologies, LLC, West Chicago, Illinois 60185, USA Daniel M. Kaplan, Thomas J. Roberts1, Jeff Terry Illinois Institute of Technology, Chicago, Illinois 60616, USA Glenn A. Horton-Smith, Bharat Ratra Kansas State University, Manhattan, Kansas 66506, USA Todd K. Pedlar Luther College, Decorah, Iowa 52101, USA H. Richard Gustafson University of Michigan, Ann Arbor, Michigan 48109, USA J. Boise Pearson NASA Marshall Space Flight Center, Alabama, USA Thomas E. Coan Southern Methodist University, Dallas, Texas 75275, USA Mark G. Raizen University of Texas, Austin, Texas 78712, USA ∗Contact person; email: [email protected]. Abstract We propose to make the first direct measurement of the gravitational accelera- tion of antimatter by taking advantage of Fermilab's unique ability to accumulate large numbers of antiprotons. Such a measurement will be a fundamental test of gravity in a new regime, directly testing both the equivalence principle and the prediction of General Relativity that matter and antimatter behave identi- cally in the gravitational field of the earth. We propose to decelerate antiprotons in the Main Injector and transfer them into an antihydrogen-production Pen- ning trap. The antihydrogen will emerge from the trap in a low-velocity beam.
    [Show full text]