1 TeVγ 線天文学の現状と将来森正樹東京大学宇宙線研究所「高エネルギー宇宙物理学の現状と将来」 2000 年 9 月 29-30 日大阪大学.

Slides:

Advertisements

Similar presentations

The MAGIC telescope and the GLAST satellite La Palma, Roque de los Muchacos (28.8° latitude ° longitude, 2225 m asl) INAUGURATION: 10/10/2003 LAT.

Advertisements

GeV-TeV Gamma-ray Astronomy Masaki Mori ICRR, Univ. Tokyo International Workshop on Extremely High Energy Cosmic Rays, March 22-23, 2001, Kashiwa

High-energy particle acceleration in the shell of a supernova remnant F.A. Aharonian et al (the HESS Collaboration) Nature 432, 75 (2004) Nuclear Physics.

Cut off more slowly ～ 50GeV Thompson astro-ph/ Credit: A.K. Harding (NASA/GSFC) Our first target: Crab pulsar/nebula The standard candle for gamma-ray.

Mathieu de Naurois, H.E.S.S.High Energy Phenomena in the Galacic Center H.E.S.S. Observations of the Galactic Center  The H.E.S.S. Instrument.

MAGIC TeV blazars and Extragalactic Background Light Daniel Mazin on behalf of the MAGIC collaboration Max-Planck-Institut für Physik, Munich.

Status of CANGAROO III Akihiro Asahara ( Kyoto Univ.) CANGAROO expanded meeting 1.Introduction 2.Resent Results 3.Brand-new! CANGAROO T2 4.Stereo Analysis.

 Jim Hinton 2006 High Energy Stereoscopic System (H.E.S.S.)  Array of four 107 m 2 telescopes in Namibia, 120 m spacing  5° FOV  Threshold 100 GeV.

VHE Gamma Ray Astronomy: a UK strategy for the next decade Paula Chadwick for the University of Durham Johannes Knapp for the University of Leeds Richard.

TeV Gamma-ray Astronomy and UHECR-1 Trevor C. Weekes, Whipple Observatory, Harvard-Smithsonian Center for Astrophysics.

Diffuse Gamma-Ray Emission Su Yang Telescopes Examples Our work.

Jamie Holder School of Physics and Astronomy, University of Leeds, U.K Increasing the Collection Area for IACTs at High Energies Future of Gamma Ray Astronomy.

John Learned, A736/P April 2005 VHE Gamma Ray Astronomy an overview John Learned University of Hawaii P711/A April 2005.

Gus Sinnis HAWC Review December 2007 Milagro a TeV Gamma-Ray Observatory Gus Sinnis Los Alamos National Laboratory.

The Transient Universe: AY 250 Spring 2007 New High Energy Telescopes Geoff Bower.

1 Gamma-Ray Astronomy with GLAST May 24, 2008 Toby Burnett WALTA meeting.

The Spectrum of Markarian 421 Above 100 GeV with STACEE Jennifer Carson UCLA / Stanford Linear Accelerator Center February MeV 1 GeV 10 GeV 100.

1 VERY ENERGETIC RADIATION IMAGING TELESCOPE ARRAY SYSTEM VERITAS Mark Lang, National University of Ireland, Galway.

Gamma-ray Astrophysics Pulsar GRB AGN SNR Radio Galaxy The very high energy  -ray sky NEPPSR 25 Aug Guy Blaylock U. of Massachusetts Many thanks.

On A Large Array Of Midsized Telescopes Stephen Fegan Vladimir Vassiliev UCLA.

VERITAS Observations of Supernova Remnants Reshmi Mukherjee 1 for the VERITAS Collaboration 1 Barnard College, Columbia University Chandra SNR Meeting,

The ANTARES Neutrino Telescope Mieke Bouwhuis 27/03/2006.

The 2009 Fermi Symposium - Washington, D.C Nov 2009 VERITAS Discovery of VHE Gamma Rays from the Starburst Galaxy M82 Niklas Karlsson for the VERITAS.

Thémis What’s new on the ground? Running Cherenkov gamma ray telescopes David A. Smith Centre d’Études Nucléaires de Bordeaux-Gradignan, In2p3/CNRS CAT.

1 Tuning in to Nature’s Tevatrons Stella Bradbury, University of Leeds T e V  -ray Astronomy the atmospheric Cherenkov technique the Whipple 10m telescope.

Seminari IEEC - 15-XII-04Oscar Blanch Bigas Cosmology with the New Generation of Cherenkov Telescopes Oscar Blanch Bigas IFAE, UAB Seminari IEEC 15-XII-04.

The VHE gamma-ray sky viewed with H.E.S.S. Werner Hofmann MPI für Kernphysik Heidelberg © Philippe Plailly HESS = High Energy Stereoscopic System.

Astrophysics With the Cherenkov Telescope Array P. Coppi (for F. Aharonian, MPIK, Heidelberg)

Incontri di Fisica delle Alte Energie IFAE 2006 Pavia Vincenzo Vitale Recent Results in Gamma Ray Astronomy with IACTs.

Gamma-ray Astronomy of XXI Century 100 MeV – 10 TeV.

Current Status of TeV Gamma Ray Astronomy M. Teshima Max-Planck-Institute for Physics, Munich.

Gus Sinnis RICAP, Rome June 2007 High Altitude Water Cherenkov Telescope  Gus Sinnis Los Alamos National Laboratory for the HAWC Collaboration.

Recent results from MAGIC Alessandro de Angelis Univ. Udine, INFN Trieste Bremen, July 2010 Alessandro de Angelis Univ. Udine, INFN Trieste Bremen, July.

1 CANGAROO-III Masaki Mori* for the CANGAROO team *ICRR, The University of Tokyo ICRR internal talk, October 19, 2005.

Recent TeV Observations of Blazars & Connections to GLAST Frank Krennrich Iowa State University VERITAS Collaboration GSFC, October 24, 2002 AGN.

The TeV Gamma-ray Universe Trevor C. Weekes Harvard-Smithsonian Center for Astrophysics Motivation/Techniques The TeV Sky Future Prospects.

Gamma-Ray Telescopes. Brief History of Gamma Ray Astronomy 1961 EXPLORER-II: First detection of high-energy  -rays from space 1967 VELA satelllites:

CANGAROO の現況 Status of CANGAROO project Masaki Mori ICRR, University of Tokyo 「 CANGAROO 望遠鏡によるガンマ線天文学の新展開」 Dec.11-12, 2003 京都大学 Workshop “ New developments.

TeV gamma-ray observation of RCW86 with the CANGAROO-II telescope WATANABE Shio (Kyoto university) for the CANGAROO Collaboration Contents The CANGAROO.

Development of Ideas in Ground-based Gamma-ray Astronomy, Status of Field and Scientific Expectations from HESS, VERITAS, MAGIC and CANGAROO Trevor C.

Observations of SNR RX J with CANGAROO-II telescope Kyoto, Dec., 16, 2003 H. Katagiri, R. Enomoto, M. Mori, L. Ksenofontov Institute for cosmic.

Jamie Holder University of Leeds August 2005 Status and Performance of the First VERITAS Telescope.

Radio galaxy Elliptical Fanaroff-Riley type I “Misaligned” BL Lac (~ 60  ) Distance 3.5 Mpc Parameter Value  (J2000) 201   (J2000) -43 

First results of Galactic observations with MAGIC Javier Rico Institut de Física d’Altes Energies Barcelona, Spain XII International Workshop on “Neutrino.

CTA The next generation ultimate gamma ray observatory M. Teshima Max-Planck-Institute for Physics.

M.Teshima MPI für Physik, München (Werner-Heisenberg-Institut) for MAGIC collaboration MAGIC.

1 Caltech Jan High Energy Gamma Astronomy Patrick Fleury (Ecole Polytechnique ) LIGO-G R.

Gus Sinnis Asilomar Meeting 11/16/2003 The Next Generation All-Sky VHE Gamma-Ray Telescope.

The science objectives for CALET Kenji Yoshida (Shibaura Institute of Technology) for the CALET Collaboration.

1 Status of the CANGAROO-III Project Masaki Mori ICRR, University of Tokyo International Symposium on High Energy Gamma-Ray Astronomy, June 26-30, Heidelberg.

HAWC Science  Survey of 2  sr (half the sky) up to 100 TeV energies Probe knee in cosmic ray spectrum Identify sources of Galactic cosmic rays  Extended.

The Spectrum of Markarian 421 Above 100 GeV with STACEE

1st page of proposal with 2 pictures and institution list 1.

Diffuse Emission and Unidentified Sources

A Future All-Sky High Duty Cycle VHE Gamma Ray Detector Gus Sinnis/Los Alamos with A. Smith/UMd J. McEnery/GSFC.

June 6, 2006 CALOR 2006 E. Hays University of Chicago / Argonne National Lab VERITAS Imaging Calorimetry at Very High Energies.

05/02/031 Next Generation Ground- based  -ray Telescopes Frank Krennrich April,

Next Generation Particle Astrophysics with GeV/TeV  -Rays D. Kieda University of Utah.

Science Capabilities - Summary 200  bursts per year  prompt emission sampled to > 20 µs AGN flares > 2 mn  time profile +  E/E  physics of jets and.

Sources emitting gamma-rays observed in the MAGIC field of view Jelena-Kristina Željeznjak , Zagreb.

Markarian 421 with MAGIC telescope Daniel Mazin for the MAGIC Collaboration Max-Planck-Institut für Physik, München

A fast online and trigger-less signal reconstruction Arno Gadola Physik-Institut Universität Zürich Doktorandenseminar 2009.

The Large High Altitude Air Shower Observatory LHAASO.

Tobias Jogler Max – Planck Institut für Physik The MAGIC view of our Galaxy Tobias Jogler for the MAGIC Collaboration.

TeV Gamma Ray Astrophysics Wei Cui Department of Physics Purdue University.

Gamma Rays from the Radio Galaxy M87

Observation of Pulsars and Plerions with MAGIC

Lecture 4 The TeV Sky Cherenkov light Sources of Cherenkov radiation.

HAWC Science Survey of 2p sr up to 100 TeV energies Extended Sources

Presentation transcript:

1 TeVγ 線天文学の現状と将来森正樹東京大学宇宙線研究所「高エネルギー宇宙物理学の現状と将来」 2000 年 9 月日大阪大学

2 Cherenkov telescope Cherenkov light from gamma-ray showers Lateral distribution & Timing distribution Konopelko, TMACD-V, 1999

3 Imaging Cherenkov technique γp

4 Satellite vs Ground-based gamma-ray telescope BaseSatelliteGround Gamma-ray detection Direct (pair creation) Indirect (atmospheric Cherenkov) Energy< 30 GeV ( → 100 GeV) >300 GeV ( → 50 GeV) ProsHigh S/N Large FOV Large area Good ⊿ θ ConsSmall area High cost Low S/N (CR bkgd.) (but imaging overcomes this!) Small FOV

5 Cherenkov telescopes in the world ( 終了 )

6 TeV gamma-ray source catalog 分類天体名グループ備考 Grade A (>5σ, multiple) Crab PSR Mrk421 Mrk501 多数 CANGAROO, Durham 多数 Plerion AGN (BL Lac) Grade B (>5σ) SN1006 Vela RXJ PKS ES BL Lac CANGAROO Durham Utah7TA Crimea SNR Plerion SNR AGN (BL Lac) Grade C (strong but with some qualifications) Cas A Cen X-3 1ES C66A Geminga B HEGRA CT Durham Whipple Crimea CANGAROO SNR X-ray binary AGN (BL Lac) AGN Pulsar Plerion T.C. Weekes, Heidelberg WS, 2000

7 TeV gamma-ray sky

8 GeV gamma-ray sky Third EGRET catalog E > 100 MeV

9 Crab nebula Unpulsed spectrum Aharonian & Atoyan, astro-ph/ / Heidelberg WS, 2000 synchrotron IC

10 Crab pulsar spectrum: where is the cutoff? Musquere, 26 th ICRC, 1999

11 Supernova remnant: SN1006 T. Naito

12 SNR: SN interpretation Synch+IC Only IC? No pro- tons? Naito et al. Astron. Nach. 320, 1999

13 Supernova remnant: Cas A Goret et al. 26 th ICRC OG2.2.18, 1999 ● HEGRA 2000

14 Supernova remnant: RXJ1713 RXJ “ SN1006 Jr. ” Muraishi et al., A&Ap 354, 2000 Tomida, Ph.D., 1999 CANGAROO

15 AGN: Mrk 421 Rapid variability: Faster at TeV? Maraschi et al. ApJL 526, 1999 (April 1998) Whipple BeppoSAX

16 AGN: Mrk 421 spectrum Synchrotron + inverse Compton model Takahashi et al. astro-ph/ One-zone SSC model δ=14, B=0.14G synchrotroninverse compton

17 AGN: TeV gamma-ray absorption by IR background Protheroe et al. astro-ph/ IR Background Mean free path for e + e - pair production

18 AGN: Mrk 501 spectrum Protheroe et al. astro-ph/ Aharonian et al. A&Ap 349, 1999 Crisis? ↓

19 Next generation projects

20 H.E.S.S. (High Energy Stereoscopic System) 23 o 16'18'' S 16 o 30'00'' E 1800 m a.s.l.

21 H.E.S.S. telescope 16 (4 init.) telescopes (120m spacing) Davies-Cotton design, F/0.8 (f=15m), 108m 2 mirror area (382 x 60cm  ) Camera: 960 x 29mm (0.16°) PMTs, 5° FOV, 600kg Readout: 1GHz FADC Total 52 ton each

22 VERITAS Mt. Hopkins, AZ (Montosa canyon or north site) (Very Energetic Radiation Imaging Telescope Array System) 23 o N 111 o W >2000 m a.s.l.

23 VERITAS telescope 7 telescopes (80m spacing) Reflector: Davies-Cotton design, D=10m (78.6m 2 ), f=12m, 244x 60cm hexagonal mirrors (glass) Camera: 499x 1 ” PMTs (0.15 o spacing), 3.5 o FOV Readout: 500MHz FADC? (This is the present 10m telescope: new design not available!)

24 MAGIC (Major Atmospheric Gamma-ray Imaging Cherenkov Telescope) La Palma, Canary Island o N o W 2200 m a.s.l.

25 MAGIC telescope Reflector: parabolic, D=17m (234m 2 ), f=17m, 976x (50x50cm 2 ) Al mirrors Camera: [classical] 397x 1 ” PMTs (0.10 o )+ 126x 1.5 ” PMTs (0.20 o ), 3.5 o FOV, ~100kg [standard] HPDs (center) + PMTs First Light in Summer 2001 (June 21, 2001)

26 CANGAROO-III Woomera, South Australia 31 o 06' S 136 o 47' E 160 m a.s.l.

27 CANGAROO-III telescope 4 telescopes (100m spacing) Parabola reflector consisting of 114 mirrors of 80cmφ (57m 2 ), f=8m, F/0.8 Camera: 4  FOV, 427x 3/4 ” PMTs (0.16 , Hamamatsu R3478UV, TTS 0.36ns) Readout: q-ADC & TDC

28 Sensitivity of Cherenkov telescopes VERITAS, ICRC1999 Major backgrounds: p: CR proton e: CR electron  : CR muon NSB: night sky background

29 Expected sensitivity

30 Monitoring the gamma-ray sky ⇒？⇒？ ⇒？⇒？ ⇒？⇒？

31 Future trends Lowering energy threshold ( → 5 GeV) Larger light collector Higher altitude Increasing FOV ( → 1 sr) “All-sky” TeV gamma-ray monitor

32 High altitude Cherenkov telescope High altitude → higher photon density → lower energy → high statistics/ overlapping to satellites

33 Cherenkov light density at high altitude Aharonian et al. astro-ph/ γp

34 Sensitivity of 4×50m 2 telescope array at 5km a.s.l. (e.g. Atacama) Aharonian et al. astro-ph/

35 All-sky TeV gamma-ray monitor 5 mφ, 1 sr telescope, 1 TeV threshold ・ CR rate (>1 TeV): 8 ･ cm -2 s -1 × 3 ・ 10 8 cm 2 = 3 kHz ・ Muons (>1 GeV): 7 ・ cm -1 s -1 × 2 ・ 10 5 cm 2 = 1.4 kHz ・ High threshold to reduce N.S.B. ・ 0.1 o resolution camera (many channels…) ・ Stereo if necessary ・ Good monitor for GRBs Not far away from the present technology! Kifune and Takahashi, TMACD-IV, 1997

36 All-sky monitor optics EUSO/OWL type large FOV optics EUSO proposal, 2000 ↑ □ movable camera? ↓

37 Science to come Plerions (pulsar nebula) Inverse Compton? ← synchrotron origin? Pulsars Cutoff in pulse component? ← polar cap/outer gap SNRs π 0 contribution? ← cosmic ray origin AGNs Gamma-ray source: e ± or p? Intergalactic IR ← cosmology EGRET unIDs, Neutralinos, GRBs, QG, Diffuse gamma, …, and more?

38 Gamma-rays and cosmic-rays T. Kifune, 2000