Performance of 10-100GeV gamma ray camera for SUBARU optical-infrared telescope A.Asahara, K.Komiyama#, G.Kosugi#, H.Kubo, S.Miyazaki#, M.Mori , M.Nakagiri#,

Slides:

Advertisements

Similar presentations

1 Observation of the Crab Nebula with the MAGIC Telescope M. López-Moya Univ. Complutense de Madrid, on behalf of the MAGIC Collaboration.

Advertisements

Analysis report of SN1006 D.Nishida( Kyoto-Univ.) JPS meeting Autumn 2005 Osaka.

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.

OBSERVATIONS OF AGNs USING PACT (Pachmarhi Array of Cherenkov Telescopes) Debanjan Bose (On behalf of PACT collaboration) “The Multi-Messenger Approach.

5th Science AGILE Workshop, June Observations of pulsars with MAGIC Marcos López (INFN/Padova) on behalf of the MAGIC collaboration.

Calibration for LHAASO_WFCTA Yong Zhang, LL Ma on behalf of the LHAASO collaboration 32 nd International Cosmic Ray Conference, Beijing 2011.

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.

WP-Technology Working Group Future of Ground Based Gamma-ray Astronomy Feb 8, Technology & Cost WP Working Group GOALS With the Current Generation.

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

TeVPA, July , SLAC 1 Cosmic rays at the knee and above with IceTop and IceCube Serap Tilav for The IceCube Collaboration South Pole 4 Feb 2009.

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.

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

Gamma-Ray Astronomy Dana Boltuch Ph. D

Jamie Holder School of Physics and Astronomy, University of Leeds, U.K Optical SETI at Leeds Using Cherenkov Light Buckets as Optical SETI Detectors RAS.

MPI Seminar, October 7, 2008Thomas Schweizer, Development of a new low-threshold Trigger M. Shayduk, M. Rissi, T. Schweizer, N. Otte, M. Lopez for the.

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.

Marcus ZieglerAPS April Meeting Gamma-Ray Pulsars in the GLAST Era Gamma-ray Large Area Space Telescope Marcus Ziegler Santa Cruz Institute for.

High Energy Detection. High Energy Spectrum High energy EM radiation:  (nm)E (eV) Soft x-rays X-rays K Soft gamma rays M Hard gamma.

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

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

A feasibility study for the detection of SuperNova explosions with an Undersea Neutrino Telescope A. Leisos, A. G. Tsirigotis, S. E. Tzamarias Physics.

Julie McEnery GLAST Science Lunch Milagro: A Wide Field of View Gamma-Ray Telescope Julie McEnery.

22 February 2006 Quo Vadis ? Wide Field Imaging A Wide Angle Very Low Threshold Air Cherenkov Imaging Telescope Razmick Mirzoyan MPI Munich, Germany.

Leroy Nicolas, HESS Calibration results, 28 th ICRC Tsukuba Japan, August Calibration results of the first two H·E·S·S· telescopes Nicolas Leroy.

International research project GALA: Monitoring of high energy gamma-ray astrophysical sources.

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

X.-X. Li, H.-H. He, F.-R. Zhu, S.-Z. Chen on behalf of the ARGO-YBJ collaboration Institute of High Energy Physics Nanjing GRB Conference,Nanjing,

EAS Reconstruction with Cerenkov photons Ching-Cheng Hsu, Jan Ching-Cheng Hsu National Taiwan Univ. Dept of physics Feb Shower Simulation.

28 th ICRC Tsukuba Conor Masterson, H.E.S.S. Observations of Galactic Sources with H.E.S.S. Conor Masterson, MPI-K, for the H.E.S.S. Collaboration.

Moriond 2001Jordan GoodmanMilagro Collaboration The Milagro Gamma Ray Observatory The Physics of Milagro Milagrito –Mrk 501 –GRB a Milagro –Description.

EAS Reconstruction with Cerenkov Photons Shower Simulation Reconstruction Algorithm Toy MC Study Two Detector Configuration Summary M.Z. Wang and C.C.

Atmospheric shower simulation studies with CORSIKA Physics Department Atreidis George ARISTOTLE UNIVERSITY OF THESSALONIKI.

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

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

TOP counter overview and issues K. Inami (Nagoya university) 2008/7/3-4 2 nd open meeting for proto-collaboration - Overview - Design - Performance - Prototype.

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

Development of TOP counter for Super B factory K. Inami (Nagoya university) 2007/10/ th International Workshop on Ring Imaging Cherenkov Counters.

Multi-TeV  -ray Astronomy with GRAPES-3 Pravata K Mohanty On behalf of the GRAPE-3 collaboration Tata Institute of Fundamental Research, Mumbai Workshop.

Nov Beam Catcher in KOPIO (H. Mikata Kaon mini worksyop1 Beam Catcher in the KOPIO experiment Hideki Morii (Kyoto Univ.) for the KOPIO.

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.

Extending the Sensitivity Of Air-Cerenkov Telescopes Steve Biller, Oxford University (de la Calle & Biller – astro-ph/ )

Design for Wide FOV Cherenkov telescope upgrading THE 2 nd WORKSHOP OF IHEP Shoushan Zhang Institute of High Energy Physics.

The Spectrum of Markarian 421 Above 100 GeV with STACEE

Hybrid measurement of CR light component spectrum by using ARGO-YBJ and WFCTA Shoushan Zhang on behalf of LHAASO collaboration and ARGO-YBJ collaboration.

Introduction Data analyzed Analysis method Preliminary results

Test beam preliminary results D. Di Filippo, P. Massarotti, T. Spadaro.

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.

Prospects to Use Silicon Photomultipliers for the Astroparticle Physics Experiments EUSO and MAGIC A. Nepomuk Otte Max-Planck-Institut für Physik München.

Rencontres de Moriond Detection of the Crab pulsar with MAGIC: First pulsar detected > 25 GeV Marcos López (INFN/Padova) T. Schweizer, N.Otte, M.Rissi,

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

Search for GRBs Using ARGO Data in Shower Mode Guo Y.Q. For ARGO-YBJ Collaboration BeiJing 2008/09/26.

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

High-energy Electron Spectrum From PPB-BETS Experiment In Antarctica Kenji Yoshida 1, Shoji Torii 2 on behalf of the PPB-BETS collaboration 1 Shibaura.

Aous Abdo Ground-based Gamma-ray Astronomy: Towards the Future. Santa Fe, NM May 11–12, 2006 Detection of Tev  -rays from the Cygnus Region with Milagro.

Current status of XMASS experiment 11 th International Workshop on Low Temperature Detectors (LTD-11) Takeda Hall, University of Tokyo, JAPAN 8/1, 2005.

MAGIC Telescopes - Status and Results 2009/ Isabel Braun Institute for Particle Physics, ETH Zürich for the MAGIC collaboration CHIPP Plenary Meeting.

Lingling Ma IHEP China Measurement of Cosmic rays with LHAASO at 10PeV~100PeV 4th Workshop on Air Shower Detection at High Altitude Institute of High Energy.

CTA-LST Large Size Telescope M. Teshima for the CTA Consortium Institute for Cosmic Ray Research, University of Tokyo Max-Planck-Institute for Physics.

1 Cosmic Ray Physics with IceTop and IceCube Serap Tilav University of Delaware for The IceCube Collaboration ISVHECRI2010 June 28 - July 2, 2010 Fermilab.

The VERITAS Trigger System A. Weinstein 1 for the VERITAS Collaboration 2 CFD x 499 (1 per pixel ) Pattern Trigger Shower Delay ( 1 PDM channel per trigger.

Tobias Jogler Max-Planck Institut für Physik IMPRS YSW Ringberg 2007 VHE emission from binary systems Outline Binary systems Microquasar Pulsar binaries.

Konstantia Balasi Institute of Nuclear and Particle Physics NCSR Demokritos NCSR Demokritos Gamma Ray Burst Neutrino Telescope GRBNeT GRBNeT: an autonomous.

HARPO, a Micromegas+GEM TPC for gamma polarimetry above 1 MeV

CANAGAROO-II PSR B Yamagata Univ. N.Sakamoto , S.Gunji

Balloon observation of electrons and gamma rays with CALET prototype

Electron Beam as a standard candle for EHECR air shower

Presentation transcript:

Performance of GeV gamma ray camera for SUBARU optical-infrared telescope A.Asahara*, K.Komiyama#, G.Kosugi#, H.Kubo*, S.Miyazaki#, M.Mori , M.Nakagiri#, D.Nishida*, R.Ogasawara#, R.Orito*, K.Sakurazawa ♭, T.Takata#, T.Tanimori* and T.Usuda# ＊ Department of Physics, Kyoto University, Japan ＃ Subaru Telescope, National Astronomical Observatory  ICRR, University Tokyo ♭ Tokyo Institute of Technology 1.Introduction 2.Detectors at GeV region 3.High altitude observation 4.“ CheSS ” gamma ray camera 5.Simulation of SUBARU with CheSS 6.Observation report 7.Summary AGENDA

1. Introduction -- Pulsars in 10GeV region -- Polar cap Outer gap Cut off very sharply ~20GeV Cut off more slowly ~50GeV Thompson astro-ph/ Credit: A.K. Harding (NASA/GSFC) Target: Crab pulsar/nebula 1.The standard candle for gamma-ray detectors. 2.SUBARU has a good location to observe it. 3.Wide band pulsed emission Pass through near the zenith. Extend above 10GeV ?

2. Detectors in 10GeV region SatelliteGround Crab Nebula (unpulsed component) EGRET ～ 10GeV STACEE CELESTE One point at 200GeV One point at 60GeV Conventional Cherenkov detectors Over 300GeV Two new type Cherenkov detectors COMPTEL MeV region

3. High Altitude Observation 10GeV gamma-seed (CORSIKA simulation)

SUBARU optical-infrared telescope FOV:0.75deg Focal length: 15m Mirror diameter:8.2m Mirror reflectivity:91%(380nm) Transmittance of correction lenses:68%(380nm) 0.75deg PMT array 0.1deg 200mm

How to set up SUBARU Prime Focus Unit CheSS SUBARU telescope PMTs Main mirrorPrime Focus Unit

4.CheSS (Cherenkov light detecting System on Subaru) １ｍ Weight ~200Kg Power consumption under 700W 200mm Acceptable trigger rate ～ 300Hz (dead time 20%) photo-cathode area ～ 233cm (without light guides) 2 44ch VME-TDC (ΔT =0.75nsec) Onboard VME-CPU 3ch VME-ADC GPS module Remote control Fast VME-based Electronics PMT array

5. Simulation of SUBARU with CheSS 1.Night Sky background ~6p.e/trigger 2.Expected trigger rate: ~30Hz 3.Energy threshold (gamma)~30GeV Jelley(1958) Same as observation data (Using CORSIKA) Cut the event when the sum of photons is under 7p.e

Sensitivity -- on-off chopping only -- PulsedUn-pulsed

6. Observation log Target:Crab pulsar Date:17, 18, and 19, December 2001 Time: on 12hours, off 12hours Weather:Fine Milky way 5min OFF 10min OFF 12min OFF On-Off chopping observation Crab 3 chopping modes: 5min, 10min, and 12min

Examples of noise reduction Timing cut Clustering cut Camera image PMT hit timing (measured by TDC) 35ns shower N.S.B ADC cut ADC N.S.B Shower (Power law) N.S.B Shower

Trigger rate Data on 17th Trigger rate of raw data ON:8 - 30Hz OFF: Hz Trigger rate after ADC cut (over 3000channel) 0.7Hz - 1.7Hz (depends on zenith angle) ONOFF

7. Summary  Gamma-ray pulsars in 10GeV region: Two emission models. polar cap or outer gap?  Cherenkov light detecting System on SUBARU: Compact detector. 1m X 1m cylindrical shape, 200 kg weight. Energy threshold is about 30GeV (simulation).  Observation of Crab On 17, 18, and 19, Dec 2001 Total time; On 12hours and Off 12hours.