All-aluminum mirrors for the MAGIC Cherenkov Telescope

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

DPG Tagung, March 2003Nadia Tonello, MPI für Physik (Werner- Heisenberg-Institut), München 1 Observations of 1ES with the HEGRA CT1 Cherenkov Telescope.

FDWAVE : USING THE FD TELESCOPES TO DETECT THE MICRO WAVE RADIATION PRODUCED BY ATMOSPHERIC SHOWERS Simulation C. Di Giulio, for FDWAVE Chicago, October.

Observations of the AGN 1ES with the MAGIC telescope The MAGIC Telescope 1ES Results from the observations Conclusion The MAGIC Telescope.

Peter Križan, Ljubljana Peter Križan University of Ljubljana and J. Stefan Institute The HERA-B RICH counter.

Telescope Tear-Down Anatomy of a 114mm f/8 Newtonian Reflector.

MAGIC II Mirrors and reflector M. Doro Udine. MAGIC Collaboration Meeting. 2006/05/10-13.

Preliminary estimate of performances using a 2- telescope system CTA meeting E. Carmona on behalf of the MAGIC collaboration Berlin, 5 May 2006.

Announcements No lab tonight due to Dark Sky Observing Night last night Homework: Chapter 6 # 1, 2, 3, 4, 5 & 6 First Quarter Observing Night next Wednesday.

Fig Reflection of an object (y) from a plane mirror. Lateral magnification m = y ’ / y © 2003 J. F. Becker San Jose State University Physics 52 Heat.

Could CKOV1 become RICH? 1. Characteristics of Cherenkov light at low momenta (180 < p < 280 MeV/c) 2. Layout and characterization of the neutron beam.

Auger Fluorescence Detector

H.E.S.S. High Energy Stereoscopic System Jon Cerny Bancroft-Rosalie School August 2002.

Wide-field, triple spectrograph with R=5000 for a fast 22 m telescope Roger Angel, Steward Observatory 1 st draft, December 4, 2002 Summary This wide-field,

Could CKOV1 become RICH? 1. Simulations 2. Sensitive area of the detection plane 3. Example of a workable solution 4. Geometrical efficiency of the photon.

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.

Sign rules (from your book) S>0 when object is on the incoming side of the lens or mirror S’>0 when the image is on the outgoing side of the lens or mirror.

M. Mariotti Padova University/INFN, CTA meeting Berlin 3-4 May 2006 >1 m 2 metallic mirror technology AIM find a suitable technology for large reflecting.

March 2, 2007 R. Mirzoyan: CTA Paris Meeting; Mount & Mirror WG Report Mount and Mirror (MM) Working Group Report Presented by Razmick Mirzoyan On behalf.

Vikrant Sista Roll No: EE10S012 IR and UV solar cells for windows and energy scavenging applications.

The Reflective Surface of the MAGIC Telescope Michele Doro on behalf of the MAGIC Collaboration University of Padova & INFN

The MAGIC Telescope Razmick Mirzoyan Max-Planck-Institute for Physics Max-Planck-Institute for Physics Munich, Germany EPS (July 17 th -23 rd 2003) Aachen,

Feasibility of Optical Wireless transmission systems for CTA R. Corsini, A. Wajahat, E. Ciaramella Scuola Superiore Sant’Anna, TeCP, Pisa, Italy R. Paoletti.

8 September Observational Astronomy TELESCOPES, Active and adaptive optics Kitchin pp

F. Goebel, MPI München, 4 May 2006, Berlin Florian Goebel Max-Planck-Institut für Physik (Werner-Heisenberg-Institut) München for the MAGIC collaboration.

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

CHIPP Plenary meeting August 2010, Gersau, Switzerland W. Lustermann, ETH Zurich TU Dortmund, Dortmund, Germany ISDC, Geneva, Switzerland EPFL,

17 November 2003EUSO meeting: R. Mirzoyan The MAGIC Telescope Project Razmick Mirzoyan Max-Planck-Institute for Physics Munich, Germany EUSO meeting.

Optics for Wide Field X-ray Imaging

May 4-5, 2006 T.Schweizer, CTA meeting Berlin Concept idea for a future telescope array observatory CTA meeting Berlin May 4-5, 2006 Thomas Schweizer.

1 Max-Planck-Institut fuer Physik, Muenchen, Germany, 2 Humboldt-Universituet Berlin, Germany, 3 Univ. Complutense, Madrid, Spain, 4 ETH, Zurich, Switzerland,

Reflection Regular reflection occurs when parallel light rays strike a smooth surface and reflect in the same direction. Diffuse reflection occurs when.

3/4/ PHYS 1442 – Section 004 Lecture #18 Monday March 31, 2014 Dr. Andrew Brandt Chapter 23 Optics The Ray Model of Light Reflection; Image Formed.

The Second International Workshop on Ultra-high-energy cosmic rays and their sources INR, Moscow, April 14-16, 2005 from Extreme Universe Space Observatory.

Upgrade plan of the MOA 1.8-m telescope F. Abe MOA collaboration 19 Jan. 2009, 13th Microlensing Paris.

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

September 16, 2008LSST Camera F2F1 Camera Calibration Optical Configurations and Calculations Keith Bechtol Andy Scacco Allesandro Sonnenfeld.

The Reflective Surface of the MAGIC Telescope Michele Doro on behalf of the MAGIC Collaboration University of Padova & INFN

7 March 2008Nicola Galante, DPG - Freiburg1 Observation of GRBs with the MAGIC Telescope Nicola Galante (MPI für Physik - München) for the MAGIC Collaboration.

Cherenkov Counters for SoLID Z.-E. Meziani on behalf of Simona Malace & Haiyan Gao (Duke University) Eric Fuchey (Temple University) SoLID Dry Run Review,

May 4th 2006R.Mirzoyan: CTA meeting, Berlin The MAGIC Project: Performance of the 1st telescope Razmick Mirzoyan On behalf of the MAGIC Collaboration Max-Planck-Institute.

Analysis chain for MAGIC Telescope data Daniel Mazin and Nadia Tonello Max-Planck-Institut für Physik München D.Mazin, N.Tonello MPI for Physics, Munich.

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

Silicon Optics for Wide Field X-ray Imaging Dick Willingale et al. – SPIE August 2013 Silicon Optics for Wide Field X-ray Imaging Dick Willingale University.

The islands method in the image analysis of atmospheric Cherenkov Telescopes data Nadia Tonello and Keiichi Mase Max-Planck-Institut für Physik München.

The MAGIC Telescope MAGIC

Status Report particle identification with the RICH detector Claudia Höhne - GSI Darmstadt, Germany general overview focus on ring radius/ Cherenkov angle.

Status of Modeling of Damage Effects on Final Optics Mirror Performance T.K. Mau, M.S. Tillack Center for Energy Research Fusion Energy Division University.

Introduction Data analyzed Analysis method Preliminary results

Tobias Jogler Max – Planck Institute für Physik MAGIC Observations of the HMXB LS I in VHE gamma rays Tobias Jogler on behalf.

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

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

Geant4 Simulation of the Pierre Auger Fluorescence Detector

Jason Koglin, APS/HEAD, April 2002 High Energy Focusing Telescope (HEFT) Caltech Space Radiation Laboratory Aleksey Bolotrikov, Hubert Chen, Walter R.

Status of the MAGIC Telescope Project Presented by Razmick Mirzoyan On behalf of the MAGIC Collaboration Max-Planck-Institute for Physics (Werner-Heisenberg-Institute)

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

MAGIC II Mirrors Features Production Calendar M.Doro for the Padova group MAGIC Collaboration Meeting Sofia May, (2007)

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

The ASTRI prototype: a pathfinder Dual-Mirror telescope for the CTA-SST array Rodolfo Canestrari for the ASTRI collaboration INAF-Astronomical Observatory.

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

First Results from the First G-APD Cherenkov Telescope Adrian Biland, ETH Zurich for the FACT Collaboration: TU Dortmund, U Geneva, EPF Lausanne, U Wuerzburg.

Development of Micro-Pore Optics at NAOC MPO research group X-ray Imaging Laboratory, NAOC Presented by Chen Zhang.

Future Imaging Atmospheric Cherenkov Telescopes:

Daniel Mazin and Nadia Tonello Max-Planck-Institut für Physik München

Date of download: 11/1/2017 Copyright © ASME. All rights reserved.

Date of download: 11/1/2017 Copyright © ASME. All rights reserved.

Observational Astronomy

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

XRT Performance Update

Warm Up Set 15 Question Two rays of light, of wavelength 600nm, reflect from glass surfaces separated by 150nm. The rays are initially in phase. What.

Presentation transcript:

All-aluminum mirrors for the MAGIC Cherenkov Telescope Nadia Tonello, for the MAGIC Collaboration Why all-aluminum mirrors Technical characteristics of the mirrors Performance Summary

Nadia Tonello, MPI für Physik, München Motivations Reduce the weight of the mirrors: limited deformation of the main frame, rapid positioning for GRB alert Parabolic (isochronous) mirror profile: many different radii of curvature, difficult to make it with glass mirrors Heating system: avoid problems of dew (ice) Reduce costs SOLUTION: diamond milled all-aluminum mirrors 50 x 50 cm2 sandwich construction DPG Tagung, March 2003 Nadia Tonello, MPI für Physik, München

Nadia Tonello, MPI für Physik, München The MAGIC Telescope ORM, La Palma (Canary Islands) Mirrors area 239 m² Camera 576 pixels FOV 4° Energy threshold 30 GeV Positioning time < 40 s DPG Tagung, March 2003 Nadia Tonello, MPI für Physik, München

Technical view of a mirror All-aluminum 50x50 cm ² sandwich = light weight (~ 4kg) Original development at MPI (Munich), production of improved raw blanks in Padua (I) Diamond milled reflecting surface Heating system Light and stiff honey-comb structure The mirrors are mounted in panels before the installation 1.0 DPG Tagung, March 2003 Nadia Tonello, MPI für Physik, München

Nadia Tonello, MPI für Physik, München Performance Reflectivity vs. wavelength for a coated mirror Roughness = 4.1 nm 87% on av. between 300 and 650 nm (sensitivity region of the PMTs) DPG Tagung, March 2003 Nadia Tonello, MPI für Physik, München

Focal spot studies Shape and size of the spot: measurement of the effective radius of curvature. 6 cm Light distribution from the center of the spot Measurements taken at 2* focal length 90% of the light is collected in a circle ~30% of a pixel ø DPG Tagung, March 2003 Nadia Tonello, MPI für Physik, München

Assembling and alignment The mirrors are assembled in panels of 4, pre-aligned and fixed. DPG Tagung, March 2003 Nadia Tonello, MPI für Physik, München

Installation on the telescope The panels are installed in the main frame . The active mirror control allow to align the panels (MG talk) DPG Tagung, March 2003 Nadia Tonello, MPI für Physik, München

Nadia Tonello, MPI für Physik, München Summary Size of a mirror 0.25 m2 Weight of a mirror 3.5 kg Reflectivity (incl. coating) ≥ 85 % Roughness 4.1 nm Average spot size (90%) 1 cm  Mirror production state: 750 / 959 Panels installation state: 98 / 245 DPG Tagung, March 2003 Nadia Tonello, MPI für Physik, München

The new technology mirrors are a good alternative to glass mirrors. Conclusions Production of light weight mirrors (weight :1/2 of glass mirrors) . Optical quality matches glass mirrors. Technology of diamond milling allows to change easily the focal length during production (for parabolic profile). Cost of diamond milling = 290 € ( incl. quartz coating) Prototypes installed in HEGRA CT1 show good quality after 5 years exposure. Control of the optical surface of the telescope with AMC (M.G. talk) Preparing next generation of 1 m2 mirrors of aspheric surface. The new technology mirrors are a good alternative to glass mirrors. DPG Tagung, March 2003 Nadia Tonello, MPI für Physik, München