Stellar Intensity Interferometric Capabilities of IACT Arrays*
|
|
- Silas Crawford
- 6 years ago
- Views:
Transcription
1 Stellar Intensity Interferometric Capabilities of IACT Arrays* Dave Kieda Nolan Matthews University of Utah Salt Lake City, Utah *for VERITAS and CTA collaborations
2 Photon Bunching & Intensity Interferometry D= Correlation Distance
3 3 SII Imaging Basic Intensity Interferometry λ B I " Measures correlation in intensity fluctuations (not amplitude!). R R. Hanbury Brown, J. Davis and L. R. Allen, MNRAS 137 (1967) 375.
4 4 SII Imaging Basic Intensity Interferometry Some Pains, But Large Gains: B I " λ -Relatively insensitive to atmospheric turbulence ( turbulence ~ khz, sampling ~100 s MHz ). - Km Baselines possible, operate at blue wavelengths ->sub milli-arcsecond resolution -No need to maintain steady optical interference path between focal planes. -> higher order intensity correlations possible Measures correlation in intensity fluctuations (not amplitude!). -Loss of phase information: Phase recovery needed.
5 5 Signal to Noise Ratio (SNR) in Intensity Interferometry Hanbury Brown 1974; Twiss 1969 Light collection area q.e. of detectors Photo-electron Rate Optical Bandwidth Electronic Bandwidth Integration Time Normalized Visibility Example Calculation: p.e./sec (m v = 1.0, A=100 m 2 = 0.3 ) Hz (for 10nm filter) -250 MHz -1 hour observation - dual polarization -Assume unresolved = 1.0 How to Improve? -Multi-Channel Intensity Interferometer: N %& improvement, (Trippe, 2015) -Redundant baselines: N ()* improvement. -Fast optics & correlators (> 1GHz). Spectral Flux Density (ph s -1 m -2 Hz -1 ) SNR = 200 (assuming ideal system, limited to bright sources)
6 2 nd -order time coherence g (2) & Fourier Image plane g (2) (0,0,0) Lab measurement of g (2) (0, 0, t ) of simulated star/thermal light Matthews, Kieda & LeBohec, accepted in J Opt (2017) +, -,. / +, - /+,. / = g(2) (u, v, t ) = 1 + ½g (1) (u, v, t)½ 2 For II: experimental time resolution t ~ 1 nsec blackbody coherence time t % ~ 4 5 ~ 10 psec g (2) (0,0,0) = 1 + ε ~ small non-gaussian fluctuations => Need large photon counts: 10+ m mirrors m g (1) (u, v, t) : first-order coherence =1 for [u, v, t=0] g (4) u, v, 0 = E I l, m e I"JK *LMNO dl dm I l, m describes the image size and brightness distribution (Van Cittert-Zernike Theorem 1934,1938) l I l, m Reconstructed SII laboratory images stellar disk (left) & binary system (right) Matthews, Kieda & LeBohec, accepted in J Opt (2017)
7 Potential SII at Optical Telescope Arrays VERITAS IACT Array VLTI- Paranal Future CTA/pSCT Array 100 m Excellent instruments for SII: -Large photon collection area (~10 m diameter mirrors) -Optically isochronous (< 5 ns) 100 m to km baselines (milli-arcsec resolution) J. Holder and S. LeBohec, Ap. J. 649 (2006) 399 D. Dravins et al., New Astronomy Reviews 56, 5 (2012) km
8 Potential VERITAS SII Augmentation VERITAS Camera 499 PMT pixels Dual polarization SII pixel (replaces 3 Center PMTs)
9 SII Data Quality Monitor GPS Timecode Generator 10 GB Ethernet 10 MHz 1 PPS WR-SWITCH Module Telescope 2 Single Mode Fiber 50m - 2 km (80 km max) Telescope 3 plastic fiber plastic fiber Telescope 4 Telescope N Telescope ft double shielded RG 223
10 SII Data Quality Monitor 10 GB Ethernet GPS Timecode Generator 10 MHz 1 PPS WR-SWITCH Module Typical SII Augmentation Standalone telescope connected only by fiber optic (White Rabbit, 10G) Telescope 2 Single Mode Fiber 50m - 2 km (80 km max) Telescope 3 plastic fiber plastic fiber Telescope 4 Replace with Custom board in camera? Telescope ft double shielded RG 223 Telescope N
11 Simple VERITAS interferometer simulation Simulated baselines Fourier image Plane sampling (vertical) 100 μ arcsec S. Lebohec et al *`ghost images caused by incomplete sampling of Fourier plane *reflection symmetry of ghost images caused by loss of phase information
12 1-2 km baselines telescopes
13 Simulated Fourier image Planes Reconstructed Binary images Input Binary images Simulated observations of binary stars with different sizes. (m V = 3; T eff = 7000 K; T = 10 h; Dt = 1 ns; l = 500 nm; Dl = 1 nm; QE = 70%) Already changes in stellar radii by only a few micro-arcseconds are well resolved. Better sampling of Fourier image plane-> no ghost images D.Dravins, S.LeBohec, H.Jensen, P.D.Nuñez:, CTA Consortium Optical intensity interferometry with the Cherenkov Telescope Array, Astropart. Phys. 43, 331 (2013)
14 f = 5.6 m, D= 9.6 m, FOV= 8 Pixel = 6 mm ( 11,328 SiPMs) PSFD68= ~ (pix= 0.06 ) CTA-US Schwarzschild-Couder Telescope Prototype is Currently under construction at VERITAS Observatory (Fall 2017 commission)
15 Schwarzschild-Couder two-mirror IACT telescope Wide field of view, excellent spot size RMS spread in arrival time of rays at focal plane as a function of field angle.. On-axis: photon timespread <0.2 nsec rms >>improved g (2) (t) >>reduced observation time 2-4Ghz sampling + SiPM (QE-0.9). SNR = 200 -> SNR =2400! V. Vassiliev, S. Fegan, P. Brousseau: Wide field aplanatic two-mirror telescopes for ground-based g-ray astronomy Astropart.Phys. 28, 10 (2007)
16 IACT Observatories are Excellent Instruments for SII Imaging Digitizing electronics/white Rabbit synchronization Standalone telescopes connected by inexpensive fiber optics km baseline separations now achievable Offline (post-observation) photon correlations Polarization data allows higher S/N, baseline noise estimation Demonstrated correlation using of pipelined FPGA for near real-time processing Higher order correlations may contain additional image information (Ofir & Ribak 2006) Near Term Implementation VERITAS Telescopes (Potential deployment/use in ) m baselines: 100 μ arcsec imaging possible Longer Term Development VLTI visible light feed /single board implementation? CTA/SCT-telescope array implementation : 1-2 km baselines, <100 μ arcsec imaging?
Ultra-High Resolution Astronomical Imaging Using Quantum Properties of Light. Dave Kieda, Nolan Matthews University of Utah
Ultra-High Resolution Astronomical Imaging Using Quantum Properties of Light Dave Kieda, Nolan Matthews University of Utah ANGULAR SCALES IN OPTICAL ASTRONOMY Rayleigh Criteria Sun, Moon ~30 arcmin Θ=1.22
More informationStellar Intensity Interferometric Capabilities of IACT Arrays
Stellar Intensity Interferometric Capabilities of IACT Arrays Dave Kieda 1 Department of Physics and Astronomy University of Utah, Salt Lake City, Utah, USA E-mail: dave.kieda@utah.edu Nolan Matthews Department
More informationAir Cherenkov Telescope Arrays!
Air Cherenkov Telescope Arrays! " " " " " " " "as SII receivers! Imaging Air Cherenkov Telescope (IACT) arrays are appealing for Intensity Interferometry because of the large number of simultaneous baselines
More informationSTELLAR INTENSITY INTERFEROMETRY. Dainis Dravins Lund Observatory
CTA Stockholm 2011-02-23 STELLAR INTENSITY INTERFEROMETRY Optical imaging with sub-milliarcsecond resolution Dainis Dravins Lund Observatory www.astro.lu.se/~dainis ANGULAR RESOLUTION IN ASTRONOMY 1 arcsec
More informationThe CTA SST-1M cherenkov telescope. for high-energy gamma-ray astronomy. and its SiPM-based camera. Victor Coco (DPNC, Universite de Geneve)
The SST-1M Cherenkov telescope for high-energy gamma-ray astronomy and its SiPM-based camera (DPNC, Universite de Geneve) on behalf of the SST-1M sub-consortium and the CTA consortium The CTA SST-1M cherenkov
More informationExtremely high angular resolution in optical astronomy
JD 1 The Highest-Energy Gamma-ray Universe IAU XVIII GA, Beijing, August 2012 Extremely high angular resolution in optical astronomy Dainis Dravins Lund Observatory, Sweden www.astro.lu.se/~dainis ANGULAR
More informationThe Cherenkov Telescope Array. Kevin Meagher Georgia Institute of Technology
The Cherenkov Telescope Array Kevin Meagher Georgia Institute of Technology Outline VHE Gamma Ray Astronomy CTA Overview Science Goals for CTA Schwarzschild-Couder Telescope Extension 2 Gamma-ray Astronomy
More informationTowards the Intensity Interferometry Stellar Imaging System
Towards the Intensity Interferometry Stellar Imaging System arxiv:0906.3276v1 [astro-ph.im] 17 Jun 2009 M. Daniel, W.J. de Wit, D. Dravins, D. Kieda, S. LeBohec, P. Nunez, E. Ribak for the Stellar Intensity
More informationIntensity Interferometry with SPADs
Intensity Interferometry with SPADs May 13, 2014 Genady Pilyavsky, Nathan Smith, Philip Mauskopf, Ed Schroeder, Ian Chute, Adrian Sinclair Arizona State University (ASU) What Is the Scientific Motivation?
More informationOptical Intensity Interferometry with Atmospheric Cherenkov Telescope Arrays
Version 1.10 Optical Intensity Interferometry with Atmospheric Cherenkov Telescope Arrays S. Le Bohec Department of Physics, University of Utah, Salt-Lake-City, UT, 84112-0830, USA lebohec@physics.utah.edu
More informationPlans for Unprecedented Imaging of Stellar Surfaces with the Navy Precision Optical Interferometer (NPOI)
Plans for Unprecedented Imaging of Stellar Surfaces with the Navy Precision Optical Interferometer (NPOI) A. M. Jorgensen Electrical Engineering Department New Mexico Tech, USA H. R. Schmitt, D. Mozurkewich,
More information1. Give short answers to the following questions. a. What limits the size of a corrected field of view in AO?
Astronomy 418/518 final practice exam 1. Give short answers to the following questions. a. What limits the size of a corrected field of view in AO? b. Describe the visibility vs. baseline for a two element,
More informationPhase-Referencing and the Atmosphere
Phase-Referencing and the Atmosphere Francoise Delplancke Outline: Basic principle of phase-referencing Atmospheric / astrophysical limitations Phase-referencing requirements: Practical problems: dispersion
More informationStellar Intensity Interferometry with Air Cherenkov Telescope arrays
Stellar Intensity Interferometry with Air Cherenkov Telescope arrays S. Le Bohec1, M. Daniel2, W.J. de Wit2, J.A. Hinton2, E. Jose1, J.A. Holder3, J. Smith1, and R.J. White2 1: Department of Physics, University
More informationTHE PATH TOWARDS THE CHERENKOV TELESCOPE ARRAY OBSERVATORY. Patrizia Caraveo
THE PATH TOWARDS THE CHERENKOV TELESCOPE ARRAY OBSERVATORY Patrizia Caraveo 5 y integration of the gamma-ray sky Optical +TeV The TeV sky > 40, Active Galactic Nuclei (Blazars) AGN TeV by electrons (strong
More informationVERITAS Design. Vladimir Vassiliev Whipple Observatory Harvard-Smithsonian CfA
VERITAS Design Vladimir Vassiliev Whipple Observatory Harvard-Smithsonian CfA VERITAS design goals VERITAS is a ground-based observatory for gamma-ray astronomy VERITAS design is derived from scientific
More informationFeasibility of observing Hanbury Brown and Twiss phase
Zurich Open Repository and Archive University of Zurich Main Library Strickhofstrasse 39 CH-8057 Zurich www.zora.uzh.ch Year: 2014 Feasibility of observing Hanbury Brown and Twiss phase Wentz, T; Saha,
More informationThe science potential of atmospheric Cherenkov arrays used as intensity interferometers
The science potential of atmospheric Cherenkov arrays used as intensity interferometers Michael Daniel for Willem-Jan de Wit w.j.m.dewit@leeds.ac.uk Atmospheric Cherenkov Telescope Arrays Multiple telescopes
More informationTOWARDS OPTICAL INTENSITY INTERFEROMETRY FOR HIGH ANGULAR RESOLUTION STELLAR ASTROPHYSICS
TOWARDS OPTICAL INTENSITY INTERFEROMETRY FOR HIGH ANGULAR RESOLUTION STELLAR ASTROPHYSICS by Paul D. Nuñez A dissertation submitted to the faculty of The University of Utah in partial fulfillment of the
More informationCherenkov Telescope Arrays
Cherenkov Telescope Arrays Michael Daniel University of Durham michael.daniel@durham.ac.uk Workshop on Stellar Intensity Interferometry 1 CONTENTS Introduction to Cherenkov telescopes Characteristics of
More informationLong-baseline intensity interferometry: data transmission and correlation
Long-baseline intensity interferometry: data transmission and correlation Erez Ribak Department of Physics Technion Israel Institute of Technology Workshop on Hanbury Brown & Twiss interferometry Nice,
More informationWhite Paper on the Revival of Stellar Intensity Interferometry
White Paper on the Revival of Stellar Intensity Interferometry E. Ribak a S. LeBohec b a Physics Department, Technion, Haifa 32000, Israel b Physics Department, University of Utah, UT 84112-0830, USA Abstract
More informationAGIS (Advanced Gamma-ray Imaging System)
AGIS (Advanced Gamma-ray Imaging System) Seth Digel, Stefan Funk and Hiro Tajima SLAC National Accelerator Laboratory Kavli Institute for Particle Astrophysics and Cosmology Outline AGIS project and status
More informationChapter 1. Intensity Interferometry
May 23, 2016 10:36 World Scientific Review Volume - 9.75in x 6.5in Handbook Dravins 160523 page 1 Chapter 1 Intensity Interferometry Dainis Dravins Lund Observatory, Box 43, SE-22100 Lund, Sweden dainis@astro.lu.se
More informationMonte Carlo Studies for a Future Instrument. Stephen Fegan Vladimir Vassiliev UCLA
Monte Carlo Studies for a Future Instrument Stephen Fegan Vladimir Vassiliev UCLA Approach to simulations CORSIKA 6200, 6500, 6502 w/bernlöhr Simulation of response of a single cell of an infinite array
More informationDevelopment of a prototype for Fluorescence detector Array of Single-pixel Telescopes (FAST)
Development of a prototype for Fluorescence detector Array of Single-pixel Telescopes (FAST) T. Fujii 1,2, P. Privitera 1, J. Jiang 1 construction is still, A. Matalon 1 in development, P. Motloch 1, M.
More informationAn introduction to closure phases
An introduction to closure phases Michelson Summer Workshop Frontiers of Interferometry: Stars, disks, terrestrial planets Pasadena, USA, July 24 th -28 th 2006 C.A.Haniff Astrophysics Group, Department
More informationarxiv: v1 [astro-ph.im] 15 Jul 2014
Silicon Photomultiplier Camera for Schwarzschild-Couder Cherenkov Telescopes arxiv:1407.4151v1 [astro-ph.im] 15 Jul 2014 J. Vandenbroucke for the CTA Consortium Physics Department and Wisconsin IceCube
More informationContinuum Observing. Continuum Emission and Single Dishes
July 11, 2005 NAIC/NRAO Single-dish Summer School Continuum Observing Jim Condon Continuum Emission and Single Dishes Continuum sources produce steady, broadband noise So do receiver noise and drift, atmospheric
More informationHigh-Resolution Imagers
40 Telescopes and Imagers High-Resolution Imagers High-resolution imagers look at very small fields of view with diffraction-limited angular resolution. As the field is small, intrinsic aberrations are
More informationTHE PATH TOWARDS THE CHERENKOV TELESCOPE ARRAY OBSERVATORY. Patrizia Caraveo
THE PATH TOWARDS THE CHERENKOV TELESCOPE ARRAY OBSERVATORY Patrizia Caraveo 1 st Interaction: X 0 40 g/cm 2 pair = 9/7 X 0 50 g/cm 2 X = X A e h/h0 and X A 10 3 g/cm 2 h pair = h 0 ln(x A / pair ) 20 km
More informationOptical interferometry: problems and practice
Outline Optical interferometry: problems and practice Chris Haniff Aims. What is an interferometer? Fundamental differences between optical and radio. Implementation at optical wavelengths. Conclusions.
More informationSpectral Resolution in Interferometry
Spectral Resolution in Interferometry Christopher Tycner Michelson Postdoctoral Fellow @ U. S. Naval Observatory Flagstaff Station Outline Spectral Resolution in Interferometry Implementation Benefits
More informationImaging applications of Statistical Optics
Imaging applications of Statistical Optics Monday Radio Astronomy Michelson Stellar Interferometry Coherence Imaging Rotational Shear Interferometer (RSI) Wednesday Optical Coherence Tomography (OCT) 03/14/05
More informationChallenges for the next generation stellar interferometer. Markus Schöller European Southern Observatory January 29, 2009
Challenges for the next generation stellar interferometer Markus Schöller European Southern Observatory January 29, 2009 VLTI Four 8.2m telescopes (UTs) All equipped with AO (MACAO) Six Baselines 47m-130m
More informationVery Large Telescope Paranal Science Operations PIONIER User Manual
EUROPEAN SOUTHERN OBSERVATORY Organisation Européene pour des Recherches Astronomiques dans l Hémisphère Austral Europäische Organisation für astronomische Forschung in der südlichen Hemisphäre ESO - European
More informationPipeline reductions of AMBER calibrator data
Pipeline reductions of AMBER calibrator data Christian A. Hummel ESO, Karl-Schwarzschild-Str. 2, 85748 Garching, Germany ABSTRACT Service (and visitor) mode operations by ESO involving the three-beam NIR
More informationEXPOSURE TIME ESTIMATION
ASTR 511/O Connell Lec 12 1 EXPOSURE TIME ESTIMATION An essential part of planning any observation is to estimate the total exposure time needed to satisfy your scientific goal. General considerations
More informationJonathan Biteau, David Chinn, Dennis Dang, Kevin Doyle, Caitlin A. Johnson, David A. Williams, for the CTA Consortium
Performance of Silicon Photomultipliers for the Dual-Mirror Medium-Sized Telescopes of the Cherenkov Telescope Array arxiv:1508.0645v1 [astro-ph.im] 5 Aug 015, David Chinn, Dennis Dang, Kevin Doyle, Caitlin
More informationFundamental Limits to Wavefront Sensing in the Submillimeter
Fundamental Limits to Wavefront Sensing in the Submillimeter E. Serabyn Jet Propulsion Laboratory, California Institute of Technology, 4800 Oak Grove Drive, Pasadena, CA, USA 91109 Copyright 2006 Society
More informationDetector R&D at KIPAC. Hiro Tajima Kavli InStitute of Particle Astrophysics and Cosmology
Detector R&D at KIPAC Hiro Tajima Kavli InStitute of Particle Astrophysics and Cosmology Detector R&D Overview Si detector ASIC Integration GLAST GeV Gamma-ray Observatory ASIC DAQ Next generation X-ray
More informationMcMath-Pierce Adaptive Optics Overview. Christoph Keller National Solar Observatory, Tucson
McMath-Pierce Adaptive Optics Overview Christoph Keller National Solar Observatory, Tucson Small-Scale Structures on the Sun 1 arcsec Important astrophysical scales (pressure scale height in photosphere,
More informationData modeling and interpretation of interferometric data. Antoine Mérand ESO/Garching VLTI Programme Scientist
Data modeling and interpretation of interferometric data Antoine Mérand ESO/Garching VLTI Programme Scientist Garching - March 6th, 2017 Tone of the talk Oriented toward instrumental aspects with important
More informationTop Le# side TEST Right side bo.om
Top bo.om e# side TEST Right side Correlation functions in optics and quantum optics, 4 University of Science and Technology of China Hefei, China Luis A. Orozco www.jqi.umd.edu The slides of the course
More informationToward a revival of Stellar Intensity Interferometry
Toward a revival of Stellar Intensity Interferometry Stephan LeBohec 1, Cesare Barbieri 2, Willem-Jan de Wit 3, Dainis Dravins 4, Philippe Feautrier 5, C dric Foellmi 5, Andreas Glindemann 6, Jeter Hall
More informationAstrometry (STEP) M. Shao
Technical Issues for Narrow Angle Astrometry (STEP) M. Shao Outline Ground based narrow angle astrometry Current state of the art (0.5~1 mas (in 30 min) What are the limiting error sources Photon noise
More informationStatus of the MAGIC telescopes
SNOWPAC 2010 Status of the MAGIC telescopes Pierre Colin for the MAGIC collaboration Max-Planck-Institut für physik (Munich) Status of the MAGIC telescopes MAGIC-1 MAGIC-2 Outline: Recent results of the
More informationOPTICAL MULTI-CHANNEL INTENSITY INTERFEROMETRY OR: HOW TO RESOLVE O-STARS IN THE MAGELLANIC CLOUDS
Journal of the Korean Astronomical Society http://dx.doi.org/10.5303/jkas.2014.47.6.235 47: 235 253, 2014 December pissn: 1225-4614 eissn: 2288-890X c 2014. The Korean Astronomical Society. All rights
More informationAstronomy 203 practice final examination
Astronomy 203 practice final examination Fall 1999 If this were a real, in-class examination, you would be reminded here of the exam rules, which are as follows: You may consult only one page of formulas
More informationApplications of Statistical Optics
Applications of Statistical Optics Radio Astronomy Michelson Stellar Interferometry Rotational Shear Interferometer (RSI) Optical Coherence Tomography (OCT) Apps of Stat Optics p-1 Radio Telescope (Very
More informationStatus of the Small-Sized Telescopes of the Cherenkov Telescope Array
Status of the Small-Sized Telescopes of the Cherenkov Telescope Array Akira OKUMURA for the CTA Consortium (Thanks to the SST teams) Institute for Space-Earth Environmental Research, Nagoya University
More informationWebster Cash University of Colorado. X-ray Interferometry
Webster Cash University of Colorado X-ray Interferometry Co-Investigators Steve Kahn - Columbia University Mark Schattenburg - MIT David Windt - Lucent (Bell-Labs) Outline of Presentation Science Potential
More informationThe Hanbury Brown Twiss effect for matter waves. Chris Westbrook Laboratoire Charles Fabry, Palaiseau Workshop on HBT interferometry 12 may 2014
The Hanbury Brown Twiss effect for matter waves Chris Westbrook Laboratoire Charles Fabry, Palaiseau Workshop on HBT interferometry 12 may 2014 Outline: Hanbury Brown Twiss effect... 1.... in optics and
More informationarxiv: v1 [astro-ph.im] 16 May 2014
1 arxiv:1405.4187v1 [astro-ph.im] 16 May 2014 The INAF ASTRI Project in the framework of CTA N. La Palombara, P. Caraveo, M. Fiorini, L. Stringhetti INAF IASF Milano, Via E. Bassini 15, 20133 Milano (I)
More informationTelescopes. Optical Telescope Design. Reflecting Telescope
Telescopes The science of astronomy was revolutionized after the invention of the telescope in the early 17th century Telescopes and detectors have been constantly improved over time in order to look at
More informationLight and Telescope 10/24/2018. PHYS 1403 Introduction to Astronomy. Reminder/Announcement. Chapter Outline. Chapter Outline (continued)
PHYS 1403 Introduction to Astronomy Light and Telescope Chapter 6 Reminder/Announcement 1. Extension for Term Project 1: Now Due on Monday November 12 th 2. You will be required to bring your cross staff
More informationChapter 5: Telescopes
Chapter 5: Telescopes You don t have to know different types of reflecting and refracting telescopes. Why build bigger and bigger telescopes? There are a few reasons. The first is: Light-gathering power:
More informationFirst Results from the HiSCORE/Siberia WR setup. Plans for CTA. and. Martin Brückner (Humboldt-Univ. Berlin) Ralf Wischnewski (DESY)
First Results from the HiSCORE/Siberia WR setup and Plans for CTA Martin Brückner (Humboldt-Univ. Berlin) Ralf Wischnewski (DESY) 7th White Rabbit workshop Madrid / Spain 28.11.2012 Outline > HiSCORE -
More informationTelescopes (Chapter 6)
Telescopes (Chapter 6) Based on Chapter 6 This material will be useful for understanding Chapters 7 and 10 on Our planetary system and Jovian planet systems Chapter 5 on Light will be useful for understanding
More informationCorrelation functions in optics and quantum optics, 4
Correlation functions in optics and quantum optics, 4 State Key Laboratory of Precision Spectroscopy East China Normal University, Shanghai, China Luis A. Orozco www.jqi.umd.edu The slides of the course
More informationIntroduction to Interferometer and Coronagraph Imaging
Introduction to Interferometer and Coronagraph Imaging Wesley A. Traub NASA Jet Propulsion Laboratory and Harvard-Smithsonian Center for Astrophysics Michelson Summer School on Astrometry Caltech, Pasadena
More informationInterferometry for pedestrians - a very brief introduction and basic concepts 1
Interferometry for pedestrians - a very brief introduction and basic concepts 1 Erik Bertram 1 Article concerning the lecture Perspektiven Moderner Astrophysik, Lecturer: Priv.- Doz. Dr. Silke Britzen
More informationSimulations for H.E.S.S.
Simulations for H.E.S.S. by K. Bernlöhr MPIK Heidelberg & HU Berlin Air shower measurement methods Imaging atmospheric Cherenkov telescopes In the imaging atmospheric Cherenkov telescope (IACT) technique,
More informationLecture 9. PMTs and Laser Noise. Lecture 9. Photon Counting. Photomultiplier Tubes (PMTs) Laser Phase Noise. Relative Intensity
s and Laser Phase Phase Density ECE 185 Lasers and Modulators Lab - Spring 2018 1 Detectors Continuous Output Internal Photoelectron Flux Thermal Filtered External Current w(t) Sensor i(t) External System
More informationIntroduction to Radio Interferometry Jim Braatz (NRAO)
Introduction to Radio Interferometry Jim Braatz (NRAO) Atacama Large Millimeter/submillimeter Array Expanded Very Large Array Robert C. Byrd Green Bank Telescope Very Long Baseline Array Radio Astronomy
More informationLecture 2. September 13, 2018 Coordinates, Telescopes and Observing
Lecture 2 September 13, 2018 Coordinates, Telescopes and Observing News Lab time assignments are on class webpage. Lab 2 Handed out today and is due September 27. Observing commences starting tomorrow.
More informationMRO INTERFEROMETER MEMO Tip/tilt
OBJECTIVE: MRO INTERFEROMETER MEMO Tip/tilt N. Thureau, G. Loos, D. Buscher, C. Haniff 19 March 2004 To determine the magnitude of the instantaneous tip-tilt motion expected at the MROI. To calculate the
More informationObservational methods for astrophysics. Pierre Hily-Blant
Observational methods for astrophysics Pierre Hily-Blant IPAG pierre.hily-blant@univ-grenoble-alpes.fr, OSUG-D/306 2016-17 P. Hily-Blant (Master2 APP) Observational methods 2016-17 1 / 323 VI Spectroscopy
More informationThe Einstein Polarization Interferometer for Cosmology (EPIC)
The Einstein Polarization Interferometer for Cosmology (EPIC) Peter Timbie UW-Madison for the EPIC collaboration Brown, Cardiff, Illinois, Ireland-Maynooth, LLNL, Manchester, Richmond, UCSD, Wisconsin,
More informationThe Gamma-ray Cherenkov Telescope
The Gamma-ray Cherenkov Telescope Pre-history, theory and experiment. CTA and the SSTs. GCT optical design. GCT mechanics. Camera. First Cherenkov light. Some things we have already learnt? What next?
More informationCorrelation functions in optics; classical and quantum 2. TUW, Vienna, Austria, April 2018 Luis A. Orozco
Correlation functions in optics; classical and quantum 2. TUW, Vienna, Austria, April 2018 Luis A. Orozco www.jqi.umd.edu Correlations in optics Reference that includes pulsed sources: Zheyu Jeff Ou Quantum
More informationRecent Results from VERITAS
Recent Results from VERITAS Physics Department, McGill University, Montreal, Canada E-mail: hanna@physics.mcgill.ca VERITAS (Very Energetic Radiation Imaging Telescope Array System) is an array of four
More informationSeptember 9, Wednesday 3. Tools for Solar Observations-I
September 9, Wednesday 3. Tools for Solar Observations-I Solar telescopes. Resolution, MTF, seeing. High resolution telescopes. Spectrographs. Types of Solar Observations Electro-magnetic observations
More informationarxiv: v1 [astro-ph.im] 1 Sep 2015
Flasher and muon-based calibration of the GCT telescopes proposed for the Cherenkov Telescope Array. arxiv:1509.00185v1 [astro-ph.im] 1 Sep 2015 Department of Physics, Durham University, DH1 3LE, UK E-mail:
More informationVery-High-Energy Gamma-Ray Astronomy with VERITAS. Martin Schroedter Iowa State University
Very-High-Energy Gamma-Ray Astronomy with VERITAS Martin Schroedter Iowa State University Summary Very-high-energy astronomy began 20 years ago with 1 source. Now ~80 more VHE discoveries have been made
More informationAS750 Observational Astronomy
Lecture 9 0) Poisson! (quantum limitation) 1) Diffraction limit 2) Detection (aperture) limit a)simple case b)more realistic case 3) Atmosphere 2) Aperture limit (More realistic case) Aperture has m pixels
More informationFirst results with AQuEYE, a precusor quantum photometer for the E-ELT
First results with AQuEYE, a precusor quantum photometer for the E-ELT C. Barbieri Department of Astronomy, University of Padova, Italy cesare.barbieri@unipd.it 9/3/2007 C.Barbieri, Erevan, August 2007
More informationCharacterizing Closure-phase Measurements at IOTA
Characterizing Closure-phase Measurements at IOTA Ragland, S. 1,2,3, Traub, W. 1, Berger, J.-P. 4, Millan-Gabet, R. 5, Monnier, J. D. 6, Pedretti, E. 6, Schloerb, F. P. 7, Carleton, N. P. 1, Haguenauer,
More informationHanle Echelle Spectrograph (HESP)
Hanle Echelle Spectrograph (HESP) Bench mounted High resolution echelle spectrograph fed by Optical Fiber Second generation instrument for HCT The project is a technical collaboration between Indian Institute
More informationAdvanced Stereoscopic Array Trigger. Frank Krennrich (Iowa State University)
Advanced Stereoscopic Array Trigger Frank Krennrich (Iowa State University) PAT Pattern Array Trigger Collaboration of Argonne National Laboratory & Iowa State University, Karen Byrum, John Dawson, Gary
More informationGamma-ray Astrophysics with VERITAS: Exploring the violent Universe
Gamma-ray Astrophysics with VERITAS: Exploring the violent Universe K. Ragan McGill University Soup & Science 11-Jan-2008 Soup & Science Jan. '08 1 How do we know about the Universe? Historically, all
More informationAstronomical Experiments for the Chang E-2 Project
Astronomical Experiments for the Chang E-2 Project Maohai Huang 1, Xiaojun Jiang 1, and Yihua Yan 1 1 National Astronomical Observatories, Chinese Academy of Sciences, 20A Datun Road,Chaoyang District,
More informationTelescope Arrays & Related Topics Bruce Holenstein, Rich Mitchell, and Dylan Holenstein
Telescope Arrays & Related Topics Bruce Holenstein, Rich Mitchell, and Dylan Holenstein Gravic Labs Workshop October 8, 2011 www.gravic.com 1 Topics The case for telescope arrays: SNR Gravic s array plans
More informationFuture Radio Interferometers
Future Radio Interferometers Jim Ulvestad National Radio Astronomy Observatory Radio Interferometer Status in 2012 ALMA Covers much of 80 GHz-1 THz band, with collecting area of about 50% of VLA, for a
More informationThe TAIGA experiment - a hybrid detector for very high energy gamma-ray astronomy and cosmic ray physics in the Tunka valley
The TAIGA experiment - a hybrid detector for very high energy gamma-ray astronomy and cosmic ray physics in the Tunka valley N. Budnev, Irkutsk State University For the TAIGA collaboration The TAIGA experiment
More informationVery High-Energy Gamma- Ray Astrophysics
Very High-Energy Gamma- Ray Astrophysics David A. Williams Santa Cruz Institute for Particle Physics UC Santa Cruz Quarknet July 12, 2013 Detecting High Energy Gamma Rays High Sensitivity HESS, MAGIC,
More informationCalibration of photo sensors for the space-based cosmic ray telescope JEM-EUSO
Calibration of photo sensors for the space-based cosmic ray telescope JEM-EUSO Michael Karus for the JEM-EUSO Collaboration Carpathian Summer School of Physics 2014 Sinaia Romania July 2014 Michael Karus
More informationSingle-Photon Techniques for the Detection of Periodic Optical Signals
Single-Photon Techniques for the Detection of Periodic Optical Signals Presentation at Vienna Fast Photometer Mini-Workshop Vienna University, Institut für Astrophysik Nov. 21, 2014 Walter Leeb 1 Publications
More informationAtmospheric phase correction for ALMA with water-vapour radiometers
Atmospheric phase correction for ALMA with water-vapour radiometers B. Nikolic Cavendish Laboratory, University of Cambridge January 29 NA URSI, Boulder, CO B. Nikolic (University of Cambridge) WVR phase
More informationAST 101 Intro to Astronomy: Stars & Galaxies
AST 101 Intro to Astronomy: Stars & Galaxies Telescopes Mauna Kea Observatories, Big Island, HI Imaging with our Eyes pupil allows light to enter the eye lens focuses light to create an image retina detects
More informationIntensity Interferometry & Optical ASTRI!
Intensity Interferometry & Optical Astronomy @ ASTRI! Dainis Dravins, dainis@astro.lu.se Lund Observatory, Box 43, SE-22100 Lund, Sweden; October 2014 1. Introduction 1. Introduction 2. Context: Angular
More informationBasic Theory of Speckle Imaging
1 Basic Theory of Speckle Imaging Elliott Horch, Southern Connecticut State University 1 arcsec BU 151AB 2 Speckle Often Means Binary Stars Stellar Masses. Mass-Luminosity Relation (MLR) Initial Mass Function
More informationA NEW GENERATION OF GAMMA-RAY TELESCOPE
A NEW GENERATION OF GAMMA-RAY TELESCOPE Aleksandar GOSTOJIĆ CSNSM, Orsay, France 11 th Russbach School on Nuclear Astrophysics, March 2014. Introduction: Gamma-ray instruments GROUND BASED: ENERGY HIGHER
More informationHow to calibrate interferometric data
National Aeronautics and Space Administration Jet Propulsion Laboratory California Institute of Technology How to calibrate interferometric data Rachel Akeson 28 July 2006 Outline Calibration basics System
More informationImaging with the SKA: Comparison to other future major instruments
1 Introduction Imaging with the SKA: Comparison to other future major instruments A.P. Lobanov Max-Planck Institut für Radioastronomie, Bonn, Germany The Square Kilometer Array is going to become operational
More informationLecture 9: Speckle Interferometry. Full-Aperture Interferometry. Labeyrie Technique. Knox-Thompson Technique. Bispectrum Technique
Lecture 9: Speckle Interferometry Outline 1 Full-Aperture Interferometry 2 Labeyrie Technique 3 Knox-Thompson Technique 4 Bispectrum Technique 5 Differential Speckle Imaging 6 Phase-Diverse Speckle Imaging
More informationRadio Interferometry and Aperture Synthesis
Radio Interferometry and Aperture Synthesis Phil gave a detailed picture of homodyne interferometry Have to combine the light beams physically for interference Imposes many stringent conditions on the
More informationLecture 14: Non-Optical Telescopes. Resolving Power. When light enters a telescope, it is bent slightly:
Lecture 14: Non-Optical Telescopes When light enters a telescope, it is bent slightly: Wave fronts Light rays D The angle of bending limits the resolution of the telescope This depends on the aperture
More informationarxiv: v1 [astro-ph.im] 3 Sep 2015
arxiv:1509.01044v1 [astro-ph.im] 3 Sep 2015 First results of the two square meters multilayer glass composite mirror design proposed for the Cherenkov Telescope Array developed at INFN C. Schultz a, M.
More informationStatus of the Schwarzchild-Couder Medium-Sized Telescope for the Cherenkov Telescope Array
Status of the Schwarzchild-Couder Medium-Sized Telescope for the Cherenkov Telescope Array W. Benbow 1,a), A. N. Otte 2, for the psct Consortium 3 and the CTA Consortium 4 1 Harvard-Smithsonian Center
More information