owl instrument concept design quantum optics @ owl ! instrument concept ideas dainis dravins lund...
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OWL Instrument Concept Design
OWL Instrument Concept Design
Quantum Optics @ OWL !
INSTRUMENT CONCEPT IDEAS
Dainis DravinsLund Observatory, Sweden
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OWLS NEED QUANTUM EYES…
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Quantum Optics @ OWLQuantum Optics @ OWL
OWL instrument design study 2005
ESO Garching; Lund Observatory; University of Padua
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HIGHEST TIME RESOLUTION, REACHING QUANTUM OPTICS
• Other instruments cover seconds and milliseconds
• QUANTEYE will cover milli-, micro-, and nanoseconds, down to the quantum limit !
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SECONDS & MILLISECONDS
• Lunar & planetary-ring occultations• Rotation of cometary nuclei• Pulsations from X-ray pulsars• Cataclysmic variable stars• Pulsating white dwarfs• Optical variability around black holes• Flickering of high-luminosity stars• X-ray binaries• Optical pulsars• Gamma-ray burst afterglows
(partially listed from pre-launch program for HSP on HST)
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MILLI-, MICRO- & NANOSECONDS
• Millisecond pulsars ?• Variability near black holes ?• Surface convection on white dwarfs ?• Non-radial oscillations in neutron stars ?• Surface structures on neutron-stars ?• Photon bubbles in accretion flows ?• Free-electron lasers around magnetars ? • Astrophysical laser-line emission ?• Spectral resolutions reaching R = 100
million ?• Quantum statistics of photon arrival
times ?
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MAIN PREVIOUS LIMITATIONS
• CCD-like detectors: Fastest practical frame rates: 1 - 10 ms
• Photon-counting detectors: Limited photon-count rates: ≳ 100 kHz
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DESIRED INSTRUMENT PROPERTIES
• Temporal resolution limited by astrophysics, not detector: ≈ 1 ns – 100 ps
• Photon-counting detectors: Sustained photon-count rates ≈ 100 MHz
• Quantum efficiency ≲ 100% from near-UV to near-IR
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INSTRUMENT DESIGN ISSUES
• Challenges are primarily in detectors & data handling
• Imaging optics may be “ordinary”
(more or less similar to those of imaging cameras)
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• 4-Dimensional detector system 2D spatial + 1D spectral & polarization + 1D temporal
• 1024 x 1024 imaging elements (possibly in sections to include calibration
objects)
• Each imaging element with spectral & polarization channels
• Spectral resolving power λ/Δλ ≈ 100,000,000
(digital intensity correlation spectroscopy)
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INSTRUMENT DESIGN ISSUES
• Possible detector layout (only APD arrays appear to match requirements)
• Detector filling factor ≪ 100% (probably requires microlens imaging)
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5 x 5 array of 20 μm diameter APD detectors (SensL, Cork)
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32x32 Single Photon Silicon Avalanche Diode Array Quantum Architecture Group, L'Ecole Polytechnique Fédérale de Lausanne
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SUSS MicroOpticsNeuchâtel
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Photonics and Optoelectronics, Edith Cowan University, Perth, WA
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•
•
“ULTIMATE” DATA RATES
* 1024 x 1024 imaging elements @ 100 spectral & polarization channels
* Each channel photon-counting @ 10 MHz, 1 ns time resolution
* Data @ 1015 photon time-tags per second = 1 PB/s (Petabyte, 1015 B) = some EB/h (Exabyte = 1018 B)
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•
•
“REALISTIC” DATA RATES
* 1024 x 1024 imaging elements one wavelength channel at a time
* Each channel photon-counting @ 10 MHz with 1 ns time resolution
* Data @ 1013 photon time-tags per second = 10 TB/s (Terabyte, 1012 B) ≈ 1 PB/min (Petabyte, 1015 B) ≈ 1 EB/few nights (Exabyte = 1018 B)
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HANDLING HIGH DATA RATES
• Digital correlator integrated onto each detector channel (or pair of channels), outputting 1024 points on correlation functions
• Sampling correlation function once per second ”compresses” data a factor 104
• Real-time system identifies the 100 most interesting spatial channels; reduces data another factor 104
• Original data rate 10 TB/s thus reduced to 100 kB/s
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INSTRUMENT DESIGN ISSUES
• How to separate spectral & polarization channels ?
(dichroic and/or variable filters ? grisms ?)
• How to realize spatial sampling ? (integral-field fiber-optics bundles ?
different detector segments ?)
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INSTRUMENT DESIGN ISSUES
• Incorporate measurements of photon orbital angular momentum ?
(or does this not specifically require ELT’s ??)
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INSTRUMENT DESIGN ISSUES
• Telescope mechanical stability ? (small and well-defined vibrations, etc.)
• Temporal structure of stray light ? (scattered light may arrive with systematic
timelags)
• Atmospheric intensity scintillation? (is OWL larger than outer scale of turbulence?)
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SPECTRAL RESOLUTION
• Resolving power λ/Δλ ≳ 100,000,000
• First “extreme-resolution” optical spectroscopy in astrophysics
• Required to resolve laser lines with expected intrinsic widths ≈ 10 MHz
• Realized through photon-counting digital intensity-correlation spectroscopy
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Photon correlation spectroscopyPhoton correlation spectroscopy
o To resolve narrow optical laser emission (Δν 10 MHz) requires spectral resolution λ/Δλ 100,000,000
o Achievable by photon-correlation (“self-beating”) spectroscopy ! Resolved at delay time Δt 100 ns
o Method assumes Gaussian (thermal) photon statistics
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Photon correlation spectroscopyPhoton correlation spectroscopy
E.R.Pike, in R.A.Smith, ed. Very High Resolution Spectroscopy, p.51 (1976)
LENGTH,TIME &FREQUENCYFORTWO-MODESPECTRUM
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Photon correlation spectroscopyPhoton correlation spectroscopy
E.R.Pike, in R.A.Smith, ed. Very High Resolution Spectroscopy, p.51 (1976)
PHOTON CORRELATION FOR A TWO-MODE SPECTRUM
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Photon correlation spectroscopyPhoton correlation spectroscopy
E.R.Pike, in R.A.Smith, ed. Very High Resolution Spectroscopy, p.51 (1976)
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Photon correlation spectroscopyPhoton correlation spectroscopy
E.R.Pike, in R.A.Smith, ed. Very High Resolution Spectroscopy, p.51 (1976)
LENGTH & TIME FOR SPECTROMETERS OF DIFFERENT RESOLVING POWER
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Photon correlation spectroscopyPhoton correlation spectroscopy
o Analogous to spatial informationfrom intensity interferometry,photon correlation spectroscopydoes not reconstruct the shape of
the source spectrum, but “only” gives linewidth information
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Photon correlation spectroscopyPhoton correlation spectroscopy
o Advantage #1:Advantage #1: Photon correlations are insensitive to wavelength shifts due to local velocities in the laser source
o Advantage #2:Advantage #2: Narrow emission components have high brightness temperatures, giving higher S/N ratios in intensity interferometry
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Information content of lightInformation content of light
D.Dravins, ESO Messenger 78, 9 (1994)
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Intensity interferometryIntensity interferometry
Narrabri stellar intensity interferomer circa 1970 (R.Hanbury Brown, R.Q.Twiss et al., University of Sydney)
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Intensity interferometryIntensity interferometry
R.Hanbury Brown, J.Davis, L.R.Allen, MNRAS 137, 375 (1967)
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Intensity interferometryIntensity interferometry
LABORATORY EXPERIMENT
• Artificial star (pinhole illuminated by white-light arc lamp)
• Two “telescopes” observe “star” with APD detectors, @ ≳ 5 MHz photon counts
• Digital cross correlation @ 1.6 ns resolution
(monitored as baseline between telescopes is changed)Ricky Nilsson & Helena Uthas, Lund Observatory (2005)
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S.Johansson & V.S.LetokhovPossibility of Measuring the Width of Narrow Fe II Astrophysical Laser Lines in the Vicinity ofEta Carinae by means of Brown-Twiss-Townes Heterodyne Correlation Interferometryastro-ph/0501246, New Astron. 10, 361 (2005)
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S.Johansson & V.S.LetokhovPossibility of Measuring the Width of Narrow Fe II Astrophysical Laser Lines in the Vicinity of Eta Carinae by means of Brown-Twiss-Townes Heterodyne Correlation Interferometryastro-ph/0501246, New Astron. 10, 361 (2005)
Expected dependence of the correlation signal as function of(a) heterodyne frequency detuning and (b) spacing of telescopes d
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Photon statistics of laser emissionPhoton statistics of laser emission
• (a) IfIf the light is non-Gaussian, photon statistics will be closer to stable wave(such as in laboratory lasers)
• (b) IfIf the light has been randomized andis close to Gaussian (thermal), photon correlation spectroscopy will reveal the narrowness of the laser light emission
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Information content of lightInformation content of light
D.Dravins, ESO Messenger 78, 9 (1994)
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R. Loudon The
Quantum Theory of
Light (2000)
QUANTUM OPTICS
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ROLE OF LARGE TELESCOPES
• VLT’s & ELT’s permit enormously more sensitive searches for high-speed phenomena in astrophysics
• Statistical functions of arriving photon stream increase with at least the square of the intensity
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Advantages of very large telescopes
Advantages of very large telescopes
Telescope diameter
Intensity <I> Second-order correlation <I2>
Fourth-order photon statistics <I4>
3.6 m 1 1 1
8.2 m 5 27 720
4 x 8.2 m 21 430 185,000
50 m 193 37,000 1,385,000,000
100 m 770 595,000 355,000,000,000
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Quantum Optics @ OWL !Quantum Optics @ OWL !
• [Almost] all our knowledge of the Universe arrives through photons
• Both individual photons and photon streams are more complex than has been generally appreciated
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Quantum Optics @ OWL !Quantum Optics @ OWL !
• Quantum optics may open a fundamentally new information channel to the Universe !
• ELT’s will bring non-linear optics into astronomy !
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The End
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