OWL Instrument Concept Design Quantum Optics @ OWL ! INSTRUMENT CONCEPT IDEAS Dainis Dravins Lund Observatory, Sweden.

OWL Instrument Concept Design

OWL Instrument Concept Design

Quantum Optics @ OWL !

INSTRUMENT CONCEPT IDEAS

Dainis DravinsLund Observatory, Sweden

OWLS NEED QUANTUM EYES…

Quantum Optics @ OWLQuantum Optics @ OWL

OWL instrument design study 2005

ESO Garching; Lund Observatory; University of Padua

HIGHEST TIME RESOLUTION, REACHING QUANTUM OPTICS

• Other instruments cover seconds and milliseconds

• QUANTEYE will cover milli-, micro-, and nanoseconds, down to the quantum limit !

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)

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 ?

MAIN PREVIOUS LIMITATIONS

• CCD-like detectors: Fastest practical frame rates: 1 - 10 ms

• Photon-counting detectors: Limited photon-count rates: ≳ 100 kHz

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

INSTRUMENT DESIGN ISSUES

• Challenges are primarily in detectors & data handling

• Imaging optics may be “ordinary”

(more or less similar to those of imaging cameras)

• 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)

INSTRUMENT DESIGN ISSUES

• Possible detector layout (only APD arrays appear to match requirements)

• Detector filling factor ≪ 100% (probably requires microlens imaging)

5 x 5 array of 20 μm diameter APD detectors (SensL, Cork)

32x32 Single Photon Silicon Avalanche Diode Array Quantum Architecture Group, L'Ecole Polytechnique Fédérale de Lausanne

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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)

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

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 ?)

INSTRUMENT DESIGN ISSUES

• Incorporate measurements of photon orbital angular momentum ?

(or does this not specifically require ELT’s ??)

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?)

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

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

Photon correlation spectroscopyPhoton correlation spectroscopy

E.R.Pike, in R.A.Smith, ed. Very High Resolution Spectroscopy, p.51 (1976)

LENGTH,TIME &FREQUENCYFORTWO-MODESPECTRUM

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

Photon correlation spectroscopyPhoton correlation spectroscopy

E.R.Pike, in R.A.Smith, ed. Very High Resolution Spectroscopy, p.51 (1976)

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

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

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

Information content of lightInformation content of light

D.Dravins, ESO Messenger 78, 9 (1994)

Intensity interferometryIntensity interferometry

Narrabri stellar intensity interferomer circa 1970 (R.Hanbury Brown, R.Q.Twiss et al., University of Sydney)

Intensity interferometryIntensity interferometry

R.Hanbury Brown, J.Davis, L.R.Allen, MNRAS 137, 375 (1967)

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)

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)

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

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

Information content of lightInformation content of light

D.Dravins, ESO Messenger 78, 9 (1994)

R. Loudon The

Quantum Theory of

Light (2000)

QUANTUM OPTICS

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

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

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

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