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“Classical” Interferometric Arrays
Andreas QuirrenbachLandessternwarte Heidelberg
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Tucson 11/14/2006 Andreas Quirrenbach 2
The VLT Interferometer
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Tucson 11/14/2006 Andreas Quirrenbach 3
Optical / Infrared Interferometry Today
Access to milliarcsecond-scale phenomenaPerform interferometric spectroscopyLots of results in stellar astrophysicsSensitivity sufficient for a few bright AGN
Small number of telescopes ⇒ parametric model fits to visibilities, no imagesSensitivity insufficient for larger samplesResolution insufficient for details / more distant objects
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Tucson 11/14/2006 Andreas Quirrenbach 4
Desirable Capabilities of a Next-Generation Interferometer
Address wide range of scientific topics ⇒flexibilityObserve faint objects ⇒ high sensitivity and dynamic rangeComplex objects / limited prior knowledge ⇒imaging capabilityAccess “famous” archetypical and rare objects ⇒ good sky coverageObserve time-variable phenomena ⇒ good snap-shot capability
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Tucson 11/14/2006 Andreas Quirrenbach 5
What’s Next?
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Tucson 11/14/2006 Andreas Quirrenbach 6
What’s Next?
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Tucson 11/14/2006 Andreas Quirrenbach 7
Think BIG!
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Tucson 11/14/2006 Andreas Quirrenbach 8
The ELSA Concept – a Strawman Interferometric Facility
Number of telescopes: 27Telescope diameter: 8 mMaximum baseline: 10 kmWavelength range: 500 nm … 20 µm (?)Beam transport: Single-mode fiber bundlesBeam combination: MichelsonSky coverage at 600 nm: & 10%Cost: ≈ 400 M€
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Tucson 11/14/2006 Andreas Quirrenbach 9
ELSA AstrometryAstrometric error due to Kolmogorovatmosphere scales with B-2/3
ELSA could reach 1 µas over 15″ arc• Sufficient to detect terrestrial planets around nearby
starsEven better precision expected due to outer scale of atmospheric turbulencePrecision requirements less stringent than for Keck / VLTI
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Tucson 11/14/2006 Andreas Quirrenbach 10
ELSA Resolution: 10 µas at 500 nm, 40 µas at 2 µm
15,000 km at 10 pc• 8 pixels across Jupiter-size object• 80 pixels across Solar-type star
0.1 AU at 10 kpc• GR effects on stars very close to the Galactic Center
200 AU (1 light-day) at 20 Mpc• Images of AGN Broad-line regions• Expansion and light echoes of supernovae
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Tucson 11/14/2006 Andreas Quirrenbach 11
Linear Resolution of ELSA in the Local Universe
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Tucson 11/14/2006 Andreas Quirrenbach 12
Linear Resolution of ELSA atλ = 500 nm
Redshift z0 2 4 6
Line
ar R
esol
utio
n [1
017
cm]
0.0
0.5
1.0
1.5
2.0
2.5
3.0
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Tucson 11/14/2006 Andreas Quirrenbach 13
ELSA Science Case (Galactic)Weather on brown dwarfsStellar surface images (spots, flares, convection, differential rotation, oscillations, …)Images of interacting and accreting binariesGaps and inner edge of YSO disks, jet formationCores of globular clustersAGB stars: dust formation, windsMovies of novaeGravitational micro-lensesGeneral relativity near Galactic Center
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Tucson 11/14/2006 Andreas Quirrenbach 14
ELSA Science Case (Extragalactic)
Stellar populations in external galaxies• Crowding important even on ELT scale
Expansion and light echoes of supernovaeImaging of Active Galactic Nuclei• Dynamics of broad line regions• Jet formation• Black hole masses from stellar orbits
Resolving gamma-ray afterglows• Asymmetries, relativistic beaming
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Tucson 11/14/2006 Andreas Quirrenbach 15
AGN Science with ELSABlack-hole mass from stellar and gas dynamicsReverberation mapping (watch line response to continuum variations in movies) ⇒ physics of BLR, geometric distancesOptical emission from milliarcsecond jets ⇒jet collimation, shocks, particle acceleration, …Details of clumpy (?) obscuring torus ⇒ dust properties, unification schemes“Mirror(s)” in HBLR objects ⇒ AGN physics, unification schemes
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Tucson 11/14/2006 Andreas Quirrenbach 16
ELSA Critical TechnologiesTelescopesArray co-phasingBeam transportBeam combinationDelay compensation
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Tucson 11/14/2006 Andreas Quirrenbach 17
ELSA Co-Phasing ConceptPhase individual telescopes with multiple (?) LGS adaptive opticsOff-axis fringe tracking on “bright” starLarge aperture ⇒ good fringe tracking sensitivity ⇒near-complete sky coverageRequirement: fringe tracking at K≈19• One of the drivers for large array elements
Fringe-tracking chain of neighboring telescopes for bright (resolved) starsFringe tracking between all telescopes for faint (unresolved) stars
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Tucson 11/14/2006 Andreas Quirrenbach 18
Limiting Sensitivity for Fringe Tracking in the R Band
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Tucson 11/14/2006 Andreas Quirrenbach 19
Sky Coverage at NGP for Different Maximum Off-Axis Angles
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Tucson 11/14/2006 Andreas Quirrenbach 20
Array Layout Optimized for Baseline Bootstrapping
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Tucson 11/14/2006 Andreas Quirrenbach 21
A Y-Shaped Configuration(15 Telescopes)
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Tucson 11/14/2006 Andreas Quirrenbach 22
ELSA TelescopesNeed to produce twenty-seven 8m telescopes for ≈ 200 M€Moveable for array reconfiguration if possibleSmall field-of-viewNo scientific instruments (acquisition and fiber-feeds only)Take advantage of ELT development• Mass production of mirror segments• Standardized structural elements
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Tucson 11/14/2006 Andreas Quirrenbach 23
Projected Cost of TelescopesTypical scaling of telescope cost with diameter is € ∝ D2.7
Scaling applies at any given time (for similar maturity of technology), not to future projectionExample: scaling holds for Keck (10m) versus CHARA (1m) telescopesApply scaling to ELT (e.g., European E-ELT concept): 42m for 700 M€ ⇒ 8m for 8 M€Proof-of-concept for ELT?
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Tucson 11/14/2006 Andreas Quirrenbach 24
Moving Big Telescopes around …
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Tucson 11/14/2006 Andreas Quirrenbach 25
… is Perfectly Doable!
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Tucson 11/14/2006 Andreas Quirrenbach 26
ELSA Beam TransportFibers are much cheaper than beam tunnels• Diffraction + field
Need advances in fiber technology• No significant light loss over 10 km• Low dispersion, polarization preserving• Fibers for infrared wavelength range
Need metrology to monitor fiber lengthsFiber bundles can handle field-of-view larger than Airy disk
LmLkD θλ +×=⇒ opt
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Tucson 11/14/2006 Andreas Quirrenbach 27
ELSA Delay CompensationSwitch between fiber segments for bulk delay compensation• Add appropriate fibers from set of (1m, 2m, 4m, …)• Dispersion is a potential show-stopper• Need low-loss fiber-fiber couplers
Fiber stretching for fine adjustment (sidereal rate plus atmosphere)• Fall-back is short classical delay line
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Tucson 11/14/2006 Andreas Quirrenbach 28
ELSA Beam CombinationVery diluted (B / D ≈ 1,000) for longest baselines ⇒ pupil plane combination preferred• Field-of-view radius is R = λ / ∆λ resolution
elementsLarger field-of-view desired for more compact configurations• Homothetic mapping (exact or densified replica of
entrance pupil) to be explored
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Tucson 11/14/2006 Andreas Quirrenbach 29
ELSA SiteNeed flat ≈ 10 km plateauGood seeing (r0, τ0, θ0) important criterionSouthern hemisphere preferredRequirements different from ELT criteriaALMA site probably (marginally) ok
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Tucson 11/14/2006 Andreas Quirrenbach 30
Exceptional Astronomical Seeing at Dome C in Antarctica (?)
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Tucson 11/14/2006 Andreas Quirrenbach 31
Potential Advantages of Dome CLarger r0 ⇒ simpler adaptive opticsLonger τ0 ⇒ better sensitivityLarger θ0 ⇒ better sky coverageLower temperature ⇒ lower IR backgroundOr same performance with smaller telescopes• 2m at Dome C ⇔ 8m at traditional sites?
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Tucson 11/14/2006 Andreas Quirrenbach 32
VLTI, ALMA, ELTs, and ELSA
ELSA has 50 times better resolution than any other facility ⇒ completely new scienceELSA draws on VLTI / ALMA / ELT heritage• VLTI: Interferometric techniques, beam
combination, …• ALMA: Moveable telescopes, site (?)• ELTs: Cheap telescopes through mass production of
optics and standardized structural elementsELSA could be feasible and affordable in 2015
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Tucson 11/14/2006 Andreas Quirrenbach 33
Conclusions (1): What we Know Already
There is a large parameter space of first-class science beyond the ELT resolution limitBaseline length of ≈10 km requiredLarge telescopes or superb site (Antarctica?) needed to get sensitivity and good sky coverageA powerful facility could become feasible and affordable in a decade
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Tucson 11/14/2006 Andreas Quirrenbach 34
Conclusions (2): What we Don’t Know Yet
Can fibers be used for beam transport and delay compensation?Which site offers the best trade-off between quality and cost?Is the science case powerful enough to make it happen?
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Tucson 11/14/2006 Andreas Quirrenbach 35
Key Technology Needs for Roadmap
Beam transport with optical fibers• Dispersion is a potential show stopper• Cost driver ⇒ top priority on my list
Beam combination concepts and integrated optics beam combinersTelescopes • Main issue is cost ⇒ link to ELT projects
Site• Evaluate Antarctica• Look for good “traditional” sites