Business opportunities in Optical Astronomy: The MAORY ... · Optical-nearIR instruments require a...
Transcript of Business opportunities in Optical Astronomy: The MAORY ... · Optical-nearIR instruments require a...
Business opportunities in Optical Astronomy:
The MAORY instrumentAdriano Fontana
INAFHead of Opt-IR Division
With contributions from: E. Cascone, V. De Caprio (INAF OA Capodimonte), D. Magrin (INAF-PD), F. Pedichini (INAF-OARoma)
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Optical system Electronic & SW
Mechanical structure
Detector
Stabilisation system
What is an astronomical instrument for a modern optical/IR telescope? ..a sort of camera…
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What is an astronomical instrument for a modern optical/IR telescope? … but a very BIG camera!
Extremely Large Telescope (ELT) The largest optical/IR telescope ever built.
Primary mirror is 40m wideOverall structure is the size of the colosseum.
ELT is being built by ESOInstruments built by scientific partners (INAF in Italy)
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Resolution is limited by atmospheric turbulence
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MAORY: THE ADAPTIVE OPTICS MODULE FOR ELT
MAORY+MICADO
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Optical system
Stabilisation system
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LARGESIZESPHERIC/ASPHERICLENSES
LargesphericmeniscuslensD=810mm(120Kg)
Highglass(SILICA)qualityandhomogeneityRefractiveindexΔn<2×10-6Bubbles<0.25mm2/cm3
HighsurfacequalityErrorsonradii<±0.3%(knowledge<0.02%)Surfacequality<60nmRMSMidfrequencies<5nmRMSMicro-roughness<2nmRMS
LargeBinocularCamera@LBT
LargemeniscuslenswithoneconicsurfaceD=930mm,oneconicsurface(K=2.0037)
Highglassqualityandhomogeneity(SILICA,BK7,F2)RefractiveindexΔn<2×10-6Bubbles<0.25mm2/cm3
HighsurfacequalityErrorsonradii<±0.1%(knowledge<0.01%)Surfacequality<50nmRMSMidfrequencies<5nmRMSMicro-roughness<2nmRMS
MAORY@ELT
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MEDIUMSIZEHIGHASPHERICLENSESHighorderasphericlensD=180mmDeviationfrombestfittingsphere>1mmSlopevariationcloseto12milliradians
Highglassqualityandhomogeneity(S-FPL51)RefractiveindexΔn<2×10-6
HighsurfacequalityErrorsonradii<±0.1%(knowledge<0.01%)Surfacequality<50nm(25nmgoal)RMSMidfrequencies<5nmRMSMicro-roughness<1-2nmRMS
ARcoating>99%inthevisible
Highprecisionmetrologyrequired!Dedicatedmeasurementset-up.
ESAmissionPLATO
Protypelens
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LARGEFLAT/SPHERIC/ASPHERICMIRRORSMAORYmirrorslikeclass
FLATMIRRORSDiameters∼ 800-1100mmSurfacequality<15nm(goal10nm)RMSResidualflatness<0.5-1wave
SPHERICMIRRORSDiameters∼ 1300-1350mmRadiusofcurvature∼ 10-20mSurfacequality<10nmRMSMicro-roughness<1-2nm
ASPHERICOFF-AXISMIRRORSDiameters∼ 600-1000mmShapes(concaveandconvex):elliptic,bi-conic,parabolic,hyperbolic,free-formSurfacequality<20-40nmRMSMidfrequencies<4nmRMSMicro-roughness<1-2nmRMS
Coating:silverprotectedVIS-NIRreflectivity98-99%
Thesemirrorswillstandinverticalposition!
Itisrequiredmetrologywithmirrorsinstalledonthemountingtocompensateforresidualerrorsduetogravity.
Metrologyofsurfaceshastobeknowwithrespecttoexternalreferences!
Nowadays,alignmentmethodsandinstrumentstabilitymonitoringrequiretheknowledgeoftheopticalsurfacespositioninginthespacewithrespecttofiducialmarkersdownto0.1mmand10-20arcsec.
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CUSTOMCOATINGSSOXSMainDichroic
• Flatsteprequiredtoallowarmscrosscalibration! custommultilayercoatingtobedesigned
• RequiredT>95%• Step‘flatness’50%,7%Ptv0
25
50
75
100
800 825 850 875 900
R(%)AOI15o T(%)AOI15o
• SimulationfromThinFilmsPhysics
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ALUMINIUMMIRRORSSOXSNIRspectrograph
• Benchsamematerialtoreducethermalissues
• Partofmountingfromthesameblock
• Roughnessproblems:hardtogounder3.5-5.0nm
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MAORY INSTRUMENT: PRESENT BASELINE MECHANICAL DESIGN
In order to fulfil all the requirements, including the best shape for a good accessibility to all opto-mechanical component, we
have chosen to design a full-custom optical bench (welded and/or bolted box structure) made in structural steel.
Cutted bottom view
Top view – overall dimensions
➢ For the optical Bench and legs we have a weight
requirement of 12tons (+ contingency),
and
➢ stability tolerances and positioning of ±0.1mm for the
optical elements.
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MAORY INSTRUMENT: PRESENT BASELINE MECHANICAL DESIGN
An Enclosure, mounted on the bench, will be
make in order to protect the internal optical
elements from the light and achieving, as
much as possible, a uniform temperature
distribution inside it.
The enclosure is made of a number of modular aluminum panels and
standard rectangular hollow sections (bolted or welded each other)
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Electronic & SW
The Instrument Control Hardware includes all the electronics infrastructure required to control the Instrument The MAORY electronic architecture design follows this guidelines: • The control HW is based on a distributed system composed by
industrial standard Commercial-Off-The-Shelf (COTS) components. • The communication between the components is based on industrial,
standard, real-time buses. Few differences in astronomical application respect industrial ones e.g. light pollution, thermal control, etc.
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ElectroniccomponentsofICH
ICH is based on Beckhoff PLC and EtherCat fieldbus. Main modules are:
•Digital I/O, for devices with discrete control signal and status output •Analog I/O, for devices with continuous control signal and status output •Communication modules, for devices with high level interface (for example serial interface) •Motion control modules, for the motorized functions •Safety
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EK1100
ES74322CHDCcontroller
ES5101DifferentialEncoder
ES1088DigitalInput
ES74322CHDCcontroller
ES5101DifferentialEncoder
ES1088DigitalInput
ES74322CHDCcontroller
ES5101DifferentialEncoder
ES1088DigitalInput
Example of distributed system
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Shopping ListItems Description
ElectronicCabinet SchroffVaristarLHX3withheatexchangerincluded
ElectronicComponentsand
CabinetManagement BeckhoffPLCwithI/Oterminal
PowerSupplies KnielLowEmissionPowerSupplies
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OPTICALDETECTORS
VISIBLE(0.3-0.9µm)
NIR-MWIR(0.9-5.0µm)
LWIR(8-14µm)
CCD
EM-CCD
CMOS
CMOS
HybridCMOS
APDarray
HybridCMOS
MicroBolometer
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VISIBLE(0.3-0.9µm)
SiPIN
CCD
EM-CCD
CMOS
DopedSiliconactivemediasubstrateCooledat-50-100Celsiusdarksignal<1e-/h
EM-CMOSUltralownoise
Work-horseofastronomy,fewelectronnoise,formatupto6kx6kpixel(Scienceimagers)
Veryfastandultralownoise<0.1e-at40Mpix/sformatupto1kx1kpixel(WaveFrontSensing)
Smallpixel,fast,largeformat,lownoise~1e-at200Mpix/s,lowcost,radiationtolerant(spacemission)
FUTURETRENDS
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NIR-MWIR(0.9-5.0µm)
CMOS
HybridCMOS
APDarray
Smallformatupto1kx1kbasedonGe(ondevelopment)
HAWAII2serieupto4kx4kpixelat16Mpix/s3-4e-noise(SciencefocalplaneforIRastronomy)
Smallpixel,fast,mediumformat(300x200),ultralownoise<0.1e-,SELEXtechnology(EU)(NIRWFS)
Ge,HgCdTeorInSbactivemediasubstrateHybridizedonaCMOSCooledbelow77KelvinTypicaldarksignal<10e-/h
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INAFDETECTORPROVIDERS:• TELEDYNE:NIRandSWIRCMOSinfraredimagingandspectroscopy,spaceapplication
• e2V:CCD,EM-CCD,sCMOSimagingandWavefrontsensing• SONY:sCMOS,CCD• ANDOR:sCMOS• HAMAMTSU:CCD,sCMOS• RAYTHEON:LWIRCMOSspaceapplication• SELEX:APDarraysWavefrontsensing
ItisnowpossibletodevelopcustomCMOSdetectors@homethankstotheEuroPracticeconsortiumatareasonablecost.
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THEMOSTUSEDDETECTORs
e2VCCD-220(Wavefrontsensor200x200pixat2kfps)
e2VCCD-4290(4kx2kpixbuttable)
TeledyneHAWAII2RG(2kx2kpixNIRbuttable)
SELEXSaphira320x200NIRWavefrontsensor
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Summary
Optical-nearIR instruments require a combination of:- highly customised optical elements (lenses & mirrors in the range 200-1000mm, potentially
aspheric);- stiff/light mechanical structures - COTS electronic for hardware control- fast/extremely low noise detectors (optical/nearIR)
Hardware cost is in the range 2-20M€/instrument
In addition to MAORY, several other instruments are under construction today - tenders will emerge in the next year(s)
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