Business opportunities in Optical Astronomy: The MAORY ... · Optical-nearIR instruments require a combination of:-highly customised optical elements (lenses & mirrors in the range

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)

1 20190607_Napoli_Industria - 12 June 2019

Optical system Electronic & SW

Mechanical structure

Detector

Stabilisation system

What is an astronomical instrument for a modern optical/IR telescope? ..a sort of camera…


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)


Resolution is limited by atmospheric turbulence





MAORY: THE ADAPTIVE OPTICS MODULE FOR ELT

MAORY+MICADO


Optical system

Stabilisation system


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


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


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.


CUSTOMCOATINGSSOXSMainDichroic

• Flatsteprequiredtoallowarmscrosscalibration! custommultilayercoatingtobedesigned

• RequiredT>95%• Step‘flatness’50%,7%Ptv0

25

50

75

100

800 825 850 875 900

R(%)AOI15o T(%)AOI15o

• SimulationfromThinFilmsPhysics


ALUMINIUMMIRRORSSOXSNIRspectrograph

• Benchsamematerialtoreducethermalissues

• Partofmountingfromthesameblock

• Roughnessproblems:hardtogounder3.5-5.0nm


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.


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)


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.


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


EK1100

ES74322CHDCcontroller

ES5101DifferentialEncoder

ES1088DigitalInput



ES1088DigitalInput



ES1088DigitalInput

Example of distributed system


Shopping ListItems Description

ElectronicCabinet SchroffVaristarLHX3withheatexchangerincluded

ElectronicComponentsand

CabinetManagement BeckhoffPLCwithI/Oterminal

PowerSupplies KnielLowEmissionPowerSupplies


OPTICALDETECTORS

VISIBLE(0.3-0.9µm)

NIR-MWIR(0.9-5.0µm)

LWIR(8-14µm)

CCD

EM-CCD

CMOS

CMOS

HybridCMOS

APDarray

HybridCMOS

MicroBolometer


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


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


INAFDETECTORPROVIDERS:• TELEDYNE:NIRandSWIRCMOSinfraredimagingandspectroscopy,spaceapplication

• e2V:CCD,EM-CCD,sCMOSimagingandWavefrontsensing• SONY:sCMOS,CCD• ANDOR:sCMOS• HAMAMTSU:CCD,sCMOS• RAYTHEON:LWIRCMOSspaceapplication• SELEX:APDarraysWavefrontsensing

ItisnowpossibletodevelopcustomCMOSdetectors@homethankstotheEuroPracticeconsortiumatareasonablecost.


THEMOSTUSEDDETECTORs

e2VCCD-220(Wavefrontsensor200x200pixat2kfps)

e2VCCD-4290(4kx2kpixbuttable)

TeledyneHAWAII2RG(2kx2kpixNIRbuttable)

SELEXSaphira320x200NIRWavefrontsensor


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)


Business opportunities in Optical Astronomy: The MAORY ... · Optical-nearIR instruments require a combination of:-highly customised optical elements (lenses & mirrors in the range

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