Bertrand Mennesson · 2018-05-08 · Image credit: Mark Garlick, space-art.co.uk 1 ... o Slew to...
Transcript of Bertrand Mennesson · 2018-05-08 · Image credit: Mark Garlick, space-art.co.uk 1 ... o Slew to...
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PerformanceandChallengesforHabEx(andLUVOIR)ExploringOtherPlanetarySystemsandEnablingaBroadRangeof
GeneralAstrophysics&SolarSystemScience
BertrandMennessonJetPropulsionLaboratory,CaliforniaInsFtuteofTechnology
andtheHabExStudyTeam©2018CaliforniaIns1tuteofTechnology,governmentsponsorshipacknowledged Imagecredit:MarkGarlick,space-art.co.uk
1KISSMeeFng,PasadenaApril112018
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HabExTopLevelScienceGoals
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HabExataglance(ArchitectureA)
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• Off-axisf/2.5monolithicprimary• CoronagraphInstrument(0.45-1.8µm)
o R=140inthevisible,R=40intheNIRo IWA=62masat0.5µm
• StarshadeInstrument(0.2–1.8µm)o R=140inthevisible,R=40inNIR,R=7inUVo IWA=60masover0.3to1.0µmo Slewtodifferentdistancestocover<0.3or>1µm
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HabExHybridDesignandObservingStrategy
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HabExcombinesthestrengthsoftwohighlycomplementarystarlightsuppressionsystems:
InternalCORONAGRAPH ExternalSTARSHADE
• Verynimble• Searchesforplanetsaroundmanystars• Takesimagesatmul1plevisitstomeasureorbits
+
• Very“photon”efficient• Accessescloser-inplanetsatagivenλ• Takesbroadspectraofallplanetsfoundin~50-100mostinteres1ngsystems
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HabExExoplanetSurveyStrategy
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BroadSurvey(3.5yeartotal)• Roughly110stars• Roughly6observa1onsofeach• 50%completenessforexo-Earths• Spectraofmostinteres1ngsystems
(andallthosewithEECs)o 0.3-1.0μmatoncewithstarshadeo R=7(grism)0.3-0.45μmo R=140(IFS)0.45-1.0μm
DeepSurvey(0.25year)• Roughly10high-priorityclose-by
(<6pc)GKdwarfs• Deepbroadbandimagetothe
systema1cfloor• Spectra
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DetecFngandCharacterizingPotenFallyHabitableWorlds
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• HabExwillsurvey~110nearbysunlikestarswiththecoronagraphtosearchforpoten1allyhabitableworldsanddeterminetheirorbits
Credit:GarrethRuane(Caltech) Credit:SergiHildebrandt(JPL)
• Mostinteres1ngsystemswillbestudiedfurtherwiththestarshade(broad-band12”x12”imageandspectraofindividualplanets)
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D = 4 m
Exo-Earth near UV to near IR Spectra
Atmosphere?
Life?
Habitability?
Credit:TylerRobinson
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Family Portraits of our Neighboring Planetary Systems
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• Spectraover0.3-1.0μmatoncewithstarshadeforplanetswithin1.5”• R=7(grism)0.3-0.45μm• R=140(IFS)0.45-1.0μm
• NearUVand/ornearUVspectraforselectsystems
Credit:TylerRobinson(NAU)
&SergiHildebrandt(JPL)
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Yields of Characterized Planets (Chris Stark, STScI)
ExpectedHabExYields*Detectandcharacterizetheorbitsandatmospheresof:• Rockyplanets:
• 92rockyplanets(0.5-1.75RE)• Includes12EarthAnalogs(0.5-1.4RE)
• SubNeptunes:• 116sub-Neptunes(1.75-3.5RE)
• GasGiants• 62gasgiants(3.5-14.3RE)
*AssumesSAG13NominalOccurrenceRates.
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Yields of Characterized Planets
Credit:TiffanyMeshkat(IPAC)
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Thisalllooksgreatbut…
• WhatassumpFonswentintothis?• Aretheyreasonable?
• ScienceyieldsensiFvitytouncertaintyonastroparametersandinstrumentalperformanceassumpFons?
!HabEx(andLUVOIR)Challenges
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Astronomical Parameter AssumpJons
Parameter Value Descrip1on η⊕ 0.24 FracFonofSun-likestarswithanexo-Earthcandidate Rp [0.6,1.4]R⊕ Planetradiusa α [0.95,1.67]AU Semi-majoraxisb e 0 Eccentricity(circularorbits)
Cosi [–1,1] Cosineofinclina1on(uniformdistribu1on) ω [0,2π] Argumentofpericenter(uniformdistribu1on) M [0,2π] Meananomaly(uniformdistribu1on) Φ Lamber1an Phasefunc1on AG 0.2 Geometricalbedoofplanetfrom0.55–1µm zc 23magarcsec-2 AverageVbandsurfacebrightnessofzodiacallightforcoronagraph
observa1onsc zs 22magarcsec-2 AverageVbandsurfacebrightnessofzodiacallightforstarshadeobserva1onsc x 22magarcsec-2 Vbandsurfacebrightnessof1zodiofexozodiacaldustd n 3 Numberofzodisforallstars
YieldesFmatesassumezeropriorknowledgeofplanetsaroundtargetsstars
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SensiJvity to Astronomical Parameters: ηEarth and exozodi level (C. Stark)
0 10 20 30 40Median Exozodi Brightness (zodis)
0.1
0.2
0.3
0.4
0.5
ηEa
rth
0 10 20 30Yield of exoEarth Candidates
0 10 20 30Yield of exoEarth Candidates
2.0 2.5 3.0 3.5 4.0 4.5 5.0D (m)
0.1
1.0
10.0
Prob
abili
ty o
f zer
o ex
oEar
th c
andi
date
s (%
)
eta=0.08
eta=0.24
eta=0.70
CurrentLBTIData
Moreworkneededin2018tofullyexplorethesensiRvityofHabExscienceyieldtomaininstrumentalandastroparameters(similartoStarketal.2014&2015),andtoprecursorobservaRonsoftargetsystems.
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Instrument Performance AssumpJons: Coronagraph
Parameter Value Descrip1on
ζ <=10-10 Rawcontrasta
Δmagfloor 26 SystemaFcnoisefloor(faintestdetectablepointsource)
Τcore 0.48 Coronagraphiccorethroughputa
Τ 0.18 End-to-endfacilitythroughput,excludingcorethroughput
IWA 2.4λ/D Innerworkingangleb
OWA 32λ/D Outerworkingangle
Δλ 20% Bandwidth
aMaximumvaluebetweentheIWAandOWA.AssumesdualPZNoperaFonbSepara1onatwhichcorethroughputreacheshalfthemaximumvalue.
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Instrumental Parameter AssumpJons: Near UV - Visible Detector
Parameter Value Descrip1on
ξ 3×10-5countspix-1sec-1 Darkcurrent
RN 0countspix-1read-1 Readnoise(N/A)
τread 1,000s ReadFme
CIC 1.3×10-3countspix-1clock-1 Clockinducedcharge
Npix 2048 x 2048 (SS IFS) Array size
FornearIRspectralcharacteriza1on,requirementsare<~10-3count/pix/sandRN<1e-ofRN:-CustomHxRG?-1024x1024SAPHIRAdetector?
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HabEx Coronagraph Challenges • Rawcontrastof~10-10orbe{erat2to3λ/DIWA,with:
o InstantaneousBWof20%.o High“core”throughput.
• Post-processingfactorof20
o Requiredtoreach4x10-11detec1onlimit,i.e.dmag=26.0• Exquisite(LO)WFS&C:limitWFfluctua1onsandsensi1vitytothem
• LargestableDMsandelectronicdrivers:
o atleast64x64for1”OWAat0.6µmwitha4mo 256x256for15mLUVOIR(?)
• Dualpolariza1onopera1onstronglypreferred:
o Higherthroughput;EnablesPDIo Planetreflectedlightpolarimetricstudies(e.gtalkbyT.Meshkat),oceanspecularreflec1ono Affectstelescopedesign(f#=2.5)
• HighContrastObserva1onsofBinaries• LUVOIR15mon-axisdeployabletelescopeshallmeetalloftheabove,forasegmentedprimarywith
centralobscuraRon(acRveresearcharea)
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HabEx Coronagraph Challenges • Rawcontrastof~10-10orbeserat2to3λ/DIWA,with:
o InstantaneousBWof20%.o High“core”throughput.
• Post-processingfactorof20
o Requiredtoreach4x10-11detec1onlimit,i.e.dmag=26.0• Exquisite(LO)WFS&C:limitWFfluctuaFonsandsensiFvitytothem
• LargestableDMsandelectronicdrivers:
o atleast64x64for1”OWAat0.6µmwitha4mo 256x256for15mLUVOIR(?)
• DualpolarizaFonopera1onstronglypreferred:
o Higherthroughputo EnablesPDIo Planetreflectedlightpolarimetricstudies(e.gtalkbyT.Meshkat)o Affectstelescopedesign(f#=2.5)
• HighContrastObservaFonsofBinaries• LUVOIR15m:alloftheabove,forasegmentedprimarywithcentralobscuraRon
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Raw Starlight Suppression • Rawcontrastof~10-10orbe{erfrom2.5to32λ/DIWA,with:
o InstantaneousBWof20%.o High“core”throughput.o DualPolariza1on.
• CurrentStateoftheArt:o WFIRSTlabdemonstra1onof10-9rawcontrastbtw3-8λ/D,10%BWaround
550nmanddualpolariza1on(HLC,Jun-ByoungSeoetal2017).o Previousdemonstra1onsof4to6x10-10halfdarkholewithpolarizedlaser
lightand“friendlier”pupil(Trauger&Traub2007,Serabyn2010TDEM)
• On-goinglabdemonstra1onsforunobscuredpupils:o Serabynetal.2014TDEM,aimingfor<10-910%BWcontrastonfrom3-8l/D
foratleastonepolariza1onstate(2ifLSinPP)o DecadalSurveyTestbedtarge1ng10-10contrastat2.5λ/Dand20%BWwithHLCandpossiblyVVCmasks
• CurrentlyBaseliningcharge6vortexo Highertheore1calresiliencetoloworderaberra1onso Widelyusedatground-basedtelescopeso HLCalsoconsideredasabackupduetoitshighTRLandtraceabilitytotheWFIRSTCGI.
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Low order WF sensing and control • HabExCoronagraphErrorBudget(B.Nema12018,usingWFIRST-CGImethodology):
HabExCoronagraphErrorBudget ExoEarthIMG 500 nm 20% BW ViewedDate:
Δ magplanet Planet-StarFluxRatio Scenario: ExoEarthIMGREQ 25.0 REQ 100 ppt targetandreferencesystemassumptions alloc.integtime 50.0 hrsCBE 25.2 CBE 84 ppt notes: timetoSNR 32.6 hrs
1.scenarioincludesnoisefromdifferentialimaging Target Fid3:STM0.7RE12pc2.diffimagingassumesadditional20%time,onrefstar hoststarV 5.23 mag
FluxRatioNoise ExoZodi/Solar 3 XALLOC 14.3 ppt ref.star Δmag 3 magCBE 12.1 ppt pl.geom.albedo 36.7 %
pl.phaseangle 90 degpl.fluxratio 100 ppt
1 PhotometricNoise 2 SystematicNoise planetsep. 83 masDetectorandshotnoise contr.Stab.w/postproc. sys.distance 12 pcCBE 10.7 ppt CBE 5.6 ppt
FluxRatio/C_CG1.12
1.1 SpeckleShotShotnoiseofmn.speckle Postproc.factor SuppressionfromsubtractionaloneCBE 3.2 ppt f_pp 25% (4X) 5.11 x
1.2 DetectorNoise 2 RawContrast 3 ContrastStablityshotnoiseofplanetsignal 3.2 λ /DCBE 0.8 ppt CBE 102.0 ppt CBE 20.0 ppt
1.3 PlanetShotshotnoiseofplanetsignalCBE 3.0 ppt
1.4 ZodiShot 2.3 2.1 2.2 3.3 3.4 3.1Exo-Zodidominated "radial" "radial" B "azimuthal" C "azimuthal" E "radial" F ACBE 9.7 ppt CBE 0.01 ppt CBE 50.00 ppt CBE 50.00 ppt CBE 1.94 ppt CBE 0.01 ppt CBE 0.01 ppt
1.5 StrayLightShot 2.4 3.2Allstraylight "azimuthal" DCBE 1.0 ppt CBE 0.04 ppt CBE 1.81 ppt
TotalThroughput0.2 mas
CBE 14% Teles.throughput CBE 0.5 CBE nm
CBE 78%Jitter: 0.5 mas
CGThroughput CBE Drift: 2.0 mas CBE nm
CBE 17%Detec.Parameters
clockinducedcharge CGmaskthputdarkcurrent Teles.Align.Stab. TelOpt.WFEStab.readnoise CBE 20% relativetoPM total
SM TM PM 1017 pmDetec.Parameters trans 1 5 nm SM 269 pm
QE rot 1 5 nrad CBE TM 269 pm
3/15/2018
3.09
LOWFS/CPointing LOWFS/CWFE
mas 0.76
TelescopeACS Teles.WFEStability
ThermalDrift ThermalDrift Staticbkgdstd
JitterInduced ThermalDrift
JitterInduced StaticBkgdMean StaticBkgdMean
Vortex_X6
RequiredSNR7
TimeMargin35%
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Low order WF sensing and control: a mulJ-stage approach
• Minimize“na1ve”telescopeWFji{er:o UsecoldgasGAIA-like(orcolloidalLISA-Pathfinder)micro-thrustersratherthanreac1on
wheelsforfineal1tudecontrol(andaconven1onalmonoprophydrazinesystemforslewingandsta1onkeepingatL2)o Usephasedarrayantennatofurtherreduceenvironmentalvibra1onandenablecon1nuous
sciencedownlink
• MinimizeWFslowdri�so Telescopethermaldesign(TBDSTOPanalysis)o UseLASERmetrologytosenseandcorrectslowde-spacingofM2andM3wrtM1
• SenseandcorrectresidualLoSji{eranddefocusduringscienceobs
o WFIRST-likeZernikeWFSanalyzingstarlightreflectedoffcoronagraph(VVC:centraldot)o UseWFIRST-likeseparatefast1p-1ltmirrorandfocusadjustment
• Minimizesensi1vitytolow-orderaberra1ons
o Usehighchargevortexcoronagraph(Ruaneetal.2018)o VVC6preservesIWAandthroughput,whileimmunizingagainstloworderaberra1ons:
Compactlasermetrologybeamlauncher(J.Nissen)
VVC6btwpolarizers(credit:E.Serabyn)
LPFclusterofµ-thrusters(Credit:ESA/Airbus)
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• VVC6onclearcircularaperturecaninprincipletoleratemuchhigherloworderaberraLonsfluctuaLonsthancommonlybelieved:
• 100sofpmtonmfor(Z4-Z10)• 0.5masofrmsLp-Lltresiduals.
Loworderwavefronterrorrequirements(withjiser)
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AberraFon Indices AllowableRMSerror(nm)permode
n m charge6 charge8 charge10
Tip-1lt 1 ±1 5.5 18 31
Defocus 2 0 4.6 15 36
As1gma1sm 2 ±2 0.36 1.0 4.6
Coma 3 ±1 0.44 0.95 5.5
Spherical 4 0 0.32 0.81 6.7
Trefoil 3 ±3 0.0065 0.35 0.71
notrejectedfirst-orderrejec1on>first-orderrejec1on
With1mas(0.04λ/D)Fp-Fltjiser
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MulF-StarDirectImagingObservaFonswithHabEx(Sirbu,Thomas&Belikov2017;Thomas,Belikov&Bendek2015)
Mul1-StarScienceSta1s1cs:- 517FGKstarswithin20pc- 259mul1-stars(op1calordynamical)- 193starslimitedat>1e-10
- 40starswithsep.<N/2λ/D
HabExassump1ons:- D=4m- λ=650nm- λ/20RMSwithf-3powerspectrum- 48x48DMNote:Contrastfloorforanon-axiscoronagraph/starshadeduetounsuppressedoff-axiscompanionstar
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On-axisblocker Off-axisblocker StarSeparaFonat<N/2λ/D*
StarSeparaFonat>N/2λ/D*
Notes
Coronagraph None(wavefrontcontrolonly)
MSWC SNMSWC Exis1ngmissionsarealreadycapableofMSWCwithnohardwaremodifica1ons.ThiscanbeextendedtoSNMSWCifthereisquil1ngontheDMoramildgra1nginthepupilplane
Coronagraph SecondCoronagraphmask
MSWC SNMSWC Thesecond(off-axis)coronagraphisnotnecessaryforawell-baffledtelescope,butmayrelaxthestrokerequirementontheDMforclosestars
Coronagraph Starshade SSWC SSWC Addingastarshadeeffec1velyreducesbinariestothesingle-starsuppressionproblem,butatasignificantincreaseinmissioncost
Starshade None(wavefrontcontrolonly)
SSWC SNWC Addingadeformablemirror(withoutacoronagraph)toastarshademissiontheoreFcallyenablesdouble-starsuppression
Starshade SecondStarshade Noac1vesuppressionrequired
Noac1vesuppressionrequired
Addingastarshadefortheoff-axisstareffec1velyreducesbinariestothesingle-starsuppressionproblem,butatasignificantincreaseinmissioncost
Starshade Coronagraph SSWC SNMSWC Theoff-axiscoronagraphisnotnecessaryforawell-baffledtelescope,butmayrelaxthestrokerequirementontheDMforclosestars.[BM:needsmildgra1nginthePP].
SSWC=SingleStarWavefrontControl(WC),MSWC=Mul1-StarWC,SNWC=Super-NyquistWC,SNMSWC=Super-NyquistMul1-StarWC
SCENARIO SOLUTIONS *AssumingDM=NxNactuators
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Conclusions
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• Wefindthata4mopFmizedoff-axistelescope/coronagraphassemblyshallbeabletodetect12+18–8exo-EarthsintheHZaroundnearby(<16pc)sunlikestarsandhundredsofothertypesofplanets
• SmallIWAinλ/Dunits,high“core”throughput,andlowsensi1vitytoaberra1onsmakethismoderatesizetelescopesolu1onscien1ficallycompelling,costeffec1veandwithintechnicalreachforaphaseAstartinthemid2020s.
• Anexternalstarshadeprovidesthemostefficientwaytospectrallycharacterizetheseplanets,yieldingspectraofallexo-Earthsand>50%ofplanetsdetectedbetween0.3and1micron
• HabExstudyInterimreportwillbepubliclyavailablethissummer:h{ps://science.nasa.gov/astrophysics/2020-decadal-survey-planning• MainTBDsbyfinalreport:
o IncorporatebinarystarsWFS&Cschemeo FullycompleteSTMusedtoderivetechrequirements,e.g.molecularabundancethresholddetec1onlevelrequirementso Fullyassessscienceyieldsensi1vitytoastroandinstrumentuncertain1eso Streamlinestarshadedesigno ConducttradeofGOvsexoplanetsurvey1mefrac1onsforprimary5yrmissiono Conductend-to-endSTOPmodelingtofinalizecoronagrapharchitecturetrade(VVC6orVVC8,HLC)o FinalizenearIRdetectortradeo ExploreArchitectureop1onB
• Maindevelopmentsinthe10yearsaheadforHabExhighcontrastcoronagraphy
o Demonstra1onofdualpolariza1on20%BW10-10contrastat~2-3 λ/D.o Demonstra1onofWFCatrequiredlevelsàWFIRSTCGIwillprovideo QualifylargerformatDMs
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Back-UpSlides
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