wide-field infrared survey telescope - aps home · 2017. 11. 13. · 05/18/17 3 historical context...

Wide-FieldInfraRedSurveyTelescope

05/18/17 1

JeffreyKruk(NASA-GSFC)

205/18/17

Outline

Ø MissionOverview§  Historicalbackground§  Observatory§  ScienceProgram

•  Weak-lensing,galaxyredshiLsurvey•  SupernovaIasurveys•  Microlensing•  Coronagraphy

Ø ProjectStatusØ Q&A

305/18/17

HistoricalContext-1

Ø 1995FirstexoplanetdiscoveredbyradialvelocityØ 1998,1999:firstpapersfindexpansionofuniverseis

acceleraVng(TypeIasupernovae)Ø 2002FirstexoplanetdiscoveredbytransitØ 2003Na4onalResearchCouncilrecommendsNASA/DOE

DarkEnergyMission(Connec'ngQuarkstotheCosmos)Ø 2003NASABeyondEinsteinproberoadmapØ 2004FirstexoplanetdiscoveredbymicrolensingØ 2004FirstNASA/DOEJointDarkEnergyMissionSDTØ 2005JDEMmissionconceptstudiesbeginØ 2006MicrolensingPlanetFinderproposalØ 2006TPF-CScience&TechnologyDefiniVonTeamreport

405/18/17

HistoricalContext-2

Ø 2007NRCrecommendsJDEM2009startØ 2009Keplerlaunch

§  2335confirmedplanetdetecVons,4496candidatesØ 2009Astro-2010whitepapersubmissions

§  Missionconcepts:•  JDEM-Omega•  MicrolensingPlanetFinder•  NearInfraRedSkySurveyor

Ø 2010NRCrecommendsWFIRST§  Mergerofabove3scienceprograms(&manynon-mission-specificwhitepapers),usingJDEM-Omegaobservatoryconcept

05/18/17 5

WFIRSTScienceProgramisguidedbyNWNH

NaVonalAcademyofSciencesAstronomy&AstrophysicsDecadalSurvey

(2010)

Na4onalAcademyofSciencesAstronomy&AstrophysicsDecadalSurvey(2010)

Wide-FieldInfraredSurveysoftheUniverse

(GuestObserver&Inves4gatorOpportuni4es)

DarkEnergyandtheFateoftheUniverse

?

??

Thefulldistribu4onofplanetsaroundstars

TechnologyDevelopmentforExplora4onofNewWorlds

OurGuidingPrinciple

705/18/17

WFIRSTpre-FormulaVon

Ø 2010WFIRSTSDT#1convenedØ 2012NASAacquisi4onof2NROtelescopesØ 2012WFIRSTSDT#2convened

§  FinalReport:hbp://arxiv.org/abs/1503.03757Ø 2014NRCdeclaresAFTAconsistentw/NWNH

§  hbp://www.nap.edu/catalog/18712/evaluaVon-of-the-implementaVon-of-wfirstaLa-in-the-context-of-new-worlds-new-horizons-in-astronomy-and-astrophysics

Ø 2016BeginPhaseA§  AppointFormulaVonScienceWorkingGroup§  Begindetailedrequirementsanalysis&engineeringdesign

WFIRSTObservatoryConcept

KeyFeaturesØ  Telescope:2.4maperture

primaryØ  Instruments

§  WideFieldImager/Spectrometer&IntegralFieldUnit

§  InternalCoronagraphwithIntegralFieldSpectrometer

Ø  DataDownlinkRate:275Mbpsdownlink

Ø  DataVolume:11Tb/dayØ  Orbit:Sun-EarthL2Ø  LaunchVehicle:DeltaIVHeavyØ  MissionDura4on:6yr,10yrgoalØ  Serviceability:Observatory

designedtoberoboVcallyserviceable

Ø  GSFC:leadsmissionandI&T,widefieldinstrument,spacecraL

Ø  JPL:leadstelescope,coronagraph

805/18/17

SASS

IC

AVIONICSMODULESX6

OBA

WFI

CGI

OBADOOR

HGAS

FCR

X

Y

Z

WFIRSTInstruments

905/18/17

Wide-FieldInstrument•  Imaging&spectroscopyover1000sofsq.deg.•  MonitoringofSNandmicrolensingfields•  0.7–2.0µm(imaging)&1.0-1.89µm(spec.)•  0.28deg2FoV(100xJWSTFoV)•  18H4RGdetectors(288Mpixels)•  7filterimaging,grism+IFUspectroscopy

Coronagraph•  Imageandspectraofexoplanetsfromsuper-

Earthstogiants•  Imagesofdebrisdisks•  430–970nm(imaging)&600–970nm(spec.)•  Finalcontrastof10-9orbeber•  Exoplanetimagesfrom0.1to1.0arcsec

PlannedSun-EarthL2haloorbit

1005/18/17

DiameterofplannedhaloorbitiscomparabletoEarth-L2distance

Telescope

1105/18/17

Telescope

1205/18/17

1305/18/17

WideFieldChannel

Ø  Verylargeimagingfieldofview(FOV)(0.8°x0.4°)Ø  HighspaValresoluVon(0.11arcsec/pixel)Ø  Stableimagequality(1.0nm

RMSwavefronterrorvariaVonin180sec)

Ø  7imagingfiltersspanningvisible&NIR:0.76to2.0μm

Ø  grismformulV-object,low-resoluVonspectroscopy

WFIRSTFOV

HSTJWST

WFIRSTProvidestheFirstWide-FieldHighResoluVonMapoftheMilkyWay

Ø  ProtostellarvariabilityØ  ClustermembershipidenVficaVondown

tothehydrogenburninglimitØ  DustexVncVonmapping

InRCW38(2MASSJ&Hshown)WFIRSTwillreach1000xdeeperwith20xbeberangularresoluVon

05/18/17 14

M31 PHAT Survey!Dalcanton et al. 2012!

432 Hubble WFC3/IR pointings!

M31 PHAT Survey!432 Hubble WFC3/IR pointings!

2 WFIRST pointings!

1705/18/17

IntegralFieldSpectrograph

§  SupernovaFOV:3x3arcsec,0.075arcsec/pixelresoluVon§  PhotometricRedshiLCalibraVonFOV6x6arcsec,0.15”/pixelresoluVon§  VeryhighsensiVvity,NIRpassband(0.45-2.0μm)§  Lowspectralresolvingpower(70-140λ/Δλ)

1805/18/17

Coronagraph

Ø TechnologyDemonstraVonInstrument

Ø Twomodes:§  hybridLyot§  shapedpupil

DesignImplementa4on Value Comments

Bandpass 430-980nm MeasuredsequenVallyin10%and18%bands

InnerWorkingAngle[radial]150mas at550nm,3λ/Ddrivenby

telescopepupilobscuraVons270mas at1μm

OuterWorkingAngle[radial]

0.5as at550nm,10λ/D,forhighestcontrast

0.9as at1μm,10λ/D0.95as at550,20λ/D,lowercontrast

1.7as At1μm,20λ/D,lowercontrast

Detec4onLimit(Contrastaberpost-processing) 3×10-9

ColdJupiters;deepercontrastunlikelyduetopupilshape&extremestabilityrequirements.

ImagingDLFOV[radius]w/omasks 2.9as Withoutmasksinplace

Imagingpixelplatescale 0.01asSpectralResolu4on 70 R=λ/δλ(IFS)

IFSSpa4alSampling 17mas 3lensletsperλ/D,beberthanNyquist

1905/18/17

CGIOperaVonalModes

Pupilmask

Lyotmask

Filterwheel

Fieldstopmask

toLOWFS

FSM

PBS

M4

M3

CORF1

R3OAP1

R3OAP2

COLF1

COLF2

FSOAP1

FSOAP2

TertiaryCollimatorAssembly(TCA)

CoronagraphInstrument(CGI)

DM2

FocMR1OAP1

R1OAP2

R2OAP1

R2OAP2

DM1

FM

IFS/ImgSelector

FocalPlanemask

RadiaVonShieldMirror

FPA

Telescope

T1

T2

CORF2

IMG

HybridLyotModeImagingin2simultaneouspolarizaVons,simulatedplanetsarecircledinred

2005/18/17

CGIOperaVonalModes

R3OAP1

TelescopeT2

Pupilmask

Lyotmask

Filterwheel

Fieldstopmask

FSM

M4

M3

CORF2

R3OAP1

R3OAP2

COLF1

COLF2

FSOAP1

FSOAP2

DM2

FocMR1OAP1

R1OAP2

R2OAP1

R2OAP2

DM1

FM

IFS/ImgSelectorFocalPlane

mask

T1

ShapedPupilSpectroscopyMode

FPA

IFS

IFS

CORF1

toLOWFS

TheIFSuses318%bandstoproduceanR=70spectrafrom600to970nm

lensletarray pinhole

maskdispersed

lensletimages

extracteddatacube

SPCimagesin318%bands



2105/18/17

CGIOperaVonalModes

R3OAP1

TelescopeT2

Pupilmask

Lyotmask

Filterwheel

Fieldstopmask

FSM

M4

M3

CORF2

R3OAP1

R3OAP2

COLF1

COLF2

FSOAP1

FSOAP2

DM2

FocMR1OAP1

R1OAP2

R2OAP1

R2OAP2

DM1

FM

IFS/ImgSelectorFocalPlane

mask

T1

ShapedPupilDiskImagingMode

CORF1

toLOWFS

DiskImagingatwavelengths465and890nm,in2simultaneouspolarizaVons



RadiaVonShieldMirror

FPA

IMG

Imagefrom2015Exo-CSTDTFinalReport

2205/18/17

ScienVficObjecVves

1)  ProduceNIRskyimagesandspectraover1000'sofsqdeg(J=27ABimaging,F_line=10-16ergcm-2sec-1)

2)  DeterminetheexpansionhistoryoftheUniverseandthegrowthhistoryofitslargeststructuresinordertotestpossibleexplanaVonsofitsapparentacceleraVngexpansionincludingDarkEnergyandmodificaVonstoEinstein'sgravity.

3)  CompletethestaVsVcalcensusofplanetarysystemsintheGalaxy,fromtheouterhabitablezonetofreefloaVngplanets

4)  DirectlyimagegiantplanetsanddebrisdisksfromhabitablezonestobeyondtheicelinesandcharacterizetheirphysicalproperVes.

5)  ProvidearobustguestobserverprogramuVlizingaminimumof25%oftheVmeoverthe6yearbaselinemissionand100%infollowingyears.





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OurGuidingPrinciple

TheUniverseasaPieChart DarkEnergyIs a repulsive force

Affects the speed at which the Universe expands

Causes everything to move away from everything else

DarkMacerAffected by the attractive force of gravity

Affects how “clustered” objects are Causes objects to want to move towards

one another

DarkEnergy~68%

DarkMaber~27%

Neutrinos

Stars

Gas

NormalMaber~5%

Push-Pull:DarkEnergyvsDarkMacer

TounderstandtheUniverse’sendfate,wemustmeasurebothdarkmaberanddarkenergy

WFIRSTDarkEnergyProgram

2605/18/17

2705/18/17

WFIRSTDarkEnergyRoadmap

High Latitude Survey Supernova Survey wide, medium, & deep imaging

+ IFU spectroscopy

2700 type Ia supernovae z = 0.1–1.7

spectroscopic: galaxy redshifts

20 million Hα galaxies, z = 1–2 2 million [OIII] galaxies, z = 2–3

imaging: weak lensing shapes

400 million lensed galaxies 40,000 massive clusters

standard candle distances!z < 1 to 0.20% and z > 1 to 0.34%

standard ruler ! distances expansion rate!

z = 1–2 to 0.4% z = 1–2 to 0.72% z = 2–3 to 1.3% z = 2–3 to 1.8%

dark matter clustering!z < 1 to 0.16% (WL); 0.14% (CL) z > 1 to 0.54% (WL); 0.28% (CL)

1.2% (RSD)

history of dark energy + deviations from GR

w(z), �G(z), �REL/�NREL

WFIRSTwillmeasuregalaxyshapestomapdarkmaberandmeasure

thegrowthofgalaxiesovertheUniverse’slife

MACSJ1206.2-0848darkmabermap

2905/18/17

Mass density contours around the cluster MACS J1206.2-0848 derived from a ground-based weak lensing survey with Subaru (red) vs. a weak lensing study with HST/ACS+WFC3 (white). The 10x higher surface density of lensed galaxies achieved from space yields ~3x higher spatial resolution maps. The HST data shown here is representative of the WFIRST-AFTA HLS. WFIRST-AFTA will make a map of this quality over 2,000 square degrees as part of its high latitude survey, a thousand-fold increase over the HST COSMOS mass map.

GravitaVonalLensing

30

MACJ1206.2-0847

PostmanHST

WFIRST

0.79deg

05/18/17

3105/18/17

GalaxyRedshiLSurvey

TheearlyUniverseimprintsclumpingonacharacterisVclengthscale,setbythesizeoftheUniversewhenmaberbecameneutral,andisknownfromtheintrinsicnon-uniformityintheCosmicBackgroundRadiaVon.

ThesebaryonacousVcoscillaVonsprovideastandardrulerin3dimensionsformeasuringcosmicexpansion.

3205/18/17

•  ColddarkmaberdistribuVonfromMillennium-IISimulaVon(Boylan-Kolchinetal.2009).

•  ZoomvariesleLtoright•  Timepassestoptobobom

•  Galaxiesformatdenseregions.•  SpacinggovernedbyimprintofBAO:standardrulergivesevoluVonofdistancescalesasfuncVonofredshiL.

3305/18/17

GalaxyRedshiLSurvey

Useimaging&slitlessspectroscopytomeasure3-DgalaxydistribuVon

GalaxyRedshiLSurvey

3405/18/17

SampleHSTWFC3-IRgrismspectrum(Ateketal2010)

3505/18/17

TypeIasupernovae

•  TypeIasupernovaehave“known”peakintensity.•  Numberofreceivedphotonstellsusdistance(1/r2).•  Obtain~100IaSNeperΔz=0.1,for0.2<z<1.7

ObservingSupernovae

3605/18/17

SomeVmesSNearewell-separatedfromtheirhostgalaxy,andsomeVmesthey’renot!Havetoaccuratelysubtractthelightofthehostgalaxy.

N.Suzukietal.2012ApJ74685doi:10.1088/0004-637X/746/1/85

3705/18/17

WFIRSTSNIa

Ø  NeedspectrumtomeasureredshiL&confirmtypeØ  Needrest-framespectralenergydistribuVonto

obtainluminosityatfiducialwavelengthsandtocorrectfordustexVncVon§  ObtainspectraormulV-bandimaginglight-curves

Ø SNdiscoveryviaimagingØ IFUSpectrophotometryforfollow-up





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OurGuidingPrinciple

3905/18/17

PlanetaryMicrolensing

Ø ObservegravitaVonallensingbyplanetsalongthelineofsighttodistantstars§ Monitor3sqdeginGalacVcBulgeat15minutecadence

Ø Obtainacensusofplanetmassesandorbitradiiatthehabitablezoneandbeyond

Ø AnVcipatediscoveryof~2600boundplanetsofMarsmassandabove,andhundredsoffree-floaVngplanets.

MicrolensingTechnique

4005/18/17GreatbenefitofspaceobservaVonsinthecrowdedgalacVcbulgefield

4105/18/17

Microlensingexample

MicrolensingeventfromJupiter-massplanetaroundanM-dwarf(Skowronetal2015):

Days

4205/18/17

MicrolensingsimulaVon

Ø  SimulatedWFIRSTmicrolensingeventbyEarth-massplanet.§  MagnificaVonbyplanetissimilartoeventonpreviousslide,butduraVonis~10Xshorter.

4305/18/17

WFIRSTComplementsKepler

CompleVngtheStaVsVcalCensusofExoplanets

4405/18/17

Combinedwithspace-basedtransitsurveys,WFIRST-AFTAcompletesthestaVsVcalcensusofplanetarysystemsintheGalaxy.

CompleVngtheStaVsVcalCensusofExoplanets

4505/18/17

Combinedwithspace-basedtransitsurveys,WFIRST-AFTAcompletesthestaVsVcalcensusofplanetarysystemsintheGalaxy.

•  2600planetdetecVons.

•  370withEarthmassandbelow.

•  Hundredsoffree-floa4ngplanets.

WFIRSTperfectlycomplements

Kepler,TESS,andPLATO.





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OurGuidingPrinciple

4705/18/17

WFIRSTCoronagraphy

•  Scienceprogramdefinedtodrivetechnology,informinstrumentdesignparameterdecisions•  DeterminecharacterisVcsofexo-zodiacaldustdisks•  Survey~200nearbystars,spanningarangeofspectraltypes,withandwithoutknownexoplanets

•  Characterize10-20planetsat>4REinreflectedlight•  5bands,10%relaVvephotometry

•  SpectroscopiccharacterizaVonof6-10planets•  DeterminedepthofH2O,methane,absorpVonto15%

•  Detectsampleat<4REinreflectedlight•  Determinesemi-majoraxis,eccentricity,ofeachplanet

Coronagraphy

4805/18/17

Ø MulV-bandimagingathighcontrastprovidesfordirectdetecVonandpreliminarycharacterizaVonofexoplanets

30 zodi disk

Planet c

Planet b

Inner working angle

Simulated WFIRST coronagraph image of the star 47 Ursa Majoris, showing two directly detected planets.

Eachcoronagraphpoin4ngwillyieldday-longWFIdeep-fields(0.28sqdeg).

2 AU R=70

0.4 0.6 0.8 1.0 1.2Wavelength (microns)

0.00

0.05

0.10

0.15

0.20

0.25

Geo

met

ric a

lbed

o

4905/18/17

WFIRSTBringsUsClosertoCharacterizingexo-Earths

Ø WFIRSTadvancesmanyofthekeyelementsneededforacoronagraphtoimageanexo-Earthü  Coronagraphü Wavefrontsensing&

controlü  Detectorsü  Algorithms

5005/18/17

WFIRSTHigh-ContrastImaging

ü WFIRSTsignificantlyexpandsthepopulaVonofcharacterizedplanets§  Figureatrightshowsknown

exoplanets(mostlyKeplerdetecVons),thosecharacterizedbytransitspectroscopy,&representaVveparameterspaceofplanetsthatwecanexpecttoexplorewithWFIRST.

0.01 0.10 1.00 10.00 100.00Semi-major axis (AU)

1

10

100

1000

Plan

et M

ass

(MEa

rth)

Direct ImagedSec. EclipseTransit Spec

WFIRST/NewWFIRST/RV

FigurefromEricNeilsen





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OurGuidingPrinciple

52

WFIRSTSurveys

Ø MulVplesurveys:§  HighLaVtudeSurvey

•  Imaging,spectroscopy,supernovamonitoring

§  RepeatedObservaVonsofBulgeFieldsformicrolensing

§  25%GuestObserverProgram

§  CoronagraphObservaVons

Ø FlexibilitytochooseopVmalapproach

05/18/17

5305/18/17

ExampleObservingSchedule

Ø  High-laVtudesurvey(HLS:imaging+spectroscopy):2.01years§  2227deg2@≥3exposuresinallfilters(2279deg2boundingbox)

Ø  6microlensingseasons(0.98years,aLerlunarcutouts)Ø  SNsurveyin0.63years,fieldembeddedinHLSfootprintØ  1yearforthecoronagraph,interspersedthroughoutthemissionØ  UnallocatedVmeis1.33years(GOprogram)

High-La4tudeSurveyArea

MicrolensingFields

Galac4cPlaneEclip4cPlaneCeles4alEquator

SNFields

5405/18/17

AstrometrywithWFIRST

Ø GAIAstarsprovidereferenceframe§  WFIRSTshouldachieve500μasorbeberoneachobservaVonofaGAIAstar

§  HighLaVtudesurvey§  ~20observaVonsperstarover~5years

•  ~100μas/yrpropermoVonsdowntoAB~23

Ø GalacVcbulgesurvey§  ~40,000observaVonsperstar§  Sub-μasastrometry?

5505/18/17

FindingtheMostDistantGalaxies

•  WFIRST’s High-Latitude Survey will yield up to 2 orders of magnitude more high redshift galaxies than currently known

•  WFIRST will find interesting distant galaxies for JWST and future narrow-field telescopes to observe

EsVmatesfromDanCoe&LarryBradley

56

ProgramStatus

Ø SubstanValtechnicalprogressonWFIRSToverthepasttwoyears:§  NIRdetectormaturaVon–nowatTRL-6

•  Readytobeginflightprocurementlaterthisyear

§  CoronagraphtechnologydemonstraVons§  Observatoryintegratedmodeling

05/18/17

57

ProgramStatus

Ø MissionConceptReviewcompletedDec8-9.Ø FormulaVonScienceteamselectedDec23Ø BeginPhaseAFebruary17,2016!Ø BeginPhaseBearly2018Ø SignificantinternaVonalinterest(Canada,ESA,Japan,Korea)

Ø Launch:mid-2025§  DependsonbudgetappropriaVons

05/18/17

ScienceInvesVgaVonTeams

5805/18/17

§  DavidSpergel WFIAdjutantScienVst§  JeremyKasdin CGIAdjutantScienVst§  OlivierDoré WeaklensingandgalaxyredshiLsurvey§  SaulPerlmuber Supernovae§  RyanFoley Supernovae§  ScobGaudi Microlensing§  BruceMacintosh Coronagraphy§  MargaretTurnbull Coronagraphy§  JasonKalirai GOscience,milkyway§  JamesRhoads GOscience,cosmicdawn§  BrantRobertson GOscience,galaxyformaVon&evoluVon§  BenjaminWilliams GOscience,nearbygalaxies§  AlexanderSzalay GIscience,archivalresearch

QUESTIONS?

5905/18/17

6005/18/17

WFIRSTMandate

Ø 2010NRC(NWNH)recommendsWFIRST:§  “Whyistheexpansionrateoftheuniverseaccelera4ng?Andarethereothersolarsystemslikeours,withworldslikeEarth?”

§  “Tomeasuretheproper4esofdarkenergy,WFIRSTwillemploythreedifferenttechniques:

•  carryoutadetailedstudyofweaklensingthatwillprovidedistanceandrate-of-growthinforma4on;

•  monitordistancesandexpansionrateusingbaryonacous4coscilla4ons

•  detectabout2,000distantsupernovaexplosions,whichcanbeusedtomeasuredistances.”

6105/18/17

WFIRSTMandate(butwait–there’smore!)

Ø 2010NRC(NWNH)recommendsWFIRST:§  “WFIRSTwillcarryoutapowerfulextrasolarplanetsearchbymonitoringalargesampleofstarsinthecentralbulgeoftheMilkyWayforsmalldevia4onsinbrightnessduetomicrolensingbyinterveningsolarsystems.Thiscensus,combinedwiththatmadebytheKeplermission,willdeterminehowcommonEarth-likeplanetsareoverawiderangeoforbitalparameters.”

§  “WFIRSTwillalsoofferaguestinves4gatorprogram”

6205/18/17

PlannedWide-areaSurveys

Ø Basedon2015ScienceDefiniVonTeamReport

Ø Thisisanexampleofhowthemissionmaybeplanned,butfinalsurveysmaydiffer§ MuchflexibilityinchoiceofDEsurveys§ Maywellchoosetogowider,shallower

6305/18/17

WeakGravitaVonalLensing

ForegroundmaberdistribuVoninducescorrelateddistorVonsinshapesofbackgroundgalaxies

UseweakgravitaVonallensingtosamplemaberdistribuVontoz~2•  ObtaindeepNIRimaginginmulVple

bands•  Measureshapesofbackground

galaxiestoz~3atsamplingdensityof≥45/squarearcminute

•  DerivephotometricredshiLsbyfi�ngspectraltemplatestomulV-bandimages

6405/18/17

WFIRSTHigh-LaVtudeSurvey

0.05

0.1

0.2

0.5

1

2

5

0.6 1.0 1.4 1.8 2.2 2.6 3.0

nP(k

=0.2

h/M

pc)

z

WFIRST-AFTA HαWFIRST-AFTA [OIII]

Euclid Hα

DESurveyspecifics

6505/18/17

WeakLensingImagingSurvey

Parameter Y J H F184

λmin(μm) 0.927 1.131 1.380 1.683

λmax(μm) 1.192 1.454 1.774 2.000

PSF(REE50) 0.12” 0.13” 0.13” 0.14”

ExpVme 5x174 6x174 5x174 5x174

5σptsrcdepth 26.56 26.70 26.54 25.76

WLNeff/sqamin N/A 32.8 35.2 19.0

Surveyarea:2227sqdegGalaxydepth~1magshallower(r1/2~0.3”)PSF~HST/WFC3-IR,withslightlysmallerpixels

SNIaDiscoveryImaging

RedshiLTier

AreaSqdeg Y J H

<0.4 27.4 27.5 27.5<0.8 9 28.3 28.3

<1.7 5 29.2 29.1

WFIparallelobservingwithcoronagraphwillgivemanydozensofdeepfields(AB~30?)

AlwaysobserveinWFI&IFU

WFIRSTPayloadOpVcalBlockDiagram

6605/18/17

282 K 2.4 m Telescope:

110 mas/pix f/7.9

Wide Field Science Channel

8 positions (6 filters, GRS grism, dark)

Grism R = 461λ

Element Wheel / Pupil Masks

Guiding during imaging & IFU performed in science focal plane and during grism

spectroscopy performed in aux FGS

M3

Wide Field Instrument Telescope

2 1kx1k, 18µm pixel size SCA; 2 Mpix; ≤100K; 0.6-2.0µm bandpass; FOV 3.00x3.15 arcsec 6.00x6.30 arcsec

75 mas/pix; f/21

6 struts with realignment capability and separate fine focus on SM; outer barrel with recloseable doors

Integral Field Unit Spectrograph Channel

GRS = Galaxy Redshift Survey SCA = Sensor Chip Assembly DM = Deformable Mirror FSM = Fast Steering Mirror LOWFS = Low Order Wavefront Sensor IFS = Integral Field Spectrograph

Temperature 170 K

Relay Slicer Assembly

Prism Spectrograph R = ~100 (2 pixel)

PM: 2.4 m aperture

SM: 30% linear obscuration from baffle

Coronagraph Instrument

2 Fixed DMs

Masks & Filters

LOWFS

Flip Mirror

Imaging Detector

IFS IFS Detector

1kx1k, Si low noise FPA; ≤165K; (430-970 nm)

1kx1k, Si low noise FPA, ≤165K; 600-970 nm bandpass; R~70, 17 masec sampling

18 4kx4k, 10µm pixel size SCAs; 302 Mpix; ≤100K; 0.76-2.0µm bandpass 0.28 deg2 active area

FSM

M3 COLLIMATOR ASSEMBLY

M4

Aux FGS 2 4kx4k, 10µm pixel size SCAs; 32 Mpix; ≤100K; 0.55-0.95µm bandpass

6705/18/17

WFIRSTSNIa

Ø IFUSpectrophotometryforlightcurves

−20 −10 0 10 20 30 40 50Rest-Frame Phase

−0.2

0.0

0.2

0.4

0.6

0.8

1.0

1.2

Coun

ts/S

ec (A

B Ze

ropo

int =

25)

−50 0 50 100Observer-Frame Phase

Triggered, targeted IFU spectrophotometry

3

1

6

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10

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10

−50 0 50 100Observer-Frame Phase

Pre-scheduled wide-field imaging with 5-day cadence,over 2 years, in two broad bands:

J129 filter

S/N per 2-pixel resolution element =

IFU Visit # IFU Visit #

TRIG

GER

DAT

E

z = 1.5B

V

U

R

Synthetic-filterphotometry from IFUspectrophotometry

−20 −10 0 10 20 30 40 50Rest-Frame Phase

Coun

ts/S

ec (A

B Ze

ropo

int =

25)

−20 0 20 40 60Observer-Frame Phase

Triggered, targeted IFU spectrophotometry

S/N per 2-pixel resolution element = 3

1IFU Visit # IFU Visit #

6

2

10

3

3

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3

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3

6

3

7

3

8

3

9

6

10

−20 0 20 40 60Observer-Frame Phase

Pre-scheduled wide-field imaging with 5-day cadence,over 2 years, in two broad bands:

z = 0.5

TRIG

GER

DAT

E

B

V

I

R

0

2

4

6

8

10

J129 filter

H158 filter H158 filter

SupernovaSpectra-types

6805/18/17

SpectralenergydistribuVonsofvariousSNtypesareshown,atpeakflux.ThisillustrateshowspectralfeaturesareusedtoidenVfytheSNtypes,andthatthefeaturesarestrongenoughtouseforredshiLmeasurement.TheblackbarsatthetopindicatetheporVonsofthespectrumthatwillbeobservedbytheIFUforvariousredshiLs.ThegreencurvesatthebobomshowthetradiVonalfilterbandpassesusedtocharacterizeSNe

SampleTiling

6905/18/17

wide-field infrared survey telescope - aps home · 2017. 11. 13. · 05/18/17 3 historical context...

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