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US Contributions to FLARE With an update on SPHEREx: Spectro-PHotometer for the Extragalactic structure, Reionization and ices Explorer Asantha Cooray Asantha Cooray, UC Irvine FLARE March 2016 Outline • CIP/SPHEREx • SPHERx -> FLARE is a natural transition • Proposed US FLARE team • US contributions to FLARE - sciences and hardware Asantha Cooray, UC Irvine FLARE March 2016 SPHEREx:AnAll-SkySpectralSurvey DesignedtoExplore ▪TheOriginoftheUniverse ▪TheOriginandHistoryofGalaxies ▪TheOriginofWaterinPlanetarySystems TheFirstAll-Sky Near-IRSpectralSurvey ARichLegacyArchiveforthe AstronomyCommunitywith100s ofMillionsofStarsandGalaxies Low-RiskImplementation ▪SingleObservingMode ▪NoMovingParts ▪LargeTechnical&ScientificMargins SPHEREx:SimpleInstrument,LargeMargins Deployed thermal shields Wide-field telescope 20 cm eff. aperture High-throughput spectrometer uses a linear-variable filter in front of each detector array Passive cooling system 185 cm BCP 100 spacecraft Parameter TelescopeEffectiveAperture PixelSize FieldofView Spectrometer ResolvingPowerand WavelengthCoverage Arrays PointSourceSensitivity (MEVPerformance) Cooling 2.5µmArrayand OpticsTemperature(Req’t) 5.3µmArrayTemperature (Req’t) PayloadMass PayloadPower Value 20cm 6.2"x6.2" 2x(3.5°x7.0°);dichroic Linear-VariableFilters R=41.5λ=0.75-4.1µm R=150λ=4.1-4.8µm 2xHawaii-2RG2.5µm 2xHawaii-2RG5.3µm 18.5ABmag(5σ)with 300%margintoreq’t All-Passive 80Kwith700%margin ontotalheatload 55Kwith450%margin ontotalheatload 68.1kg(CBE+31%Ctg) 27.8W(CBE+30%Ctg) Deployed Solar panels Parameter Spacecraft ScienceData Downlink PointingStability Pointing Control PointingAgility ObservatoryMass Observatory Power SolarArrayPower Output(EOL) Performance BallBCP100 Margin N/A 73Gb/day 97% 2.1"(1σ)over200s 43% 22.7”(1σ) 164% 70ºin116s(largeslews) 8.8’in6s(smallsteps) 173.6kg(MEV) 29% 233% 53% 171.8W(MEV) 36% 234W N/A Margins: Thermal Science Deep fields (x30 deeper; 200 sq. degrees) Point source detections Asantha Cooray, UC Irvine FLARE March 2016 Two100sq.degreeregions Atthepoleswithare~30xdeeper. Anopportunityforuniquescience SPHEREx Deep Fields Asantha Cooray, UC Irvine FLARE March 2016 SPHERExCreatesan All-SkyLegacyArchive NotableFeaturesoftheSPHERExAll-Sky Survey • HighS/Nspectrumforevery2MASS source • SoliddetectionoffaintestWISEsources Scienceapplications • Low-zgalaxyluminosityfunctions • Searchforz>6reionizationquasars • HighEWemissionlinegalaxies • Galaxyclusters(determineredshifts ~90%-100%oftheeROSITAclusters) • ApplicationswithSZandCMBmaps • ……. Asantha Cooray, UC Irvine Object Detected galaxies Galaxies σ(z)/(1+z) <0.03 #Sources LegacyScience 120million Galaxiesσ(z)/ (1+z) <0.003 9.8million Study(H,CO,O,S,H2O)lineand PAHemissionbygalaxytype. ExploregalaxyandAGNlife Simulationbased cycle onCOSMOSand Pan-STARRS CrosscheckofEuclidphoto-z. Measuredynamicsofgroups andmapfilaments. QSOs >1.5million UnderstandQSOlifecycle, environment,andtaxonomy QSOs atz>7 0-300 Rossetal.(2013) DetermineifearlyQSOsexist. Follow-upspectro-scopyprobes plussimulations EORthroughLyαforest 1.4billion Propertiesofdistantandheavily obscuredgalaxies Reference Clusterswith≥ 25,000 5members RedshiftsforalleRositaclusters. Geachetal., Viralmassesandmerger 2011,SDSScounts dynamics Mainsequence >100million stars Testuniformityofstellarmass functionwithinourGalaxyas inputtoextragalacticstudies 2MASScatalogs Mass-losing, dustforming stars Over10,000of SpectraofMsupergiants,OH/IR Astro-physical stars,Carbonstars.Stellar Quantities,4th alltypes atmospheres,dustreturnrates, edition[ed. Browndwarfs andcompositionofdust A.Cox]p.527 >400,incl.>40 oftypesTand Y Atmosphericstructureand composition;searchforhazes. Informsstudiesofgiant exoplanets dwarfarchives.or gandJ.D. Kirkpatrick,priv. comm. Starswithhot dust >1000 Discoverraredustclouds Kennedy&Wyatt producedbycataclysmicevents (2013) likethecollisionwhichproduced theEarth’smoon DiffuseISM Mapofthe Galaxy Studydiffuseemissionfrom GLIMPSEsurvey interstellarcloudsandnebulae; (Churchwell (H,CO,S,H2OandPAHemission) etal.2009) FLARE March 2016 SPHEREx Team ScienceTeam Name Jamie Bock Institution Caltech/JPL Role Responsibility PI Principal investigator, overall management Matt Ashby CfA Co-I Pipeline development Peter Capak IPAC Co-I Galaxy spectral fitting modules Asantha Cooray UC Irvine Co-I Galaxy Formation L4 lead Olivier Doré JPL/Caltech PS Project scientist; Inflationary Cosmology L4 lead Chris Hirata OSU Co-I Inflation and Cosmology studies Woong-Seob Jeong KASI Co-I KASI PI Phil Korngut Caltech Co-I Deputy instrument scientist Dae-Hee Lee KASI Co-I Ground test equipment Gary Melnick CfA Co-I Galactic Ice L4 lead Roger Smith Caltech Co-I Detector array development Yong-Seon Song KASI Co-I Cosmology interpretation Stephen Unwin JPL Co-I Galactic ice science Michael Werner JPL Co-I Legacy survey science Michael Zemcov Caltech Co-I Instrument scientist * Funding Source: N=NASA C=Contributed Collaborators Name Institution Experience Roland de Putter JPL US PI of Herschel/SPIRE and Planck./HFI;CIBER PI; BICEP2/Keck Co-PI Tim Eifler JPL Spitzer/IRAC teamFlagey Nicolas IfA PI of COSMOS survey Yan Gong UC Irvine CIBER, Spitzer, Herschel analysis Stanford Elisabeth Krause Planck, WMAP scientist, Euclid Science Team Daniel Masters Caltech Phil Mauskopf ASU Euclid Science Team Bertrand Menneson JPL NISS PI, MIRIS Hien Nguyen CIBER instrument development JPL KarinMIRIS Öbergdevelopment CfA CIBER, NISS, CMU SWAS PI Anthony Pullen Raccanelli H2RGs forAlvise diverse astronomy apps JHU PI of KASIVolker participation Tolls in DESI CfA SIM and TPF-I DPS; ExEP Dep ProgArgonne Scientist Salman Habib Spitzer PSKatrin Heitmann Argonne CIBER and QuADViero instruments Marco Stanford CompetedinDec2014SMEX;SelectedbyNASAforaPhase-AstudyinJuly2015. PhaseAreportdueinJuly2016. PhaseAdown-selection~December2016 N/C* Re L4 N Cosm Synergie N Ice sp L4 N Galax L4 N Bispec L4 N Spectral Cluster c N Ice C catalo Instrumen N L4 C Ice sc L4 N Galax Cosmic m N C Ice pip L4 N Galaxy c N Galaxy c N Intensity High-ThroughputLVFSpectrometer LinearVariableFilter FocalPlaneAssembly MethaneonPluto 1.0 0.8 I/F 0.6 0.4 0.2 0.0 InfraredSpectralImage 1.61.82.02.22.4 Wavelength(µm) LVFsusedonISOCAM,HST-WFPC2, NewHorizonsLEISA,&OSIRIX-Rex(2016launch) Spectraobtainedbysteppingsourceoverthe FOVinmultipleimages:nomovingparts SPHERExPassiveCoolingSystem HowDoesLVFSpectroscopyCompare? Low-Conductance PhotonShields Triple V-Groove Cooler CoolingDesignforSPHERExinLow-EarthOrbit JPLPassiveCoolingDesignforPlanckatL2 PassiveCoolingExamples Mission Orbit Temp COBE LEO 45 K Sun-Sync DIRBE post-cryo WISE LEO SS Mirror post-cryo Spitzer Earth-trail 27.5 K Mirror post-cryo 5.3um-FPA 11.4 2.2b 8.9 0.3 Planck L2 Telescope 2.5um-FPA 83.1 2.2b 70.6 SIDECAR 828 400 NA* 74 K 36 K Notes Volz et al. 1992 Planck et al. 2011 PassiveCoolingTemperaturesandPowerMargins Thermal Stage CBE Heat Load [mW] Total Dissip Condu ated cted Radiated Reqt [K] Predicted Temp Max Heat Load on Stage Temp [K] Margin [K] Totala [mW] Margina [mW] < 55 39.5 15.5 62.2 50.8 (450%) 10.3 < 80 46.2 33.8 666 583 (700%) 428 < 200 152 48 3950 3120 (380%) Wide-FieldTelescope Three-mirrorastigmat Spotdiagrams HowDoesLVFSpectroscopyCompare? Parameter Value EffectiveAperture 20cm PhysicalAperture 33cm FOV 3.5°x7° Focalratio f/3 Pixelsize 6.2″ λ/dat1µm 1.0″ Demoofflightfree-formmirrorgiving44nmrmsvs.80nmreq’t Pointsourcesensitivity dependsonhowmany pixels(Neff)areco-added tomeasureasource δFαNeff-1/2 Neffincludeseverything:diffraction,aberrations,tolerancingerrors, pointingjitter,sourcepositionsoverthearray Hawaii-2RGDetectorArrays HowDoesLVFSpectroscopyCompare? SPHERExOn-BoardSlopeFitting ‘Off-the-Shelf’ArraySpecifications Parameter 2.5µmArrays 5µmArrays Spec Typical Spec Typical CDSReadNoise 18e- 10.5e- 15e- 10.5e- DetectorQE 70% 75% 75% 75% DarkCurrent 0.05e-/s 0.01e-/s 0.05e-/s 0.01e-/s DarkCurrent(e-/s) Teledyne H2RG arrays - H1RGs flown on HST (1.7um), OCO (2.5um), WISE (5um) (TRL 9) - H2RGs and SIDECAR for JWST (TRL 6) - H2RGs wide use in ground-based astronomy SPHEREx Photo-I Bands1-3 SPHEREx Photo-I Band4 55K 80K Beleticetal.2008 WhyStudyIces? •Gas and dust in molecular clouds are the reservoirs for new stars and planets - In molecular clouds, water is 100-1000x more abundant in ice than in gas - Herschel observations of the TW Hydrae disk imply the presence of 1000s of Earth oceans in ice (Hogerheijde et al. 2011) - Models suggest water and biogenic molecules reside in ice in the disk mid-plane and beyond the snow line •Ideal λs to study ices: 2.5 - 5 µm - Includes spectral features from H2O, CO and CO2 - Plus chemically important minor constituents NH3, CH3OH, X-CN, and 13CO2 Schematic of a protoplanetary disk ISO absorption spectrum SPHERExGalacticIceSurvey SPHEREx will be a game changer to resolve long-standing questions about the amount and evolution of key biogenic molecules through all phases of star and planet formation Ices in each Phase of Star Formation • SPHEREx increases the number of ice spectra from ~200 to >> 20,000 • Band 4 spectral resolving power λ/Δλ = 150 chosen to isolate the absorption from each ice species The SPHEREx ice catalog will: • Contain molecular clouds, YSOs, and 1000s of protoplanetary disks • Determine the role of environment (T, n, radiation field, cosmic rays) in forming ices • Determine if ices in disks come from the parent cloud or are reformed • Measure the abundance of water and biogenic ices in disks that is available to new planets One Million Targets with |b| < 1° RedshiftswithSPHEREx Weextractthespectraofknownsources usingthefull-skycatalogsfromWISE andPanSTARRS/DES. Blendingandconfusioneasilycontrolled. Wecomparethisspectratoatemplate library(robustforlowredshiftsources): Foreachgalaxy:redshift&type Multipletypestestgalaxybiaseffects The1.6μmbumpisawellknown universalphotometricindicator (Simpson&Eisenhardt99) Wesimulatedthisprocessusingthe COSMOSdatasetusingthesame processasEuclid/WFIRST(Capaketal.). Thepoweroflow-resolutionspectroscopy hasbeendemonstratedwithPRIMUS (Cool++14),COSMOS(Ilbert++09),NMBS (vanDokkum++09). WISE PanSTARRS SPHERExLargeVolumeGalaxySurvey SPHERExSurveysMaximumCosmicVolume CatalogSplitintoRedshiftAccuracyBins σz/(1+z) SPHERExLarge-VolumeRedshiftCatalog • Largesteffectivevolumeofanysurvey,nearcosmiclimit • Excelsatz<1,complementsdarkenergymissions(Euclid,WFIRST)targetingz~2 • SPHEREx+EuclidmeasuresgravitationallensingandcalibratesEuclidphoto-zs SurveyDesignedforTwoTestsofNon-Gaussianity • Largescalepowerfrompowerspectrum:large#oflow-accuracyredshifts • Modulationoffine-scalepowerfrombispectrum:fewerhigh-accuracyredshifts SPHERExTestsInflationaryNon-Gaussianity • • • • Non-Gaussianitydistinguishesbetweenmulti-andsingle-fieldmodels ProjectedSPHERExsensitivityisδfNL<1(2σ) -Twoindependenttestsviapowerspectrumandbispectrum Competitivelytestsrunningofthespectralindex SPHERExlow-redshiftcatalogiscomplementaryfordarkenergy SPHERExMeasuresCosmicLightProduction TwoWaystoMeasureCosmicLightProduction WhatConstitutesCosmicLightProduction? Moseley & Zemcov Science 2014 13+ billion years of galaxy collisions and mergers Diffuse emission between galaxies from tidally stripped stars Inflation fraction of a trillionth of a second Cosmic microwave background ~380,000 years First stars & galaxies ~400 million years Present universe ~13.8 billion years 1)IndividualGalaxies&Redshifts Largetelescopeforpointsourcesensitivity 2)Large-ScalePatternsintheBackground Smalltelescopewithfidelityondegreescales →theamplitudeoflarge-scale(clustering) fluctuationsproportionaltototallightproduction 1)PhotonProductioninGalaxies Nucleosynthesis&blackholes,peaksatz~2 2)FirstStarsandGalaxies EpochofReionizationz>6 3)Intra-HaloLight largetelescopeforpointsourcesensitivity 4)Surprises? E.g.Lightfromparticledecay HST JWST •Galaxycountsmissfaintsourcesthat maydominatethereionizationbudget. •Currentgalaxycountsathigh-zarenot enoughtosustainionization. •Wemustbemissingalargefractionof theionizingflux. •IMstudiesaresensitivetothetotal luminosityemittedbyallgalaxies-> IntensityMappingoffersanadvantage. A near-IR application Asantha Cooray, UC Irvine FLARE March 2016 0.6 microns 0.75 microns 0.85 microns 1.25 microns 1.6 microns Hubble CANDELS fluctuations Mitchell-Wynne et al. 2015 Nature Communications Asantha Cooray, UC Irvine FLARE March 2016 Reionization signal in IR fluctuations Mitchell-Wynne et al. 2015 Nature Communications Asantha Cooray, UC Irvine FLARE March 2016 Galaxy Evolution 6>z Formation of First Stars: 15 > z > 6 Dark Ages: 15 > z • SPHEREx maps spectra lines over the cosmic history • Many lines detected as bright individual lines, rest blended with noise and background Spectral Line Intensity Mapping Asantha Cooray, UC Irvine FLARE March 2016 Line intensity power spectra at z~2 Measured with all pixels in the 3d spectral cube •Emissionlinesencode clusteringsignalateach redshiftovercosmichistory •Amplitudegiveslinelight production Spectral Line Intensity Mapping Asantha Cooray, UC Irvine FLARE March 2016 Multiplelinestracestarformation history -HighS/NinHαforz<3;OIII/Hβforz<2 -LyaprobesEoRmodelsforz>6 -HαandLyαcrossoverregion5<z<6 Crosscorrelationsallowawaytoreduce foregroundcontamination(whencomparedto theautopowerspectra) Asantha Cooray, UC Irvine FLARE March 2016 SPHERExwillmapLyαemission duringreionization. Hα Wemayseez~6Lyαfluctuations Lyα Atz>6SPHERExalonewillnot havesensitivityforadetection ofthepowerspectrum[for Hopkins&BeacomSFRD]. SPHEREx Spectral Line Intensity Mapping Asantha Cooray, UC Irvine FLARE March 2016 Outline • SPHEREx -> FLARE • US FLARE team • US contributions to FLARE - sciences and hardware Asantha Cooray, UC Irvine FLARE March 2016 Merger of CfA/WISH and the JPL/Caltech/UCI/Texas/Rochester groups. Two US names to the FLARE Science Board/builder management group: Asantha Cooray Giovanni Fazio Matt Ashby (CfA; IRAC/Spitzer/SPHEREx; high-z galaxies) Peter Capak (IPAC; COSMOS, Euclid - photo-z’s) Ranga Chary (IPAC; Planck, Euclid - SED modeling) Olivier Dore (JPL; Planck, SPHEREx; JPL Project Scientist for FLARE) Steven Finkelstein (Texas; Hubble/CANDELS; high-z galaxies) Joseph Hora (CfA; high-z galaxies) Gary Melnick (SPHEREx; Galactic sciences) Bahram Mobasher (Hubble; high-z galaxies/SEDs; PopIII stars) Hooshang Nayyeri (UCI; high-z galaxies) Jason Rhodes (US PI for Euclid; WFIRST Deputy Project Scientist) Howard Smith (CfA; Galactic sciences) Dan Stern (Euclid, NuSTAR - AGN sciences, high-z drop-outs) Volker Tolls (CfA; Galactic sciences) Steve Wilner (CfA; Galactic sciences) Michael Zemcov (Rochester Inst of Tech; detectors/fluctuations) Proposed US FLARE Team Asantha Cooray, UC Irvine FLARE March 2016 CfAStarFormationProjects FLAREcanreach~8magdeeperthanIRACsurveysat3.5μm,enablingthemeasurementoftheNIR SEDsofyoung(<104yrold)protostellarsources.YSOsdowntoabout0.2M shouldbeaccessibleout to>~1kpc. Clustersofembeddedprotostarsinsidedarkcoresalongthe Manyprotostarsareclusteredwithinasingle“core”astypically Afilamentseenat70-160-250 filamentasseenwithSpitzer(24-8-3.5) definedbythelargebeamofHerschelobservations. Á CfAStarFormationProjects FittingSEDS:Thelong-λfluxesfromcooldusthaveambiguousSEDfits,whilehigherspatial resolution,near-IRfluxesfromclusteredsourcesareoftenverymuchfainter.FLAREcanreach~8 magdeeperthanIRACsurveysat3.5μm,enablingthemeasurementoftheNIRSEDsofyoung(<104 yrold)protostellarsources. CfAcurrentlyisextendingtheRobitailleYSOgridcode withtheabilitytoobtainmost-likelyprotostellarcluster properties,includinglow-massstars,fromspatially IRAClimit YSO confusedSEDS(1-500μm)obtainedwithindifferentsize beams. stellar FLARElimit ThemodeledSEDofprotostarG030.894+0.138inan infrareddarkcloud(solidline;Robitaillemodel.) FLAREspectroscopywillprobearichenvironmentoftheseYSOs. 32 33 ExpectedNumberofGalaxiesDetectedbythe WISHUltra-DeepSurvery 34 GALAXY PHYSICS WIDE-FIELD SURVEYS USTHROUGH FLARE Team St even Finkels t ein - The University of Texas at Austin STATISTICAL METHODS Increasing Stellar Baryon Fractions at z > 4 Stellar Baryon Fraction 0.30 GALAXY PHYSICS Finkelstein+15a IO N AX 0.15 0.10 Finkelstein+15b 4.0 IZ I AT O YE VO LU T IO 4.5 5.0 N 50 LF+fesc=0.1 QSO Lyα Forest Madau99 + C(z) Madau99 + C=3 SF, Paardekooper, Behroozi+in prep Finkelstein+in prep 48 The large red circles denote our stepwise maximum likelihood luminosity function, 4 6 8 10 t-fit values given by the inset text. We do not use data below the determined 50% Redshift of our last data point denotes the 50% completeness limit in the HUDF. The dashed luminosity functions from the literature, as indicated in the legends. 7.0 ure 3 we also provide the abundance-matching-der magnitudes in each of ou Finkelstein masses 15c at all observed Unresolved bins. We note that in particular, our derived halo -2.0 3.2.1. Comparison to Previous Results LF+fesc(Mh) 6.5 Time Since Big Bang (Gyr) 10 5 3 2 The 1.5 1Although 0.8here we are 0.6specifically 0.5 concerned with N and 14 galaxies at z = 4, 5, 6, and 7, respectively. me0.0 masses of bright galaxies, in the right-hand pane dian stellar mass is slightly lower than in our fiducial sample, log(M∗ /M⊙ ) = 9.8, 9.8, 9.7 and 9.9 and z = 4, 5, 6 and 7, respectively. The amplitude of the redshift derivative -0.5 of the stellar baryon fraction is slightly lower, dSBF/dz = 0.0215 ± 0.0066, yet the evolution is still significant at the 3.2σ level. We conclude -1.0 that there is significant evolution in the stellar baryon fraction in that it decreases with decreasing redshift, and that this evolution is stable against several definitions of both the median stellar mass and the stellar mass -1.5 uncertainty. 51 5.5 6.0 Redshift F IG . 4.— The stellar baryon fraction (SBF) in bright (MUV = −21) galaxies from z = 4 to 7. We define the SBF as the stellar to halo mass ratio in cosmic baryon mass fraction Ωb /Ωm . We find that the SBF increases with increasing redshift, which may be responsible for the apparent lack of evo ∗ observed over this redshift range. characteristic magnitude MUV log Cosmic SFRD (M yr-1 Mpc-3) RE log Nion (s-1 Mpc-3) 0.20 0.00 52 Asantha Cooray, UC Irvine d(SBF)/dz ∝(0.031±0.009) 0.05 GA L 49 0.25 Consensus log(Mh /M⊙ ) = 11.35 atGalaxies z = 7 is ostensibely consiste recent clustering-based measure of log(Mh /M⊙ ) ≈ 1 Barone-Nugent et al. (2014). However, their halo m mate was for galaxies with MUV < −19.4, a sample a lower average luminosity than our sample, and thu Tot halo mass is expected. Our z = 4 results are consiste al RD lier clustering-basedSFestimates by Lee et al. (2006) ens z = 5 and z = 6, our derived halo ity masses are somewh than the clustering-based estimates from Lee et al. (2 Overzier et al. (2006), respectively, likely due to t luminosities considered in those works (MUV < −2 respectively). Although there are minor differences Consensus couraging that two independent methods, abundanc ing and clustering, tentatively agree on the halo m MD+14 mates at such high redshifts, though certainly the c Oesch+14 based can be made more robust at z > 6. Behroozi et al. (2013b) recently studied the evolution of Bouwens+15 the SMHM relation, by modeling all available observational -2.5 Finkelstein+15 constraints, including luminosity functions, stellar mass functions, and SFRs, and exploring McLeod+15 the galaxy evolution parameter space with an MCMC search.Oesch+13/14 They found that the SMHM -3.0 constant halo curve peaks at a roughly mass of log(Mh /M⊙ ) = 11.7 at z = 0–4. Specifically, MD+14 at z = 4, they found a peak SBF at a halo mass of log(Mh /M⊙ ) ≈ 12.0, consistent with -3.5 the typical halo mass we derive for our bright z = 4 galax3.2.2. 0 Then they went 2 on to find that 4 the 6 8 UV Luminosity 10 Scatter ies, log(Mh /M⊙ ) = 11.9. peak of the SMHM relation at z ≥ 5 occurs at a halo mass The halo mass estimates in § 3.1 did not explici Redshift steadily decreasing with redshift, log(Mh /M⊙ ) = 11.9, 11.6, the effect of the scatter in UV luminosity at a fi and 11.4 at z = 5, 6, and 7, respectively. This is very similar mass. The estimates compared the number density in ∗ to what we find for the typical halo masses of MUV galaxwith MUV < −21 to the number density in halos wi FLARE March 2016 Extendto8-10microns? • Therest-frameopticalisthemostimportantregimeto studyreionizationepochgalaxiesthroughLya,HeII, Hbeta,Halpha,[OII]and[OIII]. • Providesaccuratemeasuresofionizationparameter, dustextinction,metallicityandstellarmass • MostsensitivetoquantitieslikeIMFevolution,stellar rotation,binaryfraction,star-formationmechanismetc. (SeeEkstrometal.,Levesqueetal.) • Spitzerhaspioneeredthewaybydetectingnebular emissionfromz~6andz~5galaxiesinabroadband!The resultanthighEWarguesinfavorofahighionization parameter(Shimetal.2011,Charyetal.2005) TheSurprisingExcessinaBroadband VLT/CFHT Hubble Spitzer Halpha nebular emission: seen in 70% of 3.8<z<5 galaxies in Spitzer data Chary et al. 2005 Shim, RC, et al. 2011 37 PotentialGoalsofFLARE • UseLy-atogetopticaldepthevolutionwithztoz~15[butnote thatevensmallN_HcouldsuppressallLya]; • ObtainaBPTdiagramforz>6galaxies; • Understandwhichmechanism(binaries,IMFormetallicity)is responsiblefortheunusualobservedpropertiesof reionizationepochgalaxies; • Obtainanaccuratecensusofionizingphotonproduction (usingHbeta/OIII)modulatedoverlargescalestructureto understandifreionizationwastop-down(i.e.dominatedby big-halos)orbottom-up;inconjunctionwith21cm experiments. • Assesstheimpactoffeedbackmechanismsondifferences betweentheUVluminosityfunctionandtheopticalluminosity function–strongfeedbackcauseslargedivergenceinfaint-end slopes(e.g.Finlator,Daveetal.2012)