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HARMONI:AfirstlightspectrographfortheE‐ELT
FraserClarkeNiranjanThaAe(PI),MaAhiasTecza(IS)
SanHagoArribas,RolandBacon,RogerDavies,EvencioMediavilla,TheHARMONIconsorHum
Summary
• QuickoverviewofE‐ELT• SamplesciencecasesforHARMONI
• TechnicaloverviewofHARMONI
• Thepathahead
OverviewofE‐ELT• 42‐meterprimary
– 9841.45msegments
• FivemirrortelescopedesignwithintegratedadapHveopHcs
• 11instrumentports– Twoinstrumentsforfirstlight
• 1stlightcurrentlyplannedfor~2020– CerroArmazones,nearParanal(VLT)
http://www.eso.org/e-elt/
CerroArmazones
E‐ELTinstrumentsriseoftheIFU
• Eightinstrumentsstudiedforfeasibility(PhaseA),alongwithtwopost‐focalAOmodules;– CODEX– EAGLE– EPICS– HARMONI
– METIS
– MICADO– OPTIMOS‐EVE/DIARAMOS
– SIMPLE
5/8employIFUs
Putforwardfor1stlight
HARMONIGeneralOverview
• ProposedfirstlightgeneralpurposeIntegralFieldSpectrographforE‐ELT– Workhorseinstrumentwithwide
appeal
– Early‘highlight’scienceonkeyobjects/projects
• V‐K(0.5‐2.4µm)spectralcoverage
• R=4000,10000,20000resoluHons
• 40,20,10&4maspixelscales• 256x128pixelfieldofview
• GeneralusewithGLAOandLTAO
• PossibilitytoincludeSCAOmodeforbrighton‐axistargets.
10”x5”
COSMOSlens;Faure&Knieb
HARMONIKeyScience• Spectralcoveragefromredvisibletonear‐infrarednaturally
emphasizescoolobjects,highlyexHnctedregionsandhighztargets.
• StrongsynergieswithJWST/ALMA/VLT
• Prominentscienceareas
– Planetaryscience– Circumstellardisks
– Starformingregions
– StellarpopulaHons,IMF&GalacHcarchaeology
– BlackHolesandGalaxyCores– SNe&GRBs– Highredshikgalaxies(1<z<10)
The image cannot be displayed. Your computer may not have enough memory to open the image, or the image may have been corrupted. Restart your computer, and then open the file again. If the red x still appears, you may have to delete the image and then insert it again.
Δλ(0.47‐2.4µm)
@4mas/spx
• SpaHallyresolvedspectroscopyofz~1‐2.5ULIRGS
• Probedetailsoftheassemblyofthemostmassivegalaxies– Shocks,winds,IGM– StarformaHonmodes
– Nucleardiscsandrings– DistribuHonofdust
ScienceExample1:UnderstandingULIRGs
Courtesy:SanHagoArribas
ScienceExample1:UnderstandingULIRGs(andothergalaxies)
Courtesy:SanHagoArribas
Hαinz=2ULIRG
TimGoodsall
• Severalscales(andRs)allowsonetoopHmizeobservaHons– angularresoluHon– pointsourceandSBsensiHvity– FoV,etc.
• HARMONIproposedscales;– 4,10,20,and40mas/spx
– 0.5”x1”to5”x10”FoV
SamplingwellmatchedtokeystructuresingalaxiesacrossthehistoryoftheUniverse
CharacterisHcphysicalscaleHighresoluHoninthreedimensions
Samplingsmallerobjectsimpliessamplinglowermassobjects,whichinturnimplieshigherspectralresolu1ontounderstandkinemaHcs
Courtesy:AprajitaVerma
Scienceexample2:TesHngdarkenergyatz=4
• JWSTNIRCamimagingsurveytofindhighredshiksupernova– 50between1<z<5in10fieldsover5years(excludingevoluHon)– (E‐ELT+MICADOasanalternaHveimagingsurvey)
• HARMONIspectratogetSNtype&redshik– IFSveryusefultoremovegalaxycontaminaHonfromspectrum
30,000s(8hr)onredshik4supernova
SiIIλrest4000Å
Courtesy:IsobelHook
Alsoapplicabletostudyinghigh‐zGRBsites(c.f.LChristensentalk)
Scienceexample3:TesHngstellarmodelsatthelowestmasses
• HARMONIcanresolvesub‐stellarbinariesinnearbyclusters
• Fullthreedimensional(RA,dec,velocity)orbitalinformaHongivesdynamicalmassofthesystem
• Determinethefundamentalmass‐luminosityrelaHonshipdowntoplanetarymasses.– TestofstellarevoluHonarymodelsto
theverylowestmasses
Courtesy:RafaelRebolo
Scienceexample4:CharacterisingExoplanets
• HARMONIcontrastliesbetweenSPHERE(/GPI)andEPICS
• VerywellsuitedtomoredetailedstudyofSPHERE/GPIdiscoveries– R=1000vsR=100
– CharacterisaHon
4mas 10mas
R=400 28.25 28.57
R=4000 27.10 27.32
R=10000 26.35 26.72
HAB5‐sigmasensiHviHesfor(isolated)pointsourcesin5hours
OriginalplotfromEPICSsciencecasedocument
Equivalentto2Mjupplanetat1GyrinBaraffe2003models(10pc)
EPICS HARMONI
HARMONIAdapHveOpHcsmodes
• HARMONIisdesignedtoworkwitharangeofAOmodes;– GLAOprovidedbytelescope
• 1‐300mas,fullskycoverage
– LTAOprovidedbyATLASpackage• 8masFWHM,fullskycoverage
– SCAOprovidedbyinternalWFS• 8masFWHM,brightobjects
0
10
20
30
40
50
60
550 640 700 750 900 1250 1650 2200
S.R/FW
HM(m
as)
Wavelength(nm)
ATLASLTAOperformance
SR
FWHM_Gauss
LargeTelescopeAOisdifferentHugeFWHMdiff/FWHMseeingraHomeanslowstrehlcansHllgiveadiscernablecore.HighresoluHonmaybepossibleintovisible…
ATLASLTAOunit
HARMONISensiHvity(LTAO)
• 5‐sigmaperspectralpixelin5hours• 20masspaxelsprovidebestsensiHvityforpointsources• 40masspaxelsbestforextendedsources
ImageQuality&Throughput
• IFSimagequalityspecificaHonbreakatimageslicer;2Dimagequalitybeforeslicerand1Dimagequalityakerslicer.• Specassumes2spaxelFWHMsourceinallscales• EllipHcalpupilimpliesIQbeAerinspectraldirecHonthanspaHal
Severalinstrumentsshowingthislevelisachievable;SINFONI,PMAS,SWIFT,WiFeS,othersShouldbethenormforspectrographsnow!
ModularConstrucHonSystemblockdiagram
TheHARMONIimageslicer
• Glasspolishedde‐magnifyingimageslicerbasedonheritagewithSINFONIandSWIFT
• 32slicesineachslicereach128pixelslong– 8slicers(intotal)infourgroups
oftwo
– SlicewidthlessaggressivethanSINFONI/SWIFT
1of8
HARMONIOpHcallayout
LightfromE‐ELT
HARMONIMechanicallayout• 4.2mdiametercryostat
• ~12tonnemass
• SiyngonNaysmythplazorm–opHcalderotator
Somemorepictures
HARMONI–sideview
HARMONI–actualsize
HARMONIincontextSize,Weight&Schedule
12 tons
4.2m × 5.0m footprint
6.8 m in height
7 yr build phase
Timescales• 7‐8yeardesign/buildHmescale,aimingtomeetwithE‐ELTfirstlightin~2020
• Nextyear– Now:Proposingfor(UK)effortfundingfromSTFC
– 2011:Revisinginstrumentdesign
– 2011:De‐riskingkeytechnologies(coldK‐mirror,cryogenicshuAer)
– June2011:ESOdecisiononE‐ELTbuildphase2008 2009 2010 2011 2012 2013 2014 2015 2016 2017 2018 2019 2020 2021 2022
Phase A study
ESO selection
ESO tender
Preliminary Design
Final Design
MAIT
PAE
PAC
GTO science
FAC