CCAT-prime

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FrankBertoldiBonnUniversity

CMBinGermany-Garching31Januray2018

CerroChajnantorAtacamaTelescope

v.31.1.

An Extreme Field-of-View Submillimeter Telescope

CCAT-Prime 2

Ahighsurfaceaccuracy,highthroughput6maperture,submm(0.2-3mm)telescope

fordedicatedsurveys

WhatisCCAT-prime?

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2003 PartnershipworkshopPasadena2004 MoUCaltech,JPL,Cornell2005 projectoffice2006 feasibilitystudyreview2007-9siteselecTon,joiningColorado,Cologne/Bonn,AUI,Canada2010 astro2010recommendaTon2011 -14EngineeringDesignPhase(NSF-supported):referencedesign2013EDPexternalreview2013-15NSFMSIPproposalsfail;Caltech,Coloradoleave2015 MTM,Vertexprovidedturn-keydesignstudies&pricing2016 CCATterminated,CCAT-primeborn

CerroChajnantorAtacamaTelescope

Manydocuments:sciencecase&requirements,instrumentrequirements,designstudiesforsub-systems…

25mFoV30‘<15µmsurface

CCAT-Prime 4

WhoisCCAT-prime?

•  CornellUniversity,Director:TerryHerter•  Germanconsor=umUniv.Cologne&Univ.Bonn

–  joining:LMU(Mohr),MPA(Komatsu)

•  CanadianUniversityconsor=um–  Waterloo,Toronto/CITA,BriTshColumbia,Calgary,

Dalhousie,McGill,McMaster,WesternOntario•  ChileanUniversitycollaborators

–  U.Chile,PUC,UCSC,UDP,andothers•  Prime-Camcollaborators

–  U.Michigan,NIST,Stanford/SLAC,CardiffU.,andothers

UniversityconsorTumwithstrongemphasisontraining&development

Fundedby:privatedonorandCornelluniversityDFGGroßgeräte,Univ.Köln&Bonn,SFB956(CHAI)

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CerroChajnantor

CerroToco

ALMAOSF

NANTEN2ASTE

APEX

Licancabur

CerroElChascón

Licancabur5920mToco5604mChajnantor5639mElChascon5703m

ACTPasoJama

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7

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CerroChajnantor

IMWorkshopII,JohnsHopkins 912June2017

CerroChajnantorpeakat5640m

TAO CCAT-p

TAO will be a 6.5m infrared-optimized telescope on the summit of Cerro Chajnantor, promoted by the Institute of Astronomy (IoA), the University of Tokyo & other Japanese facilities incl. the National Astronomical Observatory, ISAS/JAXA, and the University of Chile.

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Whybothermovingtothepeak?

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CCATvs.ALMAsites:medianH2O0.6vs.1mm,τ(350µm)=1.1vs.1.7⇒factorof2insensi-vity

CCAT

5100misgood,5600misbener!

SubmillimetersensiTvityisallaboutatmospherictransmission.

MKeaSPoleALMACCAT

Radford&Peterson,arXiv:1602.0879Cortes,Reeves,Bustos,arXiv:1609.01252

CerroChajnantor

ALMAPlateau

MedianZenithTransmission

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CCATmediantransmissionbenerthanSPduetowarmer,

lessdenseatmosphere.Drawback:δTB

450µm

CCAT5600mSPole2650mALMA5000mMKea4100m

350µm

ChajnantorSiteopensupTHzWindows

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250–200µm

CCAT10%25%50%ALMA50%MKea50%

τ<1

Crossed-DragoneOpTcsDesign

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P-camBeam7opTcstubereceiver

ConceptbyC.Dragone1978Usedin“smallaperture”CMBexperiments(QUIET,AtacamaB-ModeSearch,QUIJOTE)Designsfor“largeapertures”tomaptheCMB~10xfaster(Niemack2016,AppliedOpTcs)WorkingwithSimonsObservatoryontelescopeandreceiveropTcsdesigns6maperturecoma-correctedf/2.6designforbothprojects(Parshley,Hills,Mauskopf,Dicker,Gallardoandothers)

highthroughput,8degfield-of-view,flatfocalplane,zerogeometricblockage

tote

lescop

e

Lyotstop(FPIforspectrometer)

OpTcstubeinstrumentmodule

Siliconlenses 20cmfilters

Detectorarray3-waferarraysin45cmopTcstubes

window

Prime-Cam

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•  7instrumentmodulesor“opTcstubes”populatedwithTES/KIDarrays

•  EachtubeFoVupto~1.3degree•  Moduldesignunderdevelopment

withSimonsObservatoryenablesupgrades

Planforfirst3op=cstubes:2broadband(bb)onespectrometer(sp)

firstlightcamera

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•  Feedhorn-coupledmulTchroicTESarrayswith4bandsperfeedhorn:740,860,1100,1300µm

•  FeedhorncoupledMKIDarrayat350µm(NIST)

•  3x15cmfeeddetectorarraysTledineachopTcstube

Danaetal.2016

DetectorconceptforPrime-Cam

3-waferopTcstube

(withNIST,Michigan,Stanford/SLAC,andothers)

Heritage:AdvancedACTPolBLAST-TNG

Fabry-PerotInterferometerforIntensityMapping

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Heritage:FPIat112µmforHIRMESonSOFIA

17January2017

Scan185-440GHzrangein4bandsacross~1deg2peropTcstubesimultaneously

!  [CII]158µmatz=3.3-9.3!  [OIII]88µmatz>6.7!  CO2-1andhigheratvirtuallyanyz

CCAT-Prime

FPIforspectrometeratPrime-CammoduleLyotstop

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•  Heterodyne,dualfrequencyarray•  500GHz(600μm)and850GHz(350μm):CO4-3,7-6[CI]2-1,1-0•  64pixels(baseline),128pixels(goal)ineachband

GalacTcEcologyinstrument:CCATHeterodyneArrayInstrument“CHAI”

Graf,Stutzkietal.

Dichroicspliner

17January2017 CCAT-Prime

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Shutter

Mirrors M1 & M2

Elevation Housing

Yoke Structure

Support Cone

Subordinatereceivermount

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Crossed-DragoneOpTcsDesignhighthroughput,8degfield-of-view,flatfocalplane,zerogeometricblockagetelescopeemissivity<2%,totalsystememissivity<7%

coma-correctedf/2.6with5.5mfreeaperture

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1

Shutter

Mirrors M1 & M2

Elevation Housing

Yoke Structure

Support Cone

CCAT-prime designedandbuiltbyVertexAntennentechnikGmbH,Duisburg

4x5minstrumentspaceca.300t,9pieces

preassemblyinDuisburg

CCAT-primeSchedule

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Telescope:4yearconstruc=on(6/2017to6/2021)-  20monthsdetaileddesign-  13monthsfabricaTonincl.trialassemblyinDuisburg-  3monthsshipping&receiving-  12monthsassembly/checkoutCamerasunderdesign&construcTon,$€sTllbeingraised(NSF:MSIP,DFG:SFB,...)Possiblepla_ormforCMB“StageIV”surveyinfutureProjecthasstarted,buts0llwelcomesnewpartners.

www.ccatobservatory.org

CCAT-Prime 3217January2017

Prime-Cam

CCAT-Prime 3317January2017

CCAT-Prime 3417January2017 M.Viero

IntensityMappingof[CII]throughoutEoR

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Measurelarge-scalespaTalfluctuaTonsoffaintgalaxiesvia[CII]158µmline.

RevealstheprocessofreionizaTonandtheunderlyingdarkmanerdistribuTonoverthecosmicTmewhenthefirstgalaxiesformed.Understand topology & timescale of reionization, i.e., how and when galaxies first formed, the properties of sources of reionization.

Inverseview:combinewith21cmHI,tracingneutralISMconcentra=ons.

ResoluTonintoindividualgalaxiesnotrequired.Clusteringscale0.5-1Mpc(1-2’)atz=3.5-9,goodmatch:40”@1mm,R~400,16sqd

f(H0) ~ 1 f(H0) ~ 10-5

z ~ 12 to 5

Poten=alfornon-Gaussianitysearchesinfuture?

CCAT-Prime 3717January2017 B.Magnelli

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1.  MusttraceFIRat350µm2.  LargerCCAT-paperture

pushesHerschelconfusionlimitsdownby~3

3.  Need~100sqdsurveytobeatvariance.

CCAT-p

ObscuredSFoverCosmicTime

!TrackgalaxyevoluTonduringthemostacTveepochofstarformaTon.

CCAT-p Herschel

CCAT-Prime 3917January2017

A.Mi=alJ.ErlerN.Ba=aglia

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CCAT-pclusterSZoutlook

"  The spectral coverage of of CCAT-pwill be similar to Planck HFI,withroughly5-15TmesbenersensiTvity(notat860GHz),allowingseparaTonofSZeffects,dust,andforegrounds.

"  CCAT-primewill be the first SZ survey experiment to provide kSZandrSZmeasurementsinlargesamples(>100)ofclusters,-  to enable cosmological modeling with direct kSZ number

counts,ratherthanpairwisekSZ.-  throughrSZ temperaturemeasurementsprovide independent

masscalibraTonofclusters,acrucialingredientforcosmology.

"  WithoutPRISM,COrE,PIXIE:CCAT-pistheuniqueopportunity.

GEco:GalacTcEcologyScience

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•  15”imagingover200sq.deg.scalesoftheMilkyWay,LMC,SMCtostudy:–  Massbudget:[CI]tracinggastemperatureandmass–  TurbulentdissipaTon:mid-high-JCO&13COtracinggasexcitaTon,shocks

•  Tracingvariableflowofgasintocoresandyoungstars

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•  Uniquesiteenablesuniquescience•  NoveltelescopedesignmaximizessurfacebrightnesssensiTvity.ExtraordinarythroughputopTmalforlarge-areasurveyscience

•  Pavingtheroad&loweringriskforalarge-aperturesubmmtelescope(atthesamesite?)

hnps://www.eso.org/sci/meeTngs/2018/AtLAST2018.html

Effortstobuilda25-50-metersubmillimetertelescope!

Lookingahead: