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TheAthenaX-rayObservatory(anditsX-rayIntegralFieldUnit)
DidierBarretIns=tutdeRechercheenAstrophysiqueetPlanétologie
ManythankstotheAthenaScienceStudyTeam:D.Lumb,K.Nandra,X.Barcons,J.W.denHerder,A.Decourchelle,A.C.Fabian,H.Matsumoto,L.Piro,R.Smith,R.Willingale,theAthenaworkinggroupsandtopicalpanels,theX-IFU
ScienceAdvisoryTeam,andtheX-IFUConsor=um
Breakingthelimits,September21st2016,Arbatax,Italy DidierBarret
Outline
-Athenascience-TheHotandEnerge=cUniverse- Athenasciencepayload- X-rayIntegralFieldUnit(X-IFU)performanceop=miza=on
- relevantprobingsuper-Eddingtonaccre=on- Athenacurrentstatus- Conclusions
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Breakingthelimits,September21st2016,Arbatax,Italy DidierBarret
Athenascience
- Scien=fictheme:TheHotandEnerge=cUniverse
- Howdoesordinaryma]erassembleinthelarge-scalestructures?
- Tool:X-rayemi_nghotgasinclusters
- Howdoblackholesgrowandshapegalaxies?- Tool:Accre=onpoweredX-raysontocompactobjects
- Togetherwith:- Observatory science from planets, stars, supernova remnants, interstellarmedium…
- Discoveryscienceenabled inpar=cular througha fastToOcapability tostudy thetransientsky
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NeedtocombinealargeapertureX-raytelescope,widefieldimaging,high-resolu=onspectroscopyandanagilespacecrac
Breakingthelimits,September21st2016,Arbatax,Italy DidierBarret
Athenainanutshell
- SecondLarge(L)missionoftheESACosmicVision2015-2035
- Launchyear:endof2028- withthenewlydevelopedAriane6(64)
- A7tonspacecractobeplacedinaL2(L1)orbit- Unprecedentedcollec=ngareainX-rays:- 2m2at1keVand0.17m2at7keV
- 5’’angularresolu=on- Twofocalplaneinstrumentswithamovablemirrorassembly
- The Wide Field Imager (WFI) op=mized for fine imaging and brightsources
- The X-ray Integral Field Unit (X-IFU) op=mized for high-resolu=onspectroscopy
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Breakingthelimits,September21st2016,Arbatax,Italy DidierBarret
TheHotUniverse-keyques=ons
-Howdobaryonsingroupsandclustersaccreteanddynamicallyevolveinthedarkma]erhaloes?
-Whatdrivesthechemicalandthermodynamicevolu=onoftheUniverselargeststructures?
-What is the interplay of galaxy, supermassive black hole, andintergalac=cgasevolu=oningroupsandclusters?
-Wherearethemissingbaryonsatlowredshicandwhatistheirphysicalstate?
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Breakingthelimits,September21st2016,Arbatax,Italy DidierBarret
HotUniverse
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Athena X-IFUXMM-Newton EPIC PNHitomi SXS
O
Fe LMg
Fe LFe L SiS
ArCa
Fe-K
Coun
ts/s
/keV
10−4
10−3
10−2
10−1
1
Energy (keV)0.2 0.5 1 2 5
Accre=onindarkma]erhaloes ChemicalenrichmentMap gasmo=ons and turbulence to understand how baryonsaccreteandevolveinthelargestdarkma]erpoten=alwellsofgroupsandclusters.
SynthesizetheabundancesusingyieldsofvariousSNtypesandAGB stars to determinewhen the largest baryon reservoirs ingalaxyclusterswerechemicallyenriched
Simulatedvelocitymaps(courtesyofPh.Peilleetal.).E9ori,Pra9etal.(2013)arXiv1306.2322
HighresoluConX-rayspectrumofaz=1cluster.Pointecouteau,Reiprichetal(2013),arXiv:1306.2319
Breakingthelimits,September21st2016,Arbatax,Italy DidierBarret
HotUniverse
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OVII Kα
OVII Kα
OVII Kβ
NeIX Kα
OVII Kα
OVIII Kα
Resid
uals
(σ)
−12
−10
−8
−6
−4
−2
0
2
4
Energy (keV)0.4 0.5 0.6 0.7
Clusterfeedback MissingbaryonsMeasurehotgasbulkmo=onsandenergystoredinturbulencedirectly associated with the expanding radio lobes tounderstand how jets from AGN dissipate their mechanicalenergyintheintraclustermedium,andhowthisaffectsthehotgasdistribu=on
Measurethechemicalcomposi=on,density,size, temperature,ioniza=onandturbulenceofthemissing50%ofbaryonsatz<2andrevealtheunderlyingmechanismsdrivingtheirdistribu=onon various scales, from galaxies to galaxy clusters, as well asmetalcircula=onandfeedbackprocesses.
SpaCallyrevolvedhighresoluConspectroscopyofthePerseuscluster-HitomicollaboraCon(2016)
MulC-filamentWHIMabsorpConX-rayspectrumusingGRBaRerglow.Barretetal.(2016),CourtesyofF.Nicastro
Breakingthelimits,September21st2016,Arbatax,Italy DidierBarret
TheEnerge=cUniverse-keyques=ons
-Howdoearlysupermassiveblackholesform,evolveandshapetheUniverse?
-What is the role of (obscured) black hole growth in theevolu=onofgalaxies?
- How do accre=on-powered oumlows affect larger scales viafeedback?
- Howdo accre=on and ejec=on processes operate in the nearenvironmentofblackholes?
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Breakingthelimits,September21st2016,Arbatax,Italy DidierBarret
Energe=cUniverse
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Blackholegrowth Obscuredaccre=onDeterminethenatureoftheseedsofhighredshic(z>6)SMBH,which processes dominated their early growth, and theinfluenceofaccre=ngSMBHontheforma=onofgalaxiesintheearlyUniverse.
Find the physical condi=ons under which SMBH grew at theepoch when most of the accre=on and star forma=on in theUniverseoccurred(z~1-4)
FluxdistribuConofAGNsincomparisonwithmodelpredicCons.Aird,Comastrietal.(2013)arXiv1306.2325
Compton thick AGN spectrum. Georgakakis, Carrera et al., (2013 )arXiv1306.2328
Breakingthelimits,September21st2016,Arbatax,Italy DidierBarret
Energe=cUniverse
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logξ=4.2 (high state)logξ=3.9 (low state)
FeXX
VI (v
=0.3
c)
FeXX
V (v=
0.3c
)Fe
XXV
(v=0.
25c)
FeXX
V (v=
0.25
c)
Coun
ts/s
/keV
0.005
0.01
0.02
0.05
0.1
Energy (keV)7.0 7.5 8.0 8.5
Fe XXV Heα
Fe XXVI HαFe XXV Heβ Fe XXVI Hβ
Norm
alize
d co
unts
/s/k
eV/c
m2
0.02
0.05
0.1
0.2
Energy (keV)6 7 8 9
AGNoumlows Blackholewinds
Characterize ejecta, by measuring ioniza=on state, density,temperature, abundances, veloci=es and geometry ofabsorp=on and emission features of the winds and oumlowsanddeterminehowmuchenergythesecarry.
Probe oumlow proper=es and disk magne=c fields in galac=cbinaries and in the same systems determine the rela=onshipbetween the accre=on disk and its hot electron plasma.Understandtheinterplayofthedisk/coronasystemwithma]erejectedintheformofwindsandoumlows.
Simulatedultra-fastou\lowspectrum-Cappi,Doneetal2013,arxiv:1306.2330
DiskwindspectrumofthestellarmassblackholeGRS1915+105-Barretetal.2016(courtesyJ.Miller)
Breakingthelimits,September21st2016,Arbatax,Italy DidierBarret
Athenaperformancerequirements
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Parameter Value Drivingsciencegoals
Op=cs
Effec=veareaat1keV 2m2 Earlygroups,clusterentropyandmetalevolu=on,WHIM,highredshicAGN,censusofAGN,firstgenera=onofstars
Effec=veareaat7keV 0.17m2 Clusterenerge=cs(gasbulkmo=ons&turbulence),AGNwindsöows,SMBH&GBHspins
PSFHEW(<8keV) 5’’onaxis,10’’offaxis HighzAGN,censusofAGN,earlygroups,AGNfeedbackonclusterscales
X-IFU
X-IFUspectralresolu=on 2.5eV WHIM,clusterhotgasenerge=csandAGNfeedbackonclusterscales,energe=csofAGNoumlowsatz~1-4
X-IFUfieldofview 5’diameter Metalproduc=on&dispersal,clusterenerge=cs,WHIMX-IFUbackground <510-3counts/s/cm2/keV Clusterenerge=cs&AGNfeedbackonclusterscales,metalproduc=on&dispersalX-IFUcountratecapability 1mCrab80%high-resevents WHIMusingGRBacerglows
WFIWFIspectralresolu=on 150eV GBHspin,reverbera=onmappingWFIfieldofview 40’x40’ High-zAGN,censusAGN,earlygroups,clusterentropyevolu=on,jet-inducedripples
WFIcountratecapability 80%throughputat1Crab GBHspin,reverbera=onmapping,accre=onphysicsWFIbackground <510-3counts/s/cm2/keV Clusterentropy,clusterfeedback,censusAGNatz~1-4Recons.astrometricerror 1’’(3sigmas) HighzAGNs
SatelliteToOtriggerefficiency 40%inlessthan4hours WHIM,firstgenera=onofstars
Breakingthelimits,September21st2016,Arbatax,Italy DidierBarret
Observatoryanddiscoveryscience
- Solarsystembodies:suninterac=on
- Exoplanets:magne=cinterplay
- Starforma=on:browndwarfs
-Massivestars:stellarwinds
- Supernovae:explosionmechanisms
- Supernovaeremnants:shockphysics
- Interstellarmedium:composi=on
- Stellarendpoints:densema]eratsupranucleardensi=es
- Discoveryscience:unknowns
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Jupiter X-IFU
SXI
SXII
CVI
Broad OVIII Ly α
Broad OVII
OVIII Ly α
OVIII Ly β
Fe XVIII
Fe XVII
Fe and Ne
Charge exchangeSolar scattered
Norm
alize
d co
unts
/s/A
ng
0
0.1
0.2
0.3
0.4
0.5
0.6
Wavelength (Ang)10 20 30 40
Breakingthelimits,September21st2016,Arbatax,Italy DidierBarret
Payload
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OpCcs WideFieldImager X-rayIntegralFieldUnit
Light-weightSi-poreopCcs AcCvePixelSensorsbasedonDEPFETsCryogenicimagingspectrometer,basedonalargeformatofTransiConEdgeSensorscooledat50mKwithanacCvebackgroundshielding
ESA&industry ConsorCumledbyMPE(K.Nandra),withotherEuropeanpartnersandNASA
ConsorCumledbyIRAP/CNES-F(D.Barret),withSRON-NL(J.W.denHerder),INAF/IAPS-IT(L.Piro)andotherEuropeanpartners,NASAandJAXA.
Breakingthelimits,September21st2016,Arbatax,Italy DidierBarret
X-IFUperformanceop=miza=on
-Poten=alforimprovements:countrate&spectralresolu=on(1.5eV)&PSFoversampling
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TESarraybaselineconfigura=on-singlesizepixels Addi=onofaSmallPixelArray
5’equivalentdiameterfieldofview Barretetal.(SPIE2016)
Breakingthelimits,September21st2016,Arbatax,DidierBarret
X-IFUcountratecapability
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LPA 1 (in focus)LPA 2 (15 mm out of focus)LPA 2 (35 mm out of focus)SPA (in focus)
GoalReq.
Frac
tion
of h
igh
reso
lutio
n ev
ents
0
0,1
0,2
0,3
0,4
0,5
0,6
0,7
0,8
0,9
1,0
Intensity (mCrab)10−2 10−1 1 101 102
LPA 1 (in focus)LPA 2 (15 mm out of focus)LPA 2 (35 mm out of focus)SPA (in focus)
Thro
ughp
ut (H
igh+
Med
ium
res
olut
ion
even
ts)
0
0.1
0.2
0.3
0.4
0.5
0.6
0.7
0.8
0.9
Intensity (mCrab)10 100 1000
Frac=onofhighresolu=onevents(2.5eV) Throughputforhighandmidresolu=onevents(<3-4eV)
1mCrab=95cps/s(overthewholedetectorarray) Barretetal.(SPIE2016)
Brightsources
Breakingthelimits,September21st2016,Arbatax,Italy DidierBarret
Effec=vearea=spectroscopiccapabili=es
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X-IFUEPIC PNSXSNuSTAR
x 15
x 10x 100
Effec
tive
are
a (c
m2)
101
102
103
104
Energy (keV)1 10
Effec=veareacomparisonbetweenX-IFUandotherfacili=es
Breakingthelimits,September21st2016,Arbatax,Italy DidierBarret
Effec=vearea=spectroscopiccapabili=es
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Athena X-IFUHitomi SXSGratings
Figu
re o
f m
erit
(m k
eV-1
/2)
0
5
10
15
20
25
Energy (keV)1 10
Figureofmeritforspectroscopymeasurements
Breakingthelimits,September21st2016,Arbatax,Italy DidierBarret
Spectroscopiccapabili=es
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X-IFU simulated spectrumXSTAR based model of NuSTAR data
NGC 1313 X-1 X-IFU 100000s
Phot
ons/
s/ke
V/c
m2
5×10−5
0.0001
0.0002
Energy (keV)1.0 1.5 2.0
X-IFU simulated spectrumXSTAR based model of NuSTAR data
NGC 1313 X-1 X-IFU 100000s
Phot
ons/
s/ke
V/c
m2
5×10−6
10−5
2×10−5
Energy (keV)7 8 9
8.8keVabsorp=onlineinNGC1313X-1seenbyXMM-NewtonandNuSTAR-Rela=vis=coumlowFeXXV(6.67keV,0.25c)orFeXXVIKα(6.97keV,0.2c) BroadbandspectroscopiccapabilityofX-IFU
Waltonetal.(20
16)
Breakingthelimits,September21st2016,Arbatax,Italy DidierBarret
CurrentstatusofAthena
-MissionConsolida=onReview(May2016)concludedthat:
- Thetwomissionsconceptsstudied(smallandlargemirrors)aresound
- Theinstrumentswitchingmechanismisthroughamovablemirrorassembly
- OffersalsodefocussingtoincreasetheX-IFUcountratecapability- Theinstrumentresourcesarechallenging:allbeingaddressedorfixed
- ThemassliccapacityofAriane64upto7tons
- Consolida=onof thecostatcomple=on is required (transferof focalplanemoduletotheinstrumentconsor=a,firmingupinterna=onalcontribu=ontothemissionandsomepayloadelements,industrialcosts,…)
- Missionconcepttobecarriedoverconsidersthelargemirror
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Breakingthelimits,September21st2016,Arbatax,Italy DidierBarret
Conclusions
- Athenawill providebreakthrough capabili=es inwidefield imagingandhighresolu=onX-rayspectroscopy
- Athenafeasibilitystudiesareprogressingwell- Thelargemirrorconfigura=onisthebaselinefortheupcomingstudyphase
- Instrument baseline designs are being consolidated with no degrada=on ofperformanceuptonow
- JointheAthenacommunityandsupportthemission
- X-IFUwillbeapowerfultooltostudysuper-Eddingtonaccre=on:- disk coronae, winds, rela=vis=c oumlows, surrounding materials thus enabling toconnect accre=on physics to feedback process across the broad mass scale ofcompactobjects
- SeemorefromC.Pinto,M.Middelton
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Breakingthelimits,September21st2016,Arbatax,DidierBarret
Holdonandthankyouforyoursupport
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X-IFU - Perseus core
Phot
ons
m-2
s-1
keV
-1
10
100
1000
Energy (keV)0.5 1 2 5
10
100
6.5 7.0
500
1000
1.0 1.2
Fe complex
Al, Si, SνF
ν200
500
Energy (keV)0.2 0.5 1
200
400
0.25 0.30
Thewealthofinforma=onprovidedbysuchaspectrum,thatwillbemeasuredonsub-arcminutescalesenablesindepthstudiesofthe physical proper=es of the hot cluster gas (e.g. temperature,density,turbulence,bulkmo=on,abundance,...)
High-zGRBacerglowsprobingtheISMcomposi=onatz>7-10andtracing the first genera=on of stars to understand cosmic re-ioniza=on, the forma=on of the first seed black holes, and thedissemina=onofthefirstmetals.
PerseuscoreX-IFUsimulatedspectrumbasedonHitomi-ModelcourtesyofC.PintoandA.Fabian Barretetal.(2016)-CourtesyofL.Piro