the athena x-ray observatory - github pages · breaking the limits, september 21st 2016, arbatax,...

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

2


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

3

NeedtocombinealargeapertureX-raytelescope,widefieldimaging,high-resolu=onspectroscopyandanagilespacecrac


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

4


TheHotUniverse-keyques=ons

-Howdobaryonsingroupsandclustersaccreteanddynamicallyevolveinthedarkma]erhaloes?

-Whatdrivesthechemicalandthermodynamicevolu=onoftheUniverselargeststructures?

-What is the interplay of galaxy, supermassive black hole, andintergalac=cgasevolu=oningroupsandclusters?

-Wherearethemissingbaryonsatlowredshicandwhatistheirphysicalstate?

5


HotUniverse

6

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


HotUniverse

7

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


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?

8


Energe=cUniverse

9

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


Energe=cUniverse

10

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)


Athenaperformancerequirements

11

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),AGNwinds&oumlows,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


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

12

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


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.


X-IFUperformanceop=miza=on

-Poten=alforimprovements:countrate&spectralresolu=on(1.5eV)&PSFoversampling

14

TESarraybaselineconfigura=on-singlesizepixels Addi=onofaSmallPixelArray

5’equivalentdiameterfieldofview Barretetal.(SPIE2016)

Breakingthelimits,September21st2016,Arbatax,DidierBarret

X-IFUcountratecapability

15

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


Effec=vearea=spectroscopiccapabili=es

16

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


Effec=vearea=spectroscopiccapabili=es

17

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


Spectroscopiccapabili=es

18

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)


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

19


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

21

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

the athena x-ray observatory - github pages · breaking the limits, september 21st 2016, arbatax,...

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