High Energy Astrophysics in the Next Decade 1 June 2006 From INTEGRAL to SIMBOL-X F. Lebrun CEA-Saclay SAp/APC

High Energy Astrophysics in the NexHigh Energy Astrophysics in the Next Decadet Decade

11June 2006June 2006

FromFrom INTEGRAL INTEGRAL toto SIMBOL-X SIMBOL-X

F. Lebrun

CEA-SaclaySAp/APC

June 2006June 2006 High Energy Astrophysics in the Next DecadeHigh Energy Astrophysics in the Next Decade 22

INTEGRAL: a European gamma-ray observatoryINTEGRAL: a European gamma-ray observatory

SPI – The gamma-ray SPI – The gamma-ray Spectrometer of Spectrometer of INTEGRAL. Excellent INTEGRAL. Excellent spectra, good imagesspectra, good images

IBIS – The gamma-IBIS – The gamma-ray Imager onboard ray Imager onboard the INTEGRAL the INTEGRAL satellite. Excellent satellite. Excellent Imaging, good Imaging, good spectraspectra

ISGRIISGRI – the IBIS – the IBIS low energy low energy camera (CdTe)camera (CdTe) Perigee: 10,000 km,

Apogee: 150,000 km

Launch: October 2002

Operations funded Operations funded till end 2008till end 2008


511 keV bulge ~ 8°(Knödlseder et al., 2005)

1043 e+/s !Light dark matter ?

Point sources > 85%(Lebrun et al., 2004, Strong et al., 2005, Bouchet et al.,

2005)

Positronium ~ 92%(Jean et al., 2005

Weidenspointner et al., 2006)

60Fe(Harris et al., 2005)

26Al(Diehl et al., 2006)

GALACTIC DIFFUSE EMISSIONGALACTIC DIFFUSE EMISSION


• More than 200 sources detected with ISGRI More than 200 sources detected with ISGRI

(Bird et al., 2005)(Bird et al., 2005)

• 55 sources are new and heavily absorbed 55 sources are new and heavily absorbed

(N(NHH~ 10~ 102323 cm cm-2-2). ).

• HMXB population doubled HMXB population doubled

(mostly pulsar+supergiant companion)(mostly pulsar+supergiant companion)

• IGR J17456-290IGR J17456-290:: A steady non-thermal source near the GCA steady non-thermal source near the GC

• IGR J00291+5934IGR J00291+5934:: Fastest ms pulsar (P=1.67 ms), pulsed Fastest ms pulsar (P=1.67 ms), pulsed fraction increases with energyfraction increases with energy

• 4444Ti linesTi lines detected in the Cas A spectrumdetected in the Cas A spectrum

• MagnetarsMagnetars: very hard spectrum: very hard spectrum

POINT SOURCESPOINT SOURCES


Conclusions about ISGRI/CdTeConclusions about ISGRI/CdTe• No failure in 44 months of flight operationsNo failure in 44 months of flight operations• Noisy detectors: only 3%Noisy detectors: only 3%• PerformancesPerformances

– Sensitivity: milliCrab (3Sensitivity: milliCrab (3σ, tσ, tobsobs= = 1 day, 1 day, ΔE=E)ΔE=E)– Actual lower threshold: 15 keVActual lower threshold: 15 keV– Spectral performance is nominal Spectral performance is nominal

• 9% at 60 keV9% at 60 keV• 5% at 511 keV5% at 511 keV

– Spectral performance degradationSpectral performance degradation: : • ~ 2.6 % / year (factor 2 in 20 years)~ 2.6 % / year (factor 2 in 20 years)• 0.7 % after the November 2003 giant solar flare0.7 % after the November 2003 giant solar flare

CdTe/CdZnTe is confirmed as the X/gamma-ray CdTe/CdZnTe is confirmed as the X/gamma-ray detector for tomorrow space astrophysicsdetector for tomorrow space astrophysics


CNES calls for proposalsCNES calls for proposals

Selected for a phase A study (on-going)Selected for a phase A study (on-going)

• Micro satellites:Micro satellites: ECLAIRsECLAIRs

devoted to GRB study launch: 2011devoted to GRB study launch: 2011

• Formation flight:Formation flight: SIMBOL-XSIMBOL-X

Focusing hard X-rays launch: 2013Focusing hard X-rays launch: 2013

Final selection next yearFinal selection next year


Multiwavelength study of Multiwavelength study of Gamma-Ray Burst prompt emissionGamma-Ray Burst prompt emission

ECLAIRsECLAIRsFrance-ChinaFrance-China

SVOM payloadSVOM payload

Gamma-ray telescopeGamma-ray telescopeX-ray telescopeX-ray telescope

Optical telescopeOptical telescope


ECLAIRECLAIRSS: The X and Gamma Camera (CXG): The X and Gamma Camera (CXG)

Wide field of view (Wide field of view (~2 sr~2 sr) coded mask telescope encircled by a graded) coded mask telescope encircled by a graded

DetectDetectionion plane ( plane (DPIXDPIX) made of 200 XRDPIX modules developed) made of 200 XRDPIX modules developed

Array of CdTe Array of CdTe detectorsdetectors

XRDPIXXRDPIXmodulesmodules

Useful area 1024 Useful area 1024 cmcm22

Spectral band Spectral band 4.0 to 250 keV4.0 to 250 keV

100 GRB/year100 GRB/year40 cm40 cm

38 cm38 cm

52 cm52 cm

in the framework of CNES/CESR and CNES/CEA R&D programsin the framework of CNES/CESR and CNES/CEA R&D programs

shield collimator to reduce the cosmic diffuse induced backgroundshield collimator to reduce the cosmic diffuse induced background


CXG Anticipated PerformancesCXG Anticipated PerformancesC

ount

s

100

200

300

0

Energy (keV)10 40 605020 30

3.5 keV

The position on the sky of all The position on the sky of all GRBs detected with a signal to GRBs detected with a signal to

noise ratio greater than 5.5 will be noise ratio greater than 5.5 will be given with an accuracy given with an accuracy ~10′~10′

GRB 030227

20°

5h

Crab Nebula

INTEGRAL

Sen

sitiv

ity (

ph c

m-2 s

-1)

10

Peak energy (keV)100 100010

1

SWIFT

ECLAIRs


SIMBOL-XSIMBOL-X

0.5 – 80 keV0.5 – 80 keV

0.1–10 keV0.1–10 keV 15 keV-10 MeV15 keV-10 MeV

Focusing hard X-rays Focusing hard X-rays using formation flight technologyusing formation flight technology


Participating Participating laboratorieslaboratories

F : F : CEA/Saclay, CESR/Toulouse, APC/Paris, CEA/Saclay, CESR/Toulouse, APC/Paris, LAOG/Grenoble, Obs.Paris/MeudonLAOG/Grenoble, Obs.Paris/Meudon

It :It : (INAF :) O.A.Brera, Roma, Palermo, (INAF :) O.A.Brera, Roma, Palermo, IASF Milano, Bologna IASF Milano, Bologna

D : D : MPE Garching, I.A.A.TübingenMPE Garching, I.A.A.Tübingen

• End ‘01 :End ‘01 : First ideas & discussions CEA/Saclay & O.A.BreraFirst ideas & discussions CEA/Saclay & O.A.Brera• End ‘03 : End ‘03 : CNES call for ideas for formation flight…CNES call for ideas for formation flight…• Mid ‘04 : Mid ‘04 : Selection of 4 missions for an assessment phaseSelection of 4 missions for an assessment phase• End ‘05 :End ‘05 : Only Simbol-X is recommended for a phase A studyOnly Simbol-X is recommended for a phase A study

Short historyShort history


Simbol-X basicsSimbol-X basics

Focusing opticsCoded mask optics

Have the XMM angular resolution and sensitivity Have the XMM angular resolution and sensitivity in the INTEGRAL/ISGRI energy rangein the INTEGRAL/ISGRI energy range

INTEGRAL > 15 keV XMM < 10 keV

30 degrees30 degrees 30 arcmin30 arcmin


Major science goalsMajor science goals

Accreting Black HolesAccreting Black Holes

Physics in single objectsPhysics in single objects

Census in UniverseCensus in Universe

Particle Particle accelerationacceleration

Mechanisms ?Mechanisms ?

Maximum energy ?Maximum energy ?


• Record of Super Massive Black Record of Super Massive Black Holes accretion activityHoles accretion activity

•• Constraints to models for the Constraints to models for the formation and evolution of formation and evolution of structures in the Universestructures in the Universe

About 50 % resolved in sources in the 7–10 keV band

Accreting Black HolesAccreting Black HolesCensus of Super Massive Black HolesCensus of Super Massive Black Holes

But less than a few % resolved But less than a few % resolved beyond 10 keV, beyond 10 keV,

at the emission peak !at the emission peak !

CXB models : major contribution from CXB models : major contribution from obscured AGNs, but parametres are not obscured AGNs, but parametres are not constrained (evolution, energy cut-off, constrained (evolution, energy cut-off, absorption)absorption)

Need : resolve > 50 % of CXB in the [20-40] keV bandNeed : resolve > 50 % of CXB in the [20-40] keV band-> sensitivity, angular resolution, field of view-> sensitivity, angular resolution, field of view


Simbol-X : understand SgrA* and its environmentSimbol-X : understand SgrA* and its environment

Simbol–X, 300 ks,

> 10 keV 10x10 arcmin2XMM-Newton

INTEGRAL/IBIS/ISGRI

Simbol-X3 , 1 hour


Acceleration : link with HESS sourcesAcceleration : link with HESS sourcesprotons in SNRs shocks ?protons in SNRs shocks ?

G347.3-0.5 - HESS @ TeV

With Simbol-X :With Simbol-X :• • mapping of the synchrotron emission, mapping of the synchrotron emission, • • determination of spectral break with X-ray alone determination of spectral break with X-ray alone • • correlation with GeV and TeV emissionscorrelation with GeV and TeV emissions

SX

SN 1006SN 1006

Simbol-X : Simbol-X : E > 10 keVE > 10 keV

100 ks 100 ks 10’x15’10’x15’


Nucleosynthesis : measure Nucleosynthesis : measure 4444Ti yieldTi yield4444Ti : explosive nucleosynthesis product Ti : explosive nucleosynthesis product Period of 85 yearsPeriod of 85 yearsLines (Lines (4444Sc) at 68 and 78 keVSc) at 68 and 78 keV

Detected only in CasA (so far), by Detected only in CasA (so far), by BeppoSAX and INTEGRALBeppoSAX and INTEGRAL

10 a

rcm

in

100 ks

Map Cas A Map Cas A emissionemission

Simbol–X 44Ti map

Measure 1987A yieldMeasure 1987A yield

Spectrum 1 arcmin2

Measure Measure velocityvelocity


And a lot more…And a lot more…

• Quiescence : physical processes at low accretion rate, « ADAF », Quiescence : physical processes at low accretion rate, « ADAF », jets ?jets ?

• Difference between accreting neutron stars and black holes ?Difference between accreting neutron stars and black holes ?

• Follow and characterize the change of states on their evolutionary Follow and characterize the change of states on their evolutionary timestimes

• Local group population ?Local group population ?Absolute luminosity, localisationAbsolute luminosity, localisationhard X-ray spectrum : population characterization, comparison with hard X-ray spectrum : population characterization, comparison with Milky Way Milky Way

• Intermediate Mass Black Holes: ULXs characterization, spectrum Intermediate Mass Black Holes: ULXs characterization, spectrum and QPOs (and QPOs ( BH mass measurement) BH mass measurement)

• Cyclotron linesCyclotron lines

• Non thermal cluster emissionNon thermal cluster emission

• Young Stellar ObjectsYoung Stellar Objects

• Gamma-ray bursts follow upGamma-ray bursts follow up


Simbol-X scientific requirementsSimbol-X scientific requirements

Energy band : Energy band : ~ 0.5 to > 80 ~ 0.5 to > 80 keVkeV

ΔΔE : < 150 eV @ 6 keV (Fe Ka)E : < 150 eV @ 6 keV (Fe Ka) < 1.3 keV @ 68 keV (< 1.3 keV @ 68 keV (4444Ti)Ti)

ΔΔ q : < 20 arcsec HPD q : < 20 arcsec HPD FOV : > 9 arcminFOV : > 9 arcminAttitude reconst. : ± 2 arcsecAttitude reconst. : ± 2 arcsec

ΔΔ t : < 100 microsecondest : < 100 microsecondes

Duration : 3 yearsDuration : 3 yearsOver 1000 targets possibleOver 1000 targets possible

Large effective area, excellent angular resolution, Large effective area, excellent angular resolution, very low backgroundvery low background

Sensitivity [1 Ms, 3 Sensitivity [1 Ms, 3 ] :] :1010-8-8 ph/cm ph/cm22/s/keV up to /s/keV up to ~ 80~ 80 keV keV1010-14-14 erg/cm erg/cm22/s [20-40 keV] (1 mCrab)/s [20-40 keV] (1 mCrab)


OpticsOptics

Focal length :Focal length : 20 - 30 m20 - 30 mShell diameters :Shell diameters : max 70 cmmax 70 cmShell thickness : 0.1 Shell thickness : 0.1 -- 0.3 mm 0.3 mmNumber of shells :Number of shells : ~ ~ 100100

• Heritage from XMM–Newton : nickel shells obtained by electroforming Heritage from XMM–Newton : nickel shells obtained by electroforming replication method; low mass obtained via a reduced thickness of shellsreplication method; low mass obtained via a reduced thickness of shells

• Coating : multi-layer Pt/C needed for requirement on large F.O.V. and on Coating : multi-layer Pt/C needed for requirement on large F.O.V. and on sensitivity up to > 80 keVsensitivity up to > 80 keV

Mirror parameters Mirror parameters to be optimized in phase Ato be optimized in phase A

Grazing incidence : Grazing incidence : Emax Emax 1/ 1/θθ Focal Length Focal Length


The focal detector assemblyThe focal detector assembly

Low energy detector (450 mm Silicon)Low energy detector (450 mm Silicon)(see L. Strüder talk on Friday)(see L. Strüder talk on Friday)

High energy detector (2 mm Cd(Zn)Te)High energy detector (2 mm Cd(Zn)Te)

Required parametRequired parameteersrs

• • Spectro-imaging system 0.5-100 keV Spectro-imaging system 0.5-100 keV

• • Pixel size ~ 500 mm (PSF oversampling)Pixel size ~ 500 mm (PSF oversampling)

• • Full size : 8x8 cm2, 128x128 pixelsFull size : 8x8 cm2, 128x128 pixels

• “• “Room temperature” operations (Room temperature” operations (~ -30°C)~ -30°C)

• • Fast reading (used in anticoincidence)Fast reading (used in anticoincidence)

Active anticoincidence shieldActive anticoincidence shield


Phase 0 result (CNES) : orbit pointing & stabilizationPhase 0 result (CNES) : orbit pointing & stabilization

20°

Sun

eclipticplane

sky area visible

at any moment 35%

360°

4,5 months

Transfer orbit

Increase of

perigee

orbital period

correction

High elliptical orbit : 44,000 - 256,000 km at launch

Orbit constraints : Orbit constraints : - have formation flight feasible (> - have formation flight feasible (> ~ 20,000 ~ 20,000 kkm)m)- minimize background (science > 75,000 km)- minimize background (science > 75,000 km)

Pointing : XMM / INTEGRAL typePointing : XMM / INTEGRAL typefixed solar panelsfixed solar panelssimplified thermal controlsimplified thermal control

Formation flight rFormation flight requirements : equirements : ± 10 cm along telescope axis± 10 cm along telescope axis± 1 cm perpendicular, knowldege @ ± 0.5 mm± 1 cm perpendicular, knowldege @ ± 0.5 mm


Phase 0 study (CNES) : detector spacecraft

COLLIMATOR

ISL back antenna

detectionradiatorand associatedheat pipe

lateralsensor

ISL antennas

fine SSTtowards -X

Detection payload


Phase 0 study (CNES) : mirror spacecraft

sun baffleISL back antenna

D=3m sky screen

thermal baffle

Wolter-I Mirror


Phase 0 study (CNES) : launch configuration

Launched as a composite under Soyuz

fairing

Masses

Detector S/C : ~ 600 kgMirror S/C : ~ 1300 kgAdapter : ~ 150 kg

Launcher capability :2.2 tons (5 deg incl.)


Status - scheduleStatus - schedule

• Simbol-X in phase A, conducted jointly by CNES & ASI, with the participation of MPE-IAAT

• Other partners are possible• End of phase A review : 2nd quarter 2007• Launch date : mid 2013

• Operations for three years (2 years of science observations)• Observation program will be composed of :

- a “core program”, with main priority science targets- and a guest observer program open to the community


Detector/Electronics requirementsDetector/Electronics requirements

• SIMBOL-X requirements:SIMBOL-X requirements:– Spatial resolution: 500 Spatial resolution: 500 μ μ small pixels small pixels– Spectral resolution: 1.3 keV @ 68 keV Spectral resolution: 1.3 keV @ 68 keV small pixels small pixels– Energy range: 10 – 100 keVEnergy range: 10 – 100 keV

• ECLAIRS CXG requirements:ECLAIRS CXG requirements:– Spatial resolution: 4 mmSpatial resolution: 4 mm– Energy range: 4 – 250 keVEnergy range: 4 – 250 keV

Front-end electronics :Front-end electronics :• - multi-channels ASIC / DC coupling - multi-channels ASIC / DC coupling • - Ultra low noise (< 40 e- RMS for stand alone chip)- Ultra low noise (< 40 e- RMS for stand alone chip)• - self triggered- self triggered• - Multiple event capabilities- Multiple event capabilities• - Low power, radiation tolerant, … as usual !- Low power, radiation tolerant, … as usual !

High Energy Astrophysics in the NexHigh Energy Astrophysics in the Next Decadet Decade

2828June 2006June 2006

High Energy DetectorArrays of Cd(Zn)Te with integrated ASICs

Tests of pixellatedCd(Zn)Te matrices

256 pixels CZT array 256 pixels CZT array 6 mm thick (eV-Products)6 mm thick (eV-Products)

256 pixels Schottky array 256 pixels Schottky array 0.5 mm thick (ACRORAD)0.5 mm thick (ACRORAD)

ASICs development (IDeF-X Vx.x)

Hybridization


« Flat » prototype / CZT + IDeF-X V1.0« Flat » prototype / CZT + IDeF-X V1.0


ISGRI : CdTe Pt/Pt : 4x4x2 mm3 / 120V / 0°C

5.6 keV FWHM2001

From ISGRI … 2001 to 2005From ISGRI … 2001 to 2005

ECLAIRS IDeF-X V1.0: CdTe In/Pt 4x4x1 mm3 / 600V / 24°C

1.8 keV FWHM2005

R&T IDeF-X V1.0 : CdTe In/Pt 2x2x0.5 mm3 / 340V / 24°C

1.1 keV FWHM(0.9 keV right side)0.73 keV FWHM

at 13.9 keV2005


ConclusionsConclusions• Current Results:Current Results:

• New low noise electronics under development for high resolution spectro-imaging New low noise electronics under development for high resolution spectro-imaging • 35 e35 e-- RMS achieved without detector RMS achieved without detector• 66 e66 e-- RMS achieved with a detector (330V, RT, dark current < 10 pA) RMS achieved with a detector (330V, RT, dark current < 10 pA)• « Flat » prototypes of 64 pixels 900µm, 1mm pitch used for evaluation and « Flat » prototypes of 64 pixels 900µm, 1mm pitch used for evaluation and

characterization of detector arrays characterization of detector arrays • CZT, CdTe and CdTe SchottkyCZT, CdTe and CdTe Schottky

• 0.5, 1 and 2 mm thick detectors are studied0.5, 1 and 2 mm thick detectors are studied

• 4 keV Low threshold value accessible with 4x4x1 Schottky detectors (600V / -4 keV Low threshold value accessible with 4x4x1 Schottky detectors (600V / -20°C) for the 20°C) for the ECLAIRsECLAIRs Mission Mission

• 1 keV FWHM at 60 keV accessible goal for 1 keV FWHM at 60 keV accessible goal for SIMBOL-XSIMBOL-X mission (small pixels) mission (small pixels)

• Current and next development steps :Current and next development steps :• New ASICsNew ASICs• Hybridization of ASICs and pixel arrays in progress Hybridization of ASICs and pixel arrays in progress • Space environment and Space qualification constraints studied simultaneously in Space environment and Space qualification constraints studied simultaneously in

the R&D programthe R&D program

Documents

High Energy Astrophysics in the Next Decade 1 June 2006 From INTEGRAL to SIMBOL-X F. Lebrun CEA-Saclay SAp/APC