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Future Polarization Future Polarization MissionsMissions
K. Hayashida (Osaka University)K. Hayashida (Osaka University)
X-ray PolarimetryX-ray Polarimetry Started in 1960’s. 1Started in 1960’s. 1stst positive detection of X-ray polarizatio positive detection of X-ray polarizatio
n in the Crab nebulae in 1970.n in the Crab nebulae in 1970. Dedicated satellites OSO-8 was launched in 1970’s, but nDedicated satellites OSO-8 was launched in 1970’s, but n
o other significant detections other than the Crab. 19.2±1.o other significant detections other than the Crab. 19.2±1.0%@2.6keV,0%@2.6keV, 19.5±2.8%@5.2keV19.5±2.8%@5.2keV
It is still an unexploited field. It is still an unexploited field. e.g. See SLAC symposium Feb 2004. http://www-conf.slac.stanford.edu/xe.g. See SLAC symposium Feb 2004. http://www-conf.slac.stanford.edu/x
ray_polar/ray_polar/
Recent status of developments of various models of X-ray Recent status of developments of various models of X-ray polarimeters in Japan is introduced.polarimeters in Japan is introduced.
PHENEX balloon experiment to observe hard X-ray polarizPHENEX balloon experiment to observe hard X-ray polarization of the Crab (mission last week!) is reported.ation of the Crab (mission last week!) is reported.
Future small satellite mission Polaris is outlined.Future small satellite mission Polaris is outlined.
Targets of X-ray PolarimetryTargets of X-ray Polarimetry Synchrotron Radiation Synchrotron Radiation
SNRSNR (( Pulsar Nebulae, Shell TypPulsar Nebulae, Shell Typee ))
Clusters of galaxiesClusters of galaxies BlazarsBlazars 、、 QuasarsQuasars
Scattered RadiationScattered Radiation Accretion disk around black holeAccretion disk around black hole Accretion Torus Seyfert galaxiesAccretion Torus Seyfert galaxies
Magnetic field and scatteringMagnetic field and scattering PulsarsPulsars
Pol
ariz
atio
n D
egre
e
©CXC/NASA
Reflection by Accretion Disk
X-ray Energy (keV)
Kii, 1987, PASJ 39,p.781
ペンシルビームでは、フラックスが弱いときに偏光度が高い。ファンビームモデルではその逆。
Energy dependence of Polarization
Accretion in Binary Accretion in Binary PulsarsPulsars
Pencil Beam Fan Beam
P
Flux
+100%
-100%
Reflection component in AGNsReflection component in AGNsScattered X-rays by Accretion Disk around BHs
Matt MNRAS 260, 1993
Polarization degree depends On the disk inclination
total1%
Inclination
reflected Inclination
Large P at Higher X-ray energy
Anomalous X-ray PulsarStrong Magnetic Field and QED
Swank et al.,2004 SLAC workshop
Polarimeter TypePolarimeter Type
Scattering Type is better in Scattering Type is better in the sensthe sensitivityitivity for hard X-ray polatimetry. for hard X-ray polatimetry.
Photo-electron-track has advantagePhoto-electron-track has advantages in soft X-ray polarimetry. s in soft X-ray polarimetry.
ScatteringScattering Photo-electron-trackPhoto-electron-trackAnistropy 1-sin2cos2 sin2cos2
Photon: travel straightPhoton: travel straight Electron: scatteredElectron: scattered
M >0.9 is possible, 0.5 is easy 0.4-0.5 was obtained
M 0.6 is max, 0.2-0.3 is easy Max ~0.07@20keV
- E>5keV + Imaging capability
Pacciani et al. 2002 SPIE
M: Modulation contrast … modulation observed against 100% polarized beam: Efficiency … the ratio of number of photons employed in the polarimetry to that incident to the polarimeter.
Mη
1/2
MinimumDetectablePolarization
Photo-electron TrackingPhoto-electron Tracking
CCD Polarimeter (Osaka Univ. Tsunemi et CCD Polarimeter (Osaka Univ. Tsunemi et al.)al.)
Capillary Plate Gas Counter (Yamagata UCapillary Plate Gas Counter (Yamagata Univ., Sakurai, Tokanai et al.)niv., Sakurai, Tokanai et al.)
GEM (RIKEN, Tamagawa et al.)GEM (RIKEN, Tamagawa et al.)-PIC (Kyoto Univ., Tsuru et al.)-PIC (Kyoto Univ., Tsuru et al.)Gas Imaging Polarimeter (Italy Group)Gas Imaging Polarimeter (Italy Group)AXP (GSFC/NASA, Swank et al.)AXP (GSFC/NASA, Swank et al.)
Gas Imaging Polarimeter(GIP)Gas Imaging Polarimeter(GIP)(Yamagata Univ. CGPC(Yamagata Univ. CGPC ))
Sakurai et al. 2003,2004
Fine Pitch GEFine Pitch GEM + CMOSM + CMOS
by Tamagawa by Tamagawa et al.et al.
φ(deg)E
ven
t C
oun
ts M = 0.3
Gas Electron Multiplier (GEM)Gas Electron Multiplier (GEM)
3 cm 50 μm
5 cm
100μm
CMOS sensor (Fine PixeCMOS sensor (Fine Pixelized electron reader)lized electron reader)
Polarimetry Sensitivity -PIC by Tsuru et al.
Ne Ar
1atm / 293K Gas depth1cmDiffusion150μm
8keV 15keVEnergy(keV)
Pixel Pitch600μm
600μm
400μm
200μm
実線:シミュレーション(現状)破線:シミュレーション(今後)点: コリメート実験値Future
Polarimeter TypePolarimeter Type
Scattering Type is better in Scattering Type is better in the sensthe sensitivityitivity for hard X-ray polatimetry. for hard X-ray polatimetry.
Photo-electron-track has advantagePhoto-electron-track has advantages in soft X-ray polarimetry. s in soft X-ray polarimetry.
ScatteringScattering Photo-electron-trackPhoto-electron-trackAnistropy 1-sin2cos2 sin2cos2
Photon: travel straightPhoton: travel straight Electron: scatteredElectron: scattered
M >0.9 is possible, 0.5 is easy 0.4-0.5 was obtained
M 0.6 is max, 0.2-0.3 is easy Max ~0.07@20keV
- E>5keV + Imaging capability
Pacciani et al. 2002 SPIE
M: Modulation contrast … modulation observed against 100% polarized beam: Efficiency … the ratio of number of photons employed in the polarimetry to that incident to the polarimeter.
Mη
1/2
MinimumDetectablePolarization
Scattering TypeScattering Type PHENEX (Yamagata, Osaka, RIKEN, ISAS)PHENEX (Yamagata, Osaka, RIKEN, ISAS) PoGO (SLAC, TITech, ISAS/JAXA, Hiroshima, YPoGO (SLAC, TITech, ISAS/JAXA, Hiroshima, Y
amagata + International Collaboration)amagata + International Collaboration) Approved by NASA balloon flight (long flight in SwedeApproved by NASA balloon flight (long flight in Swede
n) in 2009.n) in 2009. see Poster by Mizuno et al.see Poster by Mizuno et al.
GaPOM (RIKEN, Mihara et al.)GaPOM (RIKEN, Mihara et al.) Gamma-Ray Burst Polarimeter for Solar-Sail MisGamma-Ray Burst Polarimeter for Solar-Sail Mis
sion (Kanazawa Univ. Yonetoku et al.)sion (Kanazawa Univ. Yonetoku et al.) Si/CdTe Compton Camera(ISAS/JAXA, SLAC, HSi/CdTe Compton Camera(ISAS/JAXA, SLAC, H
iroshima)iroshima) SGD for NeXT (ISAS/JAXA, Hiroshima et al.)SGD for NeXT (ISAS/JAXA, Hiroshima et al.)
Polarimetry using scattering target : Polarimetry using scattering target : employed in beam polarization calibrationemployed in beam polarization calibration
E
0
200
400
600
0 90 180 270 360
Ex=10keV
cou
nts
rotation angle
KEK-PF 10keV beam by Hayashida et al.
Spring8 20keV beam by Tokanai et al.
Segmented/Active Scatter PolarimeterSegmented/Active Scatter PolarimeterScatter=Plastic Scintillator(e.g. 2mmx2mmx40mm x 54)
Absrber=CdTe (e.g.2mmx0.5mmx40mmx32)(or CSI)
Multi-Anode Position sensitive PMT
18mm
Whole detector is actrively Whole detector is actrively Shielded by BGO or CsIShielded by BGO or CsI
X-ray
Plastic CdTe or CSI
Efficiencyηfor three kinds of eventsEfficiencyηfor three kinds of events
Double eventAbsorped eventSingle event
Compton recoil not detected Compton recoil
detected
Photo Absorption
PHENEX 2006PHENEX 2006Polarimeters for High ENErgy X-raysPolarimeters for High ENErgy X-rays
Yamagata Univ. :Yamagata Univ. : Polarimeter, Monitor Counter, Polarimeter, Monitor Counter, Detector Chamber + Rotation, Batteries Detector Chamber + Rotation, Batteries
Osaka Univ. : DAQ & HK System, Sun CCD Osaka Univ. : DAQ & HK System, Sun CCD RIKEN: Sun PSD, HV Unit, Command SystemRIKEN: Sun PSD, HV Unit, Command System ISAS/JAXA: ACS System, Balloon I/FISAS/JAXA: ACS System, Balloon I/F
Polarimeter Unit
MAPMTH8500
HVDATA&COM
TrigIN
TrigOUT
CollimatorMo 1mm 、 FWHM 5°
Shield Pb2mm 、
Sn1 mm
Shrink Tube
ScintillatorsCsI x 28、Plas
tic x 36
FOP1mm
•Plastic Scintillators act as scattering target for incident hard X-rays.
•Scattering position is known from a signal by a recoiled electron produced in the Plastic Scintillator. Scattering direction is measured if the scattered X-ray is absorbed in a CsI.
•All the CsI triggered events are recorded, and will be filtered by coincidence with Plastic, to suppress most of the background.
•Low optical crosstalk CsI and Plastic.
•Compact 64ch read-out module.
Top View
CsIPlastic
Polarimeter for High ENErgy X-ray PHENEX
64ch Read Out Modulewith VA-TA chip
by CLEAR-PULSE
KEK-PF (Synchrotron) Experiment 2006Feb
Count rate modulation for each CsI ch
Overlay with adjusting the phase angle
Modulation Factor 61.7%(KEK-PF Beam Pola=90% @ 80keV is taken i
nto account )
Weighted Modulation (① × 4+② × 8+③ × 8+④ × 4+⑤ × 8+⑥ × 4)
÷ 36
For Uniform Irradiation over FOV
M=53%@80keV eff=20%
Polarimeter for High ENErgy X-ray PHENEX
80keV
Beam incident to ① to , modulation is ⑥measured.
① ② ③④ ⑤
⑥
60keV、40keV Modulation (Preliminary)
40keVをPla37ch (center ch) incident
60keV Pla37ch (center ch) incident
M-factor for center incidence
60%M-factor for center incidence
57%
Polarimeter for High ENErgy X-ray PHENEX
Monitor Counter
CsI 34x34mm
PMT used for PoGO
Anti Counter
Polarimeter Unit x 4
Detector Drum Rotate 360º
Elevation Control
DAQ Chamber
SunCCDSunPSD
GA-sensor
Rotation Wheel is used to controlthe azimuth of the gondola
DAQ SystemDAQ System
VME system
Arm-CPU+PC/104
Gondola 311kg
Flight 2006/06/13 AM5:30
B150 Flight B150 Flight 2006/06/132006/06/13
Level FlightLevel Flight
37-38km ~6.5hr 37-38km ~6.5hr
Safely Captured and Returned to SBCSafely Captured and Returned to SBC
USB memories are OK!
-200
-100
0
100
200
10000 20000 30000 40000 50000 60000
Rotation (Opt-Encoder)
sec from 2006/ 6/ 13 0:0:00 J ST
-200
-100
0
100
200
40000 42000 44000 46000 48000 50000
Rotation (Opt-Encoder)
sec from 2006/ 6/ 13 0:0:00 J ST
0
200
400
600
800
1000
1200
0
2
4
6
8
10
12
14
16
10000 20000 30000 40000 50000 60000
Scalor
CsI c/s Monitor c/s
sec from 2006/06/13 0:0:00
In future, if 9 units are available
50 〜 several100mCrab
1Crab
PHENEX2006:4unit(44cm2) ,6hours, Crab … MDP(3)=14%
Cygnus X-1Crab Nebula
Crab Pulsar 、 Sco X-1Vela X-1 、 1700-377GX 301-2 、 1657-415GX1+4 、 GX5-1NGC4151 、 Cen-ACygnus X-3 、 Her X-1
>40keV range
1day 1week
Polaris OutlinePolaris Outline Cover various classes of X-ray objects (>Cover various classes of X-ray objects (>10mCrab10mCrab) )
As Uhuru studied spectra & variabilities of representative class oAs Uhuru studied spectra & variabilities of representative class of X-ray objects 35 years ago, Polaris will establish polarization prf X-ray objects 35 years ago, Polaris will establish polarization properties of those classes of objects. operties of those classes of objects.
Hybrid polarimeters to cover wide energy band(0.25 or 4Hybrid polarimeters to cover wide energy band(0.25 or 4-80keV)-80keV) Energy dependence of polarization is important. Energy dependence of polarization is important.
Scattering type polarimeters (e.g. PHENEX) are used for Scattering type polarimeters (e.g. PHENEX) are used for hard X-ray range. Gas imaging polarimeters and/or Multihard X-ray range. Gas imaging polarimeters and/or Multi-layer reflection polarimeter are added to cover <10keV. -layer reflection polarimeter are added to cover <10keV.
To gain S/N and to enable imaging polarimetry, Multi-LayTo gain S/N and to enable imaging polarimetry, Multi-Layer Super mirrors are used. Polarimeters are set at the foer Super mirrors are used. Polarimeters are set at the focal planes of those mirrors.cal planes of those mirrors.
Polarization sensitivity below 10keVPolarization sensitivity below 10keV
Add on Li target on SAdd on Li target on Scattering Imaging Polcattering Imaging Polarimeterarimeter
Transparent type Gas Transparent type Gas Imaging Polarimeter Imaging Polarimeter (GIP) on SIP.(GIP) on SIP.
Possible with Possible with -PIC-PIC Not easy to make >20Not easy to make >20
00ch readout layout.00ch readout layout.Ti 50mFilter
Li-Target
(1 ) (2)
Multi-Layer Super Mirror & EOBMulti-Layer Super Mirror & EOB
Heritage of InFOCus,SUMIT,NeXHeritage of InFOCus,SUMIT,NeXT will be available. T will be available.
FL 6m needs to change inner mirFL 6m needs to change inner mirror radius to be 60mmror radius to be 60mm
10
100
1000
1 10 100
12m/1WXT6m/4WXT
X-ray energy(keV)
FL12m
FL6mx4units
GIP-on-SIP
LI-on-SIP
Polaris ComponentsPolaris Components 6m-Design6m-DesignWXT(Mirror)
F.L. 6m
In/Out/xNo.of Unit 60mm/200mm x4Unit
Scale on FP 1’/1.7mm
SIP( Scattering Imaging Polarimeters )
Scintillator 2.8mmx2.8mmx40mm/Pillar
No. of Scintillator Plastic 36 /CsI 28
Signal / Unit 64ch
GIP( Gas Imaging Polarimeters )
Size/Pixel pitch 10mmx10mm/0.2mm
Signalch 数 2000ch
Gas Ne/1atm/1cm
Li for SIP+LI Size 5-10mmdiameter x30mmheight
No. of Units GIP-on-SIP x1 + LI-on-SIPx3
Polarimeters MPolarimeters M1/21/2
0
0.05
0.1
0.15
0.2
0.25
0.3
0.35
0.1 1 10 100
Multi Layer GIP (Ne Gas Pixel) LI_on_SIP (Li)SIP (Plastic double-hit)SIP (Plastic single-hit)
Ex(keV)
Weight and Power ConsumptionWeight and Power ConsumptionPI WeightPI Weight ::
FL 12mFL 12m 120kg 120kg [Mirror 40kg[Mirror 40kg EOB 60kg EOB 60kg GIP-on-SIP 15kg DE5kg] GIP-on-SIP 15kg DE5kg]
FL 6m FL 6m 121kg 121kg [Mirror40kg[Mirror40kg EOB40kg EOB40kg GIP-on-SIP 15kg LI-on-SIPx3=21kg DE5kg]GIP-on-SIP 15kg LI-on-SIPx3=21kg DE5kg]
Power ConsumptionPower Consumption ::FL 12m 78WFL 12m 78W [Mirror15W [Mirror15W GIP-on-SIP GIP-on-SIP
58W DE 5W]58W DE 5W]FL 6m FL 6m 67W67W [Mirror15W [Mirror15W GIP-on-GIP-on-
SIP 32W LI-on-SIPx3=15W DE 5W]SIP 32W LI-on-SIPx3=15W DE 5W]+20%+20% のの margin margin 、、 PI Weight=145kg,PI Weight=145kg, PI PI
Power=94WPower=94W
Expected SensitivityExpected Sensitivity
0.1
1
10
100
0.001 0.01 0.1 1
MDP 4-10keV
GIP (Ne Gas Pixel) 4-10keV 100ks GIP (Ne gas Pixel) 4-10keV 1Ms SIP+Li Scatt 4-10keV 100ks SIP+Li Scatt 4-10keV 1Ms
Flux (in Crab)
0.1
1
10
100
0.001 0.01 0.1 1
MDP 10-20keVSIPL+Li Scatt 10-20keV 100ksSIP+Li Scatt 10-20keV 1Ms
Flux (in Crab)
0.1
1
10
100
0.001 0.01 0.1 1
MDP 20-40keVSIP single Hit 20-40keV 100ksSIP Single Hit 20-40keV 1Ms
Flux (in Crab)
0.1
1
10
100
0.001 0.01 0.1 1
MDP 40-80keVSIP Double Hit 40-80keV 100ks
SIP Double Hit 40-80keV 1Ms
Flux (in Crab)
SummarySummary
Recent activities for X-ray Polarimetry in JRecent activities for X-ray Polarimetry in Japan are introduced.apan are introduced.
PHENEX balloon experiment performed laPHENEX balloon experiment performed last week is reported.st week is reported.
Future Small Satellite Mission Polaris is ouFuture Small Satellite Mission Polaris is outlined.tlined.
Within a few years, X-ray polarimetry obseWithin a few years, X-ray polarimetry observations will restart, no doubt. rvations will restart, no doubt.