hard x-ray observations of cosmic-ray accelerators yasunobu uchiyama with t. tanaka & t....
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Hard X-ray Observationsof Cosmic-ray AcceleratorsHard X-ray Observations
of Cosmic-ray Accelerators
Yasunobu Uchiyama with T. Tanaka & T. Takahashi
(ISAS/JAXA)for the Suzaku team
Yasunobu Uchiyama with T. Tanaka & T. Takahashi
(ISAS/JAXA)for the Suzaku team
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X-ray Satellites X-ray Satellites ChandraChandra XMM-NewtonXMM-Newton SuzakuSuzaku
INTEGRALINTEGRAL
Launch: 23 July 1999
Vehicle: Space Shuttle
Weight: 4.8 ton
spatial resolution:
~0.5”
point-source sensitivity
~ 4e-15 erg/cm2/s
(100 ksec)
Launch: 23 July 1999
Vehicle: Space Shuttle
Weight: 4.8 ton
spatial resolution:
~0.5”
point-source sensitivity
~ 4e-15 erg/cm2/s
(100 ksec)
Launch: 10 Dec 1999
Vehicle: Ariane 5
Weight: 3.8 ton
Launch: 10 Dec 1999
Vehicle: Ariane 5
Weight: 3.8 ton
Launch: 10 July 2005
Vehicle: M-V
Weight: 1.7 ton
energy resolution:
7 eV (FWHM)
wide band:
0.2 -- 300 keV
Launch: 10 July 2005
Vehicle: M-V
Weight: 1.7 ton
energy resolution:
7 eV (FWHM)
wide band:
0.2 -- 300 keV
Hard X-ray & Gamma-raysHard X-ray & Gamma-rays
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Why X-ray ?Why X-ray ?
(1) TeV gamma-rays require multi-TeV particles(1) TeV gamma-rays require multi-TeV particles(2) Multi-TeV electrons emit synchrotron X-rays(2) Multi-TeV electrons emit synchrotron X-rays
Intimate connection between keV and TeV photonsIntimate connection between keV and TeV photons
• Superb spatial resolution (<1”) with Chandra • Superb spatial resolution (<1”) with Chandra
• All-sky monitors (RXTE, Swift, Maxi in future)• All-sky monitors (RXTE, Swift, Maxi in future)
PeV photons Hard X-rays (This talk!)PeV photons Hard X-rays (This talk!)
• Good sensitivities (< micro-Crab level)• Good sensitivities (< micro-Crab level)
clear keV-TeV connectionclear keV-TeV connection
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OutlineOutline
X-ray studies on Supernova Remnants (SNRs)
- Results from ASCA & Chandra Suzaku X-ray satelliteNew results from Suzaku
- TeV SNRs: RX J1713.7-3946 & Vela Jr.
- unID HESS sources • NeXT X-ray Satellite: to be launched
~2013
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SNRs (1) : The Remnant of SN 1006SNRs (1) : The Remnant of SN 1006
• This is the first evidence that forward shocks do accelerate electrons to “TeV” energies. (Koyama et al. 1995)
• This is the first evidence that forward shocks do accelerate electrons to “TeV” energies. (Koyama et al. 1995)• Acceleration in “thin” filamentary structures (B-field amplification: Bell-Lucek hypothesis?)• Acceleration in “thin” filamentary structures (B-field amplification: Bell-Lucek hypothesis?)
Chandra X-rayChandra X-ray
synchrotron X-rayssynchrotron X-rays
“Anniversary”: Just 1000 years old“Anniversary”: Just 1000 years old
Long et al. 2003Bamba et al. 2003
Long et al. 2003Bamba et al. 2003
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SNRs (2) : Tycho’s SNRSNRs (2) : Tycho’s SNR
Chandra X-rayChandra X-ray
synchrotron X-rayssynchrotron X-rays
shock heated ejectashock heated ejecta
forward shock:forward shock:
reverse shock: synchrotron radioreverse shock: synchrotron radio
the debris of supernova explosion in the year 1572
the debris of supernova explosion in the year 1572
shocked ISM region is quite “narrow”
R_contact / R_forwad = 0.93 !!
shocked ISM region is quite “narrow”
R_contact / R_forwad = 0.93 !!
Hwang et al. 2002
Warren et al. 2005
Hwang et al. 2002
Warren et al. 2005
•This is thinner than a hydrodynamic expectation.
• Suggests modified dynamics due to efficient cosmic-ray (protons) acceleration
•This is thinner than a hydrodynamic expectation.
• Suggests modified dynamics due to efficient cosmic-ray (protons) acceleration
4’4’
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SNRs (3) : Non-thermal SNRsSNRs (3) : Non-thermal SNRs
ASCA X-ray (Slane et al. 2001)ASCA X-ray (Slane et al. 2001)
Vela Jr.Vela Jr.RX J1713.7-3946RX J1713.7-3946
ASCA X-ray (Slane et al. 1999; Uchiyama et al. 2002)
ASCA X-ray (Slane et al. 1999; Uchiyama et al. 2002)
• Only non-thermal (synchrotron) X-ray emission • TeV Imaging shows a similar morphology (HESS)
• Only non-thermal (synchrotron) X-ray emission • TeV Imaging shows a similar morphology (HESS)
Ideal targets for Suzaku and indeed the objects of this talk: (1) XIS 0.3-10 keV with 1’ resolution (2) HXD PIN 10-50 keV with 35’ aperture
Ideal targets for Suzaku and indeed the objects of this talk: (1) XIS 0.3-10 keV with 1’ resolution (2) HXD PIN 10-50 keV with 35’ aperture
ASCA revealed a remarkable class of SNRs ASCA revealed a remarkable class of SNRs
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Suzaku X-ray Satellite
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Instruments onboard SuzakuX-ray Mirror
X-ray CCD camera
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Suzaku XIS (0.3-10 keV)
Low instrumental background thanks to low Earth orbit
Good energy response(< 1 keV)
Koyama et al. (in press)
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Suzaku HXD (10 - 600 keV)
PIN 10-60 keV (FOV 35’x 35’)GSO 30-600 keV (FOV 4 deg x 4
deg)
Compound-Eye Well-type Phoswich DetectorNon-
Imaging
Takahashi et al. (in press)
hard X-rays
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Suzaku HXD (10 - 600 keV)
Kokubun et al. (in press)
BGD
Lowest background thanks to (BGO) active shields and narrow FOV
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OutlineOutline
X-ray studies on Supernova Remnants (SNRs)
- Results from ASCA & Chandra Suzaku X-ray satelliteNew results from Suzaku
- TeV SNRs: RX J1713.7-3946 & Vela Jr.
- unID HESS sources • NeXT X-ray Satellite:
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Bright TeV SNR (1)RX J1713.7-3946
Bright TeV SNR (1)RX J1713.7-3946
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1°1°
contours: ASCA X-ray (Uchiyama et al.
2002)
contours: ASCA X-ray (Uchiyama et al.
2002)
SNR RX J1713.7-3946 SNR RX J1713.7-3946 HESS “TeV image” HESS “TeV image”
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Broadband Spectrum Broadband Spectrum
From Horns’s talk From Horns’s talk
Synchrotron + Inverse-ComptonSynchrotron + Inverse-Compton Synchrotron + pion-decaySynchrotron + pion-decay
Advantages: similar morphology Advantages: similar morphology
Disadvantages: - small B-field with large Emax - TeV spectrum unmatched
Disadvantages: - small B-field with large Emax - TeV spectrum unmatched
Advantages: - a good fit to the spectrum - energetically OK
Advantages: - a good fit to the spectrum - energetically OK
Disadvantages: - why morphology so similar?
Disadvantages: - why morphology so similar?
New keys: Suzaku hard X-ray (up to 50 keV) observations New keys: Suzaku hard X-ray (up to 50 keV) observations
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Suzaku XIS image(0.5 - 5 keV)Suzaku XIS image(0.5 - 5 keV)
We have observed RX J1713.7-3946 in September 2006 with a total of 200 ks exposure.We have observed RX J1713.7-3946 in September 2006 with a total of 200 ks exposure.
(Tanaka et al. in prep)(Tanaka et al. in prep)
Suzaku HXD PIN (10-50 keV) measurements have been made in each 11 boxes (34’x34’).
Suzaku HXD PIN (10-50 keV) measurements have been made in each 11 boxes (34’x34’).
Suzaku hard X-ray ObservationsSuzaku hard X-ray Observations
Not yetNot yet
Photon index (10-50 keV)for each box
Photon index (10-50 keV)for each box
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Suzaku Wide band spectrumSuzaku Wide band spectrumIntegrated over the entire remnant ( energy range:
0.5 - 50 keV )Integrated over the entire remnant ( energy range:
0.5 - 50 keV )Interstellar absorptionInterstellar absorption
power lawpower law steepening!!(break at ~10 keV)steepening!!
(break at ~10 keV)
Suzaku XIS+HXD spectrumSuzaku XIS+HXD spectrum
0.5 - 50 keV!! (high quality) 0.5 - 50 keV!! (high quality)Spectral steepening > 5 keVfrom a photon index
Spectral steepening > 5 keVfrom a photon index
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Multifrequency Spectrum with Suzaku/HESSMultifrequency Spectrum with Suzaku/HESSIn the Sy+IC hypothesis,it is now possible to obtain physical parameters:
In the Sy+IC hypothesis,it is now possible to obtain physical parameters:
electron index = 1.9B = 10 uGEmax = 100 TeV
electron index = 1.9B = 10 uGEmax = 100 TeV
Synchrotron + IC Model (electron cooling taken into account)
Synchrotron + IC Model (electron cooling taken into account)
(similar to Aharonian et al. 2005)(similar to Aharonian et al. 2005)
To test this hypothesis, (1) GLAST measurements (2) good statistics at ~ 100 TeV (= Emax) to see Klein-Nishina suppression
To test this hypothesis, (1) GLAST measurements (2) good statistics at ~ 100 TeV (= Emax) to see Klein-Nishina suppression
• One-zone is OK? Yes (as shown later)
• B-field seems too low (c.f. Voelk et al. 2005)
• One-zone is OK? Yes (as shown later)
• B-field seems too low (c.f. Voelk et al. 2005)
Bohm diffusion requiredBohm diffusion required
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keV-TeV ComparisonkeV-TeV Comparisonradial profilesradial profiles
pies 1-8 integrated:pies 1-8 integrated: consistent withthe ASCA resultsconsistent with
the ASCA results
Suzaku vs HESSSuzaku vs HESS
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keV-TeV Surface Brightness RelationkeV-TeV Surface Brightness Relation
keV excess
Uchiyama et al. 2003
•“keV excess” in NW and SW rims•“keV excess” in NW and SW rims
•Compact features (like filaments) would account for the excess.
•Compact features (like filaments) would account for the excess.
0.5’ TeV imaging is needed to test this.0.5’ TeV imaging is needed to test this.
ChandraChandra
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Bright TeV SNR (2)Vela Jr. (RX J0852.0-4622)
Bright TeV SNR (2)Vela Jr. (RX J0852.0-4622)
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Vela Jr. (RX J0852.0-4622) Vela Jr. (RX J0852.0-4622)
X-ray = SynchrotronTeV = IC / pion-decay
X-ray = SynchrotronTeV = IC / pion-decay
young remnant of core-collapsed SN hidden in the old Vela SNRyoung remnant of core-collapsed SN hidden in the old Vela SNRyoung remnant of core-collapsed SN hidden in the old Vela SNRyoung remnant of core-collapsed SN hidden in the old Vela SNR
ASCA X-ray (Slane et al. 2001)ASCA X-ray (Slane et al. 2001)
2 deg diameter2 deg diameter
Distance: uncertain 0.2 - 1 kpcDistance: uncertain 0.2 - 1 kpc
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Suzaku hard X-ray ObservationsSuzaku hard X-ray Observations
AO2 proposed FOVsAO2 proposed FOVsOnly a “pilot” observation has Only a “pilot” observation has been been
performed.performed.
Only a “pilot” observation has Only a “pilot” observation has been been
performed.performed.
A power law up to 30 keV has been measured
A power law up to 30 keV has been measured
We need mapping observationsto conduct keV-TeV comparisonsas we did for RX J1713.7-3946. AO2 proposal (PI: Uchiyama)
We need mapping observationsto conduct keV-TeV comparisonsas we did for RX J1713.7-3946. AO2 proposal (PI: Uchiyama) HXD PIN: ~ sensitivity limitsHXD PIN: ~ sensitivity limits
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Unidentified TeV SourcesUnidentified TeV Sources
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Suzaku Observation of HESS J1616-508Suzaku Observation of HESS J1616-508Matsumoto et al. 2006 (in
press)HESS TeV imageHESS TeV image
Non-detection in X-raysfavors “hadronic” origin of TeV gamma-rays(TeV IC without X-ray requires B < a few uG)
Non-detection in X-raysfavors “hadronic” origin of TeV gamma-rays(TeV IC without X-ray requires B < a few uG)
Fx << FtevFx << Ftev
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The Japanese “NeXT” missionThe Japanese “NeXT” mission
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Finest resolution by Space VLBIFinest resolution by Space VLBI
First Hard X-ray FocusingFirst Hard X-ray Focusingwith with
the finest X-ray spectrumthe finest X-ray spectrum
Mercury ExplorationMercury Exploration「「 BepiColombo/MMOBepiColombo/MMO 」」
Venus ExplorationVenus Exploration「「 PLANET-CPLANET-C 」」
Solar-powered Sail Solar-powered Sail
VSOP2VSOP2
NeXTNeXT
Within about 10 years (Defined in ISAS’s Long Term Vision)
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Launch ~2013NeXT Mission
inclination 31 degaltitude 550 km
weight 1.7t
Based on the proposal 2005-Oct, Approved “Completion of pre-phase A” Waiting for the transition to Phase A/B
First Hard X-ray Focusing Observation (10 - 80 keV)
Wide band observation (0.3 - 300 keV) with high sensitivity
High Resolution (7 eV) X-ray spectroscopy (0.3 - 10 keV) of diffuse sources
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Hard X-ray Imaging
Total weight : 1700 kg
Total Weight < 1700 kg
Super Mirror + Hard X-ray Imager
Multilayer Super Mirror:using Bragg reflection
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Large Area/Light Weight Mirror
with ASCA/Suzaku Style
Mirror weight/telescope
Chandra 1500 kgXMM 440 kg
Suzaku 20 kg
NeXT HXT 65 kg
Pt/C multilayer super mirror (Nagoya U.)
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Breakthrough brought byHard X-ray Focusing Telescope
Rule of thumbDetector Background ∝ Detector Volume
Super Mirror ( 0.5-80 keV )
Hard X-ray Imager
focal length 12 m
Collimator
Coded-Mask
Effective Area = Detector Area
Hard X-ray region is detector background dominated:
Sensitivity
◎ △Sensitivity
Effective Area >> Detector Area
Focusing Telescope
NeXTNeXT
SuzakuSuzaku
Integral/Integral/SwiftSwift
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Expected Performancebaseline design
Focal Plane Hard X-ray Imager (HXI)
Energy Range < 80 keV
Effective Area ~300 cm2 at 30 keV
Imaging Quality ~ 60 arcsec (HPD)
Effective FOV ~ 8 arcmin
Focal Plane Soft X-ray Spectroscopy/Imager
Energy Range < 12 keV
Effective Area ~500 cm2 at 30 keV
Imaging Quality ~ 60 arcsec (HPD)
Effective FOV ~ 12 arcmin
For Hard X-ray Imager (HXT)
For Soft X-ray Instruments (SXT)
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T.Takahashi, SPIE, Glasgow, 2004
DSSD 0.5mm thick, 400 micron pitch 24 layersCdTe Pixel Wall, 5-6 mm thick, 1-2 mm pitch
Takahashi, Makishima, Kamae, 2001Takahashi et al. SPIE, 2002
Compton kinematics inside the BGO WELL is the key to reduce the internal background
1. Select two-hits events ( e.g. one in Si and one in CdTe)
2. Calculate the direction of “incident” gamma-ray by using Compton Eq.3. Accept events only if the ring intercepts the FOV (0.5 deg for <100 keV, ~ 4 deg at 500 keV)
New Concept:
Narrow Field of View Compton telescope
SGD (Soft Gamma-ray Detector)
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ConclusionsConclusions
Suzaku is suited for X-ray studies on TeV sources
“NeXT” will realize the first Hard X-ray Focusing Telescope up to 100 keV (with 1’ resolution)
We hope the realization of TeV imaging with < 1’ resolution to be compared with X-ray and hard X-ray images