「すざく」による sn1006 の観測 suzaku observations of sn1006 aya bamba (isas/jaxa)
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「すざく」による SN1006 の観測Suzaku observations of SN1006
Aya BAMBA(ISAS/JAXA)
XIS (X-ray Imaging Spectrometer)Improved X-ray CCD with high efficiency
and good energy responseLow and stable backgroundEnergy band : 0.2-12keV
XRT (X-Ray Telescope)Large effective area
410cm2 @1.5keV
HXD (Hard X-ray Detector)Wide energy band Si-PIN (10-70keV) & GSO Scinti. (40-600keV)Non-imaging detector, but low background
XRT
XIS
HXD
Suzaku: Jp-US X-ray satelliteSuccessfully launched on 2005 July 10th.
Previous SN1006 observations
radio: faint continuumno information of MC
X-ray: synchrotron X-rays !(~10/265 SNRs)thermal X-rays
Halpha: bright in NW rim proper motion is measuredTeV: detected faint shellsoptical: detection of SN 1000yrs ago type Ia SN @NASA/HEASARC
SN1006 is a milestoneto understand the shock acceleration in SNRs
What can Suzaku achieve ?
- X-ray diagnostics of thermal emissiondensity, temperature, ….-> topic 1
- parameters of synchrotron X-raysbending ??-> topic 2
Suzaku observations
src 4pointingbg 2pointingtotal 200ks
FOV of XISFOV of HXD/PIN mapping of
whole remnant
Narrow band images of XIS-BI
He-like O line band 3 - 5 keV band
Distributions of thermal plasma and non-thermal electron are different !
Topic 1:X-ray diagnostics of thermal emission
XIS thermal emission in SE region
Plenty of emission lines
(Yamaguchi+08)
the first detection of iron K line
strong H-like and He-like O lines
thermal spectrum of whole SNR
NH [cm-2] 6.8x1020
VNEI 1 (ejecta 1) kT [keV] 1.2 nOneV [cm-3] 4.19 (4.05-4.32)x1052
VNEI 2 (ejecta 2) kT [keV] 1.9 nOneV [cm-3] 3.82 (3.77-3.89)x1053
NEI (ISM) kT [keV] 0.45 nHneV [cm-3] 3.45 (3.43-3.48)x1056
ISM density: 0.03 cm-3 (SE of SNR)
The density of acceleration site is very low !
(Yamaguchi+08)(Bamba+08)
Proper motion of SN1006 NE shell
(Katsuda+09)
filaments are moving in these 9 yrs !
2000 - 2008
v = 0.48”/yr ~ 5000 km/s
ambient density ~ 0.085 cm-3
ISM density is very low !
topic 2:Parameters of synchrotron X-rays
Spectra of whole remnant: XIS+HXD
PIN statistic errPIN systematic err
excess: 1% of bgd
The most tight upper-limit(2.7x10-5 ph/cm2/s in 10-15 keV)
XIS spectra (1)
large residuals from power-law model
emission lines + hard emission3 kT plasma (Yamaguchi+08) + power-law model
XIS FIXIS BI
synchrotron model with bending: srcut model
cut-off ? -> Emax of e, B
We need spectrawith good statistics -> Let’s see SN1006
nem
issio
nncutoff
~ Emax2B
G-12
Sync. EmissionFrom Power-law electrons
E
N(E
)
Emax
G
exp.
n
Syn
c.
em
issio
n
E2B
electron distribution
emission from an e
(SRCUT model)
3 kT plasma + srcut modelsync. emission from
electrons with PL + exp. cutoff distribution
spectral index at 1GHz: a=0.57
no residual !
non-thermal emission hassignificant cut-off !
ncutoff = 5.69 (5.67-5.71)x1016 Hz
XIS FI XIS BI
XIS spectra (2)
XIS spectrum of each rim
NE rim SW rim
cutloff freq. 6.66(6.58-6.69)x1016 Hz 4.68(4.64-4.73)x1016 Hz
cut-off freq. is larger in the NE rim
What determine cutoff energy ?
cutoff freq. = 1.6x1016 B1microG
E10TeV
2
[Hz]
(Reynolds 1998)
assumption: B=40microG (10microG outside)(Bamba+ 2003)
-> E = 9.4 TeV
B: magnetic field E: max E of e
difference of cut-off in NE and SW rimsdifference of B and/or Emax ?
-> difference of acc. efficiency ?
assump. B=40microGE = 10 TeV @ NEE = 8.5 TeV @SW
more detailed model is now needed to understand the cut-offNow we have TeV emission ! SED is available.
non-thermal flux(10-12ergs s-1cm-2arcmin-2 (2-10 keV))
therm
al fl
ux
(erg
s s
-1cm
-2arc
min
-2 (
0.5
-2 k
eV
))nonthermal flux vs. thermal flux
even low density, it might affect CR acceleration
north
inner east(Bamba+07, regected by J.Hughes)
Where is accelerated protons ?
In the case of old SNR G359.1-0.5 …
0.5-2.0 keV (Suzaku)contour: HESS
SNRsG359.0-
0.9, G359.1-0.5
(Bamba+ 2000)Only
thermal
TeV gamma-rays !
6arcmin
(Bamba+09)
neutral iron map
excess !
6arcmin
(Bamba+09)
molecular cloud
past activeGC
TeV emission is from accelerated protons ?
Summary
SN1006 is a milestone to understandCR acceleration on shocks of SNRs.
Suzaku capability to resolve thermal emission shows us that the ISM density around
SN1006 is very low. Chandra detected proper motion of the NE rim.
We detected the bending of synchrotron emission.
Now we have TeV emission, we will be able to determine the Emax.
Older SNRs should be studied morefor proton acceleration study.
3rd Suzaku conference“the Energetic Cosmos: from Suzaku to Astro-H”
June 29 – July 2, Otaru, Hokkaido, Japan
Topics: - Particle acceleration in cosmic shocks and jets - X-ray diagnostics of cosmic hot plasma - High energy aspects of the Milky Way - Magnetic activity in stellar objects - Primary and reprocessed emission from accreting objects - X-ray vies of the evolution of the universe - Highlights from the Fermi Space Gamma-Ray Telescope - Status of the MAXI experiment - From Suzaku to ASTRO-H and other missions
and further to IXO
abstract deadline: Mar. 16registration deadline: Apr. 13
Let us enjoyfresh topics and Sushi !