1. 超新星遗迹 的XTP 观测模拟
南京大学 陈阳、周平、张潇

2. 1. Non-thermal X-ray shells
A great advantage of XTP for SNR studies:
able to tell the polarized synchrotron X-rays from thermal X-rays.
Chandra discovered ~10 SNRs with nonthermal (sync.) X-ray boundaries
In some SNRs, non-thermal X-rays may be blended with thermal ones, and are needed to be differentiated
E.g.，in SNR N132D, thermal component + hard tail.
Is the hard tail synchrotron emission?

3. N132D in LMC(50kpc) for example
Powerlaw component:
S3: F(2-10keV)=4E-13 erg/cm^2/s
S4: F(2-10keV)=3E-13 erg/cm^2/s
Entire: F(2-10keV)>~1E-11 erg/cm^2/s
If at d of Galactic SNRs (~10kpc)
X-ray flux of order: 1E-10至1E-9erg/cm^2/s

4. Simulated XTP spectra of N132D
N132D S4 region  100ks

5. LFA spectrum

6. direction of effective injection:
‘quasi-parallel scenario’ vs. ‘quasi-perpendicular scenario’ (Fulbright & Reynolds 1990)
bilateral SNR, e.g. SN1006，“polar cap”or “equator”?
SN 1006 G

7. “Role of B”目标、对策 <10 keV, 一维偏振成像, 偏振度一维分布
Pix=2’
PSF=2’
30 arcmin in diameter

8. Simulated XTP spectra of SN1006
Model: phabs*srcut
 NH=6.8e20, alpha=0.57, break=5.69e16 Hz, norm=16.2
(Bamba et al. 2008)
exposure=100ks

9. 4. Pulsar wind nebulae (PWNe)
PWNe harbored in SNRs has prominent polarized sync. X-rays (radio P-degree upto 50% Reynolds 2012).
XTP observation:
beneficial to filtering PWNe in SNRs, such as the PSR and PWN in SNR G
obtains degree of polarization
(but hard for spatial structure due to small size of PWNe)
P = (s+1)/(s+7/3)

10. Simulated XTP spectra of Crab
Crab   10ks, Model: phabs*powerlaw
NH=0.32e22,
Photon index=2.1, Norm=9.65

11. Identify PWN in SNRs/UGSs
HESS J1837
(Anada, T. 2009, PASJ, 61, 183; Suzaku & ASCA)
P=70.5 ms

12. Our prediction for src1 :
for P = 50%

13. Secondary electrons’ synchrotron of SNR in molecular clouds? *
A qualitative consideration:
In the radiative stage of SNR, particle acc. essentially stops;
Major electrons can’t emit X-rays,
But: p-p coll.  decay secondary electrons X-ray synchrotron (XTP detection?)
Would be an evidence for
proton acc. & hadronic interaction
* 难点首先在于空间分辨！

14. Simulated secondary sync. of W28