Shock modification at the rim of SN 1006
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Shock modification at the rim of SN 1006 Marco Miceli University of Palermo, INAF-OAPa Collaborators: F. Bocchino, A. Decourchelle, G. Maurin, S. Orlando, J. Ballet and the “SN 1006 team” F. Acero, G. Cassam Chenai, G. Dubner, E. Giacani, E. Helder, D. Kosenko, J. Vink 38° COSPAR Scientific Assembly 18-25 July 2010 Bremen, Germany
description
38° COSPAR Scientific Assembly 18-25 July 2010 Bremen, Germany. Shock modification at the rim of SN 1006. Marco Miceli University of Palermo, INAF-OAPa. Collaborators: F. Bocchino, A. Decourchelle, G. Maurin, S. Orlando, J. Ballet and the “SN 1006 team” - PowerPoint PPT Presentation
Transcript of Shock modification at the rim of SN 1006
Shock modification at the rim of SN 1006
Marco MiceliUniversity of Palermo, INAF-OAPa
Collaborators:
F. Bocchino, A. Decourchelle, G. Maurin, S. Orlando, J. Balletand the “SN 1006 team”
F. Acero, G. Cassam Chenai, G. Dubner, E. Giacani, E. Helder, D. Kosenko, J. Vink
38° COSPAR Scientific Assembly18-25 July 2010
Bremen, Germany
Introduction
We focus on thermal limbs of SN 1006 to study how particle acceleration modifies the thermodynamical properties of the shocked ISM.We take advantage of the deep XMM-Newton observations presented in the Decourchelle’s talk
Miceli M.: Shock modification in SN 1006, Cospar 2010
high T, low EM?
low T, high EM?
pro
ject
ed B
W/C
D
angle
Miceli et al. 2009
The quest for the shocked ISM
No detection of X-ray emitting ISM in accelerating SNRs (e. g. Cassam-Chenai et al. 2004 for RX J1713.7-3946 and Cassam-Chenai & Hughes 2007 for Tycho)In archive observations of SN 1006, spectra are well described by one thermal component (ejecta), and one non-thermal component (synchrotron, SRCUT), ISM is statistically not needed (Acero et al. 2007, Miceli et al. 2009): no constrains for the ISM properties.
How can we test the presence of “modified” ISM?
Unmodified shock
Indirect proof: small distance BW-CD (Miceli et al. 2009), observed also in Tycho SNR (Warren et al. 2005)
Direct proof: failed, no detection of X-ray thermal emission
Miceli M.: Shock modification in SN 1006, Cospar 2010
The new spectra
The additional thermal component (with solar abunances significantly improves the quality of the fits! Detection of shocked ISM?
0.5-0.8 keV
Archive XMM-Newton observationsNew XMM-Newton observations
MOS 1
SRCUT + 1 Thermal component: 2=371.4 (234 d.o.f.) SRCUT + 2 Thermal components: 2=309.9 (231 d.o.f.)
WARNING: preliminary results, to be further investigated
Miceli M.: Shock modification in SN 1006, Cospar 2010
Are these values reasonable?
ISM properties
Miceli M.: Shock modification in SN 1006, Cospar 2010
In collisionless shocks at high Mach Te/Tp <<1 (e.g. Ghavamian et al. 2007). In SN 1006 Te/Tp < 0.07 (Ghavamian et al. 02), i.e.Te<3 keV, for vsh=5000 km/s (Katsuda et al. 09)
0 300 time (yr) 900 1200
Ellison et al 2010
Azimuthal and radial profiles
0.5-0.8 keV 2-4.5 keV
Miceli M.: Shock modification in SN 1006, Cospar 2010
a b,b’,b” c,c’,c” a
bc
Conclusions
The new XMM data allow us to perform a very detailed analysis
We have detected the thermal X-ray emission from the shocked ISM
Further checks and tests are necessary (BKG subtraction, proton flares, etc.)
T, n, and NEI of the shocked ISM are in agreement with those expected
Azimuthal profiles suggest larger shock modification in non-thermal limbs
Miceli M.: Shock modification in SN 1006, Cospar 2010
