observations of snr rx j0852.0-2644 with cangaroo-ii telescope kyoto, dec., 16, 2003 h. katagiri, r....
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Observations of SNR RX J0852.0-2644 with
CANGAROO-II telescope
Kyoto, Dec., 16, 2003
H. Katagiri, R. Enomoto,
M. Mori, L. Ksenofontov
Institute for cosmic ray research (ICRR)
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Introduction
But claimed by Butt et al. and Reimer et al. …
TeV detection from SNRs SN1006 (CANGAROO) => e or p Cas-A (HEGRA) => p RX J1713.2-3946 (CANGAROO) => p
RX J1713.2-3946
Inconclusive problem
Need further evidence
NANTEN supports our results (Fukui et al.)
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ROSAT X-ray image
8o
Vela SNR Maximum X-ray emission
2oSNR RX J0852.0-4622
Flu
x (p
hoto
ns/s
ec/k
eV)
(0.4<E<2.0keV)
Energy (keV)
1 5 10
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Radio
Parkes 4.85GHz survey image(gray scale)
Weak emissionSν at 1GHz =47±12Jy=>same as RXJ1713,SN1006.
Spectral index=0.400.15
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Molecular clouds
Vela SNR taken by NANTEN and soft X-ray image(gray scale) taken by ROSAT.
Around Vela Molecular ridge taken by the Colombia University 1.2m millimeter-wave telescope.
Vela region8
CO integratedIntensity map
NANTEN
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EGRET
No point sourcein CANGAROO FOV
Effected by Vela SNRand pulsar (2.5deg. distance)
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Profiles of RX J0852.0-4622
On the galactic plane => molecular clouds(l,b)=(266.2,-1.2)
Type II SNR Density within SNR
n<2.9×10-2 D1-1/2 f--1/2 (g cm-2)
low => stellar-wind cavity
Ti lineColumn density from X-rayangular size
Distance < 500pc Age 1000 yr
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CANGAROO observations
NW rim with maximum X-ray emission (,)=(132.25,-45.65) Minimum zenith angle 14.6o
=> Energy threshold 500GeV
Observation term 2002 and 2003 ON 97h OFF(background) 89hStereoscopic observation with 2 telescopes (2003) => under analysis
CANGAROO-II 10m IACT in Australia
%30E
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Procedure of analysis
1.Select clustered event
=>remove N.S.B.2.Arrival time of signal Almost the same
time at shower event
3.Cut cloudy data4.Cut low elevation
data 5.Cut hot pixels
N.S.B.
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Image analysis
Source position
Distance
Width
Length
Alpha
Width and Length are theR.M.S. of the ADC countson each axis.
In order to reject cosmic ray events as a noise
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Gamma-ray signal
(ON-OFF)8.0
Results
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Morphology
Consistent with X-ray and radio
PSFSeems to be Point source
Blue:our dataRed:ASCA X-ray dataGreen:4850MHz continuum
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max
2
2exp)(
E
E
cm
EAEQ e
e
ee
(-function approximation)
1
)(4
11)(
4
1~
)(
2
2
dE
dEEQ
d
VdE
dEEVQddE
EdF
ee
ee
Synchrotron/inverse Compton model
Source spectrum
Differential flux of photonsfrom the energy loss of electron
:
:
:
:
:
:
:
max
d
V
E
m
E
e
e Electron energyMass of the electronSpectral indexMaximum accelerated energy of electronsVolume of emission regionDistance from the earthAverage time that an electron ( ) emits a photon ( )eE E
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Inverse Compton process
CMBe EE 2
CMB
CMBTCMBeT
IC
e
IC
E
cc
E
dt
dE
E
3
4
3
41
1~
1
2
2
1
max
2
2
1
2
2
3
222
exp
3
2
4
)(
CMB
e
ee
CMBCMBT
e
IC
IC
E
E
E
cm
cm
E
cm
Ec
cm
A
d
V
dE
EdF
:
:
:
CMB
T
e
Lorentz factor of electrons
Cross section of Thomson scatteringEnergy density of CMB
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Synchrotron process
hcm
eBEE
esyncCMB 422
329.0
2
1
max
2
2
1
2
2
3
222
exp
3
2
4
)(
sync
e
ee
syncBT
e
sync
sync
E
E
E
cm
cm
E
cm
Ec
cm
A
d
V
dE
EdF
8
2BBCMB
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One-zone model: syncIC VV
EGRET:Diffuse emissionUpper limits (counts + 2)
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Two-zone model:
V
X
TeVsyncIC V
VVV
51074
X
TeV
V
V
“Simple”
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Difficulty in two-zone model
54
3
max
3
max
1074104.2
'5.0
24.0
X
TeV
X
TeV
V
V
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410
X
TeV
V
VTeVE 4max
5.2GB 2500
X-ray
TeV
0.2GB 10
Need Chandra, XMM-newton results (filaments ?)and more exact discussion (escape time, energy loss process)
(Aharonian, Atoyan, and Kifune)
Too many parameters!!!
Two-zone model:
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model (Naito-Takahara model)0
22min2
mE
EFdEF
E
20
0
dE
EEdEjdEnEF pE
EE pppp
p
p
,4
max
min
ppp nEj )( to
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max500 exp
10 p
pppp E
EE
erg
E
V
KEj
Intensity of protons
Differential cross section
dE
EEdNE
dE
EEd pp
p ,,
Low energy: isobar modelHigh energy: scaling model
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Fitting parameters
0.2 maxE2
30
500
5.0/10
kpc
d
cmprotons
n
erg
EA
Data CANGAROO EGRET diffuse (upper limits)
DOF/2
DOFDOF // 2min
2
TeVE
A
1.3
8.1
max Best fit
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8.15.0/10
2
30
500
kpc
d
cmprotons
n
erg
EA
30 /505000 cmprotonsn
ergE 50480 1010/
Best fit model
:solid angle of the observed part
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SummaryOur data strongly favour gamma rays
from neutral pions and low flux from synchrotron/inverse Compton.NANTEN data will give us more
physics.Fine structure allow two-zone model.
Chandra and XMM-newton resutlts are needed.
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Check of approximation
TeVE 73max TeVE 100max Factor is 1.5, but it does not change conclusion.
RX J1713.2-3946
Full calculation Delta function approximation