Observations of snr rx j0852 0 2644 with cangaroo ii telescope
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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). Introduction. TeV  detection from SNRs SN1006 (CANGAROO) => e or p Cas-A (HEGRA) => p

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Observations of SNR RX J0852.0-2644 with CANGAROO-II telescope

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Observations of snr rx j0852 0 2644 with cangaroo ii telescope

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)


Introduction

Introduction

TeV  detection from SNRs

SN1006 (CANGAROO) => e or p

Cas-A (HEGRA) => p

RX J1713.2-3946 (CANGAROO) => p

RX J1713.2-3946

But claimed by Butt et al.

and Reimer et al. …

NANTEN supports our results (Fukui et al.)

Inconclusive problem

Need further evidence


Snr rx j0852 0 4622

SNR RX J0852.0-4622

2o

ROSAT X-ray image

(0.4<E<2.0keV)

Maximum

X-ray emission

Vela SNR

Flux (photons/sec/keV)

8o

1

5

10

Energy (keV)


Radio

Radio

  • Weak emissionSν at 1GHz =47±12Jy=>same as RXJ1713,SN1006.

  • Spectral index=0.400.15

Parkes 4.85GHz survey image(gray scale)


Molecular clouds

Molecular clouds

CO integrated

Intensity map

NANTEN

Vela region

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.


Egret

EGRET

Effected by Vela SNR

and pulsar (2.5deg. distance)

No point source

in CANGAROO FOV


Profiles of rx j0852 0 4622

Profiles of RX J0852.0-4622

Ti line

Column density from X-ray

angular size

Distance < 500pc

Age 1000 yr

  • On the galactic plane => molecular clouds(l,b)=(266.2,-1.2)

  • Type II SNR

  • Density within SNR n<2.9×10-2D1-1/2 f--1/2 (g cm-2) low => stellar-wind cavity


Cangaroo observations

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) 89h

  • Stereoscopic observation with 2 telescopes (2003) => under analysis

CANGAROO-II 10m

IACT in Australia


Procedure of analysis

Procedure of analysis

N.S.B.

1.Select clustered event

=>remove N.S.B.

2.Arrival time of signal

Almost the same time at shower event

3.Cut cloudy data

4.Cut low elevation data

5.Cut hot pixels


Image analysis

Image analysis

In order to reject cosmic ray events as a noise

Width

Length

Alpha

Distance

Source position

Width and Length are the

R.M.S. of the ADC counts

on each axis.


Results

Results

Gamma-ray signal

(ON-OFF)

8.0


Morphology

Morphology

Blue:our data

Red:ASCA X-ray data

Green:4850MHz continuum

Consistent with X-ray and radio

PSF

Seems to be Point source


Observations of snr rx j0852 0 2644 with cangaroo ii telescope

Synchrotron/inverse Compton model

Source spectrum

Differential flux of photons

from the energy loss of electron

(-function approximation)

Electron energy

Mass of the electron

Spectral index

Maximum accelerated energy of electrons

Volume of emission region

Distance from the earth

Average time that an electron ( ) emits a photon ( )


Observations of snr rx j0852 0 2644 with cangaroo ii telescope

Inverse Compton process

Lorentz factor of electrons

Cross section of Thomson scattering

Energy density of CMB


Observations of snr rx j0852 0 2644 with cangaroo ii telescope

Synchrotron process


Observations of snr rx j0852 0 2644 with cangaroo ii telescope

One-zone model:

  • EGRET:

  • Diffuse emission

  • Upper limits

    (counts + 2)


Observations of snr rx j0852 0 2644 with cangaroo ii telescope

“Simple”

Two-zone model:


Observations of snr rx j0852 0 2644 with cangaroo ii telescope

Difficulty in two-zone model


Observations of snr rx j0852 0 2644 with cangaroo ii telescope

Two-zone model:

X-ray

TeV

(Aharonian, Atoyan, and Kifune)

Too many parameters!!!

Need Chandra, XMM-newton results (filaments ?)

and more exact discussion (escape time, energy loss process)


Observations of snr rx j0852 0 2644 with cangaroo ii telescope

model (Naito-Takahara model)

to


Observations of snr rx j0852 0 2644 with cangaroo ii telescope

Intensity of protons

Differential cross section

Low energy: isobar model

High energy: scaling model


Observations of snr rx j0852 0 2644 with cangaroo ii telescope

Fitting parameters

Data

CANGAROO

EGRET diffuse (upper limits)

Best fit


Best fit model

Best fit model

:solid angle of the observed part


Summary

Summary

  • Our 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.


Check of approximation

Check of approximation

RX J1713.2-3946

Full calculation

Delta function approximation

Factor is 1.5, but it does not change conclusion.


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