Introduction SNR Pulsar & Nebulae Tokyo-Adelaide Joint W - - PowerPoint PPT Presentation

Galactic Galactic TeV TeV Gamma Gamma-

• Ray Sources

Ray Sources & & Cosmic Cosmic-

• Ray Origin

Ray Origin

• Introduction
• SNR
• Pulsar & Nebulae

Tokyo-Adelaide Joint W ork Shop 2003、 Jan.

Kyoto University Department of Physics

Toru Tanimori (CANGAROO Collaboration)

8m Parabola Focal length 114 (57m2) 80cm CFRP mirrors 552 (1/2”) FOV ~ 3° (4° ) Number of PMTs TDC & ADC Electronics 10m telescope 0.20° (FWHM) (< 0.15° ) Point image size

The first 10m telescope

1999 7mφ

2000 10mφ 0.4TeV 1992 3.8mφ (1.2TeV)

Galactic Targets in CANGAROOII

SNR:

e(Synch.+IC) or proton?

SN006, RX J1713-3946, RCW86, RX J0852-4622,

Pulsar/nebula: Non-pulsed, Young pulsar + synchrotron

nebula IC with 2.7K or SSC by e± Crab, PSR1706, Vela Pulsar, PSR1509, PSR1259, PSRJ1420(EGRET UN ID)

Others: SS433, Galactic Center No source due to proton acceleration??

Origin of Cosmic Rays (Galactic)

• Energetics of Cosmic Rays(<1016 eV)

Required Energy Supply ~1040 erg/s (τ ~ 106~7 yrs, ρCR ~ 1 eV/cm) Unique Candidate SNR Emax＜～1015 eV

• Extra Galactic Origin (>1018 eV)

Emax~1020 eV

• Spectrum Index
• 2.5 ~ -3.0

Shock Acceleration

• Ion

Acceleration Mainly Proton

• Widely believed, but

little observational evidences (Whipple No detection from 6SNR)

Process

• f TeV Gamma-Ray Emission

Uphoton

2 max T I.C.

3 4

γ c

dt dE

σ

=       2 3 4

2 2 max T Sync

B dt dE

cγ σ

=      

6 . 1 −

∝ E

2 . 2 −

∝ E

2 . 2 −

∝ E

2 . 2 −

∝ E

2 . 2 −

∝ E

6 . 1 −

∝ E

Mechanism of TEV Gamma Emission

π0 decay induced by Proton

scattering

Index of Gammaray spectrum similar to that of progenitor proton (~ 2.2 for Shock Acceleration) Low energy cut off (70MeV)

• Inverse Compton Scattering
• f H.E. electrons with hυ

+Synchrotron (Radio to X-ray)

Flatter spectra than those of progenitor electrons (~ 1.6 )

Bremsstrahlung

In high density region (~ 2.2 for Shock Acceleration) + thermal X-ray emission + emission line (neutral Iron 6.4keV)

Observation by ASCA/SIS

• Dominant Power law from NE rim
• Pointed out the possibility TeV

Gamma-Ray Emission

Several Peaks: Thermal Emission `Power-law Synchrotron Rad.

Koyama et al.1995

Significance map

PSF ~ 0.25 deg radius. 10m result(~ 7σ） 3.8m result.(~ 7σ）

Multi band Spectrum & Fitting

Naito et al. Astron. Nach. 320, 1999

• S = -2.2
• B ~ 4 μG
• Emax ~ 50TeV

101 G

max

=       μ B TeV E

• synchro. Spec.

Durham

SN1006 (electron acceleration)

Differential flux(3.8m + 10m) Optical (Hα ) Image

Winkler et al. astro-ph/0208415

1keV 0.2keV

Recent X-ray Observation

TeVγ Emission Region

Chandra SN1006 NE Rim

XMM-Newton 2-10keV

X-ray & Gamma-Ray Observations of RXJ1713.7-3946

• Synch. X-ray Emission(ASCA)

Tomida, Ph.D., 1999

Slane et al, ApJ, 525,1999

Distance ~ 1kpc or 6kpc ?

TeV-Gamma 3.8m Tele.

Muraishi et al., A&Ap 354, 2000

Eγ > ~ 1.5TeV (E –2.5 )

Multi wavelength Spectrum of synchrotron-I.C Model (RJX1713)

Naito et al 2001(CANGAROO)

3µG 5µG 10µG 2µG 20µG

I.C.

1TeV

3.8m

Synchrotron Rad.

I.C. Rad.

RX J1713-3946 Spectrum

8 . 2 −

∝ E

X-ray TeVγ

• Infra. Red

∆θ ∆θ=0o.24(rms)

Enomoto et al, Nature, 416, 823 2002

Proximity of RXJ1713.7-3946

Radio Image @843MHz

Galactic plane CO Image

• Dist. ~6kpc

Density in SNR <<1atom/cm-3

Slane et al, ApJ, 525,1999

Multi wavelength spectrum with Proton Model

proton

Bremsstrahlung

I.C.

15µG 3µG Nature 416, 823 (2002) Bremsstrahlung X from X-ray spectrum

I.C. X

• Dist. 6kpc -> ~ 10 times of the Crab

Counterarguments

O.Reimer & M.Pohl A&A, 390, L43, 2002 M.Butt et al., Nature 418, 489, 2002

∆θ ∆θ=0o.24

0.8o

Cas.A X-ray Non-thermal Spectra

• Bremss. + Synchro.

Cas.A 3.4kpc. 5.9’x5.9’ Emission Line X-ray (6.4 keV) From neutral Iron Chandra Image

• Supernova remnant: Cas A (HEGRA)

Goret et al. 26th ICRC OG2.2.18, 1999

• HEGRA

2000

X-ray Synchrotron SNR

Bamba et al. 2000 Slane et al. 2001 RCW86

ASCA Results

RX J0852-4622 Dist > 1kpc?

• Dist. a few Kpc

Type II

RCW86 Chandra Data

Red : 0.5-1 keV, Green :1-2 keV, Blue : 2-8 keV

J.Rho et al., Astro-ph/0208013

Keplar non thermal component

From whole the SNR

Other characters

Photon Energy (keV)

X-ray Flux by RXTE (>10 keV )

Kepler’s (Index ~ 2.5)

SN1006

Free expansion X-ray remnant ( Hughes 1999 ) Expanding rate of the remnant ( Hughes 1999 )

X-ray >> radio >> optical

×1/2 ×10 –2

Hard tail

Brighter than SN1006 (×2)

In a dense region?

(Bergh et al. 1977, White et al. 1983, and Hughes et al. 1985)

(Petre et al. 1999)

CANGAROO-III (Stereo Observation)

Array of four 10m telescopes(~2004) Full Imaging:

Angular Res. ~0.1 deg.

Energy Threshold: ~100GeV

Pulsar Nebulae

Chandra Images

～10arcsec=0.087pc

～60arcsec=0.58pc

Crab

～200arcsec=4.3pc

PSR1509 PSR1706 Vela

～60arcsec=0.15pc

3.19 150 4.4 37.25 PSR1509-58 102 89 33 Period (ms) 4.24 4.05 3.10 log Age (yr) 1.8 36.53 PSR1706-44 0.5 36.84 Vela 2.0 38.65 Crab Distance (kpc) log L (erg s-1) Name

Pulsar nebulae with highest spin down luminosity (L)

Crab PSR1509-58 Vela PSR1706-44

?

Pulsar Nebula

e-

Nebula Light Cylinder

Blackbody

Synchrotron Inverse Compton 2.7 K CMB photon

X ray Gamma ray B

NASA/CXC/SAO

Crab nebula(unpulsed)

Aharonian & Atoyan, astro-ph/9803091

SSC Model OK!

• Max. of acceleration energy ?

~20 TeV or >100 TeV

Crab Nebula

Observation of Crab nebula (Highest Energy)

10mCANGAROO Tel. 10hrs, Observation 5.9σ 2TeV ~ 20TeV

0.o1

3.8m Tel. (70TeV)

X ray : Spatial resolution Chandra Gamma ray: Energy range CANGAROO - II

Multi-wavelength Model (PSR1706)

Aharonian,Atoyan and Kifune et al(1997)

<Model> Different size of Emission regions X-ray :rx < 30 arcsec B=20µG Gamma-ray:rγ< 0. ゜

1

B=3µG

IC model with 2.7K MBR Sync

PSR1706-44 unpulsed spectrum, from Nebula

3.8m

X-ray gamma-ray B ~3µG

～1 arcsec

(8.7×10-3pc)

Observations with Chandra (PSR1706)

The High Resolution Camera (HRC-I) 2000 Feb 11: 46 ksec Advanced CCD Imaging Spectrometer (ACIS-S) 2000 Aug 13 : 14 ksec ～10arcsec Archive Data HRC Image

(0.08-10 keV)

ACIS Image

(0.7-9 keV)

Nebula

ACIS radial profile 5 arcsec

ACIS PSF 80%: ~1arcsec

Black body+Power law

Pulsar

Spectral Analysis(ACIS)

Power law

Nebula

χ2/d.o.f

kT(keV) Index

Γ

14.8/8 Pulsar 4.9/7

• Nebula

39 . + 72 .

. 2

－ 34 . + 30 .

4 . 1

－ 02 . + 01 .

14 .

－

NH ～ ×1021 cm-2

35 . + 25 .

9 . 5

－

Ｒ ＜ r < 1.2”

Energy(keV)

1.2”< r < 6”

Energy(keV)

10 2 2

Photon/cm2 s keV 2×10-4 2×10-4

TeV Gamma-ray Spectrum

Alpha distribution

Durham(98) *

Compilation of Integral Flux

Preliminary

Statistic error only Crab Flux (E -1.5)

Alpha <15゜ 5.4σ 628±116 events

Differential Flux E-3.2

Multi-wavelength Spectrum of PSR 1706

TeV flux： 10 ×X ray flux Synchrotron cut off > 10keV B~ 1mG & Ee ~20TeV OR B~ 20µG & Ee ~400 TeV difficult to explain Sync-IC(2.7k CMB) model

electron Γ～2.2

• Synch. IC. Model ??

V< 24.5

Where is TeV Gamma ray from?

～0.087pc

X ray(Chandra) Optical(VLT) Size : small Magnetic field : weak Max electron energy: > 100TeV >100 TeV electrons escape quickly without synchrotron energy loss TeV gamma rays are absorbed by IR photons Optical magnitude < 24.5 The effect of absorption is low

V=17.3

Nebula Near Pulsar

TeV γ + IR photon → e+ e－

Synchrotron -IC model Contradict CANGAROO (～1TeV)

Lundqvist et al(1999)

Curvature Radiation

A Model of TeV Gamma-rayRadiation

e± →GeV gamma ray + IR photon (Curvature ) e± + IR photon →TeV gamma ray (IC) ×EGRET αinc =60°

10-10 erg cm-2 s-1

• J. Takata & S.

Shibata(Yamagata Univ)

Spectrum Model of PSR 1706-44 Infrared data→NO Optical data →upper limit Estimated IR spectrum from X ray and radio data

Summary

VHE Gamma-Ray Sources: Pulsar Nebulae, AGN, SNR Almost Sources due to electrons: I.C. Gamma Rays

Where is Proton?? Where is Cosmic Origin?? (SN1006)

But,

One Convincing Candidate of Proton Acceleration Site;

RXJ1713-3934

Another Synch.X-ray SNRs; RCW86 and RX J0852-4622 TeV Gamma-rays from pulsars: Crab & PSR1706

• synch. nebulae observed from almost gamma-ray pulsars,

but acceleration in Nebula OK?