XCTA

CTA

ppπ:
HESS, MAGIC, VERITAS etc.
CTA:CTA/X:HESS, MAGIC, Veritas etc.
CTA:

SNRs emi,ng gamma-rays

Courtesy H. Tajima

Four TeV Gamma-ray SNRsnn

4 TeV gamma ray SNRs age 2000yrs
They are interacting with ISM
RX J1713.7–3946

RX J0852.0–4622

HESS J1731–347

RCW 86

Aharonian+07

Arribas+12

Abramowski+11

Aharonian+09

dimater: ~1 deg.
age: ~1600 yr
ISM: rich CO + cold HI
X-rays: pure synchrotron~2 deg.
~1700−4300 yr
rich HI + little COpure synchrotron ?

~0.5 deg.
~3600−7200 yr
rich CO + HI cavity
pure synchrotron~0.5 deg.
~1800 yrrich HI + little COthermal + non-thermalCO transi:ons to probe molecular hydrogen• Hydrogen molecules are not observable inradio. Too high energy levels. Only inabsorp:on.
• 2.6mm Carbon monoxide CO emission isobserved in rota:onal transi:ons.
NANTEN2, Mopra, ASTE
• 12CO vs. 13CO:
12CO is important to trace all molecular gas.
• In addi:on, HI 21cm emission to probe atomic
hydrogen
GASKAP, SKA

NANTEN & NANTEN2@Las Campanas, alt.2400m@Atacama, alt.4800m

RX J1713.7-3946: 12CO(J=1-0) with X-rays-11 km/s < VLSR < -3 km/s
DAB

C

Fukui et al. 2003

SNR G347.3-0.5 (RXJ1713.7-3946)- Shell-like structure: similar with X-rays- No signiﬁcant varia:on of spectrum index
across the regions- spa:al correla:on with surrounding molecular gas

Aharonian et al. 2005

RX J1713.7-3946

Fukui et al. 2012, ApJ, 746, 82

Dark HI SE Cloud (Self-AbsorpIon)

ISM protons in RX J1713.7-3946
Support hadronic scenario

HI + 2H2

Fukui et al. 2012

Shock propaga:on into dense gas

Vsh ~ 3000 km s−1n : density of clump
n0 : ambient density (=1 cm-3)

10^4 cm-3, t 1000yrs

Penetra:ng Depth = 0.03 pc

n n0
Sano et al. 2010

Inoue, Yamazaki, Inutsuka, Fukui 2012, ApJ, 744, 71

MHD simulaIons of shock-cloud interacIon
density

Inoue+ 2010

vs.

magneIc ﬁeld

density
vs. magneIc ﬁeld
[sub-pc scale]
·½TeV gamma-ray SNR RX J0852.0-4622

Color TeV gamma rays

contour X raysRX J0852: CO distribution (interact with the SNR)n CO vs. X-rays
good spatial correspondence between theCO and X-rays
Interacting with theSNR

image: CO(1-0) I.I.
(Vlsr: 24-33 km/s)
contours: X-ray (1-5 keV)RX J0852: HI distribution (interact with the SNR)n HI vs. X-rays
HI wind bubble atsame velocity in CO
ISM cavity createdby the progenitor

Image: HI I. I.
(Vlsr: 28-34 km/s)
contours: X-ray (1-5 keV)

Vela Jr. total ISM protons & TeV γ-rays(optically thick HI corrected)(lef) Image: Total interstellar proton column density, contours: TeV γ-rays (Aharonian+07)(Right) Azimuthal plots
Fukui, Sano+15 in prep.

Comparison of young SNRs

If the γ -rays are produced predominantly by the hadronic process,- Total CR protons energy ​10↑104848–−​110
0↑4949 erg- CR accelera:on eﬃciency 0.1% - 1%

RXJ0852
Fermi LAT

Gamma-ray spectrum of RXJ1713
Abdo et al. 2011

The hard spectrum is notunique to the leptonic
scenario
The hard spectrum is
explained by energy
dependent penetra:onof CR protons intodense molecular gas.

Hadronic γ-ray spectrum for dense cloud cores
Gabici 2007, Zirakasivili Aharonian 2010,Inoue, Inutsuka, Yamazaki, Fukui 2012

n accelerated par:cles in the cavity diﬀuse into clouds and pions are createdl diﬀusion length-l mass of the cloud penetrated by CR par:cles (Dense cloud cores [ ρl Photon spectrum N(E)number of gamma rays)r- ]M(E) E -p

E 1/2-p = E -1.5 for p = 2

à The same with the leptonic spectrum by ICà Hadronic scenario is consistent with the Fermi spectrumMagellanic SNR N132D

X

d~50 kpc
TeV

SNR ~3150 yr
GMCe.g., Morse+95, Banas+97, Borkowski+07, H.E.S.S. Col.+15614

Banas+97

GMC

Borkowski+07, HS+15b

ROSAT X-ray image
SEST CO2-1 contours

BANAS ET AL.

CO & HI

Chandra X

nX~10,000 M

CO 1-0, 3-2> 6,000 M(0.5-7.0 keV)

CO 3−2/1−0↑←
Chandra X

n SNR
︎ HS+15b(> 0.8)

256-266 km/s
(0.5-7.0 keV)n H.E.S.S.
︎TeVN132D− TeV−TeVand/orà

ISMWpp(H.E.S.S. Collabora:on+15)

Wpp = 1052-3 −1(n 1 cm ) (d 50 kpc)

−2HSNRd = 50 kpc,

Wpp ~ 1×10 50 erg

nH ~ 90 cm−3HESS γ-ray excess imageChandra X-ray contours

HESS Col.+15

TeV γ vs. CO(J=1-0)

LeS: NANTEN 12CO(1-0) image (beam size : 2.7’) of the W 28 region for VLSR=0 to 10 km/s with
VHE γ ray signiﬁcance contours overlaid (green) -levels 4,5,6σ. The radio boundary ofW 28, the 68% and 95% locaIon contours of GRO J1801 2320 and the locaIon of the HIIregion W 28A2 (white stars) are indicated.
Right: NANTEN 12CO(1-0) image for VLSR=10 to 20 km/s.
(Aharonian et al. 2007)30

W44 GeV gamma & CO
Fermi/NANTEN2 results
New AGILE/NANTEN2 results
Cardillo+ 2013

Color NANTEN2 CO

CTA
TeV

HESSJ1731(XX
CTA:“RXJ1713(),W28(),RXJ0852(Vela Jr.
), W44

N132D, 30Dor C(”),

Q39
Q23,24),N49 etc.