Correlation between high energy objects and molecular clouds in the Galaxy; lessons in the SNR RXJ1713.7-3946and Westerlund 2

Astrophysics group meeting, November 19-20, 2009

Yasuo Fukui

Astrophysics lab. Radio astronomy

The Galaxy

Galactic center - magnetic flotation loops

Massive star formation – Wd2, Carina etc.

Molecular jets – Wd2, etc.

Gamma ray sources – RXJ1713, W28, Wd2, Wd1, etc.

SNR, PWN, molecular clouds

Galaxies

Magellanic clouds – GMC evolution (Kawamura)

Galactic nuclei

Aims; Star formation, gas dynamics (magnetic force, gravity), high energy phenomena (gamma, relativistic jets)

International collaborations; NANTEN2/Spitzer/Fermi/HESS/Herschel/Planck/….

Publications; PASJ two special issues / ApJ / AA /AJ / Science etc. reviews in ARAA2010, PPV etc.

3

4

NANTEN & NANTEN2

@Atacama, alt.4860m@Las Campanas,

alt.2400m

NANTEN2 at Atacama 4860m

NANTEN CO Galactic Plane Survey•12CO(J=1-0), Grid size ~ 4 (|b|<5), 8 (5<|b|<10)

•Integ. time (typ) ~5sec/point, 1,100,000 observed points

Molecular loops as evidence for magnetic flotation driven by the Parker Instability

300 pc

600 pc

30

0 p

c2

20

pc

Loop 1

Loop 2

Magnetic loop in solar corona

(TRACE：191Å)

MHD activities of galactic disks

Fukui et al. (2006)7

RXJ1713 TeV g SNR (1)

Pfeffermann and Aschenbach 1996 ROSAT

Koyama et al. 1997 ASCA

X ray absorption 6x10^21 cm-2

GC absorption 6x10^22 cm-2 1kpc

Slane et al. 1999 molecular cloud at -94 km s-1

X ray absorption 8x10^21 cm-2

N(HI) 1.2x10^22 cm-2 6.3kpc

Fukui et al. 2003

different molecular clouds at -10 km s-1 1kpc

widely accepted

identify associated gas–candidate for target proton8

RXJ1713 TeV g SNR (2)

Emission mechanism of g ray; cosmic ray protons?

leptonic (electron IC) or

hadronic (proton, neutral pion)

Aharonian et al. 2007 HESS etc.

Tanaka et al. 2008 Suzaku and HESS

strong magnetic field 100mG

IC is not effective to produce g ray

target protons are uniform

because X/ g ray is uniform

Fukui 2008 correlation btw. molecular clouds and X/ g ray suggests target protons are non uniform

9

Comparison of 12CO(J=1-0) with X-ray RXJ1713

(Fukui et al. 2003)

molecular holesurrounding boundary of the SNR

CO peaks⇔X-ray peaks show good spatial correlation(northwestern bright rim)

↓

indicates interaction of the gray peak of the SNR with molecular clouds.

D

A

B

C

RXJ1713 CO Velocity distribution by NANTEN

Moriguchi et al. 2005

VLSR and kinematic distance

NANTEN2 CO(2-1) vs X ray (XMM)

ASTE CO J=3-2

RXJ1713 Peak C : X ray vs. 12CO(J=1-0)

image:0.2-12KeV Xrayby Suzaku XIS

Takahashi et al 2008

Contour:12CO(J=1-0)by NANTEN

velocity range-12 km/s – 3km/s

min. = 3K km/sinterval = 7K km/s

Peak C : 12CO(J=3-2) vs 12CO(J=4-3)

←12CO(3-2) observed by ASTE

velocity lange : -12 - -3 km/s

min. : 3.0K km/s interval : 1.5 K km/s

Moriguchi et al 2005

↑12CO(3-2) observed by ASTE

velocity lange : -12 - -3 km/s

min. : 3.0K km/s interval : 1.5 K km/s

Red crosses show the position of the IRAS point sources in each map

12CO(3-2)

12CO(4-3)

1pc

1pc

RXJ1713/ G347.3 : TeV Gamma vs 12CO(J=1-0)

Image:

TeV gamma ray

by H.E.S.S

Contour:

12CO(J=1-0)

by nanten

velocity range

-18 km/s – 0km/s

min. = 3K km/s

interval = 7K km/s

Map of J1713.7-3946

5pc

SNR G347.3-0.5 (RXJ1713.7-3946)

-Shell-like structure: similar with X-rays- No significant variation of spectrum index across the regions-spatial correlation with surrounding molecular gas

Aharonian et al. 2005

RXJ1713 Peak C : X ray vs. 12CO(J=1-0)

image:0.2-12KeV Xrayby Suzaku XIS

Takahashi et al 2008

Contour:12CO(J=1-0)by NANTEN

velocity range-12 km/s – 3km/s

min. = 3K km/sinterval = 7K km/s

White contour:

12CO(J=1-0)

by nanten

velocity range

-18 km/s – 0km/s

min. = 3K km/s

interval = 7K km/s

White contour:

12CO(J=4-3)

by nanten

velocity range

-18 km/s – 0km/s

min. = 3K km/s

interval = 3K km/s

12CO(J=4-3)

Black contour:

0.2-12KeV Xray

by Suzaku XIS

Takahashi et al 2008

Image:

TeV gamma ray

by H.E.S.S

Aharonian et al 2007

1pc

IRAS Source

PeakC detailed analyses

Red line: Gamma-rayBlue line: HI gasBlack lime: 12CO(J=2-1)

Fig.3. Image: (a)gamma-ray (b) X-rayContour: NANTEN2 12CO(J=2-1)

-11 km/s

-4 km/s

-3 km/s

-2 km/s

Tanaka et al. 2008

B=100mG IC failshadronic supported

X/g ratio uniform

Some recent “e” injection in the west

0.1deg resolutionMuch more scattering

Targtets are non uniform

Fig.2. Image: X-ray taken by Suzaku. (Tanaka et al. 2008)Contour: 12CO(J=2-1) taken by NANTEN2.

CO vs X-ray Distributions

Fig.1. Image: Gamma-ray taken by HESS. (Aharonian et al. 2006)Contour: 12CO(J=2-1) taken by NANTEN2.

CO vs Gamma-ray Distributions

TeV g ray vs HI

Image:

HI 21cm line

by A.T.C.A.

Contour:

TeV gamma ray

by H.E.S.S.

min. = 20 count

interval = 10 count

Map of J1713.7-3946

-16 km/s - -3 km/s

Fig.4. Image: Gamma-ray taken by HESS.Contour: HI gas taken by ATCA.

SE-rim detailed analyses

Red line: Gamma-rayBlue line: HI gasBlack lime: 12CO(J=2-1)

Another one

Numerical simulations

Density log (n) |B|

(Inoue, Inutsuka 2009)

SNR RXJ1713 summary

• g ray correlates well with CO/HI, allows new detailed identification of target protons in a density range from 10 to 10^3 cm-3

(southeastern rim 10^21cm-2/3pc = 100cm-3)

• Hadronic origin is supported

• Cosmic ray proton will be estimated by careful analysis of HI and CO

• Theories seem to be consistent

Molecular Jets discovered by NANTEN

High J=2-1/1-0 ratio

Westerlund 2 (Wd2)

(l, b) = (284.27, -0 .33)

O Star 12WR Star 2

WR20a, WR20bTotal mass of stars 4500Mo

Age 2-3 Myr

(Rauw et al. 2007)

(Piatti et al. 1998)

Spitzer IRAC ; 3.5 (blue), 4.5 (green), 5.8 (orange), 8.0 (red) mm

RCW 49

Distribution of dust influencedby starsStar formation in progress

YSO 300

(Churchwell et al. 1998)

(Whitney et al. 2004)

Super star cluster

Distance vs. Temperature

Image: Tkin, Contour: 12CO(2-1),

red cross：Wd2

+16 km/s Cloud

+4 km/s Cloud

Temperature of the +4 km s-1 cloud is higher than the 16

km s-1

The molecular cloud near Wd2 is warmer than the outside.

Inside: ~70 K @ 5 pc

Outside: ~10 K @ 20 pc

G.L. 284.2-284.4Contour: 12CO(J=2-1)Blue: +4 km/s Cloud Red: +16 km/s Cloud

Cloud-Cloud Collision

16 km s-1

Distance

velocity of 16 km s-1, 4 km s-1, and -4 km s-1 components

assume the rotation curve of Brand & Blitz 1993

5.5 1.5 kpc

Mass

9.1 4.1 104 Mo

8.1 3.7 104 Mo~16 km s-1 cloud

~ 4 km s-1 cloud

Kinetic Energy

1.2 0.5 1050 ergs 3.6 1051 ergs

Energy of stellar wind

(Rauw et al. 2007)

X factor：2.0 1020 cm-2 (K km s-1)-1

12CO(J=1-0)

a) Integrated intensity of 12CO(J=1-0)

b) Position-Velocity diagramof 12CO(J=1-0)

Arc (Vlsr = 24 – 28 km/s)

min.= 2.6 K km/s (3 sigma)

interval = 1.8 K km/s

Jet (Vlsr = 28-30 km/s)

min = 2.1 K km/s (3 sigma)

interval = 0.7 K km/s

Jet 2 (Vlsr = 25 – 28 Km/s)

min = 2.4 K km/s (3 sigma)

interval = 1.6 K km/s

Cross : the center of HESS J1023-575

Yellow box & dashed lines in a)show the integrated regions ofP-V diagram of Arc & Jet.

Gray scale： HI（1 channel @26 km/s）

Red: Integrated intensity of arc

（23~28km/s）White: Integrated intensity of jet

（28~30km/s）Orange：HESS J1023-575

Results

Ｗｅｓｔｅｒｌｕｎｄ 2

Discussion: LVG analysis

Jet and Arc Formation Scenario

• Relativistic jet passes through atomic gas with non-uniform density.

• Shock wave propagates cylindrically, compressing the atomic gas and forming jet-like molecular gas. (Yamamoto et al. 2008)

• Spherical explosion compresses the atomic gas to form shell-like structure in HI and arc-like molecular cloud.

• Gamma-rays emitted from remnant neutron star?

Suggestion : Cloud and Gamma-ray Source Formation Scenario

• Progenitor has strong magnetic field of ~1013-15 G.

• Candidate objects for gamma ray bursts.

• Results of simulations show relativistic jet-like explosions.

• Remnant becomes special class of neutron star called magnetor.

About

Anisotropic supernova explosions

Takiwaki et al. 2009

Results : Ratio

At jet tip, 12CO(2-1) to 12CO(1-0) ratio is higher.

Parent cloud

candidates

Dame 2007

Discovery of jet- and arc-like molecular clouds

Parent cloud candidates Furukawa et al. 2009, Ohama et al. submitted

White：stellar cluster, Wd2

Red：TeV gamma-ray source

MOPRA 12CO J=1-0 Result s: S3

LVG analysis

S1 northern part

S1 southern part

S3 northern part

S3 southern part

S1 northern partN(H2) ~ 800 cm-3

T(kin) ~ 18 K

S1 southern partN(H2) ~ 300 cm-3

T(kin) ~ 15 K

S3 northern partN(H2) ~ 200 cm-3

T(kin) ~ 22 K

S3 southern partN(H2) ~ 300 cm-3

T(kin) ~ 65 K

G327.5

Molecular Jet Survey by NANTEN2 -12CO(J=2-1)-

SS433

MJG23.8 MJG359.5

MJG347.5

MJG343.1

MJG327.5

MJG348.5

+

GRS1915+105

Wd2

MJG343.1 MJG327.5

MJG359.5SS433 southMJG348.5 S3

Wd2

Astrophysical jets

Microquasar jets/

Anisotropic SNe

(Mirabel & Rodríguez 1994)

GRS1915+105

(3.5cm conti.)

3C296

Molecular Jets discovered by NANTEN

High J=2-1/1-0 ratio

Left: 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 of

W 28, the 68% and 95% location contours of GRO J1801－2320 and the location of the HII

region W 28A2 (white stars) are indicated.

Right: NANTEN 12CO(1-0) image for VLSR=10 to 20 km/s.

(Aharonian et al. 2007)

TeV γ vs. CO(J=1-0) W28

NANTEN2 12CO(2-1) image of the

W 28 region for VLSR=-10 to 25

km/s with VHE γ ray significance

contours overlaid (yellow) levels

4,5,6σ.

The location of the HII region

W 28A2 (white stars) are indicated.

(Aharonian et al.2008)

TeV γ vs. CO(J=2-1)

NANTEN CO Galactic Plane Survey•12CO(J=1-0), Grid size ~ 4 (|b|<5), 8 (5<|b|<10)

•Integ. time (typ) ~5sec/point, 1,100,000 observed points

3-D M-JET PROJECT 2010-2014

Future plan with NANTEN2;

3-dim molecular temperature survey

By CO J=1-0, 2-1, 3-2 at 1 arcmin

Coverage；

l = 200 deg. – 60 deg.

b= -30 deg. to 30 deg.

number of spectra 10^7

Systematic jet search；

expect new ~100 molecular jets (9 at present)

correlation with CTA gamma ray sources, ~1000 galactic sources (~50 sources by HESS)

Fermi, IR, X ray surveys, and ALMA67

ALMA (2012-)

Atacama Large Millimeter/submillimeter Array0.1”-1”(~ 0.1 pc@50kpc)