Correlation between high energy - 名古屋大学...(Whitney et al. 2004) Super star cluster...
Transcript of Correlation between high energy - 名古屋大学...(Whitney et al. 2004) Super star cluster...
![Page 1: Correlation between high energy - 名古屋大学...(Whitney et al. 2004) Super star cluster Distance vs. Temperature Image: T kin, Contour: 12CO(2-1), red cross:Wd2 +16 km/s Cloud](https://reader034.fdocuments.us/reader034/viewer/2022042917/5f597c4b53c0ab4cbb5f957f/html5/thumbnails/1.jpg)
![Page 2: Correlation between high energy - 名古屋大学...(Whitney et al. 2004) Super star cluster Distance vs. Temperature Image: T kin, Contour: 12CO(2-1), red cross:Wd2 +16 km/s Cloud](https://reader034.fdocuments.us/reader034/viewer/2022042917/5f597c4b53c0ab4cbb5f957f/html5/thumbnails/2.jpg)
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
![Page 3: Correlation between high energy - 名古屋大学...(Whitney et al. 2004) Super star cluster Distance vs. Temperature Image: T kin, Contour: 12CO(2-1), red cross:Wd2 +16 km/s Cloud](https://reader034.fdocuments.us/reader034/viewer/2022042917/5f597c4b53c0ab4cbb5f957f/html5/thumbnails/3.jpg)
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
![Page 4: Correlation between high energy - 名古屋大学...(Whitney et al. 2004) Super star cluster Distance vs. Temperature Image: T kin, Contour: 12CO(2-1), red cross:Wd2 +16 km/s Cloud](https://reader034.fdocuments.us/reader034/viewer/2022042917/5f597c4b53c0ab4cbb5f957f/html5/thumbnails/4.jpg)
4
NANTEN & NANTEN2
@Atacama, alt.4860m@Las Campanas,
alt.2400m
![Page 5: Correlation between high energy - 名古屋大学...(Whitney et al. 2004) Super star cluster Distance vs. Temperature Image: T kin, Contour: 12CO(2-1), red cross:Wd2 +16 km/s Cloud](https://reader034.fdocuments.us/reader034/viewer/2022042917/5f597c4b53c0ab4cbb5f957f/html5/thumbnails/5.jpg)
NANTEN2 at Atacama 4860m
![Page 6: Correlation between high energy - 名古屋大学...(Whitney et al. 2004) Super star cluster Distance vs. Temperature Image: T kin, Contour: 12CO(2-1), red cross:Wd2 +16 km/s Cloud](https://reader034.fdocuments.us/reader034/viewer/2022042917/5f597c4b53c0ab4cbb5f957f/html5/thumbnails/6.jpg)
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
![Page 7: Correlation between high energy - 名古屋大学...(Whitney et al. 2004) Super star cluster Distance vs. Temperature Image: T kin, Contour: 12CO(2-1), red cross:Wd2 +16 km/s Cloud](https://reader034.fdocuments.us/reader034/viewer/2022042917/5f597c4b53c0ab4cbb5f957f/html5/thumbnails/7.jpg)
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
![Page 8: Correlation between high energy - 名古屋大学...(Whitney et al. 2004) Super star cluster Distance vs. Temperature Image: T kin, Contour: 12CO(2-1), red cross:Wd2 +16 km/s Cloud](https://reader034.fdocuments.us/reader034/viewer/2022042917/5f597c4b53c0ab4cbb5f957f/html5/thumbnails/8.jpg)
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
![Page 9: Correlation between high energy - 名古屋大学...(Whitney et al. 2004) Super star cluster Distance vs. Temperature Image: T kin, Contour: 12CO(2-1), red cross:Wd2 +16 km/s Cloud](https://reader034.fdocuments.us/reader034/viewer/2022042917/5f597c4b53c0ab4cbb5f957f/html5/thumbnails/9.jpg)
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
![Page 10: Correlation between high energy - 名古屋大学...(Whitney et al. 2004) Super star cluster Distance vs. Temperature Image: T kin, Contour: 12CO(2-1), red cross:Wd2 +16 km/s Cloud](https://reader034.fdocuments.us/reader034/viewer/2022042917/5f597c4b53c0ab4cbb5f957f/html5/thumbnails/10.jpg)
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
![Page 11: Correlation between high energy - 名古屋大学...(Whitney et al. 2004) Super star cluster Distance vs. Temperature Image: T kin, Contour: 12CO(2-1), red cross:Wd2 +16 km/s Cloud](https://reader034.fdocuments.us/reader034/viewer/2022042917/5f597c4b53c0ab4cbb5f957f/html5/thumbnails/11.jpg)
RXJ1713 CO Velocity distribution by NANTEN
Moriguchi et al. 2005
![Page 12: Correlation between high energy - 名古屋大学...(Whitney et al. 2004) Super star cluster Distance vs. Temperature Image: T kin, Contour: 12CO(2-1), red cross:Wd2 +16 km/s Cloud](https://reader034.fdocuments.us/reader034/viewer/2022042917/5f597c4b53c0ab4cbb5f957f/html5/thumbnails/12.jpg)
VLSR and kinematic distance
![Page 13: Correlation between high energy - 名古屋大学...(Whitney et al. 2004) Super star cluster Distance vs. Temperature Image: T kin, Contour: 12CO(2-1), red cross:Wd2 +16 km/s Cloud](https://reader034.fdocuments.us/reader034/viewer/2022042917/5f597c4b53c0ab4cbb5f957f/html5/thumbnails/13.jpg)
NANTEN2 CO(2-1) vs X ray (XMM)
![Page 14: Correlation between high energy - 名古屋大学...(Whitney et al. 2004) Super star cluster Distance vs. Temperature Image: T kin, Contour: 12CO(2-1), red cross:Wd2 +16 km/s Cloud](https://reader034.fdocuments.us/reader034/viewer/2022042917/5f597c4b53c0ab4cbb5f957f/html5/thumbnails/14.jpg)
ASTE CO J=3-2
![Page 15: Correlation between high energy - 名古屋大学...(Whitney et al. 2004) Super star cluster Distance vs. Temperature Image: T kin, Contour: 12CO(2-1), red cross:Wd2 +16 km/s Cloud](https://reader034.fdocuments.us/reader034/viewer/2022042917/5f597c4b53c0ab4cbb5f957f/html5/thumbnails/15.jpg)
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
![Page 16: Correlation between high energy - 名古屋大学...(Whitney et al. 2004) Super star cluster Distance vs. Temperature Image: T kin, Contour: 12CO(2-1), red cross:Wd2 +16 km/s Cloud](https://reader034.fdocuments.us/reader034/viewer/2022042917/5f597c4b53c0ab4cbb5f957f/html5/thumbnails/16.jpg)
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
![Page 17: Correlation between high energy - 名古屋大学...(Whitney et al. 2004) Super star cluster Distance vs. Temperature Image: T kin, Contour: 12CO(2-1), red cross:Wd2 +16 km/s Cloud](https://reader034.fdocuments.us/reader034/viewer/2022042917/5f597c4b53c0ab4cbb5f957f/html5/thumbnails/17.jpg)
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
![Page 18: Correlation between high energy - 名古屋大学...(Whitney et al. 2004) Super star cluster Distance vs. Temperature Image: T kin, Contour: 12CO(2-1), red cross:Wd2 +16 km/s Cloud](https://reader034.fdocuments.us/reader034/viewer/2022042917/5f597c4b53c0ab4cbb5f957f/html5/thumbnails/18.jpg)
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
![Page 19: Correlation between high energy - 名古屋大学...(Whitney et al. 2004) Super star cluster Distance vs. Temperature Image: T kin, Contour: 12CO(2-1), red cross:Wd2 +16 km/s Cloud](https://reader034.fdocuments.us/reader034/viewer/2022042917/5f597c4b53c0ab4cbb5f957f/html5/thumbnails/19.jpg)
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
![Page 20: Correlation between high energy - 名古屋大学...(Whitney et al. 2004) Super star cluster Distance vs. Temperature Image: T kin, Contour: 12CO(2-1), red cross:Wd2 +16 km/s Cloud](https://reader034.fdocuments.us/reader034/viewer/2022042917/5f597c4b53c0ab4cbb5f957f/html5/thumbnails/20.jpg)
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
![Page 21: Correlation between high energy - 名古屋大学...(Whitney et al. 2004) Super star cluster Distance vs. Temperature Image: T kin, Contour: 12CO(2-1), red cross:Wd2 +16 km/s Cloud](https://reader034.fdocuments.us/reader034/viewer/2022042917/5f597c4b53c0ab4cbb5f957f/html5/thumbnails/21.jpg)
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)
![Page 22: Correlation between high energy - 名古屋大学...(Whitney et al. 2004) Super star cluster Distance vs. Temperature Image: T kin, Contour: 12CO(2-1), red cross:Wd2 +16 km/s Cloud](https://reader034.fdocuments.us/reader034/viewer/2022042917/5f597c4b53c0ab4cbb5f957f/html5/thumbnails/22.jpg)
![Page 23: Correlation between high energy - 名古屋大学...(Whitney et al. 2004) Super star cluster Distance vs. Temperature Image: T kin, Contour: 12CO(2-1), red cross:Wd2 +16 km/s Cloud](https://reader034.fdocuments.us/reader034/viewer/2022042917/5f597c4b53c0ab4cbb5f957f/html5/thumbnails/23.jpg)
-11 km/s
![Page 24: Correlation between high energy - 名古屋大学...(Whitney et al. 2004) Super star cluster Distance vs. Temperature Image: T kin, Contour: 12CO(2-1), red cross:Wd2 +16 km/s Cloud](https://reader034.fdocuments.us/reader034/viewer/2022042917/5f597c4b53c0ab4cbb5f957f/html5/thumbnails/24.jpg)
-4 km/s
![Page 25: Correlation between high energy - 名古屋大学...(Whitney et al. 2004) Super star cluster Distance vs. Temperature Image: T kin, Contour: 12CO(2-1), red cross:Wd2 +16 km/s Cloud](https://reader034.fdocuments.us/reader034/viewer/2022042917/5f597c4b53c0ab4cbb5f957f/html5/thumbnails/25.jpg)
-3 km/s
![Page 26: Correlation between high energy - 名古屋大学...(Whitney et al. 2004) Super star cluster Distance vs. Temperature Image: T kin, Contour: 12CO(2-1), red cross:Wd2 +16 km/s Cloud](https://reader034.fdocuments.us/reader034/viewer/2022042917/5f597c4b53c0ab4cbb5f957f/html5/thumbnails/26.jpg)
-2 km/s
![Page 27: Correlation between high energy - 名古屋大学...(Whitney et al. 2004) Super star cluster Distance vs. Temperature Image: T kin, Contour: 12CO(2-1), red cross:Wd2 +16 km/s Cloud](https://reader034.fdocuments.us/reader034/viewer/2022042917/5f597c4b53c0ab4cbb5f957f/html5/thumbnails/27.jpg)
Tanaka et al. 2008
![Page 28: Correlation between high energy - 名古屋大学...(Whitney et al. 2004) Super star cluster Distance vs. Temperature Image: T kin, Contour: 12CO(2-1), red cross:Wd2 +16 km/s Cloud](https://reader034.fdocuments.us/reader034/viewer/2022042917/5f597c4b53c0ab4cbb5f957f/html5/thumbnails/28.jpg)
B=100mG IC failshadronic supported
![Page 29: Correlation between high energy - 名古屋大学...(Whitney et al. 2004) Super star cluster Distance vs. Temperature Image: T kin, Contour: 12CO(2-1), red cross:Wd2 +16 km/s Cloud](https://reader034.fdocuments.us/reader034/viewer/2022042917/5f597c4b53c0ab4cbb5f957f/html5/thumbnails/29.jpg)
X/g ratio uniform
Some recent “e” injection in the west
![Page 30: Correlation between high energy - 名古屋大学...(Whitney et al. 2004) Super star cluster Distance vs. Temperature Image: T kin, Contour: 12CO(2-1), red cross:Wd2 +16 km/s Cloud](https://reader034.fdocuments.us/reader034/viewer/2022042917/5f597c4b53c0ab4cbb5f957f/html5/thumbnails/30.jpg)
0.1deg resolutionMuch more scattering
Targtets are non uniform
![Page 31: Correlation between high energy - 名古屋大学...(Whitney et al. 2004) Super star cluster Distance vs. Temperature Image: T kin, Contour: 12CO(2-1), red cross:Wd2 +16 km/s Cloud](https://reader034.fdocuments.us/reader034/viewer/2022042917/5f597c4b53c0ab4cbb5f957f/html5/thumbnails/31.jpg)
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
![Page 32: Correlation between high energy - 名古屋大学...(Whitney et al. 2004) Super star cluster Distance vs. Temperature Image: T kin, Contour: 12CO(2-1), red cross:Wd2 +16 km/s Cloud](https://reader034.fdocuments.us/reader034/viewer/2022042917/5f597c4b53c0ab4cbb5f957f/html5/thumbnails/32.jpg)
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
![Page 33: Correlation between high energy - 名古屋大学...(Whitney et al. 2004) Super star cluster Distance vs. Temperature Image: T kin, Contour: 12CO(2-1), red cross:Wd2 +16 km/s Cloud](https://reader034.fdocuments.us/reader034/viewer/2022042917/5f597c4b53c0ab4cbb5f957f/html5/thumbnails/33.jpg)
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
![Page 34: Correlation between high energy - 名古屋大学...(Whitney et al. 2004) Super star cluster Distance vs. Temperature Image: T kin, Contour: 12CO(2-1), red cross:Wd2 +16 km/s Cloud](https://reader034.fdocuments.us/reader034/viewer/2022042917/5f597c4b53c0ab4cbb5f957f/html5/thumbnails/34.jpg)
-16 km/s - -3 km/s
![Page 35: Correlation between high energy - 名古屋大学...(Whitney et al. 2004) Super star cluster Distance vs. Temperature Image: T kin, Contour: 12CO(2-1), red cross:Wd2 +16 km/s Cloud](https://reader034.fdocuments.us/reader034/viewer/2022042917/5f597c4b53c0ab4cbb5f957f/html5/thumbnails/35.jpg)
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)
![Page 36: Correlation between high energy - 名古屋大学...(Whitney et al. 2004) Super star cluster Distance vs. Temperature Image: T kin, Contour: 12CO(2-1), red cross:Wd2 +16 km/s Cloud](https://reader034.fdocuments.us/reader034/viewer/2022042917/5f597c4b53c0ab4cbb5f957f/html5/thumbnails/36.jpg)
Another one
![Page 37: Correlation between high energy - 名古屋大学...(Whitney et al. 2004) Super star cluster Distance vs. Temperature Image: T kin, Contour: 12CO(2-1), red cross:Wd2 +16 km/s Cloud](https://reader034.fdocuments.us/reader034/viewer/2022042917/5f597c4b53c0ab4cbb5f957f/html5/thumbnails/37.jpg)
Numerical simulations
Density log (n) |B|
(Inoue, Inutsuka 2009)
![Page 38: Correlation between high energy - 名古屋大学...(Whitney et al. 2004) Super star cluster Distance vs. Temperature Image: T kin, Contour: 12CO(2-1), red cross:Wd2 +16 km/s Cloud](https://reader034.fdocuments.us/reader034/viewer/2022042917/5f597c4b53c0ab4cbb5f957f/html5/thumbnails/38.jpg)
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
![Page 39: Correlation between high energy - 名古屋大学...(Whitney et al. 2004) Super star cluster Distance vs. Temperature Image: T kin, Contour: 12CO(2-1), red cross:Wd2 +16 km/s Cloud](https://reader034.fdocuments.us/reader034/viewer/2022042917/5f597c4b53c0ab4cbb5f957f/html5/thumbnails/39.jpg)
Molecular Jets discovered by NANTEN
High J=2-1/1-0 ratio
![Page 40: Correlation between high energy - 名古屋大学...(Whitney et al. 2004) Super star cluster Distance vs. Temperature Image: T kin, Contour: 12CO(2-1), red cross:Wd2 +16 km/s Cloud](https://reader034.fdocuments.us/reader034/viewer/2022042917/5f597c4b53c0ab4cbb5f957f/html5/thumbnails/40.jpg)
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
![Page 41: Correlation between high energy - 名古屋大学...(Whitney et al. 2004) Super star cluster Distance vs. Temperature Image: T kin, Contour: 12CO(2-1), red cross:Wd2 +16 km/s Cloud](https://reader034.fdocuments.us/reader034/viewer/2022042917/5f597c4b53c0ab4cbb5f957f/html5/thumbnails/41.jpg)
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
![Page 42: Correlation between high energy - 名古屋大学...(Whitney et al. 2004) Super star cluster Distance vs. Temperature Image: T kin, Contour: 12CO(2-1), red cross:Wd2 +16 km/s Cloud](https://reader034.fdocuments.us/reader034/viewer/2022042917/5f597c4b53c0ab4cbb5f957f/html5/thumbnails/42.jpg)
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
![Page 43: Correlation between high energy - 名古屋大学...(Whitney et al. 2004) Super star cluster Distance vs. Temperature Image: T kin, Contour: 12CO(2-1), red cross:Wd2 +16 km/s Cloud](https://reader034.fdocuments.us/reader034/viewer/2022042917/5f597c4b53c0ab4cbb5f957f/html5/thumbnails/43.jpg)
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
![Page 44: Correlation between high energy - 名古屋大学...(Whitney et al. 2004) Super star cluster Distance vs. Temperature Image: T kin, Contour: 12CO(2-1), red cross:Wd2 +16 km/s Cloud](https://reader034.fdocuments.us/reader034/viewer/2022042917/5f597c4b53c0ab4cbb5f957f/html5/thumbnails/44.jpg)
12CO(J=1-0)
![Page 45: Correlation between high energy - 名古屋大学...(Whitney et al. 2004) Super star cluster Distance vs. Temperature Image: T kin, Contour: 12CO(2-1), red cross:Wd2 +16 km/s Cloud](https://reader034.fdocuments.us/reader034/viewer/2022042917/5f597c4b53c0ab4cbb5f957f/html5/thumbnails/45.jpg)
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.
![Page 46: Correlation between high energy - 名古屋大学...(Whitney et al. 2004) Super star cluster Distance vs. Temperature Image: T kin, Contour: 12CO(2-1), red cross:Wd2 +16 km/s Cloud](https://reader034.fdocuments.us/reader034/viewer/2022042917/5f597c4b53c0ab4cbb5f957f/html5/thumbnails/46.jpg)
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
![Page 47: Correlation between high energy - 名古屋大学...(Whitney et al. 2004) Super star cluster Distance vs. Temperature Image: T kin, Contour: 12CO(2-1), red cross:Wd2 +16 km/s Cloud](https://reader034.fdocuments.us/reader034/viewer/2022042917/5f597c4b53c0ab4cbb5f957f/html5/thumbnails/47.jpg)
Results
![Page 48: Correlation between high energy - 名古屋大学...(Whitney et al. 2004) Super star cluster Distance vs. Temperature Image: T kin, Contour: 12CO(2-1), red cross:Wd2 +16 km/s Cloud](https://reader034.fdocuments.us/reader034/viewer/2022042917/5f597c4b53c0ab4cbb5f957f/html5/thumbnails/48.jpg)
Westerlund 2
![Page 49: Correlation between high energy - 名古屋大学...(Whitney et al. 2004) Super star cluster Distance vs. Temperature Image: T kin, Contour: 12CO(2-1), red cross:Wd2 +16 km/s Cloud](https://reader034.fdocuments.us/reader034/viewer/2022042917/5f597c4b53c0ab4cbb5f957f/html5/thumbnails/49.jpg)
Discussion: LVG analysis
![Page 50: Correlation between high energy - 名古屋大学...(Whitney et al. 2004) Super star cluster Distance vs. Temperature Image: T kin, Contour: 12CO(2-1), red cross:Wd2 +16 km/s Cloud](https://reader034.fdocuments.us/reader034/viewer/2022042917/5f597c4b53c0ab4cbb5f957f/html5/thumbnails/50.jpg)
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?
![Page 51: Correlation between high energy - 名古屋大学...(Whitney et al. 2004) Super star cluster Distance vs. Temperature Image: T kin, Contour: 12CO(2-1), red cross:Wd2 +16 km/s Cloud](https://reader034.fdocuments.us/reader034/viewer/2022042917/5f597c4b53c0ab4cbb5f957f/html5/thumbnails/51.jpg)
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
![Page 52: Correlation between high energy - 名古屋大学...(Whitney et al. 2004) Super star cluster Distance vs. Temperature Image: T kin, Contour: 12CO(2-1), red cross:Wd2 +16 km/s Cloud](https://reader034.fdocuments.us/reader034/viewer/2022042917/5f597c4b53c0ab4cbb5f957f/html5/thumbnails/52.jpg)
Results : Ratio
At jet tip, 12CO(2-1) to 12CO(1-0) ratio is higher.
![Page 53: Correlation between high energy - 名古屋大学...(Whitney et al. 2004) Super star cluster Distance vs. Temperature Image: T kin, Contour: 12CO(2-1), red cross:Wd2 +16 km/s Cloud](https://reader034.fdocuments.us/reader034/viewer/2022042917/5f597c4b53c0ab4cbb5f957f/html5/thumbnails/53.jpg)
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
![Page 54: Correlation between high energy - 名古屋大学...(Whitney et al. 2004) Super star cluster Distance vs. Temperature Image: T kin, Contour: 12CO(2-1), red cross:Wd2 +16 km/s Cloud](https://reader034.fdocuments.us/reader034/viewer/2022042917/5f597c4b53c0ab4cbb5f957f/html5/thumbnails/54.jpg)
MOPRA 12CO J=1-0 Result s: S3
![Page 55: Correlation between high energy - 名古屋大学...(Whitney et al. 2004) Super star cluster Distance vs. Temperature Image: T kin, Contour: 12CO(2-1), red cross:Wd2 +16 km/s Cloud](https://reader034.fdocuments.us/reader034/viewer/2022042917/5f597c4b53c0ab4cbb5f957f/html5/thumbnails/55.jpg)
![Page 56: Correlation between high energy - 名古屋大学...(Whitney et al. 2004) Super star cluster Distance vs. Temperature Image: T kin, Contour: 12CO(2-1), red cross:Wd2 +16 km/s Cloud](https://reader034.fdocuments.us/reader034/viewer/2022042917/5f597c4b53c0ab4cbb5f957f/html5/thumbnails/56.jpg)
![Page 57: Correlation between high energy - 名古屋大学...(Whitney et al. 2004) Super star cluster Distance vs. Temperature Image: T kin, Contour: 12CO(2-1), red cross:Wd2 +16 km/s Cloud](https://reader034.fdocuments.us/reader034/viewer/2022042917/5f597c4b53c0ab4cbb5f957f/html5/thumbnails/57.jpg)
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
![Page 58: Correlation between high energy - 名古屋大学...(Whitney et al. 2004) Super star cluster Distance vs. Temperature Image: T kin, Contour: 12CO(2-1), red cross:Wd2 +16 km/s Cloud](https://reader034.fdocuments.us/reader034/viewer/2022042917/5f597c4b53c0ab4cbb5f957f/html5/thumbnails/58.jpg)
G327.5
![Page 59: Correlation between high energy - 名古屋大学...(Whitney et al. 2004) Super star cluster Distance vs. Temperature Image: T kin, Contour: 12CO(2-1), red cross:Wd2 +16 km/s Cloud](https://reader034.fdocuments.us/reader034/viewer/2022042917/5f597c4b53c0ab4cbb5f957f/html5/thumbnails/59.jpg)
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
![Page 60: Correlation between high energy - 名古屋大学...(Whitney et al. 2004) Super star cluster Distance vs. Temperature Image: T kin, Contour: 12CO(2-1), red cross:Wd2 +16 km/s Cloud](https://reader034.fdocuments.us/reader034/viewer/2022042917/5f597c4b53c0ab4cbb5f957f/html5/thumbnails/60.jpg)
Astrophysical jets
Microquasar jets/
Anisotropic SNe
(Mirabel & Rodríguez 1994)
GRS1915+105
(3.5cm conti.)
3C296
![Page 61: Correlation between high energy - 名古屋大学...(Whitney et al. 2004) Super star cluster Distance vs. Temperature Image: T kin, Contour: 12CO(2-1), red cross:Wd2 +16 km/s Cloud](https://reader034.fdocuments.us/reader034/viewer/2022042917/5f597c4b53c0ab4cbb5f957f/html5/thumbnails/61.jpg)
Molecular Jets discovered by NANTEN
High J=2-1/1-0 ratio
![Page 62: Correlation between high energy - 名古屋大学...(Whitney et al. 2004) Super star cluster Distance vs. Temperature Image: T kin, Contour: 12CO(2-1), red cross:Wd2 +16 km/s Cloud](https://reader034.fdocuments.us/reader034/viewer/2022042917/5f597c4b53c0ab4cbb5f957f/html5/thumbnails/62.jpg)
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
![Page 63: Correlation between high energy - 名古屋大学...(Whitney et al. 2004) Super star cluster Distance vs. Temperature Image: T kin, Contour: 12CO(2-1), red cross:Wd2 +16 km/s Cloud](https://reader034.fdocuments.us/reader034/viewer/2022042917/5f597c4b53c0ab4cbb5f957f/html5/thumbnails/63.jpg)
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)
![Page 64: Correlation between high energy - 名古屋大学...(Whitney et al. 2004) Super star cluster Distance vs. Temperature Image: T kin, Contour: 12CO(2-1), red cross:Wd2 +16 km/s Cloud](https://reader034.fdocuments.us/reader034/viewer/2022042917/5f597c4b53c0ab4cbb5f957f/html5/thumbnails/64.jpg)
![Page 65: Correlation between high energy - 名古屋大学...(Whitney et al. 2004) Super star cluster Distance vs. Temperature Image: T kin, Contour: 12CO(2-1), red cross:Wd2 +16 km/s Cloud](https://reader034.fdocuments.us/reader034/viewer/2022042917/5f597c4b53c0ab4cbb5f957f/html5/thumbnails/65.jpg)
![Page 66: Correlation between high energy - 名古屋大学...(Whitney et al. 2004) Super star cluster Distance vs. Temperature Image: T kin, Contour: 12CO(2-1), red cross:Wd2 +16 km/s Cloud](https://reader034.fdocuments.us/reader034/viewer/2022042917/5f597c4b53c0ab4cbb5f957f/html5/thumbnails/66.jpg)
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
![Page 67: Correlation between high energy - 名古屋大学...(Whitney et al. 2004) Super star cluster Distance vs. Temperature Image: T kin, Contour: 12CO(2-1), red cross:Wd2 +16 km/s Cloud](https://reader034.fdocuments.us/reader034/viewer/2022042917/5f597c4b53c0ab4cbb5f957f/html5/thumbnails/67.jpg)
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
![Page 68: Correlation between high energy - 名古屋大学...(Whitney et al. 2004) Super star cluster Distance vs. Temperature Image: T kin, Contour: 12CO(2-1), red cross:Wd2 +16 km/s Cloud](https://reader034.fdocuments.us/reader034/viewer/2022042917/5f597c4b53c0ab4cbb5f957f/html5/thumbnails/68.jpg)
ALMA (2012-)
Atacama Large Millimeter/submillimeter Array0.1”-1”(~ 0.1 pc@50kpc)