NRO Galactic Plane Survey(FUGIN) Legacy ProjectUmemoto, T. (NRO)
andthe FUGIN team

Nagoya. Univ.
NRO
Tachihara, K.
Umemoto, T.
Nishimura, A.
Minamidani, T.
Joetsu Edu. Univ.
Sano, H.
Torii, K.
Hattori, Y.
Tosaki, T.
NAOJ
Yoshiike, S.
Kobayashi, Y.
Kohno,M.,
Mizuno, N.
Cotes, J.
Tsukuba Univ. Muller, E.
Osaka Pref. Univ.
Kuno, N.
Morokuma, K.
Onishi, T.
Fujita, S.
Hirota, A.
Tokuda, K.
Kuriki, M.
Honma, M.
Takahashi, R.
Matsumoto, N.
RIKEN
Kagoshima Univ.
Kamegai,K.
Higuchi,A.
Handa, T.
Saitama Univ. Inoue, T.
Nakanishi, H.
Kwansei Gakuin
Meisei Univ.
Oasa, Y.
Omodaka, T.
Univ. Tokyo
Univ. Seta, M.
Onodera, S.
Shinnaga, H.
Ohashi, S.
ISAS/JAXA
Tsuda, Y.
Matsuo, M.
Tsuboi, M.
Kuwahara, S. Univ. Nigeria
Koide, N.
Ozawa, T.
Chibueze, J.
Yamagishi, M.
Sofue, Y.

Members

Missing Link

galaxies

Formation process of dense clumps
studied in nearby GMCs in theGalaxy
Linkage
between starformation study
cores/clumps
in the GalaxyandKoda+ 2011
study of molecular gas
in galaxiesEvolutionary process of ISM studied in
GMC scaleTatematsu +1993

Missing Link
All-sky image of molecular gas seen by Planckgalaxies

Formation process of dense clumps
studied in nearby GMCs in theGalaxy
Linkage
between starformation study
cores/clumps
in the Galaxy
andKoda+ 2011
study of molecular gas
in galaxiesEvolutionary process of ISM studied in
GMC scaleMulti-line survey of the Galactic plane withhigh angular resolution by the 45m
Tatematsu +1993

FUGIN Project“Wind god and Thunder god” by Ogata Korin

FUGIN Project• Using multi-beam receiver FOREST, OTF

mapping of the Galactic plane in 12CO(1-0),
13CO,(1-0), C18O(1-0), simultaneously
The CO Galactic Plane Survey by simultaneous
3CO lines
with the highest angular resolution(~15”)!

FUGIN Project• Using multi-beam receiver FOREST, OTF

mapping of the Galactic plane in 12CO(1-0),
13CO,(1-0), C18O(1-0), simultaneously• Large mapping area
• Inner Galaxy l: 10°~ 50° b: ±1°(80 deg2)• Outer Galaxy l: 198°~236° b: ±1°• Sensitivity• Trms(Ta*) =0.12K @13CO dv= 1.3 km/s
• Trms(Ta*) =0.12K @12CO dv= 5 km/s (~0.24 K dv=1.3 km/s)

FUGIN Project• Using multi-beam receiver FOREST, OTF

mapping of the Galactic plane in 12CO(1-0),
13CO,(1-0), C18O(1-0), simultaneously• Large mapping area Obs. Time：1,200h(3 yeras)• Inner Galaxy l: 10°~ 50° b: ±1°(80 deg2)• Outer Galaxy l: 198°~236° b: ±1°• Sensitivity• Trms(Ta*) =0.12K @13CO dv= 1.3 km/s
• Trms(Ta*) =0.12K @12CO dv= 5 km/s (~0.24 K dv=1.3 km/s)

Observed Regions To Date
• magenta: planned, red: observed• Period: March 2014 - May 2016

Observed Regions To Date
• magenta: planned, red: observed• Period: March 2014 - May 2016

2(76%)
Observed:118deg•• Inner Galaxy: X-scan 70deg2 (Y-scan 17deg2)• Outer Galaxy: X-scan-48deg2

OpticalFUGIN
R: 12COG: 13CO
B: C18O

Spitzer
R: 24µm
G: 8µm
B: 5.4µm

M17

W33

Here

Integrated Intensity Maps

Zoom up

12CO(1–0)

13CO(1–0)

C18O(1–0)

v= 45 – 55 km/s

W51
One of most ac/ve high mass starforming region in the Galaxy with asize of ~100 pc, Mass~106 Mo(Carpenter & Sanders 1998) at a
distance of 5.4kpc in tangen/al
point of SagiNarius arm (Sato 2010)55 – 65 km/s

Density StructureHigh density clumps are
surrounded by diffuse and low
density gas
65 – 75 km/s
W51A

W51B
~68 km/s, ~100 pc~45 – 65 km/s complex
W51mainbreak 1Hm
ity Strea
cole
Vhig

break 2(HVS)

Fujita et al.

Fujita et al. in preparation

Probability13CO(J=1–0)

W51B

W51C
W51A

PC1(massive star forming region)

select 10 clouds

PC 2

Decomposi/on withDendrogramsPC 4(Rosolowsky et al. 2008)
H2 Column density (log)Characteris/cs of the clouds
Name

W51

gray scale: Spitzer 8µm

MLTE[104 Msun]

13CO(1-0)

13CO(3-2)[km/s]

radius[pc]

12CO(1-0)

13CO(1-0)

N(H2) max
[ cm-2]

1.8

4.4

1.4

0.30 ±0.03

0.66 ±0.05

3.5x1022

122.7
37.3

Vrms

8µm intensity number of[MJy/sr]
YSOs (>8Mo)

31.2

PC26.69.4

440.35 ±0.06

0.75 ±0.11

33 x1022PC3

1.9

6.0

3.5

0.36 ±0.06

0.20 ±0.03

2.0x1022

174.5
56.2

PC4

3.4

3.4

6.0

0.28 ±0.05

0.99 ±0.14

6.7x1022

PC5

1.1

4.4

0.8

0.39 ±0.07

0.52 ±0.07

2.5x10220

active22
3active141

Fujita et al. in preparation

Discussion – 1. The structure of GMC in W51

1.1 Collisions of internal clouds
uNew candidates of collisions of internal clouds• Common characteristic-complementary distribution of blue & red components-YSOs on site of collisions• Many candidates of collisions of internal clouds in W51A andW51B

ØCollisions of internal clouds within GMC
W51A

W51B

massive YSO
many massive YSOs
no HII region

with HII region

no HII region

Discussion – 2. Massive star formation in W51
Feedback scenario of massive star formation
Massive & high column density cloud
Trigger by cloud-cloud collision

Formation of massive stars• Heating of Parent Cloud by radiation

increase 8 µm, 13CO (3–2)/(1–0)ratio• acceleration of internal clouds

Massive & high column density cloud

Trigger by cloud-cloud collision

Interaction of SNR G33.6+0.1(Kes79)
12CO(J=1-0)
Integrated Intensity (black contour)

30 km/s cloud

Color：
X-ray（0.3 – 10 keV）

Kuriki et al.
HPBW ~ 18”

80 km/s cloud

100 km/s cloud

blue contour：
radio continuum（1.4 GHz）

12CO(J=3-2)/12CO(J=1-0) Ratio Map

30 km/s cloud

80 km/s cloud

100 km/s cloud- the molecular cloud complementary distributed with X-ray radiation- an expanding shell structure- the large CO 3-2 to 1-0 ratio region around the SNR→Possibility of interaction with the molecular cloud at VLSR~80km/s

Molecular clouds in the Outer Galaxy

10 objects aredetected at R> 16 kpc

Iden/ﬁed 1317 molecular clouds

R = 15.3 kpc
cloud radius = 0.76 pc
line width = 1.3 km/s
Mco = 82 M0

Iden/ﬁca/on of Molecular Clouds• Apply to IR2.1 13CO cube data for the Inner Galaxy– 1180+310 clouds were found (within 31 deg^2)– determina/on of the distance and mass (not yet)14

Publication Status
Theme
Project overview
Star formation in M17 regionDense cores in M17 region
PDR in M17 region
Cloud-cloud collision in W33 region
Molecular clouds in W51 region
ShellsMolecular clouds in outer Galaxy
Cloud-cloud collision in Spitzer bubbles
Interaction between molecular clouds and SNRs
PDF
NH3 survey towards coresPI
T. Umemoto
A. Nishimura
T. Tosaki
M.Yamagishi
M. Kohno
S. Fujita
Y. Tsuda
M. Matsuo
K. Torii

Statussubmitted
writing
writing
will be publishedwriting
writingin preparation
writing
writing
M. Kuriki & Sano
writing
T. Handain preparation
T. Handain preparation

Data Release Policy• Open all after 1yr from the end of theobservations of this project• Calibrated data• 3-D FITS (overall map and/or sub-maps within several degree）• Open on the project website（in preparation）• Many catalogs• molecular clouds, clumps, filaments, shells• Provide original catalogs to the detailed observations by ALMA

• Open widely to the community, the researchersof various wavelengths utilize these data, andgenerate new scienceSummary• We are conducting the Galactic Plane Survey with thehighest angular resolution by simultaneous 12CO, 13CO
and C18O J=1-0 lines (FUGIN) as the NRO legacy projectusing the FOREST installed on the Nobeyama 45m
telescope.

• To date, we have covered 118 deg^2 (76% of the plan).
• We have revealed a wide range and detailed structuresof molecular clouds not seen in previous surveys.

• In ALMA era, this project must make a linkage between

the study of star formation in the Milky Way Galaxy andstudy of molecular gas in galaxies.

• After the end of the project, open all data, 3-D fits,catalogs of clouds/clumps etc.. We hope theresearchers of various wavelengths utilize these data.
+theorist