FOREST Unbiased Galactic
plane Imaging survey with theNobeyama 45-m telescope(FUGIN)
Umemoto, T., Minamidani, T. Torii,K., Matsuo, M.
(NRO), Nishimura, A., Fujita, S., Kohno, M.(Nagoya Univ.),
Kuriki, M., Kuno, N.(Univ. of Tsukuba), Tsuda, Y.(Meisei Univ.),
Ohashi, S.(Univ. of Tokyo), Tosaki, T.(Joetsu Univ. of Edu.),and the FUGIN team

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

MembersNRO
Nagoya. Univ.
Tachihara, K.
Umemoto, T.
Nishimura, A.
Minamidani, T.
Sano, H.
Joetsu Edu. Univ.
Liverpool JohnTorii,K.
Fujita, S.
Tosaki, Univ.
T.
MooresMatsuo, M.
Hattori, Y.
Kobayashi,Y.
Moore,T.
NAOJ
Yoshiike, S.
Tsukuba Univ. Hasegawa, T.
Kohno,M., Okawa, K.
Eden, D.
Costes, J., Inoue, T.Cardiff Univ.
Kuno, N.
Mizuno, N.
Osaka Pref. Univ.
Saito,H.
Rigby,A.
Muller, E.
Onishi, T.
Kuriki, M.
Hirota, A.
Tokuda, K.
RIKEN
Takada, S.,Takahashi, R.
Honma, M.
Kagoshima Univ.
Higuchi, A. Matsumoto, N.
Handa, T.
Ohashi, S.
Kamegai, K.
Nakanishi, H.
Saitama Univ.
Omodaka, T.
Kwansei Gakuin
Meisei Univ.
Oasa, Y.
Shinnaga, H.
Univ. Seta, M.
Onodera,S.
Univ.
Tokyo
Koide, N.
Sato, M.
Tsuda, Y.
Mizukubo, M. ISAS/JAXA
Tsuboi, M.,Morokuma, Kuwahara, S. Univ. Nigeria
Uesugi, K.
Ozawa, T.
Sofue, Y.
Chibueze, J.
K. Yamagishi, M.

Members

Infrared & Submm Cont. Surveys• GLIMPSE & MIPSGAL by Spitzer (Benjamin et al. 2013, Carey et al. 2009)• Hi-GAL by Herschel (Molinari et al. 2010, 2016), AKARI(Doi et al. 2015)• ATLASGAL(Schuller et al. 2009) BGPS(Aguirre et al. 2011) SCUBA-2(Parsons 2013)• Identify SF activity and revealed structure of molecular clouds

Spitzer GLIMPSE: 3.6, 4.5, 5.8, and 8.0 μm, MIPSGAL: 24 and 70 μm

Observations of Spectral Lines+1°#

La,tude#• Dynamical state and interaction ofmolecular clouds

0°#

334°#

333°#

Longitude#

332°#

Hi-GAL: (70,) 160, 250, 350 (and 500) μm

331°#

Fig. 1: Three-colour image (blue 70µm, green 160µm, red 350µm) of a 3-tile mosaic field around 330 . ` .335 .

Molinari et al.: Hi-GAL Data Release 1.

'1°#• The survey in spectral lines with wide

coverage & enough angular resolution
comparable to the IR surveys ishighly required

FUGIN Project

FOREST Unbiased Galactic plane Imaging survey with the Nobeyama
45-m telescope“Wind god and Thunder god” by Ogata Korin

FUGIN Project(Umemoto et al. 2017 PASJ, 69,78)• Using multi-beam receiver FOREST, OTF

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

FUGIN Project(Umemoto et al. 2017 PASJ, 69,78)• Using multi-beam receiver FOREST, OTF

mapping of the Galactic plane in 12CO, 13CO,
C18O(J=1-0), simultaneously• Large mapping area
• 1st quadrant l: 10°~ 50° b: ±1°(80 deg2)• 3rd quadrant l: 198°~236° b: ±1° (76 deg2)• Target Sensitivity• Trms(Ta*) =0.12K @13CO dv= 1.3 km/s (Tsys=150 K)• Trms(Ta*) =0.12K @12CO dv= 5 km/s (~0.24 K dv=1.3 km/s)(Tsys=250 K)

l=198l=236

Mapping area:
inner disk: l = 10°〜50° |b|≦1°

l=50

Spiral arms, interarm, bar/barend,outer disk: l = 198°〜236° |b|≦1°Comparison with inner disk

l=10NASA/R. Hurt

Observed Regions• magenta: planned, red: observed• Period: March 2014 - May 2017
• Observed: 130 deg2 (84% of the plan)• 1st quad.: 80deg2 (X-scan:Complete, Y-scan 28deg2)• 3rd quad.: 50deg2 (X-scan)FUGIN Status

2013-2016

Inner

Outer

Obs Time(h)808Final status: Area(deg^2) 108(80/28)

293
50•1st quad.: l ~ 10° – 50°, b < |1°|
•3rd quad:l = 198° - 209°,213° - 218°, 232° - 235°, b=0° -1°
l = 198° - 204°,208° - 214°, 217° - 236°, b=-1°-0°•sampling grid: 8.5”--> effective beam sizes: 20”•ch resolution: ~0.65km/s (effective: 1.3km/s)•Trms(Tmb): 0.7K@13CO & C18O, 1.5K@12CO
Achevment:•All the observations in March-May 2017 were canceled because abig trouble on the master collimator in the 45m telescope.

•We could not compete our project, especially Y-scan in the 1stquadrant and X-scan in the 3rd quadrant --> 67% complete.

Visible

電波FUGIN
R: 12COG: 13CO
B: C18O

W33

M16

M17

Infrared Spitzer
R: 24µm
G: 8µm
B: 5.4µm

#01 Molecular Cloud Identification

Current Status (1st quadrant)
We have started tests in L=12–16 deg region. In the figures below, theclouds were identified by assuming 𝛥V < 10km/s.
・color : velocity component
red : ~ 17.5 km/s
blue : ~ 34.5 km/s

A1

A2

C2

B1

B4A5B4A3C2

B1

A1
C1A5A4

R : 0.04–24 pc, 𝛥V : 0.45–6.0 km/s, MMC : 0.3–2.3x105 Mo (near-distance is assumed.)#01 Molecular Cloud Identification

Current Status (3rd quadrant)
An example of small molecular cloud with star formation(Matsuo et al. in prep.)

Average CO spectra
12CO13COC18O

WISE 3color
B: 3.4 µm
G: 4.6 µm
R: 12 µm
Contours: 13CO

UKIDSS 3color
B: J band
G: H band
R: K band
Contours: 13CO

2: (Massive) Star formation• Studies of the individual massive star-forming regions- Properties of GMCs with signatures of CCC (i.e.,complementary distribution and/or broad bridge feature
between two velocity clouds)- Already done on M17, W33 (accepted by PASJ), andSpitzer bubbles N18, N35 and W51 (submitted to PASJ)- Compared to the theoretical models, observationalsignatures of CCC were identified in all the GMCs.
Takahira+14; Haworth+15a,b

#?? Cloud-cloud collision

CCC candidate without star formation(Tsuda, Torii et al. in prep.)-Discovered a MCwith 2 signatures ofCCC without any
indication of SF.
- It may be either a
CCC without SF, orin very early
evolutionary phaseResults: SNR Kes 79 (Kuriki, Sano+2017 submitted)
Red: Radio Continuum
Green: Molecular Cloud (FUGIN)
Blue: Thermal X-rays

Molecular gas associated with Kes 79- SNR shows good spatial correspondencewith the molecular gas at VLSR~80 km s−1- Expanding gas motion originated by SNR- High-temperature gas by shock heating

Distance & Age- Distance ~5.4 kpc (previous study ~7.1 kpc)
- Age ~10,000 (Sedov self-similar solution)

Total energy of CR protons

Total CR proton energy

Mean gas density ~ 400 cm−3

Acceleration efficiency ~0.4 %(Theoretical value ~1−10 %, e.g., Gabici+2013)

Kuriki, Sano+2017

Publication Plan & Status
Theme
Project overview and initial results
PDR in M17 region
Star formation in M17 region
Cloud-cloud collision in W33 region
Cloud-cloud collision in Spitzer bubble N35
Cloud-cloud collision in Spitzer bubble N18Interaction between molecular clouds and SNRs
Molecular clouds in W51 region
Molecular clouds in outer Galaxy
Dense cores in M17 region
ShellsCloud-cloud collision in outer Galaxy
PDF of molecular clouds
Cloud identification
Final results of the survey
NH3 survey towards cores
Hot core survey

PI
T. Umemoto
M.Yamagishi
A. Nishimura
M. Kohno
K. Torii
K. Torii
M. Kuriki & Sano
S. Fujita
M. Matsuo
T. Tosaki
Y. Tsuda
N. Koide
T. Handa
H. Saito
T. Minamidani
T. Handa
K.Sato & T. Hasegawa

Statuspublishedpublishedaccepted
accepted
submitted
submitted
submitted
submitted
writing
writingin preparationin preparationin preparationin preparationin preparationin preparationin preparation

Data Release Policy• Open all after 1yr from the end of theobservations of this project (2018.6)• Calibrated data
• 3-D FITS (overall map and sub-maps within several degree) & images• Open on the JVO（in preparation）• Plan to publish 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 and theorist utilize
these data, and generate new scienceLinkage by FUGINgalaxies

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 galaxiesImaging survey withprocess of ISM studied in
FOREST Unbiased Galactic planeEvolutionary
the Nobeyama 45-m telescope

Tatematsu +1993

GMC scaleSummary• We have conducted the Galactic Plane Survey with the highest

angular resolution by simultaneous 12CO, 13CO and C18O J=1-0lines (FUGIN) as the NRO legacy project using the FOREST
installed on the Nobeyama 45m telescope.

• We covered 130 deg2 (83% of the plan).
• All the data will be open in 2018.6, including 3-D fits files andrms images. We also plan to publish catalogs of clouds/clumps
etc.. We hope the researchers of various wavelengths andtheorist utilize these data.

• In the ALMA era, this project must make a linkage between thestudy of star formation in the Milky Way Galaxy and study ofmolecular gas in galaxies.

• Comparative studies with other CO J transitions and otherwavelengths shall provide important clue to understand ISMand star formation.