FOREST Unbiased Galactic plane Imaging survey with the Nobeyama - - PowerPoint PPT Presentation

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FOREST Unbiased Galactic plane Imaging survey with the Nobeyama - - PowerPoint PPT Presentation

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FOREST Unbiased Galactic plane Imaging survey with the Nobeyama 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,

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SLIDE 1

FOREST Unbiased Galactic plane Imaging survey with the Nobeyama 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

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SLIDE 2

Members

Kagoshima Univ. Handa, T. Nakanishi, H. Omodaka, T. Shinnaga, H. Koide, N. Mizukubo, M. Uesugi, K. Ozawa, T. Osaka Pref. Univ. Onishi, T. Tokuda, K. Takada, S.,Takahashi, R.

  • Nagoya. Univ.

Tachihara, K. Nishimura, A. Sano, H. Fujita, S. Hattori, Y. Yoshiike, S. Kohno,M., Okawa, K. Costes, J., Inoue, T. Joetsu Edu. Univ. Tosaki, T. Kobayashi, Y. ISAS/JAXA Tsuboi, M.,Morokuma,

  • K. Yamagishi, M.

NRO Umemoto, T. Minamidani, T. Torii, K. Matsuo, M. NAOJ Hasegawa, T. Mizuno, N. Muller, E. Hirota, A. Honma, M. Matsumoto, N. Kamegai, K.

  • Univ. Tokyo

Sato, M. Kuwahara, S. Sofue, Y.

Meisei Univ. Onodera, S. Tsuda, Y.

RIKEN Higuchi, A. Ohashi, S.

Tsukuba Univ. Kuno, N. Saito, H. Kuriki, M.

Saitama Univ. Oasa, Y.

  • Univ. Nigeria

Chibueze, J. Kwansei Gakuin

  • Univ. Seta, M.
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SLIDE 3

Members

Kagoshima Univ. Handa, T. Nakanishi, H. Omodaka, T. Shinnaga, H. Koide, N. Mizukubo, M. Uesugi, K. Ozawa, T. Osaka Pref. Univ. Onishi, T. Tokuda, K. Takada, S.,Takahashi, R.

  • Nagoya. Univ.

Tachihara, K. Nishimura, A. Sano, H. Fujita, S. Hattori, Y. Yoshiike, S. Kohno,M., Okawa, K. Costes, J., Inoue, T. Joetsu Edu. Univ. Tosaki, T. Kobayashi, Y. ISAS/JAXA Tsuboi, M.,Morokuma,

  • K. Yamagishi, M.

NRO Umemoto, T. Minamidani, T. Torii, K. Matsuo, M. NAOJ Hasegawa, T. Mizuno, N. Muller, E. Hirota, A. Honma, M. Matsumoto, N. Kamegai, K.

  • Univ. Tokyo

Sato, M. Kuwahara, S. Sofue, Y.

Meisei Univ. Onodera, S. Tsuda, Y.

RIKEN Higuchi, A. Ohashi, S.

Tsukuba Univ. Kuno, N. Saito, H. Kuriki, M.

Saitama Univ. Oasa, Y.

  • Univ. Nigeria

Chibueze, J. Kwansei Gakuin

  • Univ. Seta, M.

Liverpool John Moores Univ. Moore, T. Eden, D. Cardiff Univ. Rigby, A.

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SLIDE 4

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
333°# 332°# 331°# 334°# '1°# 0°# +1°#

La,tude# Longitude#

Spitzer GLIMPSE: 3.6, 4.5, 5.8, and 8.0 μm, MIPSGAL: 24 and 70 μm Hi-GAL: (70,) 160, 250, 350 (and 500) μm

  • Dynamical state and interaction of

molecular clouds

  • The survey in spectral lines with wide

coverage & enough angular resolution comparable to the IR surveys is highly required

Observations of Spectral Lines

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FOREST Unbiased Galactic plane Imaging survey with the Nobeyama 45-m telescope

“Wind god and Thunder god” by Ogata Korin

FUGIN Project

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  • 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)

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SLIDE 7
  • 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)

FUGIN Project

(Umemoto et al. 2017 PASJ, 69,78)

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SLIDE 8

NASA/R. Hurt

Mapping area: inner disk: l = 10°～50° |b|≦1° Spiral arms, interarm, bar/barend,

  • uter disk: l = 198°～236° |b|≦1°

Comparison with inner disk

l=10 l=50 l=198 l=236

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SLIDE 9

Observed Regions

  • magenta: planned, red: observed
  • Observed: 130 deg2 (84% of the plan)
  • 1st quad.: 80deg2 (X-scan:Complete, Y-scan 28deg2)
  • 3rd quad.: 50deg2 (X-scan)
  • Period: March 2014 - May 2017
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SLIDE 10

Achevment:

  • All the observations in March-May 2017 were canceled because a

big trouble on the master collimator in the 45m telescope.

  • We could not compete our project, especially Y-scan in the 1st

quadrant and X-scan in the 3rd quadrant --> 67% complete.

Final status:

  • 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

FUGIN Status

2013-2016 Inner Outer Obs Time(h) 808 293 Area(deg^2) 108(80/28) 50

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SLIDE 11

M17 W33

Infrared Spitzer

R: 24µm G: 8µm B: 5.4µm

電波FUGIN

R: 12CO G: 13CO B: C18O

Visible

M16

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SLIDE 12

#01 Molecular Cloud Identification

Current Status (1st quadrant)

A1 A2 A3 A4 A5

・color : velocity component red : ~ 17.5 km/s blue : ~ 34.5 km/s

A1 B1 B4 C1 C2 B4 C2 B1 A5

We have started tests in L=12–16 deg region. In the figures below, the clouds were identified by assuming 훥V < 10km/s.

R : 0.04–24 pc, 훥V : 0.45–6.0 km/s, MMC : 0.3–2.3x105 Mo (near-distance is assumed.)

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SLIDE 13

#01 Molecular Cloud Identification

An example of small molecular cloud with star formation (Matsuo et al. in prep.)

Current Status (3rd quadrant)

Average CO spectra

12CO 13CO

C18O

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

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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), and

Spitzer bubbles N18, N35 and W51 (submitted to PASJ)

  • Compared to the theoretical models, observational

signatures of CCC were identified in all the GMCs.

Takahira+14; Haworth+15a,b

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SLIDE 15

CCC candidate without star formation

(Tsuda, Torii et al. in prep.)

#?? Cloud-cloud collision

  • Discovered a MC

with 2 signatures of CCC without any indication of SF.

  • It may be either a

CCC without SF, or in very early evolutionary phase

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SLIDE 16

Results: SNR Kes 79 (Kuriki, Sano+2017 submitted)

Molecular gas associated with Kes 79

  • SNR shows good spatial correspondence

with the molecular gas at VLSR~80 km s−1

  • Expanding gas motion originated by SNR
  • High-temperature gas by shock heating

Red: Radio Continuum Green: Molecular Cloud (FUGIN) Blue: Thermal X-rays

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

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SLIDE 17

Publication Plan & Status

Theme PI Status Project overview and initial results

  • T. Umemoto

published PDR in M17 region M. Yamagishi published Star formation in M17 region

  • A. Nishimura

accepted Cloud-cloud collision in W33 region

  • M. Kohno

accepted Cloud-cloud collision in Spitzer bubble N35

  • K. Torii

submitted Cloud-cloud collision in Spitzer bubble N18

  • K. Torii

submitted Interaction between molecular clouds and SNRs

  • M. Kuriki & Sano

submitted Molecular clouds in W51 region

  • S. Fujita

submitted Molecular clouds in outer Galaxy

  • M. Matsuo

writing Dense cores in M17 region

  • T. Tosaki

writing Shells

  • Y. Tsuda

in preparation Cloud-cloud collision in outer Galaxy

  • N. Koide

in preparation PDF of molecular clouds

  • T. Handa

in preparation Cloud identification

  • H. Saito

in preparation Final results of the survey

  • T. Minamidani

in preparation NH3 survey towards cores

  • T. Handa

in preparation Hot core survey K.Sato & T. Hasegawa in preparation

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SLIDE 18
  • Open all after 1yr from the end of the
  • bservations 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 researchers
  • f various wavelengths and theorist utilize

these data, and generate new science

Data Release Policy

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SLIDE 19

Koda+ 2011

galaxies

Tatematsu +1993

cores/clumps

Formation process of dense clumps studied in nearby GMCs in the Galaxy Evolutionary process of ISM studied in GMC scale

Linkage by FUGIN

Linkage between star formation study in the Galaxy and study of molecular gas in galaxies

FOREST Unbiased Galactic plane Imaging survey with the Nobeyama 45-m telescope

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Summary

  • We have conducted the Galactic Plane Survey with the highest

angular resolution by simultaneous 12CO, 13CO and C18O J=1-0 lines (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 and

rms images. We also plan to publish catalogs of clouds/clumps etc.. We hope the researchers of various wavelengths and theorist utilize these data.

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

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

  • Comparative studies with other CO J transitions and other

wavelengths shall provide important clue to understand ISM and star formation.