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

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

NRO Nagoya. Univ. Members 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. NAOJ Yoshiike, S. Tsukuba Univ. Kohno,M., Okawa, K. Hasegawa, T. 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. ISAS/JAXA Sato, M. Tsuda, Y. Mizukubo, M. Univ. Nigeria Kuwahara, S. Tsuboi, M.,Morokuma, Uesugi, K. Ozawa, T. Sofue, Y. Chibueze, J. K. Yamagishi, M.

NRO Nagoya. Univ. Members Tachihara, K. Umemoto, T. Nishimura, A. Minamidani, T. Sano, H. Joetsu Edu. Univ. Torii, K. Liverpool John Fujita, S. Tosaki, T. Moores Univ. Matsuo, M. Hattori, Y. Kobayashi, Y. Moore, T. NAOJ Yoshiike, S. Tsukuba Univ. Kohno,M., Okawa, K. Eden, D. Hasegawa, T. Costes, J., Inoue, T. Kuno, N. Cardiff Univ. 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. ISAS/JAXA Sato, M. Tsuda, Y. Mizukubo, M. Univ. Nigeria Kuwahara, S. Tsuboi, M.,Morokuma, Uesugi, K. Ozawa, T. Sofue, Y. Chibueze, J. K. Yamagishi, M.

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 μ m, MIPSGAL: 24 and 70 μ m Observations of Spectral Lines +1°# • Dynamical state and interaction of molecular clouds La,tude# 0°# • The survey in spectral lines with wide coverage & enough angular resolution comparable to the IR surveys is '1°# highly required 334°# 333°# 332°# 331°# Longitude# Hi-GAL: (70,) 160, 250, 350 (and 500) μ m

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 12 CO, 13 CO, C 18 O(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 12 CO, 13 CO, C 18 O(J=1-0), simultaneously • Large mapping area • 1st quadrant l: 10°~ 50° b: ±1°(80 deg 2 ) • 3rd quadrant l: 198°~236° b: ±1° (76 deg 2 ) • Target Sensitivity • T rms (Ta*) =0.12K @ 13 CO dv= 1.3 km/s (T sys =150 K) • T rms (Ta*) =0.12K @ 12 CO dv= 5 km/s (~0.24 K dv=1.3 km/s) (T sys =250 K)

l=198 l=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=10 NASA/R. Hurt

Observed Regions • magenta: planned, red: observed • Period: March 2014 - May 2017 • Observed: 130 deg 2 (84% of the plan) • 1st quad.: 80deg 2 (X-scan:Complete, Y-scan 28deg 2 ) • 3rd quad.: 50deg 2 (X-scan)

FUGIN Status 2013-2016 Inner Outer Obs Time(h) 808 293 Area(deg^2) 108(80/28) 50 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) • T rms (Tmb): 0.7K@ 13 CO & C 18 O, 1.5K@ 12 CO 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 1 st quadrant and X-scan in the 3 rd quadrant --> 67% complete.

Visible 電波 FUGIN R: 12 CO G: 13 CO B: C 18 O W33 Infrared Spitzer M17 R: 24µm G: 8µm M16 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, the clouds were identified by assuming 훥 V < 10km/s. ・ color : velocity component red : ~ 17.5 km/s blue : ~ 34.5 km/s A1 A2 C2 B1 B4 B1 A5 C2 A1 B4 A5 A3 C1 A4 R : 0.04–24 pc, 훥 V : 0.45–6.0 km/s, M MC : 0.3–2.3x10 5 Mo (near-distance is assumed.)

Average CO spectra #01 Molecular Cloud Identification Current Status (3rd quadrant) An example of small molecular cloud with star formation (Matsuo et al. in prep.) 12 CO 13 CO C 18 O UKIDSS 3color WISE 3color B: J band B: 3.4 µm G: H band G: 4.6 µm R: K band R: 12 µm Contours: 13 CO Contours: 13 CO

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

#?? Cloud-cloud collision CCC candidate without star formation (Tsuda, Torii et al. in prep.) -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

Results: SNR Kes 79 (Kuriki, Sano+2017 submitted) Red: Radio Continuum Molecular gas associated with Kes 79 Green: Molecular Cloud (FUGIN) - SNR shows good spatial correspondence Blue: Thermal X-rays with the molecular gas at V LSR ~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 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

Data Release Policy • Open all after 1yr from the end of the observations 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 of various wavelengths and theorist utilize these data, and generate new science

Linkage by FUGIN galaxies Formation process of dense clumps Linkage between star studied in nearby GMCs in the Galaxy formation study cores/clumps in the Galaxy and study of molecular gas Koda+ 2011 in galaxies FOREST Unbiased Galactic plane Imaging survey with Evolutionary process of ISM studied in the Nobeyama 45-m telescope GMC scale Tatematsu +1993