ALMA/45m/ASTE Users Meeting 2017
Dec. 27th, 2017

45m Legacy

COMING

CO Multi-line Imaging of Nearby Galaxies
SORAI, Kazuo
Hokkaido Univ./Univ. of Tsukubaand COMINGersCOMINGers
Kwansei Gakuin
Univ.
Salak, D.
Noma, Y.
Seta, M.

Nagoya Univ. NAOJ
Hokkaido Univ. Univ. of Tsukuba
Takeuchi, T. T. Miyamoto, Y. Sorai, K.
Kuno, N.
Yoda, M.
Kaneko, H.
Nakai, N.
Umie, M.＊
Watanabe, Y.
Segawa, Y.＊
Hatakeyama, T.
Tashiro, T.＊＊Kishida, N.＊
Yamaguchi Univ./NAOJ
Yajima, Y.
Tanaka, T.
Matsumoto, N.
Shibata, S.
Tomiyasu, Y.＊
Kagoshima Univ.
Tokyo Univ. Kawahara, Y.＊
Sato, Y.
Nakanishi, H.
of Science
Yasuda, A.
Saita, C.＊
Oi, N.
Kita, S.
Osaka Prefecture Univ.
Ueno, S.
Komatsuzaki, R.
Muraoka, K.
Ezoe, S.＊
(Sorai, K.)
ISAS
Baji, H.＊(*：graduated)
Academia Sinica Institute
Takeda, M.＊ Morokuma, K.
Astronomy and Astrophysics
Yanagitani, K.＊
PAN, H-A.
Kuroda, M.

1. BACKGROUND

Molecular gas and star formation
2.0log SFR (M☉ yr-1)• molecular gas in thecontext of galaxyevolution• what happens
within a galaxy?
• lack of molecular
gas information

1.00.0
-1.0
-2.0
8.0

9.0 10.0 11.0 12.0
log Mstar (M☉)(based on Schiminovich, et al. 2007)

Recent CO surveys• COLDGASS (Saintonge+ 11)> 300 galaxies, pointing• EDGE (the Extragalactic
Database for Galaxy
Evolution survey)(Bolatto+ 17)
126 galaxies, CARMACOLDGASS

EDGE

2. SAMPLES & OBSERVATIONSOriginal & observed samples• targets: 238 FIR bright galaxies• morphology• distance40200

not observedobservedmorphology

not observed

40

observed

200

ES0+S0/a
SaSabSbSbc
ScScd
Sd
Sdm
SmIm
I0Pec
n.c.

number60

60

0

10 20 30 40
distance (Mpc)

50

Observations• OTF with the 45-m telescope w/ FOREST• 2015, Apr. – 2017, Mar. (~1,320 hr)• 12CO, 13CO, C18O J=1–0 (simultaneously)• Dv = 10 km s-1• DTA* = 30 mK• mapping area: 70% of D25• observed targets: 127 galaxies(~53 % of the original samples)Auto-Reduction Tool (COMING ART)
raw data

split

scaling

auto-flagging

baseline ranges (assumed)
FFT & salvage factor (parameter)(checking spurious)

basket weaving x, y, individuallychecking baseline ranges
checking rms

cutting edges of spectra

auto-rebase

selecting salvage factor &mask widths

change baseline ranges

rotation

final data cube

3. RESULTS

Molecular gas in barred spirals• COMING (12CO & 13CO J=1–0) + JCMT (12CO600
J=3–2) & RADEX
open N3627• less dense and large
velocity width in bar• Yajima, et al., in prep.

n(H2) (cm-3)

NGC 3627 NGC 4303

filled N4303
armbar end
bar

400
20004080 120
DV (km s-1)

160

Molecular gas and star formation• COMING (12CO J=1–0) + IRAM (12CO J=2–1)• 12CO J=2–1 / J=1–0 (≡R2–1/1–0)– higher in arms than inter-arm region– related to star formation rate
12CO J=1–0

R2–1/1–0

WISE 22 µm

NGC 628• Komatsuzaki & Kuno, this morning

Deriving stellar mass
• using WISE 3.4 µm because we can get data of
the whole targets• but many Galactic stars in each field...
• auto-masking tool has been completed, thensoon deriving stellar mass

4. STATUS & NEAR FUTURE PLAN

Observations• observations of not-observed targets– we’d like to complete our original targets– in especial, galaxies with large appearance• multi-transition observations (J=2–1, J=3–2)– deriving physical properties more precisely• high-resolution observations with ALMA
– what happens in GMA – GMC scale

Scientific activity• sub-working groups– distribution & dynamics (DD): Miyamoto– physical properties (PP): Muraoka– environmental effect (EE): Kaneko– welcome to join us now, please contact us• planning a workshop “COMING 2018”

Publication Plan
1. NGC 2903: Muraoka+ 2016, PASJ, 68, 89
2. NGC 2976: Hatakeyama+ 2017, PASJ, 69, 67
3. overview: Sorai+, in prep.
4. distribution & dynamics: Miyamoto+, in prep.
5. kinematics: Salak+, in prep.
6. SFE: Muraoka+, in prep.
7. conversion factor: Yasuda+, in prep.
8. group galaxies: Kaneko+, in prep.
9. NGC 4303: Yajima+, in prep.
10. resolved K-S relation: Yoda+, in prep.

5. SUMMARY• COMING observed 127 galaxies• data reduction of > 110 galaxies has been
completed• achievement of 53%, but stacking analysis
may help us• now compiling our CO data and trying toderive stellar mass and star formation rate• moving to observation & reduction phase toscientific activity phase