Poster No. 13
Astrometry of the Galactic star-forming region IRAS 05358+3543 with VERA
Kohei Mizukubo(Kagoshima University)
Several studies have suggested that IRAS05358+3543 have massive stars, outflows, various molecule gases, anda protostellar disk. Although a number of studies has used 1.8kpc as the distance to this object, most of thembased on the kinematic distance or luminosity distance. However, it is less reliable, because this object locates at( l, b) = (173.4845,+02.4337), where all objects degenerate 0 radial velocity. Therefore, annual parallax is very
important. We succeeded to measure its parallax with VLBI Exploration of Radio Astrometry(VERA) in H2O
maser emission line at 22GHz. We get π = 1.150±0.068mas or D = 0.865kpc and the proper motions of eachmaser spot. Based on our distance estimation we review the physical properties of the sources in this region.
••••

STAR-FORMINGDISTANCE
VLBI

Kohei Mizukubo

PARALLAX

Ginsburg+ 2009

Resolving High Velocity Components
in NGC2023 MM1 Outflows

No. 15

Li-Wen Liao1 and Vivien Chen1,2
CO (2-1)

CO (3-2)

LV

Li Wen Liao

Sandell et al. 1999

HV

Astrometric observations of protoplanetary nebula
OH231.8+4.2 with VERA
 #.* '7 , *(' 03 * & 5 7.'$( , &3"'(.1'('(0. -# 
.1'('(0.,.# * 0.)$"2

&.1'(, -(4$01(27 2(.- +120.-.,(" +!1$04 2.07.% / -• -.0#$02..!2 (- - --3 +/ 0 ++ 6/0./$0,.2(.--##(120(!32(.-5$.!1$04$#, 1$0(-/0.2./+ -$2 07-$!3+   5(2'H2O maser distribution

Madoka Ohyama~17km/s

9  8, 1  8 */"~57”

~150 mas~10km/s~15km/s

Large discrepancy!!
200-400km/s
HST WFPC2

Large scale outflow of OH231.8+4.2

Our results

FUGIN : Molecular clouds toward W33; possible evidence
for a cloud-cloud collision triggering O star formation-0.2

Galactic Latitude [degree]

Galactic Latitude [degree]

Galactic Latitude [degree]

-0.1

-0.1

-0.1

-0.2

-0.2

Mikito Kohno (Nagoya Univ.)

Kohno et al. PASJ, in press, arXiv:1706.07964
-0.3

-0.3

-0.3

5pc

-0.4
13.0
12.9
12.8
12.7
Galactic Longitude [degree]
G012.745-00.153
Vlsr: 29.5 - 39.5 km/s
Contour levels : min 13 K km/s, step 15 K km/s

Galactic Latitude [degree]-0.1 -0.1

12.9
12.8
12.7
Galactic Longitude [degree]
Vlsr: 39.5 - 53.5 km/s
Contourlevels : min 17 K km/s, step 10 K km/s
-0.1

-0.4
13.0

-0.1

12.9
12.8
12.7
Galactic Longitude [degree]
Vlsr: 57.5 - 63.5 km/s
Contour levels : min 6 K km/s, step 8 K -0.1
km/s-0.1-0.1

Galactic Latitude [degree]

-0.4
13.0

J=1-0(c) 12(b)CO12CO
J=1-0(b) 12(a)CO12CO
J=1-0
J=1-0(a) 12CO J=1-0

W33B
W33 Main−1

G012.884-00.237
Fig. 4. R3−2/1−0
maps of the (a) 35 km s , (b) 45 km s−1 , and (c) 58 km s−1 cloud are shown in the color image. Contours show the 12 COJ =3–2
W33 B1-0.2 -0.2
-0.2 -0.2-0.2 -0.2
W33 Main1
emission, which was spatially smoothed 50′′ . Plots are same as Figure 1.
W33A
W33A1-0.3 -0.3
N-0.3 -0.3

G012.820-00.238

WN(a)

HPBW
-0.4 -0.4
13.0 13.0

G012.692-00.251
HII region
WN
ContoursK km/s
G012.745-00.153
Log
White : 0VLA
90MJy/srcm
125 250(b) HPBW
5pc
HPBW
5pc 5pc
Pink: ATLASGAL
8702.60μm HPBWHPBW
Vlsr:
29.5 2.00- 39.5 2.30
km/s
5pc
-0.4 -0.4

Mikito Kohno

G012.907-00.277
W

13.0 13.0

12.9 12.9
12.8 12.8
12.7 12.7
Galactic Longitude [degree]

12.9 12.9

Nobeyama13(d)CO
J=1-0(e) 13
CO
J=1-0Contour levels (white) : min 50 mJy/beam, Step 150 mJy/beam

Fig. 1. Three color image of W33 with blue, green, and red corresponding to Spitzer/IRAC 3.6 µm (Benjamin et al. 2003), Spitzer/IRAC 8 µm (Benjamin et-0.1al. 2003), and Spitzer/MIPS 24 µm (Carey et al. 2009) respectively. Large black crosses indicate the dust clumps (W33 Main, W33 A, W33 B, W33 Main1,Galactic Latitude [degree]

W33 A1, and W33 B1) identified with APEX in 870 µm by Contreras et al. (2013), and Urquhart et al. (2014). Orange and white circles indicate O and B-type
II

Galactic Latitude [degree]

28-0.2-0.3-0.3
NNW-0.4
13.0
HPBW-0.4
13.0

K km/s12 CO(1-0) 35 km/s

13Nobeyama
CO J=1-0 CO(1-0) 58 km/s(f) 13(e)CO
J=1-0

12-0.1 -0.1

-0.1

-0.2 -0.2-0.2-0.3 -0.3

-0.3

-0.3

-0.3 -0.3

W040 120080 25001250120250 250
5pc39.5
HPBW- 53.5
Vlsr:Vlsr:
53.539.5- 62.5km/skm/s
HPBW
Vlsr:
53.5 -km/s
Vlsr:- 29.5
39.5 km/s
5pc 5pc
1.90
2.45 3.00-0.4-0.4 -0.4
1313.0 13.0
12.9 12.9
12.8 12.8
12.7 12.7
12.8 12.8
12.7 12.7-0.2-0.2 -0.2-0.2

K km/s
K km/s

K km/s
K km/sLog MJy/sr-0.1

star identified by Messineo et al. (2015). White and pink contours show the VLA 90 cm and ATLASGAL 870 µm continuum image. White arrows show H-0.1 -0.1-0.1
regions identified with the WISE satelite (Anderson et al. 2014, 2015).

-0.3-0.3 -0.3W33 has two velocity components of CO clouds. (35km/s and 58 km/s)• The Spitzer 8 μm PAH emission is distributed along
the 35 km/s, 58km/s clouds, and HII region.
• The distribution of the 35 km/s and 58 km/s cloudare spatially anti-correlatedaround W33. KKkm/s
K km/skm/s
K km/sW33 is 5pc
likelyto be formed by a cloud-cloud
collision.
5pc
5pc
5pc
•

Galactic Latitude [degree](d) 13CO J=1-0 Contour levels (blue) : min 1 Jy/beam, Step 2 Jy/beam-0.2NNWW060 120060 120060
120-0.4
Vlsr:
29.5- 39.5Vlsr:
29.5
39.5km/s
Vlsr:
39.5
53.5km/s
HPBW
HPBW
13.0
12.9
12.8
12.7 km/s
12.9
12.8
12.7
HPBW5pc
HPBW-0.4 -0.4-0.4 -0.4
Galactic Longitude [degree]
Galactic Longitude [degree]
13.0
12.8
12.7
13.0 13.0
12.9 12.9Contour
12.8
12.9
12.8 min 50 K12.7
12.9 12.9
levels (Blue):12.7
min 50 K km/s, Step13.0
30 K km/s
Contour levels (Blue):km/s, Step 30 K km/s

60 40
12000 20
- 53.5
Vlsr:Vlsr:
53.539.5- 62.5km/skm/s

12.8 12.8

12.7 12.7-0.4
13

Newly Discovered Large scale structures in ELAIS-N1 field
Minhee Hyun¹, Myungshin Im¹, Jae-Woo Kim2 and Seong-Kook Lee¹
¹CEOU,Seoul National University, South Korea, 2Korea Astronomy and Space Science Institute, South Korea≳Minhee Hyun2017 EAST ASIAN YOUNG ASTRONOMERS MEETINGMy
Poster is
No. 18!
:)

Galaxies Experienced
MoreNa-Eun Shin
1. Select massive ellipticals
2. Classify as an Isolated or a high-density environment
3. Galaxy spectrum analysis with STARLIGHT

The Impact of Galactic Environment onStar-forming Clouds

Ngan K. Nguyen1*, Alex R. Pettitt1, Elizabeth J. Tasker2, Takashi Okamoto1

Ngan Kim Nguyen

ALMA Observations of Spiral Accretion FlowsNO. 21Towards Extremely Young Protostars
Pou-Ieng Cheong1, Shih-Ping Lai1, Sheng-Jun Lin1 (NTHU), Tao-Chung Ching2 (NAOC), Nadia Murillo3(Lieden), Zhi-Yun Li4 (Virginia)

Pou-leng Cheong✦

We identified three spiral-likestructures toward VLA1623.
✦ Two spiral-like structures havekinematics consistent with theCMU model.
✦ We generated the derived
trajectories in 3-dimension
space (ppp).

Poster
No. 22Dating a prestellar core: L1512
Sheng-Jun Lin; Shih-Ping Lai (NTHU, Taiwan);
Laurent Pagani (Observatoire de Paris, France)

3D Non-LTE radiativetransfer modelDensity Profile
Temperature Profile
N2H +, N2D +, DCO +, andH2D+ Line Observations

Sheng-Jun Lin

Abundance Profiles

Solve deuterium
chemical network
CO/N2 Depletion
Profile▲CFHT J/H/Ks+Spitzer IRAC2▲IRAM 30m+JCMT+GBT

Estimate the age ofthe prestellar core

Photometric Reverberation Mapping withMedium-bands and Large FOV Telescope

BLR

Sungyong Hwang
30~40 AGN are matched withqso catalog (Shen +11)
Five medium band filters have proper
bandwidth (FWHM ~ 50nm) to track
typical emission lines of type-1 AGN

Several hundreds of BH mass can be estimatedSearch for Exoplanets around Young Stellar Objects
Taichi Uyama (the University of Tokyo) et al.

Poster No. 24

Direct imaging explorarGon for exoplanetstarget: Young Stellar Objects- younger than ~10Myr- with protoplanetary disksAsymmetric disk (so called “transiGonal disk”)- implicaGon of planet formaGon
We observed about 70 YSOs, reduced more than 100 data in total

Taichi Uyama(leF) an example of the disk observaGon (SAO 206462; Garuﬁ et al. 2013)(right) one of our direct imaging results for a new companion around HIP 79462