14. Outbursting Young Stellar Object PGIR 20dci in the Perseus ArmLynne A. Hillenbrand, et al.
15. The Pictoris b Hill sphere transit campaign. Paper I: Photometric limits to dust and rings
M. A. Kenworthy, et al.
16. The warm-up phase in massive star-forming cores around RCW 120
M. S. Kirsanova, et al.
17. New low-mass members of Chamaeleon I and Cha
K. Kubiak, et al.
18. ALMA Observations of Massive Clouds in the Central Molecular Zone: Ubiquitous Protostellar Outflows
Xing Lu, et al.
19. Characterizing the dust content of disk substructures in TW Hya
Enrique Macias, et al.
20. Radiative scale-height and shadows in protoplanetary disks
Matías Montesinos, et al.

14. Outbursting Young Stellar Object PGIR 20dci in the Perseus Arm
Lynne A. Hillenbrand, et al.

15. The Pictoris b Hill sphere transit campaign. Paper I: Photometric limits to dust andM. A. Kenworthy, et al.

b Pic M=1.797M8, t=21Myrb Pic b m=11.1MJ, a=9.76AU
rHill =1.1AUb Picb Pic b1981 b Pic 4% 数⽇明るさの変動b Pic b の周惑星円盤による掩蔽？
2017,2018 b Pic の光度モニター
予想時期に暗くなった形成はなし。

16. The warm-up phase in massive star-forming cores around RCW 120
M. S. Kirsanova, et al.

HIIHerschel image 70 µm
ATLASGAL 870 µm
コア1PDR

コア2

コア1

コア2

CH3OH, C34S

CH3OH, C34S
CH3CN, SO2

T<100K

K<100Kn~105-7cm-3Less evolved

分⼦少ない。
Warm-up phase17. New low-mass members of Chamaeleon I and e Cha
K. Kubiak, et al.

カメレオン領域の星形成史
Cha I D=190pc 250YSOs (~2Myr)
Cha II D=210pc 51YSOs (2-4Myr)
Cha III No YSOse Cha moving group (5-10 Myr)

Gaia + 2 MASS
Ha emission line EW, a shallow Na I absorption,
mid IR excess, X-ray è pre-main-sequence
Cha I 7個、Cha II 2個、e Cha 15個

Lower Centaurus Crux
(A0 group of LCC)

3D構造

2MASSJバンドソースの距離別分布

e Cha moving
groupRegion A

⾊等級図

固有運動

分光：e Chaの年齢 8-10 Myr

銀河回転
C 10Myr
B 9.3Myr

A 7.2Myr<latexit sha1_base64="QYuUgUgvzyKHZAgQhQtIxQ3UIpE=">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</latexit>

銀河中⼼e Cha>

7Myr
A0 e Cha<latexit sha1_base64="XUovV+jOWGv0ynK1UPpjcohcXm4=">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</latexit>

77<77

銀河中⼼LCC from Goodman+2018

18. ALMA Observations of Massive Clouds in the Central Molecular Zone: Ubiquitous Protostellar Outflows
Xing Lu, et al.

CMZは、星形成効率が10倍くらい低い。
Lu+2020 ALMA conti à 2000AU規模、834個のコア à
ここで、skockトレーサーでアウトフローは⾒つかるか。

37(highly likely)+6(candidate)
791 no detection

H2Oメーザー源
SiO

1.3mm 連続波
SO

CH3OH

834コア
43コアがアウトフロー付き
残り791コアがなし。
★分⼦雲により4~7%がアウトフロー付き

積分強度

H2CO

HC3N

1Myr

HNCO

`
<latexit sha1_base64="TLIRTHI7FhxCHk6Ty/ysSvRpiJI=">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</latexit>

τ~10Myr( /1度)
Vorb~80km/s

0.9MyrLongmore+2013

0.6Myrτprestellar期=1-2Myrなら
τoutflow付き=0.05-0.1Myr

H2に相対的なabundance

L1157 low mass star formation
NGC 7538 S high mass star formation
L1157でCOが光学的に厚くなっている可能性(Bachiller & Pérez Gutiérrez 1997)
H2を過⼩評価。
shock tracer 分⼦の存在⽐を過⼤評価HC3Nに相対的なabundance
HC3Nに相対的な存在⽐
CMZの特殊性は⾒られない。

19. Characterizing the dust content of disk substructures in TW Hya
Enrique Macias, et al.

20. Radiative scale-height and shadows in protoplanetary disks
Matías Montesinos, et al.

Muller, Kley, Meru 2012