THE STAR FORMATIONNEWSLETTER
No. 291 (#36-40)
塚越崇(茨城大)19 May. 2017

1. Two dimensional ice mapping of molecular cores
2. Large-Scale Spectroscopic Mapping of the ρ Ophiuchi Molecular
Cloud Complex I. The C2H to N2H+ Ratio as a Signpost of Cloud
Characteristics
3. ALMA Observations of Vibrationally Excited HC3N Lines Toward
Orion KL
4. The turbulent life of dust grains in the supernova-driven, multiphase interstellar medium
5. The anatomy of the OrionB Giant Molecular Cloud: A local
template for studies of nearby galaxies

c IRAC 1 is the flux at 3.6 µm, extracted from the Spitzer c2d catalogues used tod Distances come from Murdin & Penston (1977); Racca et al. (2009); Lee & M

Two dimensional ice mapping of molecular cores
J.A. Noble et al.

• iceとgasの直接比較はchemical networkの制限などで重要だが、iceの観測はchallenging• 明るいbackgroundの吸収線として見る必要がある• gas量を説明するようにiceの存在量を推測することが多い(diskのsnow lineなど)• gas-grain reaction modelに依存してしまう• AKARIデータを使用[Noble+2013]• CO, H2O, CO2 iceの2D分布を出す(手法のテスト)• a few 1000 au resolutionの分解能を目指す• 4つの分子雲(14 objects)• 全天体でWater iceを検出,CO2 ice,CO iceも検出したがconfusionあり• Av↑でiceの密度↑• 高密度なコアでiceが多いことを示すが、localconditionに依るかもしれない• ice柱密度マップ• BHR59,DC300(+#13)は星なしコア
他はprotostar• H2O ice柱密度mapとAvの相関が良い• CO2,COも#3以外はH2Oと相関が良い• ice-gas柱密度比較• SP index↑でH2O ice↑
• CO gasとiceで相関がありそう• 必ずしもダスト↑でice↑ というわけではないK km s-1

-24°10’I

DEC (J2000)

20’
30’

DG

J

B2
B1
CANWK

H

FL

40’

M

1W50’

324

S-25°00’

L1689 L1688

10’16h32m00s

16h30m00s

16h28m00s

16h26m00s

16h24m00s

16h26m00s

16h24m00s

RA (J2000)-24°10’
20’
30’
40’
50’
-25°00’10’16h32m00s

16h30m00s

16h28m00s

• Nautilusによる化学反応計算

10[C2H]/[H]• pure gasとgas-grain chemistryを比較• gas-grain反応を入れると[C2H]は進化後期で変化大-> Oが凍り(H2O)、C2H->CO変換が不活性になる•

NH=5.0 × 103 cm-3

-6

10-810-1010 K
20 K
30 K
40 K

10-12

[C2H]/[N2H+]と温度データをモデルと比較

10-1410-6なるが、実際の密度もばらつきがあるので、化学年齢と密度のcombinationによって5-110という比のばらつきが生まれているのだろう

gasの存在を示唆• C2Hマップの広がりは、younger– 28 –

ダストコアの密度
NH=5.0 × 103 cm-3

1000

NH=1.0 × 105 cm-3

NH=2.0 × 104 cm-3

10-10
10-1210-1410-1610-1810-20
1010[C2H]/[N2H+]• 密度によって年齢が一桁程度変わりうる。
• ダストコア密度を考えると(>~105 cm-3)、~104yr程度の年齢と[N2H+]/[H]

10-8

105

100

NH=1.0 × 106 cm-3

10-5101

102

103

104

105

Time (Year)106

107 101

1[C2H]/[N2H+]

100

Fig.

1010K
20K
30K
40K

[C2 H]/[N2 H+ ]. Each column shows theL1688 Data
L1689 Data

12×1047.— The gas-grain model calcu

105YEAR106 104

105
YEAR3105 2×105 3×105×10 104
5YEAR

as the titles of the first plots of the co51×104
3×10
YEAR line, light green dash-dot line, and red dALMA Observations of Vibrationally Excited HC3N Lines Toward Orion KL
Y. Peng et al.

• Hot coreのheating sourceは？
=>HC3Nの観測が有効• KLではまだlow-resolutionの観測しかない• ALAM SV data + IRAM30m

• Euの上昇とともに線幅は狭くなる傾向• Eu増加につれ、Trot大, Ntot小• 高励起の放射はhot coreにピークが無い
ため、internal sourceによるheatingではなさそう (externally heated)
Figure 7. Plot of line widths as a function of upper-level energies (E u ). Thesquare, solid circle, and open circle denote the line widths derived from hotcore, HC-North, and IRc7 positions, respectively.

no a single massive protostellar source in the hot core (MentenReid 1995; Greenhill et al. 2004; Friedel & Snyder 2008).
• Source&Iが起源？
We also ﬁnd that the molecular gas at the center has lower gas
temperature and higher column density, and the intensity peaks
move from southeast to northeast of Source I with increasing
E u (see Figure 5). Our results appear to not support internal
heating in the OrionKL hot core. SourceI has been considered=>高励起放射のピークはずれている

高励起HC3NはSiOアウトフローとのinteractionにより生成？

as the most likely external candidate based on the observationsof lines and continuum (Blake et al. 1996; Wilson et al. 2000).
However, there is offset between SourceI and the peaks ofvibrationally excited states of HC3N (de Vicente et al. 2002).

The turbulent life of dust grains in the supernova-driven, multi-phase interstellar medium
nuscript T.
no. Petersorionbet al.

observed field of view.

• ORION-B project000

6 00.12000
8 45.38000
5 32.48000
4 28.7000
6 33.26( x, y)(00 ,00 )( 33.35, 00.07)(+32.87, 01.33)(+13.72, 09.42)(+20.54, 29.43)(+05.49, 31.04)

Parallax

Distance

VLSR

maspc
km s
• 多輝線同時観測によるデータベース化
2.5806 ± 0.0088
387.5 ± 1.3
15.0 ± 1.6
5.90 ± 1.29
169 ± 37
18.1 ± 4.5• extra-gal.のテンプレートとして2.776 ± 0.271
362 ± 35
7.7 ± 2
(1)

(1)

(2)

(2)

• IRAM30mによる観測(3)—3.4 ± 0.2(5)• 複数輝線の観測+ extinction, T

1(3)415(4)

294 ± 21(5)maps—3.7 ± 1.3

DR1 Gaia Collaboration (2016); Lindegren et al. (2016); Fabricius
dust
Hummel et al. (2013)• 様々な数値を比較• Av毎の比較 ->高密度(のみ)トレーサーN2H+• Tdの比較• Av-柱密度 -> C18O, HNCで良い相関• 輝線同士の比->高密度トレーサー, PDRトレーサーの調査(詳しくは元論文参照)

nn1.
dseas
vne

•

• FLASH4による計算

磁場なしの等温シート
4 • INDIVIDUAL
TRAJECTORIES• ISM dust models typically represent the ISM phases
While+
H+,H,Hcharacteristic
2,C ,O,CO, etemperature, a more accuratewith a• singlephasedefinition assigns a whole temperature range to each• supernovaのinput
phase (e.g. Ferrière 2001). Guided by our previous study ofdensity peak, mixed• random,ISM phasesin the SILCC simulations by Walch et al. (2015),
per Myr• 15 supernova
we consider
four di↵erent
phases defined by temperaturecuts
in this paper:
ISMのphaseに着目して解析
time-dependent chemical network•(i) molecular phase (T < 50 K),(ii) cold phase (50 6 T < 300 K),(iii) warm phase (300 6 T < 3 ⇥ 105 K),(iv) hot phase (T > 3 ⇥ 105 K).

z (kpc)•y (kpc)

yegues
meeesyxorkwe
ata anatomy
region of ofdiameter⇠ 0.2
kpc inthe first Cloud:10 MyrAbecause
Thethe OrionB
GiantMolecular
local template for studies of nearby galaxies
The turbulent life of dust grains 5of the described runaway process. Supernova explosion sites
J. Pety et al.
random driving
propagate radially outwards from the location of therandom
firstdriving
t = 40 Myr
t = 40 Myr
explosion. At 40 Myr, the ISM has a complex structure
and0.20.2
ISM中のdust形成/進化を計算
the tracer particles are fully mixed. However, the initially0.1
0.1
chemistryで重要• UV shieldやgrainclusteredsupernova explosions
have created a cavity thatremains
the rest of the simulation runtime.0.0Since super0.0
SILCCforproject
novae are injected at density peaks, much less hot gas is
0.1
0.1
the LifeCycle of• SImulating
created,and almost no galactic wind is driven (Girichidis
et al.molecular2016). At Clouds
80 Myr, the gas density in the 0.2
disc is higher0.2
thanfor random and mixed driving, and the tracer particles• ラグランジアン的なダスト滞在時間
are more homogeneously distributed.の見積もりのpilot study• 結果の様々なcut -> SNのpositionに依存
The turbulent life of dust grains

randomrandomdriving
driving

100 01010 1

10 3 3101010 4 400

X

fpart
X

H2
HH+

10 2 2101010202030
30

4050
40
50t t(Myr)
(Myr)

60
6070
70

H2H
H+

10 2

10 3

molecular
coldwarmhot

10 408080

mixeddriving
driving
mixed

100 0
1010203040t (Myr)

5060

70

10 1

10 2 21010 3 31010 4 41000

X

fpart
XH2HH+202030304050
4050(Myr)t t(Myr)

60
60

70
70

10 2

10 4080
80

peak driving

100

H2HH+

10 3

molecular
coldwarmhot
10101020

10 13040t (Myr)

50

60

70

10 1X

molecular
cold
warm
hot

10 380peak driving

100

10 280

mixed driving

100

10 1 1
10X

random driving

100

10 1 1
109H2
H
H+

10 2

10 3

10 40

10

20

30

40t (Myr)

50

60

70

mass fraction (Temp cuts)

80

10 40102030

40t (Myr)

50

60

70

80

mass fraction (abund. cuts)

ractionsFigure
X (right)
for the di↵erent
defined
cutsX (right) for the di↵erent ISM phases defined by chemical abundances
4. Particle
fractions ISM
fpartphases(left) andtotalby
gastemperaturemass fractions
peak (bottom)driving.
as functionof time t for random (top), mixed (middle) and peak (bottom) driving.

transition rate

Figure 5. Transition rates of particles moving between di↵erent ISM phas• peak drivingではSN

14Thomas Peters
et al.
40Myrにおける粒子のISM
phase滞在時間
random driving

106

molecular
coldwarm
hot105

によって効率的に分106105• residence timeは単位

104

Npart

子雲が壊される

Npart

104
103

102

101

101

値ではなく幅広く分
布1061020304050
tres (Myr)60• pilot studyであり、よ106

molecular
cold
warm
hot

105

Npart

102

101

101

1020304050
tres (Myr)6070100080peak driving

106

molecular
coldwarm
hot

105

105

304050tres (Myr)

60

70

80

60

7080

607080

mixed driving
H2
H
H+

1020

30

4050
tres (Myr)peak driving
H2
HH+

104

Npart

Npart

104
103

103

102

102

101

101

100
020103

102

106を目指す

10104

103

1000り詳細な長時間計算• self-consistent• stellar feedback• complete treatment of SF

100080104

Npart

G2D比が10%ほど減る[Zhukovska+2008のダスト進化モデル]

70

mixed driving

105• =>分子雲寿命が変わり

103

102

1000random driving
H2HH+

1020304050
tres (Myr)

60

7080

10001020304050
tres (Myr)