THE STAR FORMATIONNEWSLETTER
No. 300 (#1-10)
塚越崇(茨城大)22 Dec. 2017

1. A Green Bank Telescope Survey of Large Galactic HII Regions
2. ALMA Discovery of Dust Belts around Proxima Centauri
3. On the Formation of Multiple Concentric Rings and Gaps inProtoplanetary Disks
4. Observing the linked depletion of dust and CO gas at 0.1-10 au
in disks of intermediate- mass stars
5. Measurement of Circumstellar Disk Sizes in the Upper Scorpius
OB Association with ALMA
6. New massive members of Cygnus OB2
7. HD 169142 in the eyes of ZIMPOL/SPHERE
8. On the fragmentation of filaments in a molecular cloud simulation
9. The ALMA early science view of FUor/EXor objects - V: continuum
disc masses and sizes
10.ALMA observations of Elias 2-24: a protoplanetary disk with multiple
gaps in the Ophiuchus Molecular CloudObserving the linked depletion of dust and CO gas at 0.1-10 au indisks of intermediate- mass stars
A. Banzatti et al.
• Herbig型星周りの円盤: Group I, Group II[Dullemond&Dominik2004]• 既存データベースで円盤内側の構造をカテゴライズ• 3つのパラメータに着目してガス・ダスト両成分を調べる

A&A proofs: manuscript no. 32034corr• Rovibrational CO(a)

HD163296

HD244604• FWHMCO

HD36112
HD135344B

HD142527

HD144432S

HD142666
HD98922

HD139614

HD101412

HD179218

HD142666

HD98922
HD31293high-NIR
cavities

HD135344B

HD139614

HD169142

HD141569

HD97048

HD250550

HD34282

GI

HD100546

HD142527

HD179218

HD101412

GII

HD141569
HD97048

(c)

solar

HD31648

HD135344B HD100453

HD169142

HD100546(d)

HD141569

HD36112

HD31293
HD98922

no/small cavities HD37806 HD98922

HD150193
HD31648

HD144432S
HD144668

HD101412

HD163296
HD31293

HD144432S

HD169142

HD139614

HD36112

HD179218

no/small cavities
CO

HD31648
HD142527

low-NIR
cavities
HD100546

HD142666

HD135344B

HD97048

solar
Fe/H

HD100546
HD139614

HD37806

HD95881

HD163296• 3つのパラメータは円盤構造

HD97048 HD179218

HD169142

HD142666• inner diskのdustにリンクしており、パラメー
タ上で切り分けるが可能

GI

HD31293

CO excitation• IR超過HD104237

HD144432S• v2/v1強度比• dust cavityの有無/accretion

HD163296
HD36112

solar

HD142527

回転構造からRCOに焼き直し• Fe/Hアバンダンス比(b)

HD190073

HD31648

F30/F13 < 2.2 (GII)F30/F13 > 2.2 (GI)HD141569

high-NIR cavities
solar
Fe/H

CO
planets?

low-NIR cavities
sub-solar
Fe/HCO

planets?

•strong silicate
weak/no silicate
and Rco moves to larger disk radii). As a simple test of whether
F↓でFe/H↓,
Fe/H↓でR↑
emissionemissionIa
NIR of CO gas and dust from the inner disk
CO maya linked depletion
globally reproduce the observed trends, we adopted a parametrichigh-NIR
Ia Ia
Ib
cavities
description of
inner dust減少かつガスもdepleteしdisk structure in hydrostatic equilibrium,• aninneras based on workby Kama et al. (2009) and summarized in Apている->回転速度減少
Ib
IIa
pendix C. The disk temperature decreases with disk radius asGroup
Iは2箇所に分離する
r 0.5 , and we
explored how
FNIR decreases as the radius of theinnermost dust (Rdust ) was sequentially increased to mimic theformation of anFinnerの大小で分かれる
hole.
Ib
Ib
•
NIR
Ib
A decrease of FNIR with increasing hole size (red curve in
no/small cavities
Ia• GIなのでどちらもギャップ天体だ
Fig. 1c) is naturally
produced by a decreasing temperature of the
Ia
Ia
low-NIRemitting dust, as
hotter dust at smaller radii is removed. In thisが、内側にダストが残存するかどう
cavities
Ib
scenario, Rco could
trace
the
size
of
an
inner
dust-depleted
disk
かで異なる
region, as suggested from previous observations (Brittain et al.
2003, 2007).
Keplerian line featureは単純なprofiles are modeled assumFWhen
NIRとsilicate
ing a power-law radial brightness (e.g., Salyk
2011),
Rco the linked depletion of dust and CO gas
Banzattietetal.
al. 2017:
Observing
as defined here can be several times larger than Rdust (taken as
Fig. 3. FNIR and F30/F13 for this sample of Herbig disks, highlight関係ではない
No/small cavity
Large cavity
Gas-poor
the innermost
radius
where
CO
gas
can
also
exist).
Themodel
ing the three classes as in Figure 1. Following Meeus et al. (2001),
We note that FNIR does not show a monotonic relation withcurve in Fig.
1c shows
Rdust
multipliedbyµm
7, silicate
by assuming
thewe mark disks where the 10 µm silicate emission has been detected
F30/F13(Figure3) andthat the 10
emission
is foundsilicatefeatureの弱いGIでもF
が大•NIR
median scaling
factorbetweenRvaluesandtheRvaluescodust level of FNIR(“IIa”
in disks with cavities regardlessof the measured. and “Ia”) or not (“Ib”); we keep the color-coding for the Ia/Ib
きいものが存在from Lazare↵etal.
(2017)
forthissample.
By
assuming
devoidWhile F30/F13 traces the depletion of intermediate disk labels
re- from Maaskant et al. (2013) to facilitate comparison to that work.
High-NIR
GI silicate emission is tightlyGas-poor
inner holes,
this->inner
simplethemodel
onlyK)a trend
ofemission
the loweris proMaaskant et al. (2013) showedthatrelated GIto
gions
where
warmprovides(⇠ 200–400
silicate
diskのダストが残存(HD135344B)
Large GII
(HD141569)
the
F30/F13
ratio;
instead,Fisunrelated(Sect.
4.2).
boundary duced
to the (Maaskant
data pointsetinal.thefigure.
the diskshigh must2013),FNIRReproducing
in the high-NIR
NIR(HD163296)
be円盤進化への示唆
producedbyHerbiga hotterdisks
disk region
closerto the star. We alsonear-IR excess
of somehas beena long-standing
note
that
no
Herbigdisk
inthissamplehasF⇠ 0, except formodeling challenge that is still unsolved (see, e.g.,NIR
Dullemond
Small GII
Gas-poor GII
and outer disk,
whereLow-NIR
the resupply
of inner disk dust by
inwardHD141569,
which
beenNew
proposed
to be e↵orts
globallycould
dispersing
これまでのpre-transitional
diskの定GI
et al. 2001;
Vinković
et al. has
2006).
modeling(HD150193)(HD145263)•(HD100546)
toward the(e.g., Whiteet al.values
2016). Thisdrift from the outer disk is inhibited (see, e.g., discussions
F30/F13 in> 2.2
be devoteditstogas
studying
howdebris
FNIR disk
can phasebe increased
toward
義では捉えられないinner
diskを切り
CO
gas,
Hot
dust,
Cold
dust
F30/F13 < 2.2
suggeststhat
innercavities
in
Herbigdisks
aredepletedbut
neverAndrews
et
al.
2011;
Kama
et
al.
2015).
measured in the high-NIR GI disks (25–35%) by keeping an in分けることが出来る
completely
devoid ofwhilematerial,
consistentresidual dustof CO
gasthatinappear
a dust-depleted
cavity ofFig.survival
4. Evolutionary
paths
possible by combining
thisHerwork
ner residual
dust component
inner
cavities withare formingat de- The
tected at the sublimation radius by NIR interferometry (Lazare↵and theanalysisof Garufi
et al. (2017).by
TheBrudererdichotomy
in innerThedisk
wasspecificallyinvestigated(2013).
larger disketradii.
Such a structure is supported by recent obser- big disks•al. Herbig型星で考えられている円盤進2017) and with significant accretion rates measured evencavities
is
shown
at
the
center:high-NIR
cavitieshavearesidual
study showed that as long as inner disks are still gas rich (N(H2in)vations of inthesedisks,disks.
as discussed
below.
化のうち、cavity円盤の進化のinner
low-NIR
The moderate/highaccretion rates measured 27
ner dust
2 component, possibly a belt/warp, that shields UV radiation and⇡ 10 cm at <1 au), the radial distribution of CO gas does notin somestars
with large inner disk cavities currently provide one enables CO (vibrationally cold) to survive into the cavity; low-NIR cavhot
dustのon/offの振る舞いを切り分
dependpresenceof gas-depleted,dust, as the anddensityof CO
molecules
itiesonaretheinsteaddust- andCO (herevibrationallyhot)of the main open problems in understanding the structure and
is
well
above
the
columnneededtoself-shieldfromUV
pho4. Discussion
けうるかもしれない
isdetected
only
close
to
the
cavitywall.
origin of disk cavities (e.g., Owen 2016; Ercolano & Pascucci
todissociation (Visser et al. 2009). When instead the total gas2017); interestingly, CO gas depletion in the disk has recently
HD142527

HD36112

HD31293•

HD100453

HD98922 HD37806

HD144668

HD95881

HD101412

HD135344B

HD150193

HD104237

HD144432S

HD31648 HD142666
HD163296

HD97048

HD169142

HD139614

HD179218

HD100546

HD141569••

HD34282

observe the CO J = 3-2 line at 345.79599 GHz. The observations had angular resolution between

00
00Disk Sizes in the
00 Upper Scorpius OB Association with ALMA
Measurement of Circumstellar
0 .35 and 0 .73 with a median of 0 .37 and a continuum rms ranging from 0.13 mJy/beam to 0.26
S.A. Barenfeld et al. mJy/beam, with a median of 0.15 mJy/beam.

• (比較的)年齢の進んだ領域のPPDの円盤質量とサイズを調査
3. Continuum Modeling• ALMA band7観測Our(c0,c2)
goal in modeling the continuum data was to determine the radial extent of the dust for• 345GHz連続波およびCO(3-2)
the 55 continuum-detected disks in our sample. To accomplish this, we compared our observed
visibilities to the synthetic visibilities of a model disk, deriving the model visibilities from an• Paper I[Barenfeld+2016]のデータを使用し、詳細なモデリングを実行• 連続波

assumed dust density distribution in a self-consistent way.

••

For our model disk, we parameterized the dust surface density as a function of radius using a
truncated diskでRADMC3D計算
truncated power law: -> ビジビリティフィッティング
✓
◆ 1
R
,
(1)
scale heightはMathews+2013の値を固定 ⌃(R) = ⌃0 10au••

for R between the dust inner and outer radii, Rin and Rdust , with ⌃ = 0 outside of this range. We
fixed Rin at the values found by the SED fitting of Mathews et al. (2013) for the 24 sources we”輝度分布”をフィットしてサイズ導出
share with their survey. For our remaining sources, we set Rin to be equal to the dust sublimation
radius, calculated based on the stellar luminosities from Paper I. The choice of Rin does not impact
連続波円盤モデルから予想される輝線強度を観測値と比較
our results.

• 分子輝線=>検出天体はscatterが大きい,上限値としてはconsistent

The continuum signal-to-noise ratio for the majority of our sample is too low to simultaneously
constrain the dust outer radius and the slope of the surface density power law. We therefore adopted
Fig. 3.— Observational and model fluxes for CO J = 3 2 emission for sources detected in th
a fixed R 1 parameterization for the surface density, which is fairly typical for disks (e.g., Kitamura
continuum, for models with (left panel) and without (right panel) photodissociation. Model fluxe
et al. 2002; wereAndrews& Williams
et al. CO
2007,
2010a; given
Guilloteau
et al.
2011).
Assuming
calculated
based 2007;
on theIsella
expectedemission
the disk
dust
properties,
as discusse
0.5
1.5
⌃/R
and
⌃
/
R
power
laws
resultedinslightly
smallerorlargerdisk
sizes,
respectively,
in Section 4.2. CO detections are shown as black points, while upper limits are shown with blubut did notarrows.
qualitatively
impactour results or sources
conclusions.
The fourwell-constrainedwith larger CO outer radii than dust outer radii arshown as(e.g.,stars.Hughes
Horizontal
represent
the2009;
68.3%Isellaconfidence
range Andrews
for the model
Some authors
et al.error
2008;bars
Andrews
et al.
et al. 2009;et fluxe
dashedline2010;
represents
betweenthe model
observed
fluxes.
al. 2010a,b;The
Hugheset al.
Isella agreement
et al. 2010a,b;Andrews
et al.and
2011;
Guilloteau
et al. 2011;
Andrews et al. 2012) have parameterized the disk surface density using the self-similar solution
for a viscously evolving disk, which can be approximated as a power law with an exponential tail.

• Rout(gas) v.s. Rout(dust)• ガスが大きいが同サイズもある• dust inward migrationの可能性もあるが, 光学的厚みの効果もありうる(いわゆる相似解円盤)– 41 –• Luminosity-size関係[Tripathi+2017]との比較• 単純なダスト成長+migrationでは
難しく、optically thickな
substructureの存在を要請• 本研究での結果はTripathiの12

関係性とよく合致する=>optically thickな
substructureのfilling factor
が進化と共に変化していないことを示すstellar host (see Eq. 9). The luminosities and e↵ective
radii corresponding to those intensity profiles were calculated as in Sections 3.3 and 3.4.
Figure 11 shows a highly condensed summary of themodels compared with the size and luminosity metrics
inferred from the data. These models actually do a reasonably good job at reproducing the observed mean trendwith a Md /M⇤ distribution from ⇠0.5–10%, a modest
range of initial Rc of ⇠60–150 AU, and relatively low
turbulence levels, ↵t . 0.001, but preferentially at earlypoints in the evolutionary sequence (<1 Myr).
While individual young star ages are notoriously uncertain (e.g., Soderblom et al. 2014), the nominal cluster
Figure 12. Comparisons of the measured size–luminosity relation
ages from which this sample is drawn are thought towith simple models for the optically thick disk structures; symbols
be more like 2–3 Myr. By those times, the model preare as in Fig. 11. The red curve is a purely optically thick modelwith the sample median temperature profile as given in Eq. (9).
dictions have diverged up and to the left in the {Lmm ,The blue curve corresponds to that same model with a (uniformlyRe↵ }-plane (away from the mean relation, with larger
distributed) 10% (areal) filling factor. The inferred distribution ofdisks in at
the 0.88{Lmm ,mm
Re↵ }-plane
could be reproducedby opticallyRe↵ thanof the radius
sample targets
a given Lmm) density
Fig. 7.—
Dust>90%e↵ective
versus forcontinuum
flux
for circumstellar
disks
thick regions with filling factors of a few tens of percent. The
due to both viscous spreading and a relative depletion
green curve is a toy variant of the pure optically thick model, with

Fig. 5.— Continuum (black circles) and CO (open circles) deprojected visi
with well-constrained dust and CO outer radii. The black and blue curves shfor the dust and CO, respectively. Four sources, 2MASS J16001844-223011
2040087, 2MASS J16123916-1859284, and 2MASS J16142029-1906481, exemission extending beyond their dust emission.

The ALMA early science view of FUor/EXor objects - V: continuum disc masses and sizes
L.A. Cieza et al.
mJy/beam• FUor/EXorの星周環境調査

V883Ori ALMA band 6

RT modelResidual

120
100

0.5

80

arcsec• FUor - “Luminosity Problem”のキー• 主な4つのモデル• MRI+GI, disk fragmentation+inward

200mJy/beam

HBC494 ALMA band 6

RT model80

Residual

0.5
arcsec• 連続波(メイン), CO同位体(paper 1)

40

0.5

migration, thermal viscosity, instabilities
by companions/planets• ALMA cycle2

60

0.0

• 連続波データに着目,ガウシアン

60

40

0.0

5

0.5

20

0

Table 1. Detected discs (sorted by declining disc mass)
フィットで円盤構造を導出

mJy/beam60

V2775Ori ALMA band 6

RT modelResidual50

HBC 494

V2775 Ori

0.5 Ori
V1647

NY Ori

V1143 Ori

V1118 OriASASSN-13db

Object TypeSpectral Type

FUor......

FUor......

FUor......

FUor/EXor0.0......

EXor
G6-K2

EXor
......

EXor
M1

EXor
M5

LBol [L ]

400

300

22-28

0.5
34-44

......

......

7.25

0.2

Companions......

......

Y? (1100 )......

N......

Y (0.1800 )......

F1.3mm [mJy]353±35113±11106±1078±8

32±3

2.3±0.2

1.3±0.1

0.3±0.07

Major axis [mas]

307±3

143±3

151±1

174±2

276±4

unresolved

unresolved

unresolved

Minor axis [mas]

247±4

47±8

146±2

154±2

194±6

unresolved

unresolved

unresolved

Position Angle [deg]

32±3

120±2

48±26

139±5

113±2

......

......

......

disc radius [au]

64

30

31

36

57

< 40

< 40

< 40

Inclination [deg]

37

70

15

28

45

......

......

......

MDU ST [M ]

1800

570

530

390

160

12

6.5

1.5

Mdisc [MJU P ]

570

180

170

120

50

3.8

2.0

0.5

arcsecV883 Ori

40

30

20

10

0

ψ!

• TTS円盤よ重い• TTS円盤よりコンパクト(中心集中)γ!
Mdisk%
TTS円盤よりsharpな面密度分布•• FUorγ > TTS平均(γ~0.86)• FUor円盤の特徴? or 円盤粘性進化の初期?

ψ"ψ"=>gaussian fitとconsistent• FUorの特徴

RC%

hC%

This study
TTauri disk [Andrews+2010]hC%• RADMC3D• similarity solution• a=0.1um-3mm

hC%

を実行

RC%

• SNの良いFUorには放射輸送計算

C%

RC%

hC%

ψ!

Mdisk%

Figure 3. Same as Figure 2, but for V883 Ori and HBC 494.

• メカニズムの分離
Table 2. Disc parameters from Radiative Transfer Modeling
FUorの放射輸送計算の結果

Figure 6. Disc masses as a function of Rc (and upper size limits) for our 8 targets (green points) compared to the sstars (red points) studied by Andrews et al. (2010). We find that the FUor objects (V883 Ori, HBC 494, and V2775
larger masses than the EXor sources (NY Ori, V1143 Ori, V1118 Ori and ASASSN-13db). The borderline object V1647
disc properties to Name
V2775 Ori. The FUorRsources
haveM
largerhcsize than the T Tauri stars. N
cdiscdisc masses for a given disc
trend followed by T Tauri stars (blue line). The other EXor objects have no size measurements, but they are unlikely(au)(MJU Pau) in radius. The black arrow(au)shows the general evolution etrend, unless they have tiny discs that are less than 0.1-5
1/2
conservation of angular momentum in a viscous disc, given by Md / Rc
. The FUor objects in our sample are embed
+6
+50
+0.04
that might evolve V883
onto theOri
T Tauri locus
31 as6 they evolve.
600 601.48 0.06
4.2+1.8
0.86+0.08
0.6
0.16
+0.04
+7.1
+0.32
HBC 494
21+712100+70
1.94
1.6
1.52
80
0.30
0.8
0.28
+0.06
+0.4
+0.11
V2775 Ori
42+22
80+10
1.44
4.7
0.60
10
0.06
0.3
0.08
+3
+10
+0.68
+1.1
+0.18
V1647 Ori
40 3
80 10
0.57 0.13
4.2 0.7
0.99 0.19
+5
+10
+0.11
+1.0
+0.12
c 0000
RAS, MNR
NY Ori76 7
40 101.29 0.10
4.6 0.8
0.98
0.17• FUorはGIの可能性があるが、高分解能観
測ではspiralなどは見えていない• burstしてない天体がspiralをもつケースも見つかっている• EXorは軽いのでGIではないだろうγ!

• burst現象を調べるには104個の天体を10年間モニターする必要があるA Green Bank Telescope Survey of Large Galactic HII Regions
L.D.Anderson et al.

• HII領域の再結合線によるサーベイ観測(HRDS)• 線幅の狭い再結合線を検出, <1100K相当のturbulence• 最も明るいHII領域の検出• 最も大きい(>100pc)HII領域の検出• 全部で887のHII領域をカタログ化 (これまでの倍以上)
ALMA Discovery of Dust Belts around Proxima Centauri
G. Andlada et al.

• ALMA 1.3mm観測によって、プロキシマ・ケンタウリの1-4auの位置に~40Kのダストベルトを検出• ダストベルトの質量は0.01Mearthでカイパーベルトとconsistent• その他marginalな発見• 30auの10Kダストベスト• unknown millimeter source (~2au SE)

On the Formation of Multiple Concentric Rings and Gaps in Protoplanetary Disks
J. Bae, Z. Zhu, L. Hartmann• 惑星による形成されるspiral armのうちsecondary成分を2D hydrostatic

simulationで調べた• secondary/tertiary armもギャップを開けるので、低質量惑星でも複数の円盤ギャップを形成しうる• HLTauへの応用; 30Mearth at 68.8auでHLTauギャップを説明可能• ギャップは惑星質量と温度分布に依存する(ので温度構造の観測が重要)

New massive members of Cygnus OB2
S.R. Berlanas et al.

• OB richなCygnus OB2領域に対し、よりcompleteなサンプルを目指
して、領域内のOB型星のサンプル数を増やす• Intermediate resolution spectra(R~5000)によるspectralclassification (HeI-IIとメタルline)• 42/61天体のOB型星をID• age-longitudeの相関関係をconfirm• Cygnusではまだ多くのO, early-B型星が埋もれているHD 169142 in the eyes of ZIMPOL/SPHERE
G.H.-M. Bertrang et al.

• Zurich Imaging Polarimeter on VLTでの新しいデータ• 3.5au—126auまでをカバー• inner hole, bright inner ring(21au,NIR新検出), 楕円状gap(29-55au)の構造を検出• これまでに見つかっていたgap構造をconfirmした+star-disk offsetや
sub-structureといった惑星形成に関連しそうな構造を検出した

On the fragmentation of filaments in a molecular cloud simulation
R.A. Chira et al.

• FLASHを用いたシミュレーション(kpcスケール)で、分子雲内のフィ

ラメント形成を調べる• DisPerSeアルゴリズムによるフィラメント同定• フィラメントの線密度はself-gravity開始以降増大, fragmentationは比較的早期に生じる(~16M⦿/pc)• 分子雲の圧縮がフィラメント形成にとって重要

ALMA observations of Elias 2-24: a protoplanetary disk with multiple gaps in the Ophiuchus
Molecular Cloud
L.A. Cieza et al.

• ALMA 1.3mm連続波観測 (0.2”;25au分解能)でEL24を観測• 20,52,87auでgapを検出• ギャップ位置はCO, N2のcondensation frontとconsistent• ギャップ幅はそれぞれ0.2-1.5MJ, 1.0-8.0MJ, 0.02-0.15MJの惑星の4-8– 13 –

ヒル半径で説明できる
massと整合的• この惑星質量はギャップで期待されるmissing– 12 –
mJy/beam
40
35
30

mJy/pixel

1.0(a) Elias 2-24 CLEAN (uniform)(b) Elias 2-24 MEM

0.4

1.0

0.3

15
10
5

0

0.5

0.5

0.0

0.0

0.5

0.5

1.0

1.0

Dec (arcsec)

20

Dec (arcsec)

25

0.2

0.1

0.0