THE STAR FORMATIONNEWSLETTER
No. 315 (#34-43)
塚越崇(NAOJ)
24 May. 2019

1. The nitrogen carrier in protoplanetary disks
2. Observing the gas component of circumplanetary disks around wideorbit planet-mass companions in the (sub)mm regime
3. A high resolution mid-infrared survey of water emission fromprotoplanetary disks
4. ALMA High Angular Resolution Polarization Study: An Extremely YoungClass 0 Source, OMC-3/MMS 6
5. Polarization of stars with debris disks: comparing observations with models
6. The survivability of planetary systems in young and dense star clusters
7. Spatial segregation of dust grains in transition disks. SPHERE
observations of 2MASS J16083070-3828268 and RXJ1852.3-3700
8. Ejection History of the IRAS 04166+2706 Molecular Jet
9. Luminosity outburst chemistry in protoplanetary discs: going beyond
standard tracers
10.External photoevaporation of protoplanetary discs in Cygnus OB2: linking
discs to star formation dynamical history

Observing the gas component of circumplanetary disks around wide-orbit planet-masscompanions in the (sub)mm regime
Rab, Ch. et al.

• Wide-orbitのplanetary mass companionで周惑星円盤が受からないのはなぜか？

• モデルと放射輸送計算を行い、ALMAの感度と比較• サイズが大きい周惑星円盤だと分子輝線観測で受かるかも• Wide-orbitのPMCを想定してモデル化• 原始惑星系円盤に”埋もれていない”状態• power-law density prof., disk/planet mass ratio=1%,
Rout=1/3 Hill radius• CSChaのALMA non-detectionを念頭に[Wu+2017a,Ginski+2018]• PRODIMO codeによる化学&放射輸送計算• Synthetic observables• ALMA Band6-10 & Band6 of ngVLAを想定• ALMA/CASA simulation, 6hours integration, dv=1km/s
Ch. Rab et al.: Observing the gas component of CPDs in the (sub)mm regime

Fig. 3. Left panel: Location of the main emitting region for the near-infrared and (sub)mm dust emission and the 12 CO J = 3 2 line in the reference
model. The vertical lines of the boxes denote the radii where the cumulative flux in radial directions reaches 15% and 85%, respectively. The
horizontal lines denote the heights where the cumulative flux integrated vertically reaches 15% and 85% at each radial position. The coloured
contours show the CO number density and the dotted grey line shows where the visual extinction AV reaches unity. Right panel: Normalizedradial intensity profiles (azimuthally averaged) for the dust continuum and line images. Shown are profiles derived from images convolved withrepresentative beam sizes for SPHERE (blue, FWHM = 0.03100 ), ALMA (black, FWHM = 0.01200 ), and ngVLA (red, FWHM = 0.00400 ).

• 各Bandでの放射強度と感度• COもダストも円盤サイズ↑で強度↑• ALMA Bandsでは円盤質量への依存性弱• 光学的に厚いため
Ch. Rab et al.: Observing the gas component of CPDs in the (sub)mm regime
CSCha観測上限値[Wu+2017]

5. Comparison of CO line and continuum peak fluxes from CPD
PMC光度と放射場に対する変化• Fig.
models with varying structure properties (radius and mass) to 5 detec12

tion limits
for one band of ngVLA and various ALMA bands (see ApダストはPMC光度にsensitive
pendix C for details). The dust emission is reported at the same wavelength放射場の変化はCOのみ↑
as the corresponding line. A beam of 0.100 ⇥ 0.100 is assumed.
For the lines a channel width of 1 km/s was used. The peak flux is the
maximum flux value in the synthetic images; for the lines all channels
are considered to evaluate the peak flux (see Appendix D for details).
The diamond symbols show the fluxes for the lines and the star symbols
Fig. 6. Same as Fig. 5 but for models with varying dust properties. The Fig.
Same as Fig. 5continuum
but for models
withvaryingthe7.corresponding
fluxes.
The
black radiation
solid andproperties
dashed lines
underlying model is always the reference model with Lp = 10 2 L , of indicate
the PMCtheandtheenvironment(backgroundfield).
The underlying
sensitivity limits for the line and continuum,
respectively.
Md = 0.2 Mamaxはあまり影響がない
disk
structureis alwaysthat fromthe reference
model. levels as reported
J , and rout ⇡ 11 au.
Thelight greybox shows
the rangeof 3 sensitivity
submm放射は光学的に厚く、内側の by Wu et al. (2017a) for their ALMA Band 6 continuum non-detectionsof a sample of wide-orbit PMCs.

••(Rtap =
but cawith thmodelsr ⇡ 1
disk isrout .
is smaet al. (results
the anaradiald/g =disks (
To
lines crout ⇡
is best
might
becom

Ch. Rab et al.: Observing the gas component of CPDs in the (sub)mm regime• ダスト進化の依存性••

暖かい領域で決まるinner
regionsion is not significantlya↵ected although the hot
emission
at most a↵ected line. The continuum fluxes drop by factors of 1.9
those wavelengths should be dominated by large dust grains to 3 compared to the reference model, with the lowest change
ダスト質量を減らすと円盤質量&サイズ↓• 100(agrain &µm). In the models presented in this work, the in but
the arengVLAband and thehighestchangein models
ALMA theB10.best
TheS/Nnot detectablein thelines.
For allに伴いフラックス↓(sub)mm dust
emission is dominated by optically thick emission dust
moresensitive
the opticalemissionof the theis temperaturereached withis thengVLA
andto ALMA
Band
7, whereas
and the sensitivity to the dust grain size is therefore lost. In the companion
and is thereforebands
more (Bandsa↵ected8byof the for
ALMA high-frequency
to the10)decrease
are not suited
COにはほとんど影響なし
amax =•1 µm model, the 860 µm emission is optically thick up to photosphericluminosity.
For
the
gas,
the
far-ultraviolet(far-UV)
detections of CPDs such as those modelled in this work.
r ⇡ 1.7 au and the average dust temperature in the emitting re-3.3. D

Similalikelying inand cobrown
of Zhucess iseral) thlower
Zhu etare sigthat atdust poWe

A&A proofs: manuscript no.

• CSCha(c)との比較••

solvedstraint
Dust disk model [Ginski+2018]disk. W-3
as our
• Mp=20MJ, Lp=2.5x10 L⦿,whetheMcpd=2x10-4MJ, amax=1um
As
light
im
Ginskiモデルだと6時間積分でも検出はsize. W
難しい
using aaxis a• tapered edgeにすればCOなら検出
mass o
できるかもしれない
ski etestima• ダスト検出は難しいが、ダストサイ
tent w
ズが大きければ受かる可能性がある
tance e179±1
A&A proofs: manuscript no. Rab_wocpd(GAIA
from tFig. tion
8. SameFig.disk
5 butaroundfor the CS
Cha companion
model.
of aasgas
a wide-orbit
PMC.
TheShown
flexibleCollab
mode
are theoriginal
Ginskietal.
(2018)
model
andseveraltapered-edge
Cha ispresented in this work allows us to make accurate prediction
models with di↵erent dust-to-gas mass ratios (d/g) and dust composi- have afor both the dust and gas observables of the potential CPD cantions/populations (large grains).
tancesdidates. As observing such CPDs will be time consuming
eve
model
with ALMA or ngVLA, such models are crucial to optimize observing
dependingbackgroundon the known
properties
ofInthTo
study programmes
the impact of enhanced
radiation,we
CPDm
軌道半径が大きければ大きい円盤が期• Fig.
showcompanionin
7 models
10 and 100 times stronger ISM
and itswith
hostastar.
ters ofradiation field ( ISM = 10, ISM = 100) and a model where we
model
待できるので検出される可能性がある
assume that the additional stellar radiation heats the dust disk to a
4.2.
What
can we
learn
from
gas
observations
minimum
temperature
of T
25 K.
Relativeto the reference we als
d,min =
Rout>10auくらいで、円盤全体で光学•
model the line fluxes increase in all three cases whereas the dust dust pr
used b
4.2.1.
Companion
andwith
diskTproperties
is onlya↵ectedin the model
的に厚ければ受かる
d,min = 25 K. We note thatfor the ISM = 100 model CO is efficiently photodissociated in origina
Current continuum
observationsof Jwide-orbit
PMCs indicat
-4M
12
COならM
くらい
the outer disk and
CO J = 3 d~10
2 emission
becomes optically the lin• theregimesmall
dust
disks,
eitherbecausetheyareunresolved(Ginskiet athin at r ⇡ 9 au compared to r ⇡ 10 au in the reference model.
Ginski2018)theor higher
not detected
at all (Wueasily
et al. 2017a).
However,
However,gas temperaturescompensate
for the in a com(sub)mpactemitting
CPD thedust might evolve on much shorter timescales
thasmallerregion.
The re
in
T
Tauri
disks
and
rapid
radialmigration
can
lead
to
stronglGenerally speaking, the size of the CPD has more impact
clude a• CPD検出のfeasibility

A high resolution mid-infrared survey of water emission from protoplanetary disks
Salyk, C. et al.

• CTTS&TDに対するH2O輝線の高分散中間赤外分光• CTTSの方が検出率高い• スペクトル形状から放射領域を推定• 円盤 + Wind• 将来観測への布石: JWST(励起を多くする)や30m望遠鏡(SNR向上)• MIR spectrographs on Gemini North• TEXES (R~100000, dv=3km/s), Michelle (R~25000, dv=12.5km/s)• 8 CTTSs & 3 TDs

7

Rotation diagram

TABLE 5Model fits

High-Res
Spitzer
SourceT [K]log Nfixed−Ω a [cm−2 ] log Rfixed−N b [AU] T [K]log N [cm−2 ] log Rc [AU] Spitzer Ref
DoAr 44534 ± 36
18.23 ± 0.22
0.12 ± 0.11
450
18.3
-0.036
2
DR Tau (T)726 ± 13718.04 ± 0.37
0.025 ± 0.19
500
18.6
0.18
2
DR Tau (M)725 ± 4618.30 ± 0.17
0.15 ± 0.09
FZ Tau (T)748 ± 5417.83 ± 0.18
−0.09 ± 0.09
550
19.0
−0.15
3
FZ Tau (M)1014 ± 161 17.36 ± 0.27
−0.32 ± 0.14
HL Tau396 ± 89
20.41 ± 0.60
1.2 ± 0.3
750
19.0
−0.097
3
IRAS 04303+2240 425
19.8
0.9
250
20.9
0.43
3
RW Aur591 ± 300
18.7 ± 2.0
0.35 ± 1.0
600
18.3
0.20
1
T Tau N479 ± 156
19.8 ± 0.7
0.9 ± 0.4
700
19.6
0.0
3
AS 205520 ± 75
19.36 ± 0.54
0.68 ± 0.27
300
20.6
0.34
2
RNO 90595 ± 160
18.11 ± 0.99
0.06 ± 0.50
450
18.3
0.23
2
(1) Carr & Najita (2011) (2) Salyk et al. (2011a) (3) This work.
Ω0a Not a true column density. The true column density, N = N
22
fixed−Ω Ω where Ω0 = π(1 AU) /d and Ω is the true emitting solid angle.
For Nfixed−Ω ! 1019 cm−2 , N must be < Nfixed−Ω for lines to remain optically thin.
b Emitting radius assuming N = 1018 cm−2 and Area = πR2 .
c Assuming distance given in Table 2• Trot=400-1000K• Spitzerデータより高く出る=>波長分解能をあげるとコンパ
クトな高温領域をトレースする

スペクトルを波長補正後concatして形状を評価

CO回転振動励起と比較• H2OはCOより線幅が狭い• COはbroad+narrow成分を持っており、disk+wind成分に対応している[Banzatti&Pontoppidan2015]• COのnarrow componentに近いプロファイ
ルを持つ天体があり、これらはwind起源だと思われる• もしnarrow componentが円盤とすると、

R>100auが必要となるが、IRS/SpitzerとPACS/HerschelのH2Oの結果は~a few auの円盤で再現されておりinconsistentFig. 7.— Comparison of composite TEXES emission line profiles and CO fundamental emission line profiles obtained with
(Banzatti & Pontoppidan 2015). ‘NC’ refers to the narrow component extracted from the CO profiles (see Banzatti & Pontopp

ケプラー回転円盤でフィット
L(R) ∝ R p (Rin < R < Rmid)∝ R q (Rmid < R < Rou t)• Single peak profile• Rのcutoffなし(Rmidなしで決まる)

Bestfit, min, maxdS• inclinationのせいではない• Double peak profile• Rmid=0.5-30au• Tex>3500Kなので、基本的にはsnowline
ではなく温度勾配を見ているのだろう• ただ、HLTauの例ではRmidはsnowline(13au)に対応しており、しH2O
アバンダンスやガス密度のtruncationがあれば見えるのかもしれない

S
d
d
d

• RWTau,DRTauでは時間変動• 2007~2011~2013• 円盤構造(tidal arm), dust settlingなどによる温度変化 or chemical changeSSpatial segregation of dust grains in transition disks. SPHERE observations of 2MASSJ16083070-3828268 and RXJ1852.3-3700
Villenave, M. et al.

• 遷移段階円盤2つの高分解能近赤外線観測 with SPHERE• ALMAデータを含めてモデル化• mmダストの方がコンパクトな分布 (radial, verticalどちらも)• 文献も含めて近赤外の穴の位置とミリ波ピーク位置を比較• 惑星で作られた構造かも• IRDIS-SPHERE/VLT, J- and H-bands, DPI• 二つの遷移段階円盤 (J1608, J1852)• ALMAアーカイブデータも使用• MCFOST[Pinte+2006,2009]によるRTC• PSFによるconvolution (≠obs. simulation)
A&A proofs: manuscript no. Transition_disks_J1608_J1852_acceptedA&A proofs: manuscript no. Transition_disks_J1608_J1852_accepted• 3つの円盤構造で再現• Tenuous inner disk-> silicate feature• Inner ring-> SEDのジャンプ, 内側の散乱光円盤• Outer ring-> ミリ波

he
15,
mto
illd
in
.

rien
al.
oar
lli
at
esill
nd
ht
al.

o94;
de-

HD142527

22天体で比較• NIRのcavityよりmm-ringの方が遠い場所にピーク

PDS70
J1852

J1608

[de Juan Ovelar+2013]
Fig. 10. Comparison of the cavity sizes as measured in the millimeter deand Juanin scattered
light for a sample of 22 transition disks.
Ovelar+2013のモデルと比較
The cyan points correspond to the two systems modeled in thispaper, while the yellow star symbols refer to HD 142527 that hasa stellar惑星質量を満たす天体は15個存在
companion in the cavity, and PDS 70 where a planet has
been detected. The upper limits, indicated with arrows, refer tosystems for which scattered light cavities could not be measured
down to the coronagraphic radius. Horizontal bars correspond to
one tenth of the millimeter beam, while vertical bars represent
the interval between the cavity radius and the peak in scattered
light (Table 3). The red region shows the ratio for which theplanet mass inferred with the prescription of de Juan Ovelar••

The nitrogen carrier in protoplanetary disks
Pontoppidan,K.M. et al.

ALMA High Angular Resolution Polarization Study: An Extremely Young Class 0 Source, OMC-3/
MMS 6
Takahashi, S. et al.

Polarization of stars with debris disks: comparing observations with models
Vandeportal, J. et al.

The survivability of planetary systems in young and dense star clusters
van Elteren, A. et al.

Ejection History of the IRAS 04166+2706 Molecular Jet
Wang, L.Y. et al.

Luminosity outburst chemistry in protoplanetary discs: going beyond standard tracers
Wiebe, D.S. et al.

External photoevaporation of protoplanetary discs in Cygnus OB2: linking discs to star formation
dynamical history
Winter, A.J. et al.