SFN #368 1-14
担当：土井 聖明 (総研大D2)
1. Spectral survey of a Hot core with an Eruptive Accretion in S255IR NIRS3 (SHEA): The discovery of

flclass I and class II millimeter methanol maser transitions
2. Isolating Dust and Free-Free Emission in ONC Proplyds with ALMA Band 3 Observa- tions
3. Tracing snowlines and C/O ratio in a planet-hosting disk: ALMA molecular line obser- vations towards
the HD169142 disk
4. Chemical evolution of some selected complex organic molecules in low-mass star-forming regions
5. The potential of VLTI observations for the study of circumstellar disk variability
6. Forming Gas Giants Around a Range of Protostellar M-dwarfs by Gas Disk Gravita- tional Instability
7. HH 80/81: Structure and Kinematics of the Fastest Protostellar Out ow A
8. Keplerian disk with a four-arm spiral birthing an episodically accreting high-mass protostar
9. The Orion-Taurus ridge: a synchrotron radio loop at the edge of the Orion-Eridanus superbubble
10. JWST reveals excess cool water near the snowline in compact disks, consistent with pebble drift
11. CoCCoA: Complex Chemistry in hot Cores with ALMA. Selected oxygen-bearing species
12. New radio lobes at parsec scale from the East-West protostellar jet RAFGL2591
13. A magnetically driven disc wind in the inner disc of PDS 70
14. MagAO-X and HST high-contrast imaging of the AS209 disk at Hα

8.

A Keplerian disk with a four-arm spiral birthing an episodically accreting high-mass
protostar

R. A. Burns, Y. Uno, N. Sakai, J. Blanchard, Z. Rosli, G. Orosz, Y. Yonekura, Y. Tanabe, K. Sugiyama, T.
Hirota, Kee-Tae Kim, A. Aberfelds, A. E. Volvach, A. Bartkiewicz, A. Caratti o Garatti, A. M. Sobolev, B.
Stecklum, C. Brogan, C. Phillips, D. A. Ladeyschikov, D. Johnstone, G. Surcis, G. C. MacLeod, H. Linz, J.
O. Chibueze, J. Brand, J. Eislöﬀel, L. Hyland, L. Uscanga, M. Olech, M. Durjasz, O. Bayandina, S. Breen,
S. P. Ellingsen, S. P. van den Heever, T. R. Hunter, X. Chen F High-mass protostars (M? > 8 M ) are thought
to gain the majority of their mass via short, intense bursts of growth. This episodic accretion is thought to be facilitatedby gravitationally unstable and subsequently inhomogeneous accretion disks. Limitations of observational capabilities, pairedwith a lack of observed accretion burst events has withheld aﬃrmative confirmation of the association between disk accretion,
instability and the accretion burst phenomenon in high-mass protostars. Following its 2019 accretion burst, a heat-wave driven
by a burst of radiation propagated outward from the high-mass protostar G358.93-0.03-MM1. Six VLBI (very long baseline
interferometry) observations of the raditively pumped 6.7 GHz methanol maser were conducted during this period, tracing
ever increasing disk radii as the heat-wave propagated outward. Concatenating the VLBI maps provided a sparsely sampled,
milliarcsecond view of the spatio-kinematics of the accretion disk covering a physical range of ⇠ 50 - 900 AU. We term thisobservational approach ‘heat-wave mapping’. We report the discovery of a Keplerian accretion disk with a spatially resolved
four-arm spiral pattern around G358.93-0.03-MM1. This result positively implicates disk accretion and spiral arm instabilities
into the episodic accretion high-mass star formation paradigm.

VLBI観測の複数epochでの観測から大質量星周りの円盤中に4本のスパイラルを発見した論文
The Orion-Taurus ridge: a synchrotron radio loop at the edge of the Orion-Eridanus
大質量星は、アウトバーストにより、大部分の質量を獲得すると考えられているsuperbubble

Andrea Bracco, Marco Padovani, Juan D. Soler F Large-scale synchrotron loops are recognized as the main source of
G358.93-003周りの円盤のメタノールメーザーを6エポックで観測した。
diﬀuse radio-continuum emission in the Galaxy at intermediate and high Galactic latitudes. Their origin, however, remains
rather unexplained. Using a combination of multi-frequency data in the radio band of total and polarized intensities, for the
メーザーの放射位置はアウトバーストの開始後に外側に移動
first time in this letter, we associate one arc – hereafter, the Orion-Taurus ridge – with the wall of the most prominent stellarfeedback blown shell in the Solar neighborhood, namely the Orion-Eridanus superbubble. We traced the Orion-Taurus ridge
それをつなげると4本のスパイラル状に見える
using 3D maps of interstellar dust extinction and column-density maps of molecular gas, NH2 . We found the Orion-Taurus ridge
212
重力不安定性が駆動するスパイラルと、それによるアウトバーストが起きていることを観測的に
at a distance of 400 pc, with a plane-of-the-sky extent of 180 pc. Its median NH2 value is (1.4+2.6
)
⇥
10
cm
. Thanks to the
0.6
broadband observations below 100 MHz of the Long Wavelength Array, we also computed the low-frequency spectral-index map
明らかにof synchrotron emissivity, , in the Orion-Taurus ridge. We found a flat distribution of with a median value of 2.24+0.03

イントロ

Articlehttps://doi.org/10.1038/s41550-023-01899-w
LSR velocity (km s–1)

LSR velocity (km s–1)

LSR velocity (km s–1)・大質量星の形成について
・大質量星は円盤からのアウトバースト的なaccretionにより多くの質量を得ると考えられている
・重力不安定がスパイラルやclumpを形成し、それが間欠的に中心星へと降着・少ない(=遠い)、円盤 が光学的に厚い ことにより、観測が難しい
・観測・対象天体：G358.93-0.03-MM1
・9-15 M̲sun、face-on disk (i=10-35 )・6.7 GHzメタノールメーザーにより2019年1月に発見（Hitachi 32m)・大質量星アウトバーストはメーザー放射を伴う傾向
・100-150 Kのダストによる20-30 um赤外線により励起される
・VLBIを用いた150日間での6エポック観測
–20

–18

–16

–20

–18

–16

Day: 19–29 51 45.55

–20

–18

–16

Day: 45

Day: 58

Declination (J2000)

45.60

45.65

45.70

45.75

45.80

1,000 AU

1,000 AU

1,000 AU45.85

17 43 10.110

10.10510.10010.09510.09017 43 10.110

Right ascension (J2000)

–20

–18

10.10510.10010.09517 43 10.110

10.105Right ascension (J2000)

–16

–20

–18

10.10010.09510.090

Right ascension (J2000)
–18

–20

–16

Day: 125–29 51 45.55

10.090–16

Day: 144

Day: 257

Declination (J2000)

45.60

45.65

45.70

45.75

45.80

1,000 AU45.85

17 43 10.110

10.10510.10010.0951,000 AU

10.09017 43 10.110

Right ascension (J2000)

10.10510.10010.095Right ascension (J2000)

Fig. 1 | Moment maps of the 6.7 GHz methanol masers in G358-MM1. First
moment (velocity) maps are shown in colour, where the source velocity with respect
to the Local Standard of Rest (LSR) is vLSR = −16.5 ± 0.3 km s−1 (ref. 27). Contours show
the zeroth moment (flux density) map for each epoch, produced for emission above

1,000 AU

10.09017 43 10.110

10.10510.10010.09510.090

Right ascension (J2000)

five times the noise root mean square (r.m.s.) listed in Table 1. Contours begin at
1 Jy beam−1 m s−1. Coordinates and colour scales for velocities are common to all
maps. The white cross indicates the position of the millimetre core27. The time of theobservation in days since the flare onset is shown in the top right of each panel.

Table 1 | Observation parameters
Facility
nameParticipating
stations

Observation date Observationcode

SpectralImage r.m.s.
resolution (kHz) (mJy beam–
1channel–1)

Beama (mas × mas;degrees)

Astrometric
uncertaintyb (mas)LBA

AT CD HH HO MP
WA

2 Feb 2019

VC026A

0.98

77.5

10.1 × 3.0/−51.43

1.30

LBA

AT CD HO MP PA
WA

28 Feb 2019

VC026C

0.98

231.7

8.6 × 3.6/−89.69

1.22

EVN

JB EF MC TR YS SR
HH WB

13 Mar 2019

RB005

1.95

284.7

37.4 × 11.6/−72.44

5.03

VLBA

BR FD HN KP LA MKNL OV PT

19 May 2019

BB414

3.91

40.4

17.2 × 2.6/−18.65

1.99

VLBA

BR FD HN KP LA MKNL OV PT

7 Jun 2019

BB412

3.91

88.7

17.5 × 8.4/3.89

2.60

LBA

AT CD HH HO KE
MP PA WA

28 Sep 2019

V581A

0.98

42.9

37.4 × 11.6/−72.44

1.55

Synthesized beam semimajor, (x) semiminor axes and (;) position angle in degrees bAstrometric uncertainties for each VLBI epoch were derived using the estimation method described inref. 74. Individual spot positional uncertainties were calculated by this number, and the two-dimensional Gaussian fitting error for each spot, and the reference quasar, added in quadrature.
ahttps://doi.org/10.1038/s41550-023-01899-w
LSR velocity (km s–1)
–20

–18

LSR velocity (km s–1)

–16

–20

–18

LSR velocity (km s–1)

–16

Day: 19–29 51 45.55

–20

–18

–16

Day: 45

Day: 58

45.60

Declination (J2000)

・メーザー放射の位置はだんだん外に・速度 >0.01c で広がる
ガスの運動やショックよりも早い
メーザーの励起条件(温度)の伝搬
・最も外で 917 auでメーザーが検出~ 940 au (ALMAで推定したディスクサイズ)

Article

45.65

45.70

45.75

45.80

1,000 AU

1,000 AU

1,000 AU45.85
17 43 10.110

10.10510.10010.09510.09017 43 10.110

Right ascension (J2000)
–20

–18

10.10510.10010.09510.09017 43 10.110

Right ascension (J2000)

–16

–20

–18

10.10510.10010.09510.090

Right ascension (J2000)
–20

–16

Day: 125–29 51 45.55

–18

–16

Day: 144

Day: 257

45.60

Declination (J2000)

結果

45.65

45.70

45.75

45.80

1,000 AU45.85
17 43 10.110

10.10510.10010.0951,000 AU
10.09017 43 10.110

Right ascension (J2000)

10.10510.10010.095Right ascension (J2000)

Fig. 1 | Moment maps of the 6.7 GHz methanol masers in G358-MM1. First
moment (velocity) maps are shown in colour, where the source velocity with respect
to the Local Standard of Rest (LSR) is vLSR = −16.5 ± 0.3 km s−1 (ref. 27). Contours show
the zeroth moment (flux density) map for each epoch, produced for emission above

1,000 AU
10.09017 43 10.110

10.10510.10010.09510.090

Right ascension (J2000)

five times the noise root mean square (r.m.s.) listed in Table 1. Contours begin at
1 Jy beam−1 m s−1. Coordinates and colour scales for velocities are common to all
maps. The white cross indicates the position of the millimetre core27. The time of theobservation in days since the flare onset is shown in the top right of each panel.

Table 1 | Observation parameters
Facility
nameParticipating
stations

Observation date Observationcode

SpectralImage r.m.s.
resolution (kHz) (mJy beam–
1–1

Beama (mas × mas;degrees)

Astrometric
uncertaintyb (mas)結果(続き)・全部重ねて書くと a のパネル
・点源の位置は、スパイラル状
・phi-ln(R)状でMCMCすると2本フィットできた・two-dimensional cross-correlation analysisでもう2本もスパイラルを検出(?)
ピッチアングルは 21.2 0.2
Articlehttps://doi.org/10.1038/s41550-023-01899-w
・速度構造はケプラー円盤b

LSR velocity (km s–1)
–20

–18

–16

–29 51 45.55

–20

800

–4

600

–3

400
200

45.65

–18

45.70
45.75
–16

45.80

–2
–18

–1
0
1
2

–16

3
4

1,000 AU45.85
17 43 10.115–20

LSR velocity (km s–1)

Declination (J2000)

Radius (AU)LSR velocity (km s–1)

45.60

c

Velocity offset (km s–1)a10.11010.10510.100–1,000

–500

0

500

1,000

Positional offset (AU)10.095 10.090

Right ascension (J2000)

Fig. 2 | Methanol maser spatio-kinematics in G358-MM1. a, Zeroth (contours)
and first (colours) moment maps of the 6.7 GHz methanol maser emission in
G358-MM1 created by combining all six VLBI maps shown in Fig. 1, in which zeroth
moments were summed and first moments were averaged. Contours begin at
1 Jy beam−1 m s−1 and increase in a geometric sequence (1, 2, 4, 8, 16, ...). The whitecross indicates the position of the G358-MM1 millimetre core27. b, Spotmap of

the combined six-epoch data sets centred on the G358-MM1 position. The blackline indicates the direction of largest velocity gradient to which the positionvelocity cut was taken. Spiral arms identified in this work (Methods) are plottedas thick grey lines. c, Position-velocity diagram of maser spots taken along the cut
indicated in the central panel. The Keplerian function for an 11.5 M⊙ enclosed mass
(Methods) is shown as a black line.

10.

JWST reveals excess cool water near the snowline in compact disks, consistent withpebble drift

Andrea Banzatti, Klaus M. Pontoppidan, John Carr, Evan Jellison, Ilaria Pascucci, Joan Najita, Carlos E.
Munoz-Romero, Karin I. Oberg, Anusha Kalyaan, Paola Pinilla, Sebastiaan Krijt, Feng Long, Michiel Lambrechts, Giovanni Rosotti, Gregory J. Herczeg, Colette Salyk, Ke Zhang, Edwin Bergin, Nick Ballering, Michael
R. Meyer, Simon Bruderer, the JDISCS collaboration F Previous analyses of mid-infrared water spectra from young
protoplanetary disks observed with the Spitzer-IRS found an anti-correlation between water luminosity and the millimeter dust
disk radius observed with ALMA. This trend was suggested to be evidence for a fundamental process of inner disk water enrichment, used to explain properties of the Solar System 40 years ago, in which icy pebbles drift inward from the outer disk andsublimate after crossing the snowline. Previous analyses of IRS water spectra, however, were uncertain due to the low spectral
4resolution that blended lines together. We present new JWST-MIRI
spectra of four disks, two compact and two large withmultiple radial gaps, selected to test the scenario that water vapor inside the snowline is regulated by pebble drift. The higher
spectral resolving power of MIRI-MRS now yields water spectra that separate individual lines, tracing upper level energies from900 K to 10,000 K. These spectra clearly reveal excess emission in the low-energy lines in compact disks, compared to the large
disks, demonstrating an enhanced cool component with T ⇡ 170-400 K and equivalent emitting radius Req ⇡ 1-10 au. Weinterpret the cool water emission as ice sublimation and vapor diﬀusion near the snowline, suggesting that there is indeed ahigher inwards mass flux of icy pebbles in compact disks. Observation of this process opens up multiple exciting prospects tostudy planet formation chemistry in inner disks with JWST.

JWSTによる円盤水輝線の観測

CoCCoA: Complex Chemistry in hot Cores with ALMA. Selected oxygen-bearing species

Y. Chen, M. L. van Gelder, P. Nazari, C. L. Brogan, E. F. van Dishoeck, H. Linnartz, J. K. Jørgensen, T. R.
JWSTのMIRIを用いて4つの円盤(ミリ波でのサイズが大と小)の水輝線の観測
Hunter, O. H. Wilkins, G. A. Blake, P. Caselli, K. -J. Chuang, C. Codella, I. Cooke, M. N. Drozdovskaya, R.
T. Garrod, S. Ioppolo, M. Jin, B. M. Kulterer, N. F. W. Ligterink, A. Lipnicky, R. Loomis, M. G. Rachid, S.
円盤の大きさと、低温の水輝線の強度に反相関がある
Spezzano, B. A. McGuire F Complex organic molecules (COMs) have been observed to be abundant in the gas phase toward
protostars. Deep line surveys have been carried out only for a limited number of well-known high-mass star forming regions using
大きい円盤では円盤外側のpebbleが堰き止められて、水の供給が少ない、というシナリオと整合的
the Atacama Large Millimeter/submillimeter Array (ALMA), which has unprecedented resolution and sensitivity. Statisticalstudies on oxygen-bearing COMs (O-COMs) in high-mass protostars using ALMA are still lacking. With the recent CoCCoA
survey, we are able to determine the column density ratios of six O-COMs with respect to methanol (CH3 OH) in a sample
of 14 high-mass protostellar sources to investigate their origin through ice and/or gas-phase chemistry. The selected species
are: acetaldehyde (CH3 CHO), ethanol (C2 H5 OH), dimethyl ether (DME, CH3 OCH3 ), methyl formate (MF, CH3 OCHO), glycolaldehyde (GA, CH2 OHCHO), and ethylene glycol (EG, (CH2 OH)2 ). DME and MF have the highest and most constantratios within one order of magnitude, while the other four species have lower ratios and exhibit larger scatter by 1-2 ordersof magnitude. We compare the O-COM ratios of high-mass CoCCoA sources with those of 5 low-mass protostars available
from the literature, along with the results from experiments and simulations. We find that the O-COM ratios with respect to–1.0–4
teraction-induced
warp
is
absentintheresidual
map. The spiral arm pattern
–3
Data
Model
・速度
>0.01cで広がる
ussedmap, indicating no obvious–4 in this work is superposed on the residual–1.5
Residualciation of ガスの運動やショックよりも早い
super- or sub-Keplerianmotions with the arms.

–2
–3
–4

–0.5
–1.0

Residual–1.5el) (km s–1)

–2
–0.5
–3

matic) (km s–1)

–1.5

)

議論

–2

Residual0matic) (km s–1)
model) (km s–1)

m s–1)–1systematic) (km s–1)

0 –4

ocity residuals upon subtracting the Keplerian disk model.
an interaction-induced warp is absent in the residual map. The spiral arm
astrometricdata.warpb, Expected
at themap.
locationsof detected
メーザーの励起条件(温度)の伝搬
raction-induced
is absentvelocities
in the residual
The spiralarm pattern discussed in this work is superposed on the residual map, indicating nosumingpurelyKeplerianrotation.
c, residual
Residualmap,
velocities
after no obvious association of super- or sub-Keplerian motions with the arms.
sed in thiswork
issuperposedontheindicating→ 元々、スパイラルが存在していたgthe velocities
ofsub-Keplerian
the model fromthe data.
The
ation
of super- or
motionswiththeexpected
arms. signature of・GIがスパイラルを作るとし、円盤質量を見積もる
29
3
HNCO emissionin G358-MM1 (ref. )=and
theぐらいdisk model of ref. ,m=4を作るのは、M̲d/M
0.25
−5
̇
stimate a円盤質量の見積りとして有効
steady-state disk accretion rate of Msteadydisk =2.56 × 10
29
−1
mplistic
considerationofaccretion
rates
shows
that
GI
is
a
and
HNCO
emissioninG358-MM1(ref.
) and the disk moder at a radius of ~1,000 AU. This radius represents a bottleneck
29
3
・GI由来のoutburstの重要性̇onsequenceofdisk
accretion.
Infallfromtheprotostellar
weestimateasteady-state
disk
accretion
rate
of
M
HNCO
emissioninG358-MM1
(ref.
)
and
the
disk
model
of
ref.
,
steadydisk =2
re spherical accretion transitions to disk accretion. Even when
−1
−5
̇
̇
towards
theparameters,
protostellar
disk,, occurs
onaccretion
timescalesM⊙ yr at a radius of ~1,000 AU. This radius represents a bo
Minfalltimatea steady-state
disk accretion
rate
of M
×of
10 remains=2.56rate
α円盤の定常降着を考えると、
steadydisk
pting
these
the
steady-statedisk−1−3 represents
−4
−1
at
a
radiusof~1,000AU.
This
radiusabottleneck
of
free
fall.
As
material
approaches
theprotostar,theconserwhere
spherical
accretiontransitions
todisk
accretion.
Evrder ofmagnitude below the 10 –10 M⊙ yr needed to avoid
エンベロープの降着は
eangularspherical
accretion transitions
disk accretion.
Eventowhenmomentumcounteractstocontraction,
leadinga adopting these parameters, the steady-state disk accretion rate
way fragmentation
by sufficiently processing envelope infall. Our−3−4−1
もし、M̲d/Mになると円盤が分裂して大質量星になれない
tingthese parameters,
the steady-state
disk accretion
remains an order of magnitude below the 10 –10 M yr needed
n to slower,
disk-mediatedaccretion wherematerialrate
accretes⊙clusionis that, to avoid disk fragmentation,−3−4−1the spiral density waves
̇derMofmagnitude–10 M
neededto avoid runaway fragmentation by sufficiently processing envelope in
GIにより、1桁程度、降着が促進されている
of. Infall ratesbelow
from the 10
envelope
onto
disk exceed⊙ yr thedisk
358-MM1
would
need
to
provideangularmomentumdissipationway
fragmentation
by sufficiently
processing
envelopean
infall.
Our conclusion is that, to avoid disk fragmentation, the spiral dens
y-stateaccretion
throughthedisk
byapproximately
order
GIが円盤質量をself-regulateしている
rate
of
an
order
of
magnitudelargerthan
thesteady-state
disk
̇
̇
usion
is
that,
to
avoid
disk
fragmentation,thespiraldensitywaves
tude, that is Minfall ≫ Mdisk , naturally leading to overdense in G358-MM1 would need to provide angular momentum dis
etion
rate.
This
is
consistentwithmodelsoftheaccretion
rates
in
58-MM1
would
need
to
provideangularmomentumdissipatione growing disk mass leads to higher disk-to-star-mass ratios, at a rate of an order of magnitude larger than the steady-s
58
58
-mass
protostellar
disksspiralpattern
instabilities. accretion rate. This is consistent with models of the accretio
ate
ofthe
an
order ofmagnitude
than
the steady-state
disk
hing
systemtowards
GIwith. larger

5
tion
rate.
This
is
consistentwithmodelsoftheaccretion
rates
inulations show that rapid angular momentum transport via high-mass protostellar disks with spiral pattern instabilities

イントロ
・円盤中でダストは成長し、内側にドリフトする・円盤の大きさは多様
・大きい円盤ではリング構造が多くみられ、そこではダストが堰き止められている可能性
・Spitzer IRSでは、低温の水輝線の強度と、ミリ波円盤サイズに反相関が見られる
JWST reveals excess cool water in compact disks→ 小さい円盤のみ低温の水は外から輸送(?)
・Spitzerではlineがブレンド(R~700)→密度に数桁の不定性
・JWST MIRIではラインを分解(R=1500-3500)
JWST-MIRI
Hotter layer

注：JWSTで見れるのは高温の水が中心で、多少は低温のも見れる(高温成分は表層で光学的に厚い)

Spitzer-IRS
Colder layer & Snowline

Herschel-PACS

3

T = 800 K, log N = 1e18 , Req = 0.5 au
T = 400 K, log N = 5e17 , Req = 1 au
T = 150 K, log N = 1e17 , Req = 5 au

Figure 1. The distribution of upper level energies Eu and Einstein-A coefficients (top plots, with color-coding reflecting Eu
values) across infrared wavelengths naturally traces radial temperature gradients in inner disks within and across the water
snowline (bottom plot, where the spectrum is scaled to a distance of 130 pc). Partly adapted from Figure 1 in Blevins et al(2016) and Figure 13 in Banzatti et al. (2023). The MIRI lines used in the analysis in Section 3 are marked with black circles.

Herschel showed that the region near the water snowline

an excess cool water reservoir near the snowline region

HCN
C2H2
CO2

H2O ro-vib.

H2O rotational

OH

観測
Figure 2. JWST MIRI-MRS spectra for the four disks. For clarity, the spectra are o↵set vertically by the following additive
・対象天体
shifts: 0.05 Jy in CI Tau, 0.17 Jy in GK Tau, 0.4 Jy in HP Tau. Illustrative models of molecular emission are shown for
guidance at the bottom. Prominent dust features are approximately identified and marked with shaded regions. The estimated
ミリ波でのサイズ以外似た4天体
continuum that is subtracted before analyzing the water spectra is shown in red on each spectrum. Two ALMA images areshown to the right for reference of disk sizes and structures (the whole sample is included in Appendix A).
小さい円盤には構造が見えない
Table 1. Sample properties.
・装置
Name
Dist
T
M
L
log L
log M
n
R
Incl
CO FW10%-50% R
10-50% R
JWST MIRI(pc)(K)(M ) (L )(L )(M /yr)(au)(deg)(km/s)
(au)
(au)
CITau
GKTau
HPTau
IQTau

160
129
177
131

e↵

?

?

4162.
4067.
4375.
3704.

0.65
0.58
0.84
0.42

1.65
1.48
1.89
0.86

acc

-0.7
-1.39
-1.09
-1.40

acc

-7.6
-8.67
-8.17
-8.54

13 26

disk

-0.51
-0.40
0.06
-0.74

190.5
12.9
22.1
109.6

50
39
18
62

JWST reveals excess cool water in compact disks

265–105
180–85
115–40
190–150CO

snow

0.02–0.12
0.03–0.11
0.02–0.18
0.03–0.05

2.7
0.9
1.7
0.9

13

Note— References – distances are from GAIA DR3 (Gaia Collaboration et al. 2016, 2022), stellar and accretion properties are from
Herczeg & Hillenbrand (2014); Donati et al. (2020); Manara et al. (2022); Gangi et al. (2022); Rdisk and disk inclinations are fromLong et al. (2019); n13 26 is measured from the MIRI spectra in this work; near-infrared CO line widths are measured at the 10%
and 50% of the line peak from the stacked profiles shown in Appendix A; RCO is the Keplerian radius of infrared CO emission fromthe half line width velocities at 10% and 50%. Rsnow is an expectation for the midplane snowline radius as set by accretion following
Equation 2 in Mulders et al. (2015) as previously adopted for a general comparison across disks in Banzatti et al. (2017).

We note that HP Tau may have a small inner dust
⇡ 1800 s in CI Tau and IQ Tau) and reduced as decavity, as suggested by the relatively high infrared index
scribed in Pontoppidan & al. (2023) (henceforth Paper
n13 26 measured in MIRI spectra instead of the SpitzerI from the JDISCS collaboration). Two standard calbased n13 30 index (see Appendix D in Banzatti et al.
ibrators (asteroids) from program GO-1549 were used2020). The ALMA image with 0”.12 resolution does not
to maximize the quality of fringe removal, the specresolve this putative cavity, even with super-resolution
tral response function, and flux calibration across thetechniques (Jennings et al. 2022b; Zhang et al. 2023),
four MIRI channels (Paper I). Target acquisition was
Figure 8. ALMA
imagesfor cavity,
the sample
orderedby diskradius,used
fromto Longal. (2019).
suggestingthat theif present,
is smallerthanensureetpointing
precision and match across dif-

解析・方針：円盤間で比較し、水輝線の強度に影響するファクターを切り分ける
・100本のブレンドしてない輝線を選び、高温(E̲u=900-3000 K)と低温(E̲u=6000-8000 K)に分ける
・高温成分は、降着量と強い相関
・低温成分はズレあり→ 他の要因が効いている
4Black:

compact disks

Grey:large-structure
disks

HCN
C2H2
CO2

H2O ro-vib.

H2O rotationalOH

Figure 2. JWST MIRI-MRS spectra for the four disks. For clarity, the spectra are o↵set vertically by the following additive
shifts: 0.05 Jy in CI Tau, 0.17 Jy in GK Tau, 0.4 Jy in HP Tau. Illustrative models of molecular emission are shown for
guidance at the bottom. Prominent dust features are approximately identified and marked with shaded regions. The estimatedcontinuum that is subtracted before analyzing the water spectra is shown in red on each spectrum. Two ALMA images areshown to the right for reference of disk sizes and structures (the whole sample is included in Appendix A).

JWST reveals excess cool water in compact disks

5

Table 1. Sample properties.
Name

Dist
(pc)

Te↵
(K)

M?
(M )

L?
(L )

log Lacc(L )log Macc(M /yr)

CITau
GKTau
HPTau
IQTau

160
129
177
131

4162.
4067.
4375.
3704.

0.65
0.58
0.84
0.42

1.65
1.48
1.89
0.86

-0.7
-1.39
-1.09
-1.40

-7.6
-8.67
-8.17
-8.54

n13

26

Rdisk
(au)

Incl
(deg)

CO FW10%-50%(km/s)

RCO 10-50%
(au)

Rsnow
(au)

-0.51
-0.40
0.06
-0.74

190.5
12.9
22.1
109.6

50
39
18
62

265–105
180–85
115–40
190–150

0.02–0.12
0.03–0.11
0.02–0.18
0.03–0.05

2.7
0.9
1.7
0.9

Note— References – distances are from GAIA DR3 (Gaia Collaboration et al. 2016, 2022), stellar and accretion properties are from
Herczeg & Hillenbrand (2014); Donati et al. (2020); Manara et al. (2022); Gangi et al. (2022); Rdisk and disk inclinations are fromLong et al. (2019); n13 26 is measured from the MIRI spectra in this work; near-infrared CO line widths are measured at the 10%
and 50% of the line peak from the stacked profiles shown in Appendix A; RCO is the Keplerian radius of infrared CO emission fromthe half line width velocities at 10% and 50%. Rsnow is an expectation for the midplane snowline radius as set by accretion following
Equation 2 in Mulders et al. (2015) as previously adopted for a general comparison across disks in Banzatti et al. (2017).

We note that HP Tau may have a small inner dust
⇡ 1800 s in CI Tau and IQ Tau) and reduced as deFigure 3. Correlations between water linecavity,
luminosities
andaccretion
luminosity.
Left:using blended water lines at 17.1–
as suggested by the relatively high infrared index
scribed in Pontoppidan & al. (2023) (henceforth Paper
17.4 µm from Spitzer-IRS (data and regression
adoptedfrom
etofal.
using
high-energyK)
n13 26
measured in
MIRI Banzatti
spectra insteadthe 2020).
Spitzer- Middle:
I from the
JDISCS
collaboration).(6000–8000
Two standard calAppendix
D in
Banzatti et al.(900–3000
ibrators K)(asteroids)
program
30 index
water lines from JWST-MIRI from this workbased
andn13Paper
I; (seeright:
using
low-energy
waterfromlines(seeGO-1549
Figurewere1). used

As the MIRI
(90 200 km s2020). The ALMA image with 0”.12 resolution does not
to maximize the quality of fringe removal, the specthis putative cavity, even with super-resolution
tral response function, and flux calibration across theresolving power of R =resolve
1500
3500
themselvesastemplatesfor comparison between small
techniques (Jennings et al. 2022b; Zhang et al. 2023),
four MIRI channels (Paper I). Target acquisition was
1suggestingthat the cavity, if present,
is smaller
thanas follows.
used to ensure pointing precision and match across dif) cannot resolve the gas
kinematics
vs large
disks,

解析・方針：円盤間で比較し、水輝線の強度に影響するファクターを切り分ける
・100本のブレンドしてない輝線を選び、高温(E̲u=900-3000 K)と低温(E̲u=6000-8000 K)に分ける
・高温成分は、降着量と強い相関
・低温成分はズレあり→ 他の要因が効いている
4Black:

compact disks

Grey:large-structure
disks

HCN
C2H2
CO2

H2O ro-vib.

・円盤間でのライン強度の比をとる
・低温成分ほど、小さい円盤で強度が大きい

H2O rotationalOH

Figure 2. JWST MIRI-MRS spectra for the four disks. For clarity, the spectra are o↵set vertically by the following additive
shifts: 0.05 Jy in CI Tau, 0.17 Jy in GK Tau, 0.4 Jy in HP Tau. Illustrative models of molecular emission are shown for
guidance at the bottom. Prominent dust features are approximately identified and marked with shaded regions. The estimatedcontinuum that is subtracted before analyzing the water spectra is shown in red on each spectrum. Two ALMA images are
JWST reveals
excesswater
compactshown
to cool
the right
for inreferenceof disks
disk sizes and structures (the 7whole sample is included in Appendix A).

8

Table 1. Sample properties.

・小さい円盤-大きい円盤の残差が低温の水の放射として、LTEモデルを作成
snowline前後の中心面付近の水をトレース

Name

Dist
(pc)

Te↵
(K)

M?
(M )

L?
(L )

log Lacc(L )log Macc(M /yr)

CITau
GKTau
HPTau
IQTau

160
129
177
131

4162.
4067.
4375.
3704.

0.65
0.58
0.84
0.42

1.65
1.48
1.89
0.86

-0.7
-1.39
-1.09
-1.40

-7.6
-8.67
-8.17
-8.54

n13

26

-0.51
-0.40
0.06
-0.74

TableIncl
2. LTEmodel fits toRrotational
Rdisk
CO FW10%-50%
Rsnowlines.
CO 10-50% water
(au)
(deg)
(km/s)(au)(au)
ObjectH2 O high energy

190.5
50
12.9
39 Req22.1
18 (au)109.6
CI Tau 62 0.65

265–105Tlog N
180–85(K) (cm 2 )115–40
190–150840
1.0e18

H2 O low-energy excess

0.02–0.12
ReqT
0.03–0.11(au) (K)
0.02–0.18
0.03–0.05
–
–

2.7
log N
0.9
(cm 2 )
1.7
0.9 –

0.38 stellar
850 and
1.1e18– are from–
Note— References – distances are from GAIA DR3 (Gaia Collaboration etIQal.Tau
2016, 2022),
accretion –properties
Herczeg & Hillenbrand (2014); Donati et al. (2020); Manara et al. (2022);HP
Gangi(2022);
Rdisk1.1e18
and disk 1.00
inclinations
from
Tau et al.0.46
820
510 are 1.1e17
Long et al. (2019); n13 26 is measured from the MIRI spectra in this work;
line widths
10%GKnear-infraredTau
0.45 CO830
7.1e17are measured
1.06 370at the4.8e17
and 50% of the line peak from the stacked profiles shown in Appendix A; RCO is the
KeplerianradiusofinfraredCOemissionfroma– radius –as set by
0.87
420 following
3.5e17the half line width velocities at 10% and 50%. Rsnow is an expectation forGK
the Tau
midplane –snowline
accretiona
GK Tau across– disks– in Banzatti–
8.6(2017).
170
3.1e16Equation 2 in Mulders et al. (2015) as previously adopted for a general comparison
et al.
Note—See Section 3 for details on the separation of components. For the high-energy component, we report fit results
to the 12–16 µm range from Appendix C. For the cool excess
We note that HP Tau may have a small inner dust
⇡ 1800s in CIweTau
andresults
IQ Tau)and reduced
component,
reportobtainedby using as
thedespectrum
of
CI
Tau
as
template
for
the
inner
hot
component
cavity, as suggested by the relatively high infrared index
scribed in Pontoppidan & al. (2023) (henceforth Paper(seeFigureWhile collaboration).
IQ Tau shows some
excess incomn13 26 measured in MIRI spectra instead of the SpitzerI fromthe 5).
JDISCS
Twocool
standard
calparison to CI Tau (Figure 6), it is too weak for the fit to
Figure 5. Overview of excess cool components in compact disks by using water spectra in large disks as reference templates
based
n
index
(see
AppendixD
in
Banzattietal.
ibrators(asteroids) from program GO-1549 were used
13
30
converge. a Results from the two-temperature fit to MIRI
for the hotter inner component, as explained in Section 3. The orange area in the top plots is the high-energy luminosity ratio2020).
The ALMA
imageThewith0”.12 resolution
does value
not of the to maximize
the qualityof infringeremoval,the specexpected from using the correlation with Lacc shownin Figure3 (3- region).
red-dashedline is the medianand IRS residuals
reported
AppendixB.
line luminosity ratio at Eu ⇠ 6000–9000 K. The
datapoint
gradientcavity,
reflects theEu withvalue (xaxis) of each water line. tral response function, and flux calibration across theresolvethiscolor
putativeeven
super-resolution
A single-temperature LTE fit to line fluxes measured in the excess cool component is shown in grey in the middle (line flux
techniques (Jennings et al. 2022b; Zhang et al. 2023),
four MIRI channels (Paper I). Target acquisition was
residuals) and bottom (population diagram) plots, with parameters shown in the box.

suggesting that the cavity, if present, is smaller thanused to ensure pointing precision and match across dif-

議論
・高温の水
・強度は、中心星への降着量が決めている・降着 → UV → 水の生成 & 励起・低温の水・小さい円盤の方が低温の水の強度が大きい
・外からのペブルドリフトにより、snowlineへの水の供給~170 K

Large + gaps&rings

Compactionsu

Vapor diﬀusion& heatingDiﬀ

Ice sublimation~800 K~1100 K(ro-vib.)

9~170 K~400 K~800 KJWST reveals excess cool water in compact disks~800 Ke-

ReducedDiﬀ
cooler waterIce sublimation~ 170 K
H2O

Higher H2O
abundanceEﬃcient pebble drift

Lower H2O
abundance

1 au

H2O

line
w
o
sn

Icy pebbles trapped in rings

Gap

Gap

Large disk with gaps & rings

Compact dust disk
0.1 auReduced drift

e

lin
w
o
n

s

ut

-o
eze

fre

Drift

~400 K

n

o
usi

Hot
layer

out

z
free

~400 K

10 au

100 au0.1 au

1 au

10 au

100 auFigure 7. Illustration of the interpretation of the results in the context of the long-established paradigm of inner water
enrichment by pebble drift (Cyr et al. 1998; Ciesla & Cuzzi 2006). The insets show the main processes of pebble drift, ice
sublimation, and vapor di↵usion as included in recent model explorations by Kalyaan et al. (2021, 2023) in the context of how
ice delivery and inner disk water enrichment may be regulated by dust gaps observed with ALMA.

area. We visualize the proposed approximate radial andtent with static chemical models, and does not neces-

MagAO-X and HST high-contrast imaging of the AS209 disk at H↵

10. Gabriele Cugno, Yifan Zhou, Thanawuth Thanathibodee, Per Calissendorﬀ, Michael R. Meyer, Suzan Edwards,

Jaehan Bae, Myriam Benisty, Edwin Bergin, Matthew De Furio, Stefano Facchini, Jared R. Males, Laird M.
Close, Richard D. Teague, Olivier Guyon, Sebastiaan Y. Haﬀert, Alexander D. Hedglen, Maggie Kautz, Andrés
Izquierdo, Joseph D. Long, Jennifer Lumbres, Avalon L. McLeod, Logan A. Pearce, Lauren Schatz, Kyle Van
Gorkom F The detection of emission lines associated with accretion processes is a direct method for studying how and wheregas giant planets form, how young planets interact with their natal protoplanetary disk and how volatile delivery to theiratmosphere takes place. H↵ ( = 0.656 µm) is expected to be the strongest accretion line observable from the ground withadaptive optics systems, and is therefore the target of specific high-contrast imaging campaigns. We present MagAO-X andHST data obtained to search for H↵ emission from the previously detected protoplanet candidate orbiting AS209, identified
through ALMA observations. No signal was detected at the location of the candidate, and we provide limits on its accretion.
Our data would have detected an H↵ emission with FH↵ > 2.5 ± 0.3 ⇥ 10 16 erg s 1 cm 2 , a factor 6.5 lower than the HST
flux measured for PDS70b (Zhou et al., 2021). The flux limit indicates that if the protoplanet is currently accreting it is likelythat local extinction from circumstellar and circumplanetary material strongly attenuates its emission at optical wavelengths.
In addition, the data reveal the first image of the jet north of the star as expected from previous detections of forbidden lines.
Finally, this work demonstrates that current ground-based observations with extreme adaptive optics systems can be moresensitive than space-based observations, paving the way to the hunt for small planets in reflected light with extremely large
telescopes.

MagAO-XとHSTによるAS→ cubes:Core
未検出
ALMA-IMF VII – First 209円盤中の惑星候補の観測
release of the full spectral line
kinematics traced
by DCN J=(3-2)

N. Cunningham, A. Ginsburg, R. Galván-Madrid, F. Motte, T. Csengeri, A. M. Stutz, M. Fernández-López, R.
H. Álvarez-Gutiérrez, M. Armante, T. Baug, M. Bonfand, S. Bontemps, J. Braine, N. Brouillet, G. Busquet,
D. J. Díaz-González, J. Di Francesco, A. Gusdorf, F. Herpin, H. Liu, A. López-Sepulcre, F. Louvet, X. Lu, L.
Maud, T. Nony, F. A. Olguin, Y. Pouteau, R. Rivera-Soto, N. A. Sandoval-Garrido, P. Sanhueza, K. Tatematsu,
A. P. M. Towner, M. Valeille-Manet F ALMA-IMF is an Atacama Large Millimeter/submillimeter Array (ALMA) Large
Program designed to measure the core mass function (CMF) of 15 protoclusters chosen to span their early evolutionary stages.
It further aims to understand their kinematics, chemistry, and the impact of gas inflow, accretion, and dynamics on the CMF.
We present here the first release of the ALMA-IMF line data cubes (DR1), produced from the combination of two ALMA
12m-array configurations. The data include 12 spectral windows, with eight at 1.3mm and four at 3mm. The broad spectral
coverage of ALMA-IMF ( 6.7 GHz bandwidth coverage per field) hosts a wealth of simple atomic, molecular, ionised, andイントロ
円盤中の惑星は、惑星の形成過程や降着過程を探る上で重要
これまで確認されたのは PDS 70 のみ
赤外連続波：熱放射
Hα：降着
ALMA：CPD

ff

The AstrophysicalJournal Letters, 934:L20 (16pp), 2022 August 1
対象天体：AS
209
13COでCPDが検出(?)→ Hαがあるか探す(赤外連続波では見つからず)

Ha ert et al. 2019
Bae et al.

The Astrophysical Journal Letters, 934:L20 (16pp), 2022 August 1

13

観測装置：HST/WFC3/UVISMagellan/Mag-AO-X
連続波とHαを撮って差分をとる

結果
惑星は検出されず
Jetは発見The Astronomical Journal, 166:162 (9pp), 2023 October

Cugno et al.

Figure 1. MagAO-X AS209 residuals in the Hα (left panel), in the continuum (middle panel), and in the continuum-subtracted Hα frames (right panel). North points
to the top and east to the left. The white star indicates the position of the central star. The position of the CPD candidate is marked with a white dashed circle. The jet
can be identiﬁed as the extended emission North of the star in both the left and the right panels. The rectangular mask applied for the jet brightness measurement isshown in the right panel.

The Astronomical Journal, 166:162 (9pp), 2023 October議論
惑星の質量は、赤外から0.5-4 M̲jとした
Hαが検出されないことから、降着量の上限がつく
2 Myr(円盤の年齢)までに、現在の降着量では成長できない→ 初期に大きな降着 or 周囲の物質による強い減光

The Astronomical Journal, 166:162 (9pp), 2023 October

AOを用いた地上観測は、HSTよりも感度がある

Figure 5. Mass accretion rate upper limit of the protoplanet candidate as afunction of the planet mass Mp under different scenarios. The orange dashedline represents the average mass accretion necessary to build a planet of a given
mass in 2 Myr. The blue and gray circles represent the mass accretion rateestimated using the shock-heated accretion models from Aoyama et al. (2021)
using the observed Hα luminosity (AHα = 0 and 2 mag, respectively). Blackand green diamonds indicate the mass accretion rate when applying theand 2 mag,respectively.
magnetospheric accretion model for AHα = 0 mag
Cugno
et al.

and 4 MJ (see Section 5.1) and radii were drawn uniformly
between 1 and 3 RJ.
In order to consider magnetospheric accretion, we use themodels from Thanathibodee et al. (2019) to generate a large
grid of scenarios producing Hα lines. For each calculation, we
systematically varied the planets’ and model’s parameters,
encompassing a wide range of values whose boundaries are
given either by the AS209 system’s possible properties or by
extreme scenarios. Using masses between 0.5 and 4 MJ, we
adopted evolutionary models from Mordasini et al. (2017) toestimate radii for each mass consistent with 1–2 Myr (Rp in the
1.9–3.1 RJ range). For a given set of mass and radius, we
calculate a grid of 4050 models varying the magnetosphericparameters. The mass accretion rate log (M acc MJ yr−1) was
taken between −9 (weak Hα produced) to −5 (typical stellar
accretion rate), the maximum ﬂow temperature from 7000 K to
19

perio
unde
lowe
plane
accre
Figur
Mp–M
diam
mode
Th
mass
to th
rµ
for ﬁ
Conv
of th
incre
Hα
comp
mode
than
accre
accre
Ho
stron
the p
light
small
Huan
detec
ties o
meas
sourc
locat
Fro
Hash
PDS7
AV ≈
consi
mate
candi