星形成ゼミ 2024/6/28 #375 68-81 ⾠⾺ (理研iTHEMS)
68. MINDS. The DR Tau disk I: combining JWST-MIRI data with high-resolution CO spectra to characterise the hot gas
69. The Epoch of Giant Planet Migration Planet Search Program. II. A Young Hot Jupiter Candidate around the AB Dor
Member HS Psc
70. Formation and Structure of Circumplanetary Disks and Envelopes during the Late Stages of Giant Planet Formation
71. Fragmentation of Dense Rotation-Dominated Structures Fed by Collapsing Gravomagneto-Sheetlets and Origin of
Misaligned 100 au-Scale Binaries and Multiple Systems
72. The SPHERE view of the Orion star-forming region
73. Polarization Holes as an Indicator of Magnetic Field-Angular Momentum Alignment I. Initial Tests
74. Disk Wind Feedback from High-mass Protostars. III. Synthetic CO Line Emission
75. Discovery of widespread non-metastable ammonia masers in the Milky Way
76. The First Spatially-resolved Detection of 13CN in a Protoplanetary Disk and Evidence for Complex Carbon Isotope
Fractionation
77. Relative velocities between 13CO structures within 12CO Molecular clouds
78. The environment around young eruptive stars. SPHERE/IRDIS polarimetric imaging of 7 protostars
79. Gas in ows from cloud to core scales in G332.83-0.55: Hierarchical hub- lament structures and tide-regulated
gravitational collapse
80. The Multilayer Nature of Molecular Gas toward the Cygnus Region
81. Surveys of clumps, cores, and condensations in Cygnus X: Temperature and nonthermal velocity dispersion
revealed by VLA NH3 observations
fi

fl

1

NIR bands are characterized by a cooler M-type spectrum exhibiting a forest of atomic and molecular features. All
together, the spectra demonstrate that WTP 10aaauow is an FU Ori type outburst. Ongoing systematic infrared
searches will continue to reveal the extent of this population in the Galactic disk.

MINDS. The DR Tau disk I: combining JWST-MIRI data with high-resolution CO
8. spectra to characterise the hot gas
MINDS collaboration - Milou Temmink et al. F The MRS mode of the JWST-MIRI instrument has been shown

to be a powerful tool to characterise the molecular gas emission of the inner region of planet-forming disks. Here,
we analyse the spectrum of the compact T-Tauri disk DR Tau, which is complemented by high spectral resolution(R 60000-90000) CO ro-vibrational observations. Various molecular species, including CO, CO2 , HCN, and C2 H2 aredetected in the JWST-MIRI spectrum, for which excitation temperatures of T 325-900 K are retrieved using LTE
slab models. The high-resolution CO observations allow for a full treatment of the line profiles, which show evidence
for two components of the main isotopologue, 12 CO: a broad component tracing the Keplerian disk and a narrowcomponent tracing a slow disk wind. Rotational diagrams yield excitation temperatures of T>725 K for CO, withconsistently lower temperatures found for the narrow components, suggesting that the disk wind is launched from alarger distance. The inferred excitation temperatures for all molecules suggest that CO originates from the highest
atmospheric layers close to the host star, followed by HCN and C2 H2 , which emit, together with 13 CO, from slightly
deeper layers, whereas the CO2 originates from even deeper inside or further out in the disk. Additional analysis of
the 12 CO line wings hint at a misalignment between the inner (i 20 degrees) and outer disk (i 5 degrees). Finally,
we emphasise the need for complementary high-resolution CO observations, as in combination with the JWST-MIRI
observations they can be used to characterise the CO kinematics and the physical and chemical conditions of the otherobserved molecules with respect to CO.

The Epoch of Giant Planet Migration Planet Search Program. II. A Young Hot Jupiter
9. Candidate around the AB Dor Member HS2 Psc

1Long et al.

MINDS. The DR Tau disk I: combining JWST-MIRI data with high-resolution CO spectra tocharacterise the hot gas (Temmink et al. 2024)• JWST-MIRIのMRSモード(R~1500–3500)を⽤いて、Tタウ
リ円盤DR Tauの内側領域からの分⼦ガス放射を調べた。

• Medium Resolution Spectroscopy• Mid-InfraRed Instrument• MIRI mid-INfrared Disk Survey

1.3 mm• DR Tau: 中⼼星質量0.93 Msun, 195 pc(Long et al. 2019)• 降着が活発 (2 x 10-7 Msun/yr)• ALMA観測によると、ダスト円盤は54 auと⼩さく、Fig. 1: The JWST-MIRI MRS spectrum of DR Tau over channels 1 through 3 (4.9-17.98 µm). The di↵erent wavelength ranges(subbands) of each MIRI channel are indicated in the top panel in blue (‘A’), green (‘B’), and orange (‘C’), respectively. The blackline displays the estimated continuum. The bottom panel shows the continuum subtracted JWST-MIRI spectrum and contains azoom-in on the CO transitions (4.9-5.3 µm). The red line in the bottom panel highlights the zero flux level.

substructureは検出されていない。

• visibilityなどは、22 auと42.5 auに2つのリングがあることを⽰唆している。

• 13COとC18Oの観測は、ガス円盤は246 auの⼤きさで、ダスト進化とradial driftを⽰唆している。

Fig. 2: The continuum-subtracted iSHELL spectrum of DR Tau. The wavelength gaps visible in the spectrum have either not been
observed, or were removed due to interference from telluric lines.

• 地上望遠鏡の⾼スペクトル分解能(R~60000–92000)のCO回転振動輝線観測(IRTF-iSHELLデータ)も⽤いた。
are not present in the extremely line-rich spectrum of DR Tau.
Instead we base our values for on the median continuum flux

3

Article number, page 4 of 26

level in each combination of channels and ranges, and divide
this by the highly idealised signal-to-noise ratio (S /N) acquiredlated by multiplying the column density with the emitting area:
N=N⇡R2em . The best fitting slab models are displayed in Figure
MINDS. The DR Tau disk I: combining JWST-MIRI data withhigh-resolution
to4, whereas
the 2 -maps are shown inCO
Figurespectra
C.1.

characterise the hot gas (Temmink et al. 2024)

Table 1: Parameters of the best-fitting slab models for the di↵erent molecules observed with JWST-MIRI.

• LTE slab model
log10 (N)T
Rem
N
• 3つのパラメータで tting: 柱密度N, ガス温度T, 放射領域πRem2
Molecule[cm 2 ]
[K]
[au]
13.6-16.3 µm ( =2.19-2.23 mJy)
• JWSTの結果
12
+50
+0.36
43
CO2
17.4+0.7325
0.53
4.96⇥10
0.2
100
0.06
+4.96
+50
42
HCN
14.7+2.1
900
4.83
8.22⇥10• CO, 12CO2, HCN, C2H2など多様な分⼦を検出した。
4.38
0.6
50
+5.6
+150
+8.56
42
Milou Temmink et al.: MINDS. The DRCTau
disk
I:
combining
JWST-MIRI
data
withhigh-resolutionCO
spectra
H
15.0
775
1.45
1.48⇥10
2 2
1.7
1.32
625
• H2Oは他の論⽂で議論。
• 13CO2は検出されなかった。
4.1.1. 12CO2• HCNは光学的に薄い。
The Q-branch of 12CO2 is well detected in DR Tau, whereas• C2H2は光学的に薄い/厚いの境界。
individual P- and R-branch, and the hot-bands are not strongly
HCN Q-branchdetected.
Our fit only extends over the Q-branch, which yields a
HCN
hot-band
17.4
2
12CO Q-branchcolumn density of N=10cm
, a gas temperature of T =325
2

K and an emitting radius of R=0.53 au. Compared to H2 O, our
12
CO2 Q-branch is significantly weaker. This is similar to Sz 98(Gasman et al. 2023) and EX Lup (Kóspál et al. 2023), but totally the opposite for GW Lup (Grant et al. 2023b) and PDS 70
C2H2 Q-branch(Perotti et al. 2023). The di↵erence with GW Lup is also visualised in Figure 5, which displays a zoom-in on the normalised
12Fig. 4: Best fitting slab models of 12CO2 , HCN,C2 H2 in the As
13.6-16.3µm wavelength
region.we
Thedo
topnotpanel
displaystheCOandopposedto GW Lup,
detectany
2 Q-branch.
continuum subtracted JWST spectrum in a specific region, while the full model13spectrum is shown in red. In addition, the horizontal
emissionfromCO2panel.
bars show for each molecule the spectral windows
usedsignaturein the 2 fits.
The bottom
shows the models for the individuallydetected molecules. The H2 O and OH slab models are shown for completeness. Their model properties will be presented in Temmink
et al. (in prep.)
Article number, page 6 of 26
fi

4

MINDS. The DR Tau disk I: combining JWST-MIRI data with high-resolution CO spectra to
A&A proofs: manu
characterise the hot gas (Temmink et al. 2024)• COについて
A&A proofs: manuscript no. aanda
Milou Temmink et al.: MINDS. The DR Tau disk I: combining JWST-MIRI data with high-resolution CO spectra• JWST-MIRIによる12CO: rotational diagramによる解析• 励起温度は3503 K, 柱密度は1.3 x 1017 cm-2, 放射領域半径は0.4 au• ただし光学的に厚い場合は、実際の温度はもっと低くなる。
• JWSTの分解能だと12COのnarrow成分(NC)とbroad成分(BC)をMilou Temmink

et al.: MINDS. The DR Tau disk I: combining JWST-MIRI data with high-resolution CO spectra} iSHELL
A&A proofs: manuscript no. aanda

区別できなかった。

• ⾼分解能のiSHELLは12COのNCとBCを区別できた。
←曲線: 光学的に厚いことが原因

Fig. 6: A rotational diagram of the 12CO v=1-0 transtions. As
JWST-MIRI is unable to distinguish between the narrow (NC)and broad (BC) components, their contributions have been added
together. The black squares indicate the fluxes inferred from theiSHELL observations, while the ones marked denote the transitions that are also observable with JWST-MIRI. Errorbars on theiSHELL observations are plotted, however, these are too small
with respect to the size of the squares. The circles in green are theintegrated fluxes inferred from the JWST-MIRI observations using a pseudo-Voigt profile. The red, dashed line is a fit to the redpoints, used to derive what excitation temperature JWST-MIRI
would probe as seen with the iSHELL observations (T =2992±40K). The green dashed line indicates the excitation temperature
derived from these observations, T =3503+318
269 K.

Fig. 7: The fitted iSHELL line profiles for the 12CO v=1-0, v=2-1, v=3-2, and the 13CO v=1-0 transitions. The median line profile isFig. 8: The rotational diagrams for 12CO v=1-0 (top left), v=2-1 (top right), v=3-2 (bottom left), and 13CO v=1-0 (bottom right).
12
shown in black, whereas the fitted linetransitions, we have indicated the narrow and broad
In each panel, the slab models are given by the solid line. For the 12CO transitions, the narrow and broad components (NC and BC,
12 profile is shown in green. For the CO1312
13
ted iSHELL
profiles forblue
the andCO
v=2-1,
v=3-2,
andthe inCOv=1-0transitions.
The
medianline(top
profileis v=2-1
componentsline
in, respectively,
red.v=1-0,
The faint,
grey 8:line
profilesvisiblethebackgroundcorrespondtotheindividual
linerespectively)
are
shown
separately.
The
integrated
fluxesforthenarrow
component
aregiven by(bottom
the dots, while
those for the broadFig.
The
rotational
diagrams
for
CO
v=1-0
left),(topright),
v=3-2(bottomleft),
andCO
v=1-0
right).
12k, whereas
theinfitted
linetheprofileis shown innormalised
green. For
CO transitions, we have indicated the narrow and broad
profiles usedcreating
weighted-averaged,
linetheprofile.
component are indicatedby the squares. The two lines in each model correspond the R- and P-branches.
12

In eachpanel,
slab
models correspondare given tobythethe
solid5line.
n, respectively, blue and red. The faint, grey line
profilesvisiblethein thebackgroundindividualline For the CO transitions, the narrow and broad components (NC and BC,
Table 2: Best fit parameters
acquiredthroughthe rotational
analysisfor the iSHELL
data.
respectively)
arediagram
shown
separately.
The
integrated fluxes for the narrow component are given by the dots, while those for the broadn creating the weighted-averaged,
normalised
line
profile.

v=1-0 (BC)
-1.2
33.5
6.3⇥1017 1725 0.38 >6.3⇥1044
Milou Temmink et al.:43MINDS. The DR Tau disk I: combini
17
v=2-1 (NC)
-4.1
12.5
7.9⇥101050 0.21 >2.3⇥10
MINDS. The DR Tau disk I: combining
JWST-MIRI
data
withhigh-resolutionCO
spectrato17
43
v=2-1 (BC)
-0.5
35.8
5.0⇥102175 0.22 >1.6⇥10
18
42
v=3-2
(NC)
-0.7
16.9
5.0⇥101800
0.05>8.8⇥10characterise the hot gas (Temmink et al. 2024)
v=3-2 (BC)
-1.0
36.6
1.6⇥1018 2025 0.13 >1.9⇥1043
13
17
43
12
CO
v=1-0
-3.2
16.5
1.6⇥10725
0.47>2.4⇥10• ⾼分解能観測iSHELLからは2つの CO成分の証拠を得た:
C 18O
v=1-0
-4.2
10.3
2.0⇥1016
975 0.23
7.4⇥1041• 熱い内側領域のケプラー円盤をトレースするbroad成分(BC)Notes. (↵): V is the o↵set of the line center with respect to the heliocentric velocity of DR Tau, ⇠27.6 km s .
( ): As both CO and CO are found to be optically thick (see Section 4.2.3), the values listed for the total number of molecules must be treated• ↑よりは冷たい遅い円盤⾵をトレースするnarrow成分(NC)as lower limits.
1

12

13

• rotational diagramから、12COと13COは光学的に厚いことがわかった。
Keplerian rotation:
averaged line profiles displayed in Figure 7, for simplicity we
18• iSHELLではC Oは検出されなかった(VLT-CRIRESでは検出)。
have taken the HWHM equal to half the FWHM listed in Ta!
12
13
2
The fitted iSHELL line profiles for the CO v=1-0,
v=2-1,
v=3-2, and the CO v=1-0 transitions. The medianble
line2.profileissin(i)
Assuming
the inclination of the inner disk of DR Tau to12n•black,
whereas the fitted line profileis shown
in green.
and broad
R = GM, For the CO transitions, we have indicated the(2) narrow
COの放射半径は、で求めた結果(i=5.4°)とrotational
diagramの結果で異なる。
⇤
be equal to the inclination of the outer disk, we use i=5.4 (Longv
ents in, respectively, blue and red. The faint, grey line profiles visible in the background correspond to the individual lineFig. 10: The left panel shows the acquired line Gaussian line profile fo
etis al. 2019). theFurthermore,as thisThemethodonly
appliesto thelines temusedFig.
in•theweighted-averaged,
normalised
line
profile.
7:creating
The
fittediSHELLline
profilesfortheCO
v=1-0,
v=2-1,
v=3-2,
and
the
CO
v=1-0
transitions.
The
medianline
profilerotational
diagram.
rotational
diagramyieldsanexcitation
原因:
inner
diskとouterdiskの(companionsによる？)misalignment
where
the inclinationv is the line
width,
often
takenandto broadbroadened by the Keplerian rotation, we calculate the (inner)
shown in black, whereas the fitted line
profileiisisshownin green. For theand
CO transitions,
we haveindicated
the narrow
12

13

12

components in, respectively, blue and
The faint,
greyhalfline width
profiles visible
the background(HWHM).
correspond toThethe individual
line
bered.
equal
to throughtheat halfin
maximum
inneremitting radius only for the broad components of the di↵erent
Table
2:
Best
fit
parameters
acquiredtherotational
diagramanalysisforthe
iSHELL
data.
Table 3: The derived
profiles used in creating the weighted-averaged, normalised line profile.
12
13 (inner) emitting radii for the ro-vibrational

emitting radius can, subsequently, also be estimated by taking v)
equal acquired
to thehalf FWHM
width
at 10%
etdata.
al.( 2022).
Table 2: Bestfit parameters
the rotational
diagramanalysis
theiSHELL
Molecule
Vibr.
Trans.
V (↵)throughN(HW10%;
T forBanzatti
RemN
1
Both theandderivedfromthe[kmHWHMs (↵)] [kms 1the] HW10%[cm 2 ] have[K] been
[au]
( )
12

CO

Molecule

Vibr. Trans.

v=1-0 (NC)
12 v=1-0 (BC)CO
v=1-0 (NC)v=2-1v=1-0(NC)(BC)
v=2-1v=2-1(BC)(NC)
v=3-2v=2-1(NC)(BC)
v=3-2 (NC)v=3-2v=3-2(BC)(BC)13
CO 13CO v=1-0
v=1-0
18
18
C
O v=1-0
v=1-0
C O

V

FWHM

-4.2
11.6
[km s 1 ] [km
s 1]
-1.2
33.5
-4.2
11.6
-1.2
33.5
-4.1
12.5
-4.1
12.5
-0.5
35.8
-0.5
35.8
-0.7
16.9
-0.7
16.9
-1.0
36.6
-1.0
36.6
-3.2
16.5
-3.2
16.5
-4.2
10.3
-4.2
10.3

N

T

R

em
17
3.2⇥101000[cm 2 ]
[K]
[au]
17
17
6.3⇥103.2⇥1010001725
0.46
17 17
6.3⇥1017251050
0.38
7.9⇥1017 17
7.9⇥10105021750.21
5.0⇥105.0⇥1017 182175 0.22
5.0⇥101800
18
5.0⇥101800 0.05
18
18
1.6⇥101.6⇥1020252025
0.13
17 17
1.6⇥101.6⇥10725 7250.47
16 16
2.0⇥10975 9750.23
2.0⇥10CO line profiles
andCO13CO
v=1-0
profile. The
calcu12transitionsof theCO andusingline
an inclinationof i=5.4.
lated values are listed in Table 3.

N

0.46 >4.6⇥1043
44
43
0.38
>4.6⇥10>6.3⇥10
43
44>6.3⇥10>2.3⇥10
0.21
43
43
>2.3⇥10>1.6⇥10
0.22>1.6⇥1043
420.05 >8.8⇥10>8.8⇥1042
43
43
0.13
>1.9⇥10>1.9⇥1043
43
0.47>2.4⇥10>2.4⇥10
7.4⇥10417.4⇥1041
0.23

Notes. (↵): V is the o↵set of the line center with respect to the heliocentric velocity of DR Tau, ⇠27.6 km s 1 .
1
1213 line center with respect to the heliocentric velocity of DR Tau, ⇠27.6 km s .
↵): (V):isAsthe
o↵set
of
the
both 13CO and CO are found to be optically thick (see Section 4.2.3), the values listed for the total number of molecules must be treated12
oth as CO
lowerandlimits.CO are found to be optically thick (see Section 4.2.3), the values listed for the total number of molecules must be treatedlimits.

6

Molecule
12

CO

13

CO
Molecule
12

CO

13

CO

Vibr. Trans.

HWHM
RCO
[km s 1 ][au]number, 0.03
page 9 of 26
v=1-0 Article16.8
v=2-1
17.9
0.02
v=3-2
18.3
0.02
v=1-0
8.3
0.11
Vibr. Trans. HW10% RCO,in[km s 1 ]
[au]
v=1-0
29.5
0.01
v=2-1
32.0
0.01
v=3-2
32.7
0.01
v=1-0
14.4
0.04

nee
reso
mo
fit p
see
tran
LTE
ere
LTE

Bas
(T
Kf
are
et a
to t
hig
the

MINDS. The DR Tau disk I: combining JWST-MIRI data with high-resolution CO spectra tocharacterise the hot gas (Temmink et al. 2024)• COの放射領域• 12COのbroad成分(BC)はダスト昇華半径(1500 K)よりも内側。
• もしくは、円盤上層。
Milou Temmink et al.: MINDS. The DR Tau disk I: combining JWST-MIRI data with high-resolution CO spectra• 13COは12COよりも光学的厚さが⼩さく、励起温度も低いため、より円盤の深いところ。
• CO以外の分⼦の放射領域
T = 1000 K• 励起温度によると、HCN, C2H2, CO2の順で深くなる。
T = 900 K

T = 1725 K

T = 775 K
T = 325 K
0.5

5.0

Fig. 12: Cartoon visualising the expected emission regions, based on the slab models and interpreting the emitting radius as the disk
radius, for our investigated molecules (CO, CO2 , HCN, and C2 H2 ).

7been funded by Spanish MCIN/AEI/10.13039/501100011033
grants PID2019-

Christiaens, V., Gonzalez, C., Farkas, R., et al. 2023, The Journal of Open Sourceoccurs and, if so, the masses and orbital parameters of the stellar companions formed.

. The SPHERE view of the Orion star-forming region

P. -G. Valegard, C. Ginski, A. Derkink, A. Garufi, C. Dominik, A. Ribas, J. P. Williams, M. Benisty, T.
Birnstiel, S. Facchini, G. Columba, M. Hogerheijde, R. G. Van Holstein, J. Huang, M. Kenworthy, C. F.
Manara, P. Pinilla, Ch. Rab, R. Sulaiman, A. Zurlo F We present SPHERE/IRDIS H-band data for a sample of

23 stars in the Orion Star forming region observed within the DESTINYS (Disk Evolution Study Through Imaging
of Nearby Young Stars) program. We use polarization diﬀerential imaging in order to detect scattered light fromcircumstellar dust. From the scattered light observations we characterize the disk orientation, radius and contrast.
We analyse the disks in context of the stellar parameters and the environment of the Orion star-forming region. We
use ancillary X-shooter spectroscopic observations to characterize the central stars in the systems. We furthermore
use a combination of new and archival ALMA mm-continuum observations to characterize the dust masses present
in the circumstellar disks. Within our sample we detect extended circumstellar disks in 10 of 23 systems. Of these,
three are exceptionally extended (V351 Ori, V599 Ori and V1012 Ori) and show scattered light asymmetries which
may indicate perturbations by embedded planets or (in the case of V599 Ori) by an outer stellar companion. Ourhigh resolution imaging observations are also sensitive to close (sub)stellar companions and we detect 9 such objects
in our sample of which 5 were previously unknown. We find in particular a possible sub-stellar companion (either
a very low mass star or a high mass brown dwarf) 137 au from the star RY Ori. We find a strong anti-correlation
between disk detection and multiplicity, with only 2 of our 10 disk detections located in stellar multiple systems. We
also find a correlation between scattered light contrast and the millimetre flux suggesting that disks that have a highdust content are typically bright in near-infrared scattered light. Conversely we do not find significant correlations
between scattered light contrast of the disks and the stellar mass or age.
25
8
Polarization Holes as an Indicator of Magnetic
Field-Angular Momentum Alignment I.

Disk Evolution Study Through Imaging of Nearby Young Stars (DESTINYS):The SPHERE view of the Orion star-forming region (Valegård et al. 2024)• ⼤質量星形成領域の環境が円盤進化に与える影響を調べるため、オリオン星形成領域の近⾚外散乱光観測を⾏った。
• 強い紫外線の輻射場があると、externalな光蒸発が円盤進化に影響を与える。
• 伴星があると、円盤が断ち切られ、スパイラル/warp/misalignmentなどの原因となる。
• 伴星や褐⾊矮星は検出されやすいが、substellarなものはほとんど検出されない。
Name
d [pc]SpTTL
M
t [Myr]
これまでに確認された円盤に埋もれた原始惑星:•
Kiso A-0904 06 A
339.78
K6
4205
0.45
0.82
6.66
Valegård, P.-G., et al.: A&A, 685, A54 (2024)

Table 2. Stellar properties of the sample.

e↵

(1)

PDS 70, HD169142, AB Aur• DESTINYSプログラム(6つの星形成領域の85個のターゲット)のうち、オリオンの23個のSPHERE/IRDIS Hバンド(1.625 µm)でのコロナグラフを⽤いた観測を解析した。

• polarization di erential imagingを⽤いて、円盤の向き、半径、
明るさを調べた。

• 中⼼星の性質はVLTのX-shooter分光観測を⽤いて調べた。
• 星周円盤のダスト質量はALMA mm波連続光(Band 6, 1.24 mm)を⽤いて調べた。
ff

9(1)

Kiso A-0904 06 B(1)Brun 216(2)Brun 252(3)Haro 5-38
HD 294260
HD 294268
PDS 110
PDS 113(4)RV OriRY Ori
TX Ori
V351 Ori
V499 Ori
V543 Ori(1)V578 Ori
V599 Ori(2)V606 Ori
V1012 Ori(2)V1044 Ori
V1650 Ori(3)V1787 Ori
V1788 Ori
V2149 Ori A(3)V2149 Ori B(3)

+1.74
1.84
+1.74
339.78 1.84
383.52+3.36
2.52
+6.66
383.64 6.43
400.35+2.92
2.58
+3.03
387.44 2.42
361.98+1.98
1.48
+2.82
343.66 2.75
352.25+2.33
2.27
+2.44
397.54 2.41
346.82+2.29
2.44+37.91415.53 33.04
323.82+3.14
3.09
+1.59
331.61 1.48
338.39+1.84
2.09
+2.02
375.21 1.97
401.07+4.06
3.27
+3.66
400.14 2.86
376.23+6.60
5.79
+2.70
384.31 2.77
342.41+5.63
5.46
+2.86
393.08 2.73
347.65+4.98
5.95
+5
388 5
388+55
(2)

K6
F8
G1
K7
G1
G0
F6
F3+F4
K5
F5
K4
A9
K6
K4
K7
A5
K5
A3
G6
F8
A5
A0
F8
F8

+235
105
+235
4205 105
6170+80160+1205890 120
4050+250
60+505880 110
5970+8040+210
6340 60
6750+7080+150
4450 150
6510+160
160+210
4620 220
7440+150220+2404200 100
4590+240
150+250
4050 60
8000+250
250+150
4450 150
8500+250250+705590 40
6160+100100+1858150 160
9700+1000
400+1106180 110
6180+110
110

+0.08
0.02
+0.08
0.45 0.02
9.55+2.20
1.04
+2.51
7.16 0.38
1.19+0.01
0.06
+0.40
5.59 0.37
5.67+1.29
0.27
+0.87
6.70 0.18
3.75+0.82
0.38
+0.03
0.57 0.11
7.17+0.61
0.82
+0.02
3.57 0.45
25.49+1.50
1.54
+0.06
0.36 0.05
0.36+0.36
0.14
+0.32
1.08 0.08
27.54+1.15
1.15
+0.03
0.67 0.13
5.89+0.72
0.64
+0.23
4.64 0.09
9.53+0.25
0.78
14.13+4.07
2.64
+9.19
19.06 2.89
17.9+2.80
0.45
+2.80
17.9 0.45
(3)

+0.18
0.13
+0.18
0.82 0.13
1.80+0.25
0.09
+0.25
1.68 0.09
0.58+0.31
0.05
+0.13
1.53 0.03
1.49+0.15
0.02
+0.10
1.46 0.04
1.32+0.05
0.06
+0.06
0.95 0.04
1.45+0.11
0.03
+0.35
1.30 0.36
2.08+0.05
0.02
+0.19
0.81 0.11
0.82+0.23
0.10
+0.31
0.59 0.07
2.03+0.10
0.10
+0.06
1.03 0.13
1.30+0.07
0.07
+0.06
1.64 0.02
1.71+0.05
0.07
+0.09
1.66 0.08
2.20+0.08
0.20
+0.16
2.1 0.07
2.1+0.16
0.07

+5.55
3.14
+5.55
6.66 3.14
4.46+0.25
1.47
+1.24
6.30 2.18
1.01+0.91
0.11
+0.80
7.93 1.70
8.84+0.51
2.21
+0.73
9.82 1.47
16.67+0.54
1.41
+8.40
8.29 2.82
10.12+0.90
1.65
+1.06
0.98 0.40
4.20+0.49
0.25
+3.90
9.84 4.65
22.90+22.18
16.38
+1.11
1.16 0.43
4.29+0.42
0.54
+6.98
6.47 2.33
8.47+1.06
0.89
+0.36
6.00 0.59
6.20+0.96
0.41
+0.59
7.43 1.05
5.08+3.17
0.11
+0.14
3.57 0.99
3.57+0.14
0.99(4

Disk Evolution Study Through Imaging of Nearby Young Stars (DESTINYS):
Valegård, P.-G., et al.: A&A, 685, A54 (2024)
The SPHERE view of the Orion star-forming region (Valegård
et al. 2024)• 9つの系に(sub)stellar companionsを検出した。
sample.•
Theそのうち6つの系は初検出。
figure shows a stellar map with the location of the sources in this paper. The thumbnails show disk detections
anions (orange), and non-disk detections (yellow.) The extent of the coronagraph is displayed as a gray circle in each thumbnail
r map was generated with Stellarium (open source software https://stellarium.org/) and the IR extinction map (darkted from•
Megeathet al. (2012)
basedV2149
on GutermuthOri,
et al. (2011).
V1788
Ori,
Kiso A-090460は既知。

the photometric and astrometric extraction together with the estimated spectral class and mass of companions.

companionsの性質

ObjectKiso A-0904 60
Brun 252
RY Ori
TX Ori
V 599 Ori
V 1650 Ori
V 1787 Ori
V 1788 Ori (b)V 1788 Ori (c)V 2149 Ori

Derived SpC

Mass M

K6
M0

0.8
0.6
0.076
0.2
0.1
0.8
0.2
0.9
0.7
2.1

M5
M6
K7
M3
K6
K7
F8

Sep (arcsec)
±0.01

1.96
0.22
0.39
0.11
2.05
0.32
0.22
0.43
0.56
0.37

PA ( )±0.48

128.9582.42
45.57
248.8440.40
144.09189.931.65
0.49
288.34

mag
0.75
2.69
6.26
2.14
5.59
2.83
5.22
2.47
2.84
0.58

RY Oriのcompanion: stellar-substellarの境界

d deviation of these nine backgroundm these measurements, the contrast between
companion was calculated.

f the systems

ctral classes of the stellar companions wereSiess et al. (2000) pre-main-sequence stels, assuming that the age and distance of theame as the age and distance of the primary.
H-band magnitudes (Cutri et al. 2003) for
nent and our measured H-band contrast to

calculate the absolute magnitude in the H band for the companions via the distance modulus. Since the 2MASS H-bandmeasurement is a combination of the components in the system,
we adopted the magnitude adjustment ofFig.
the1.primarydescribed
Imagery of
the sample. The figure shows a stellar map with the location of the sources in this paper. The thumbnails show disk detections
detected companions
in Bohn et al. (2020) to account for this. (blue),
The H-band
reddening (orange), and non-disk detections (yellow.) The extent of the coronagraph is displayed as a gray circle in each thumbnail
used. The stellar map was generated with Stellarium (open source software https://stellarium.org/) and the IR extinction map (darkwas obtained by converting the AV into Awhen
H using the conversion
adapted from Megeath et al. (2012) based on Gutermuth et al. (2011).
described by Cardelli et al. (1989). Here,grayweclouds)
brieflywas
discussthe⻘: 円盤検出individual cases.
Table 3. Values from the photometric and astrometric extraction together with the estimated spectral class and mass of companions.
Kiso A-090460. The wide binary companion at PA =128.95 has a separation of 1.9600 , which agrees with previous Object
10 Themeasurements for the separation (Tokovinin et al. 2020).

橙: companions検出

Derived SpC

Mass M

⻩: 円盤未検出
Sep (arcsec)
PA ( )
mag
±0.01
±0.48

Valegård, P.-G., et al.: A&A, 685, A54 (2024)

Disk Evolution Study Through Imaging of Nearby Young Stars (DESTINYS):
ObjectPA ( )r (mas)2024)
r (au)
OffsetOffset angle ( )The SPHERE view of the Orion star-forming
regioni ( )(Valegård
et al.
RA/Dec (mas)Table 4. Results of geometric fit to detected scattered light disks.

Valegård, P.-G., et al.: A&A, 685, A54 (2024)

Table 4. Results of geometric fit to detected scattered light disks.

• 23個のうち10個に広がった星周円盤を検出した。
• δpol: polarized-to-stellar light contrast• δpol ≤ 3: faint, δpol > 3: bright• そのうち3つ(V351 Ori, V599 Ori, V1012 Ori)は明るく

HD 294260
HD 294268
PDS 110
PDS 113
RV Ori
V 351 Ori(1)V 599 Ori
V 606 Ori(2)V 1012 Ori
V 1650 Ori

⾮常に広がっており、散乱光の⾮対称性を⽰した。

21.68 ± 3.09
Object
35.93± 8.0221.36 ± 3.31
60.31
7.31
HD±294260
56.08HD± 294268
10.29
PDS
63.2110
PDS 11356.86
4.02
RV±Ori25± 5Ori(1)
V 351
70.05
± 5.55
V 599
Ori
V 606
Ori(2)
30.47± 8.03
V 1012 Ori
V 1650 Ori

118.64 ± 11.22
389.01 ± 5.01
151 ± 2–13.94/18.23
i ( )± 18.87 174.23
PA ( ) ± 14.12 r (mas)(au)
Offset204.2263 ± 5 r–8.64/
25.23
203.50 ± 13.09
187.91 ± 2.63
65 ± 1 –13.75/RA/Dec
2.47 (mas)214.60± 9.60118.64
252.39± 18.37
21.68 ± 3.09
± 11.22389.01 ± 89
5.01± 6 151–38.21/24.44±2–13.94/18.23
35.93 ± ±8.02
± 18.87
174.23 ± 73
14.12
± 5 –8.64/ 25.23
244.2327.28204.22
183.84± 29.35± 12 63–3.32/-19.26
21.36± 3.31 203.50 ± 13.09± 2.63320.161120 ± 187.91
60 361± 20 65 ± 1 ––13.75/ 2.47
60.31 ± 7.31
214.60 ± 9.60 252.39 ± 18.37
89 ± 6 –38.21/24.44
137.10±4.29
551.16
±
21.07
221
±
9
56.08 ± 10.29 244.23 ± 27.28 183.84 ± 29.35
73 ±–53.67/85.18
12–3.32/-19.26
240
±
10
380
±
20
152
±
8
–
63.2
320.161120 ± 60 361 ± 20–
204.61± 4.31 137.10
473.63± 37.71± 15 221 63.24/44.63
56.86 ± 4.02
± 4.29551.16 ±17821.07
±9–53.67/85.18
25 ± ±
5 27.73 240± 10 ± 11.66 380 ±±8–
224.75161.815520± 4 152–16.03/
27.30
70.05 ± 5.55
30.47 ± 8.03

204.61 ± 4.31
224.75 ± 27.73

178 ± 1555 ± 463.24/44.63–16.03/ 27.30

305.21149.593.92 ± 0.82
0.1 ± 0.1

Notes.
For V351 Ori we report the inclination and PA retrieved from the ALMA millimeter observations. Radius is estimated from the Q(2)image. We note that for the weak disk V606 Ori the radius and PA were estimated by eye (see Sect. 4).

V351 Oria

明るいringb

V1012 Ori edge-on

V599 Ori
e
f

star

h
d

前⽅散乱

c

arc-like

0.5”

0.5”

⽰唆しているかもしれない。

I• 暗い円盤は⼩さく、substructureがない。
• ⾮検出のものはコロナグラフの⼤きさ(30–37 au)が• 10個のうち2つの円盤のみcompanionsがあった。

473.63 ± 37.71
161.81 ± 11.66

37.41
0.86 ± 0.13
Offset161.09angle ( ) 0.19 ±pol0.09
100.210.26 ± 0.09
57.40
0.64
37.41
0.86±± 0.14
0.13
161.090.19±± 0.87
0.09
170.231.97
0.26±± 0.80
0.09–100.215.65
57.40
0.64 ± 0.14
32.22
3.51
170.231.97±± 0.53
0.87
– –
1.03
±
1.00
5.65 ± 0.80
305.21
3.92
32.22
3.51±± 0.82
0.53
1.03±± 0.1
1.00
149.59–0.1

Notes. (1) For V351 Ori we report the inclination and PA retrieved from the ALMA millimeter observations. Radius is estimated from the Q
image. (2) We note that for the(1)weak disk V606 Ori the radius and PA were estimated by eye (see Sect. 4).

• V351 Ori: スパイラルかwarp?
• V599 Ori: スパイラル? 800 auに伴星?
• V1012 Ori: inner diskのmisalignmentかwarp?
• 埋もれた惑星か、(V599 Oriの場合は)外側の伴星を円盤サイズの上限。

pol

0.5”

II

h

I, IIで明るい⽅向が違う

lower 散乱⾯
0.5”
g

0.5”

0.5”

Fig. 3. Images showing the asymmetry of the three bright ( pol > 3) large disks in the sample. Top row: from left to right, the H-band observationsof V351 Ori, V599 Ori, and V1012 Ori. Bottom row: images showing the asymmetry in the disk. These were created by dividing the original frame
by a frame with the inverted disk along its minor axis. From left to right, V351 Ori, V599 Ori, and V1012 Ori.

Fig. 3. Images showing
the asymmetryof the inthreebright A.
( pol3) large
disksdisk
in theflippedsample.
Top row:
fromright, theobservations
emission
as is describedAppendix
All>themeasuredframe.
In thiswayleft
we tohighlight
the H-band
relative intensities
inof V351 Ori, V599 Ori,
and
V1012
Ori.
Bottomrow:
imagesshowingtheasymmetry
in
the
disk.
These
were
createdby
dividing
theoriginal
frame
parameters are listed in Table 4.
the asymmetries.
by a frame with the inverted
alongtheits minor
left to right,
V351 theOri, V599 Ori, and V1012 Ori.
To disk
evaluate
actual axis.
diskFrom
brightness,
we usedpolarized-to-stellar light contrast, pol (Garufi et al. 2017; 4.2.1. Bright disk of V351 Ori
11BenistyinetAppendix
al. 2023). Thisa measurement
frac- frame. In this way we highlight the relative intensities inemission as is described
A. contrast
All theismeasured
disk of the
flippedThe disk surrounding V 351 Ori is the most extended disk in ourDisk Evolution Study Through Imaging of Nearby Young Stars (DESTINYS):The SPHERE view of the Orion star-forming region (Valegård et al. 2024)• 円盤の明るさと中⼼星・円盤の性質との関連• Garu et al. (2018): 中間・遠⾚外が強く近⾚外が弱い天体のほうが、近⾚外が強い天体よりも散乱光が明るい。
→ ⼤きなinner cavityを持つ円盤(=近⾚外が弱い)の外側領域が照らされる。遷移円盤と呼ばれる。
↔ 近⾚外が強い円盤はinner cavityがなく、外側まで光が届かないため暗くなる。
Valegård, P.-G., et al.: A&A, 685, A54 (2024)• cavityを持つ遷移円盤は、Kバンドから5 µmまでのスペクトルの傾きがαK-5 ≤ 0、5–22 µmはα5-22 ≥ 0。
The low-surface-brightness disk, V606 Ori, is viewed face
↔ cavityが⼩さいか存在しない円盤は、どちらもconstantか≤0。

on, and is possibly the largest (⇠380 mas corresponding toV599
Ori: in the disk can be iden⇠152 au)Ori,
of thefaint Ori,disks.V351
No features• 明るいV1012
tified at this low surface brightness. It is also not possible to use→ innerdiskが存在する。
• 近⾚外が少しある
our automatic routine,
described
in Appendix C, to measure thedisk
inclination,PA,andradius.
We
havetherefore
estimatedthe• α5-22は⼤きなcavityも存在していることを⽰唆している。
radius of the disk and can conclude that it is oriented at a low.) The low brightness in scattered
light could,
294260:(25cavityが存在しないか、outerdiskが• 暗いHD inclination
together with the disk’s high millimeter flux, if the disk is notinner diskで⾃⼰遮蔽されているか、outerparticularly flared, indicate that the bulk ofdiskにダストが少ない。
the dust is located in
the inner disk so that the dust can effectively shadow the disk.

↑ 遷移円盤

fi

4.2.5. Non-detections

In the remaining 13 targets, we do not detect any scattered lightsignal that can be interpreted as coming from a disk. The corona12
graph covers 92.5 mas (⇠30 to ⇠37 au depending on the distanceFig. 4. Comparison between spectral slopes of the SED and the brightness of the disk, pol , given by the colorbar. Sources without thedetection of a disk in scattered light are marked with a cross.

Disk Evolution Study Through Imaging of Nearby Young Stars (DESTINYS):The SPHERE view of the Orion star-forming region (Valegård et al. 2024)• 円盤散乱光の相対的明るさ(polarized-to-stellar light contrast)とミリ波フラックスに相関が⾒られた。
• Kendall τ-coe cient (Kendall 1938)を計算 → 20%の確率で独⽴。
• ⼀⽅、円盤散乱光の相対的明るさと中⼼星質量・年齢には相関が⾒られなかった。
Valegård, P.-G., et al.: A&A, 685, A54 (2024)• 年齢とは77%の確率で独⽴、中⼼星質量とは65%の確率で独⽴。
a)

b)

c)

Fig. 5. Polarized-to-stellar light contrast compared to, (a) Stellar mass, (b) age, and (c) 1.3 mm Flux.

ffi⌧-coefficient. We find a correlation between the millimeter flux
and pol , ⌧K = 0.23, with a probability of ⇠20% that the twoquantities are independent of each other. This finding is further
discussed in Sect. 5.2.

given byP(r, b, m , mmax ) = ⇡r2 ⇢(b, m , mmax )(2)

13 from the star, b the galactic longitude,
where r is the separation

of a mild warp or small misalignment (Muro-Arena et al. 2020; be responsible for the disk asymmetry in V599 O
spiralarm in the disk. However, dedicated hydrod
Disk Evolution Benisty
StudyetThroughImagingof caused
NearbyYoung Stars(DESTINYS):
al. 2018). These
could beby gravitationaltions are needed to determine if an orbit configur
instability(Kratter&Lodato2016),
dynamic
interactions
with
The SPHERE view
of
the
Orion
star-forming
region(Valegård
et
al.
2024)
with
the
current
projected position brings the costellar companions (Bae & Zhu 2018), or interaction between an
enough to the disk to drive a large-scale spiral arembeddedplanetandthedisk(Zhangetal.
2018).
• 円盤の⾮対称性について
The lack of an outer companion in V 1012 Or
Of the three systems in question, V 1012 Ori does not show
→ そのうち10個に広がったダスト円盤を検出• ⾚外超過があるオリオンの23個の系を観測
a visible stellar companion within
the field of view of our suggests that disk gravitational instability or e
SPHERE observations (radius of 600 , see Appendix C for detec- ets may be responsible for the 2 observed asym
→ そのうち5つが150 au以上の半径 → そのうち3つが明るい(V351
Oriが最も明るく⼤きい,
360⇠10au) then gravitati
00
M
/M
are
largerthan
disk⇤tion limits). We detect a faint point source 1.7 to the east of
could be the reason (Kratter & Lodato 2016). W
V
351
Ori.
This
objectwasalreadydetectedbyWagneretal.
• 明るい3つ全てが散乱光に強い⾮対称性: warpかinner disk misalignmentによる影?
(2020), who disregarded it as a companion and classified it as mated the dust disk mass, assuming that there ar→ 重⼒不安定、伴星との相互作⽤、円盤に埋もれた惑星との相互作⽤による?
a background field star due to its rather neutral color using Ks conditions at = 1.3 mm (⌫ = 230 Ghz) andand L’ photometry. We see no further stellar companion can- isothermal, with
Oriの伴星は背景星かもしれない。V599 Oriは伴星の可能性がある。
• V1012 Oriのみ伴星が⾒つからず。V351
didates within the SPHERE field of view (see Appendix C forF ⌫ D2detection
limits.) In the case of V599 Ori we detect a faint com- Mdust =.
→ V351 OriとV1012
Oriのミリ波フラックスから円盤質量を⾒積もると、⌫ B⌫ (T dust )panion 2.0400 to the northeast of the primary star. By comparison
Valegård, P.-G., et al.: A&A, 685, A54 (2024)
円盤質量/中⼼星質量=0.039,
0.024となり、0.01より⼤きいので重⼒不安定かもしれない。
with VLT/NACO data,
taken
in
2008,
we
find
that
the
companrespectively. Not taking the temperature effects into account, thisD is the distance and B⌫ (T dust ) is the Planck func
ion proper motion is consistent
with shows
being
with
V599
crude approximation
thatboundgravitational
instability
couldOri.
betemperature. We used the dust temperature, T d =• UV-radiationについて
a plausible explanation.
Following examples suchAsymmetry
as Dietrich& Ginski(2018);
Bohn 2.3 cm2 g 1 for the absorption coefficient. To obta
could also arise
from the presenceof an embeddedthe
planetthat warps orof
misaligns
the disk (Bitschet (2014),
al. 2013;
etal.
(2020),
whichuse
approach
Lillo-Boxetal.
FUVの強さが~300
Gを超えると広がった円盤がないことが分かった。
•
0mass we then assumed a gas-to-dust ratio of 100
Xiang-Gruess & Papaloizou 2013; Nealon et al. 2018), subsewe tried to evaluate theprobability
that
observed
companquently
casting a shadow
overthethe disk.
Substellar massbodies
then
comes
out
as
0.039
and
0.024
for
V351
Ori
and
planets,
embedded
in
the
disk,
have
also
been
shown
to
drive
Oriは最も低いFUV• 最も広がった円盤V351
ion is a fieldstar. The vortexes
probability,
P, of observing a physicallyand density waves that induce spiral arms in the disk
6 http://stev.oapd.inaf.it/cgi-bin/trileg(Ogilvieat& Lubow
2002; Mutoet al. 2012;inZhutheet al.sky2015).isunrelated star in the fielda specificlocation
Embedded planets open gaps in the disk, trapping dust grains• ただし円盤半径とFUVの強度に相関は⾒られなかった。
in the pressure bump at the outer edge of the gap (Paardekooper& Mellema 2004; Zhu et al. 2014; Pinilla et al. 2016). These
processes slow down dust migration and effectively increase thelifetime of the outer disk, resulting in the disk being large andextended for a longer period. Embedded planets in the disksof V351 Ori, V599 Ori and V1012 Ori could thus explain not
only the asymmetries observed in scattered light, but also the
14in these systems.
exceptional radial extent of the disks↑ 300

Fig. 6. Graph showing the disk radius of each source in the FUV fieldof the three O stars, ✓1 Ori, Ori, and NU Ori. Local extinction has notbeen taken into account. Systems with detected disks are black and systems without a detected disk are blue. Upper limits for non-detections
were derived using the angular size of the coronagraph. Binary systems
are indicated with a white marker. No disks are detected at FUV fields
higher than ⇠300 G0 .

Athe 12 CO line wings hint at a misalignment between the inner (i 20 degrees) and outer disk (i 5 degrees). Finally,
we emphasise the need for complementary high-resolution CO observations, as in combination with the JWST-MIRI
observations they can be used to characterise the CO kinematics and the physical and chemical conditions of the otherobserved molecules with respect to CO.

The Epoch of Giant Planet Migration Planet Search Program. II. A Young Hot Jupiter. Candidate around the AB Dor Member HS Psc
Quang H. Tran, Brendan P. Bowler, William D. Cochran, Samuel Halverson, Suvrath Mahadevan, Joe P.
Ninan, Paul Robertson, Guðmundur Stefánsson, Ryan C. Terrien F We report the discovery of a hot Jupitercandidate orbiting HS Psc, a K7 (⇡0.7 M ) member of the ⇡130 Myr AB Doradus moving group. Using radial
velocities over 4 years from the Habitable-zone Planet Finder spectrograph at the Hobby-Eberly Telescope, we find+0.044a periodic signal at Pb = 3.986 0.003 d. A joint Keplerian and Gaussian process stellar activity model fit to the RVs
yields a minimum mass of mp sin i = 1.5+0.6
0.4 MJup . The stellar rotation period is well constrained by the Transiting
Exoplanet Survey Satellite light curve (Prot = 1.086 ± 0.003 d) and is not an integer harmonic nor alias of the orbital
period, supporting the planetary nature of the observed periodicity. HS Psc b joins a small population of young,close-in giant giant planet candidates with robust age and mass constraints and demonstrates that giant planets caneither migrate to their close-in orbital separations by 130 Myr or form in situ. Given its membership in a young
moving group, HS Psc represents an excellent target for follow-up observations to further characterize this young hot
Jupiter, refine its orbital properties, and search for additional planets in the system.

24

15

0. Formation and Structure of Circumplanetary Disks and Envelopes during the Late
Stages of Giant Planet Formation

Aster G. Taylor, Fred C. Adams F Giant planets are expected to form within circumstellar disks, which shape

their formation history and the local environment. Here, we consider the formation and structure of circumplanetarydisks that arise during the late stages of giant planet formation. During this phase, when most of the final mass isaccumulated, incoming material enters the Hill sphere and falls toward the planet. In the absence of torques, the fallingparcels of gas conserve their specific angular momentum and collect into a circumplanetary disk. Generalizing previous
work, we consider a range of possible geometries for the flow entering the sphere of influence of the planet. Specifically,
we consider five geometric patterns for the inward flow, ranging from concentration toward the rotational poles of thesystem to isotropic flow to concentration along the equatorial plane. For each case, we derive analytic descriptions
for the density field of the infall region, the disk surface density in the absence of viscosity, and steady-state solutions
for viscous disks. These results, in turn, specify the luminosity contributions of the planet, the circumplanetary disk,
and the envelope. These power sources, in conjunction with the surrounding material, collectively determine theobservational appearance of the forming planet. We conclude with an approximate determination of these radiative
signatures.

Fragmentation of Dense Rotation-Dominated Structures Fed by Collapsing Gravomagneto1. Sheetlets and Origin of Misaligned 100 au-Scale Binaries and Multiple Systems
Yisheng Tu, Zhi-Yun Li, Zhaohuan Zhu, Chun-Yen Hsu
F The majority of stars are in binary/multiple sys16

and the envelope. These power sources, in conjunction with the surrounding material, collectively determine theobservational appearance of the forming planet. We conclude with an approximate determination of these radiative
signatures.

Fragmentation of Dense Rotation-Dominated Structures Fed by Collapsing Gravomagneto1. Sheetlets and Origin of Misaligned 100 au-Scale Binaries and Multiple Systems
Yisheng Tu, Zhi-Yun Li, Zhaohuan Zhu, Chun-Yen Hsu F The majority of stars are in binary/multiple sys-tems. How such systems form in turbulent, magnetized cores of molecular clouds in the presence of non-ideal MHD
eﬀects remains relatively under-explored. Through ATHENA++-based non-ideal MHD AMR simulations with ambipolar diﬀusion, we show that the collapsing protostellar envelope is dominated by dense gravomagneto-sheetlets, aturbulence-warped version of the classic pseuodisk produced by anisotropic magnetic resistance to the gravitational
collapse, in agreement with previous simulations of turbulent, magnetized single-star formation. The sheetlets feed
mass, magnetic fields, and angular momentum to a Dense ROtation-Dominated (DROD) structure, which fragments
into binary/multiple systems. This DROD fragmentation scenario is a more dynamic variant of the traditional disk
fragmentation scenario for binary/multiple formation, with dense spiral filaments created by inhomogeneous feedingfrom the highly structured larger-scale sheetlets rather than the need for angular momentum transport, which isdominated by magnetic braking. Collisions between the dense spiraling filaments play a key role in pushing the local
magnetic Toomre parameter Qm below unity, leading to gravitational collapse and stellar companion formation provided that the local material is suﬃciently demagnetized, with a plasma- of order unity or more. This mechanism cannaturally produce in situ misaligned systems on the 100-au scale, often detected with high-resolution ALMA observations. Our simulations also highlight the importance of non-ideal MHD eﬀects, which aﬀect whether fragmentation
occurs and, if so, the masses and orbital parameters of the stellar companions formed.

2. The SPHERE view of the Orion star-forming region

P. -G. Valegard, C. Ginski, A. Derkink, A. Garufi, C.17Dominik, A. Ribas, J. P. Williams, M. Benisty, T.

dust content are typically bright in near-infrared scattered light. Conversely we do not find significant correlations
between scattered light contrast of the disks and the stellar mass or age.

Polarization Holes as an Indicator of Magnetic Field-Angular Momentum Alignment I.
. Initial Tests

Lijun Wang, Zhuo Cao, Xiaodan Fan, Hua-bai Li F The formation of protostellar disks is still a mystery, largely

due to the diﬃculties in observations that can constrain theories. For example, the 3D alignment between the rotationof the disk and the magnetic fields (B-fields) in the formation environment is critical in some models, but so far
impossible to observe. Here, we study the possibility of probing the alignment between B-field and disk rotation
using “polarization holes” (PHs). PHs are widely observed and are caused by unresolved B-field structures. With
ideal magnetohydrodynamic (MHD) simulations, we demonstrate that diﬀerent initial alignments between B-field andangular momentum (AM) can result in B-field structures that are distinct enough to produce distinguishable PHs.
Thus PHs can potentially serve as probes for alignments between B-field and AM in disk formation.

. Disk Wind Feedback from High-mass Protostars. III. Synthetic CO Line Emission

Duo Xu, Jonathan C. Tan, Jan E. Staﬀ, Jon P. Ramsey, Yichen Zhang, Kei E. Tanaka F To test theoreticalmodels of massive star formation it is important to compare their predictions with observed systems. To this end,
we conduct CO molecular line radiative transfer post-processing of 3D magneto-hydrodynamic (MHD) simulations ofvarious stages in the evolutionary sequence of a massive protostellar core, including its infall envelope and disk wind
18
outflow. Synthetic position-position-velocity (PPV) cubes of various transitions of CO, 13CO, and C18O emission areusing “polarization holes” (PHs). PHs are widely observed and are caused by unresolved B-field structures. With
ideal magnetohydrodynamic (MHD) simulations, we demonstrate that diﬀerent initial alignments between B-field andangular momentum (AM) can result in B-field structures that are distinct enough to produce distinguishable PHs.
Thus PHs can potentially serve as probes for alignments between B-field and AM in disk formation.

. Disk Wind Feedback from High-mass Protostars. III. Synthetic CO Line Emission

Duo Xu, Jonathan C. Tan, Jan E. Staﬀ, Jon P. Ramsey, Yichen Zhang, Kei E. Tanaka F To test theoreticalmodels of massive star formation it is important to compare their predictions with observed systems. To this end,
we conduct CO molecular line radiative transfer post-processing of 3D magneto-hydrodynamic (MHD) simulations ofvarious stages in the evolutionary sequence of a massive protostellar core, including its infall envelope and disk windoutflow. Synthetic position-position-velocity (PPV) cubes of various transitions of CO, 13CO, and C18O emission are
generated. We also carry out simulated Atacama Large Millimeter/submillimeter Array (ALMA) observations of thisemission. We compare the mass, momentum and kinetic energy estimates obtained from molecular lines to the true
values, finding that the mass and momentum estimates can have uncertainties of up to a factor of four. However,
the kinetic energy estimated from molecular lines is more significantly underestimated. Additionally, we compare themass outflow rate and momentum outflow rate obtained from the synthetic spectra with the true values. Finally,
we compare the synthetic spectra with real examples of ALMA-observed protostars and determine the best fitting
protostellar masses and outflow inclination angles. We then calculate the mass outflow rate and momentum outflow
rate for these sources, finding that both rates agree with theoretical protostellar evolutionary tracks.

5. Discovery of widespread non-metastable ammonia masers in the Milky Way

Y. T. Yan, C. Henkel, K. M. Menten, T. L. Wilson, A. Wootten, Y. Gong, F. Wyrowski, W. Yang, A.
Brunthaler, A. Kraus, B. Winkel F We present the results of a search for ammonia maser emission in 119 Galactic
19

high-mass star-forming regions (HMSFRs) known to host 22 GHz H2 O maser emission. Our survey has led to thethe kinetic energy estimated from molecular lines is more significantly underestimated. Additionally, we compare themass outflow rate and momentum outflow rate obtained from the synthetic spectra with the true values. Finally,
we compare the synthetic spectra with real examples of ALMA-observed protostars and determine the best fitting
protostellar masses and outflow inclination angles. We then calculate the mass outflow rate and momentum outflow
rate for these sources, finding that both rates agree with theoretical protostellar evolutionary tracks.

. Discovery of widespread non-metastable ammonia masers in the Milky Way

Y. T. Yan, C. Henkel, K. M. Menten, T. L. Wilson, A. Wootten, Y. Gong, F. Wyrowski, W. Yang, A.
Brunthaler, A. Kraus, B. Winkel F We present the results of a search for ammonia maser emission in 119 Galactic

high-mass star-forming regions (HMSFRs) known to host 22 GHz H2 O maser emission. Our survey has led to thediscovery of non-metastable NH3 inversion line masers toward 14 of these sources. This doubles the number of known
non-metastable ammonia masers in our Galaxy, including nine new very high excitation (J, K) = (9,6) maser sources.
These maser lines, including NH3 (5,4), (6,4), (6,5), (7,6), (8,6), (9,6), (9,8), (10,8), and (11,9), arise from energy levelsof 342 K, 513 K, 465 K, 606 K, 834 K, 1090 K, 942 K, 1226 K, and 1449 K above the ground state. Additionally, we
tentatively report a new metastable NH3 (3,3) maser in G048.49 and an NH3 (7,7) maser in G029.95. Our observations
reveal that all of the newly detected NH3 maser lines exhibit either blueshifted or redshifted velocities with respect tothe source systemic velocities. Among the non-metastable ammonia maser lines, larger velocity distributions, oﬀset
from the source systemic velocities, are found in the ortho-NH3 (K = 3n) than in the para-NH3 (K 6= 3n) transitions.

. The First Spatially-resolved Detection of CN in a Protoplanetary Disk and Evidence
for Complex Carbon Isotope Fractionation
13

Tomohiro C. Yoshida, Hideko Nomura, Kenji Furuya, Richard Teague, Charles J. Law, Takashi Tsukagoshi,
Seokho Lee, Christian Rab, Karin I. Öberg, Ryan A. Loomis F Recent measurements of carbon isotope ratios in20

the source systemic velocities. Among the non-metastable ammonia maser lines, larger velocity distributions, oﬀset
from the source systemic velocities, are found in the ortho-NH3 (K = 3n) than in the para-NH3 (K 6= 3n) transitions.

6. The First Spatially-resolved Detection of CN in a Protoplanetary Disk and Evidence
for Complex Carbon Isotope Fractionation
13

Tomohiro C. Yoshida, Hideko Nomura, Kenji Furuya, Richard Teague, Charles J. Law, Takashi Tsukagoshi,
Seokho Lee, Christian Rab, Karin I. Öberg, Ryan A. Loomis F Recent measurements of carbon isotope ratios inboth protoplanetary disks and exoplanet atmospheres have suggested a possible transfer of significant carbon isotope
fractionation from disks to planets. For a clearer understanding of the isotopic link between disks and planets, it isimportant to measure the carbon isotope ratios in various species. In this paper, we present a detection of the 13 CN
N = 2 1 hyperfine lines in the TW Hya disk with the Atacama Large Millimeter/submillimeter Array. This is the first
spatially-resolved detection of 13 CN in disks, which enables us to measure the spatially resolved 12 CN/13 CN ratio for13
the first time. We conducted non-local thermal equilibrium modeling of the CN lines in conjunction with previously
observed 12 CN lines to derive the kinetic temperature, H2 volume density, and column densities of 12 CN and 13 CN.
The H2 volume density is found to range between (4 10) ⇥ 107 cm 3 , suggesting that CN molecules mainly reside
26
+9
12
13
in the disk upper layer. The CN/ CN ratio is measured to be 70 6 at 30 < r < 80 au from the central star, which
is similar to the 12 C/13 C ratio in the interstellar medium. However, this value diﬀers from the previously reported
values found for other carbon-bearing molecules (CO and HCN) in the TW Hya disk. This could be self-consistently
explained by diﬀerent emission layer heights for diﬀerent molecules combined with preferential sequestration of 12 C
into the solid phase towards the disk midplane. This study reveals the complexity of the carbon isotope fractionation
operating in disks.

Relative velocities between

13

CO structures within
21

12

CO Molecular clouds

Lixia Yuan, Ji Yang, Xuepeng Chen, Yang Su, Shaobo Zhang, Xin Zhou, Zhiwei Chen, Qing-Zeng Yan, Minvalues found for other carbon-bearing molecules (CO and HCN) in the TW Hya disk. This could be self-consistently
explained by diﬀerent emission layer heights for diﬀerent molecules combined with preferential sequestration of 12 C
into the solid phase towards the disk midplane. This study reveals the complexity of the carbon isotope fractionation
operating in disks.

Relative velocities between 13 CO structures within 12 CO Molecular clouds

Lixia Yuan, Ji Yang, Xuepeng Chen, Yang Su, Shaobo Zhang, Xin Zhou, Zhiwei Chen, Qing-Zeng Yan, Min
Fang, Fujun Du, Yan Sun, Hongchi Wang, Ye Xu F Velocity fields of molecular clouds (MCs) can provide crucial

information on the merger and split between clouds, as well as their internal kinematics and maintenance, energy
injection and redistribution, even star formation within clouds. Using the CO spectral lines data from the Milky
Way Imaging Scroll Painting (MWISP) survey, we measure the relative velocities along the line of sight ( VLOS )between 13 CO structures within 12 CO MCs. Emphasizing MCs with double and triple 13 CO structures, we find thatapproximately 70% of VLOS values are less than ⇠ 1 km s 1 , and roughly 10% of values exceed 2 km s 1 , with a1
13
maximum of ⇠ 5 km s . Additionally, we compare VLOS with the internal velocity dispersion of CO structures( 13 CO,in ) and find that about 40% of samples in either double or triple regime display distinct velocity discontinuities,
i.e. the relative velocities between 13 CO structures are larger than the internal linewidths of 13 CO structures. Amongthese 40% samples in the triple regime, 33% exhibit signatures of combinations through the two-body motion, whereas
the remaining 7% show features of configurations through the multiple-body motion. The VLOS distributions for13
MCs with double and triple CO structures are similar, as well as their VLOS / 13 CO,in distributions. This suggeststhat relative motions of 13 CO structures within MCs are random and independent of cloud complexities and scales.

The environment around young eruptive stars. SPHERE/IRDIS polarimetric imaging. of 7 protostars

A. Zurlo, P. Weber, S. Pérez, L. Cieza, C. Ginski, R.22G. van Holstein, D. Principe, A. Garufi, A. Hales, J.

that relative motions of

CO structures within MCs are random and independent of cloud complexities and scales.

The environment around young eruptive stars. SPHERE/IRDIS polarimetric imaging. of 7 protostars

A. Zurlo, P. Weber, S. Pérez, L. Cieza, C. Ginski, R. G. van Holstein, D. Principe, A. Garufi, A. Hales, J.
Kastner, E. Rigliaco, G. Ruane, M. Benisty, C. Manara F Eruptive stars are a class of young stellar objects thatshow an abrupt increase in their luminosity. These burst-like episodes are thought to dominate the stellar accretion
process during the class 0/class I stage. We present an overview of a survey of seven episodically accreting protostars
aimed at studying their potentially complex circumstellar surroundings. The observations were performed with the
instrument SPHERE, mounted at the VLT. We observed the eruptive stars in H-band with the near-infrared imager
IRDIS and used the polarimeter to extract the polarized light scattered from the stars’ surroundings. We produced
polarized light images for three FUor objects, Z CMa, V960 Mon, and FU Ori, and four EXor objects, XZ Tau, UZ
Tau, NY Ori, and EX Lup. We calculated the intrinsic polarization fraction for all the observed stars. In all systems weregistered scattered light from around the primary star. FU Ori and V960 Mon are surrounded by complex structures
including spiral-like features. In Z CMa, we detected a point source 0.7 arcsec to the northeast of the primary. Basedon the astrometric measurements from archival Keck/NIRC2 data, we find this source to be a third member of thesystem. Further, Z CMa displays an outflow extending thousands of au. Unlike the other EXor objects in our sample,
XZ Tau shows bright, extended scattered light structures, also associated with an outflow on a scale of hundreds of au.
The other EXors show relatively faint disk-like structures in the immediate vicinity of the coronagraph. Asymmetricarms were only found around FUor objects, while faint disks seem to predominantly occur around EXors. Importantly,
for Z CMa the detection of the faint extended structure questions previous interpretations of the system’s dynamic
state. The streamer which was associated with a fly-by object turned out to be part of a huge outflow extending 6000
au.
23

state. The streamer which was associated with a fly-by object turned out to be part of a huge outflow extending 6000
au.

Gas
inflows
from
cloud
to
core
scalesin
G332.83-0.55:
Hierarchicalhub-filament
struc9.
tures and tide-regulated gravitational collapse

J. W. Zhou, S. Dib, M. Juvela, P. Sanhueza, F. Wyrowski, T. Liu, K. M. Menten F The massive star-forming

region G332.83-0.55 contains at least two levels of hub-filament structures. The hub-filament structures may form
through the "gravitational focusing" process. High-resolution LAsMA and ALMA observations can directly trace thegas inflows from cloud to core scales. We investigated the eﬀects of shear and tides from the protocluster on the surrounding local dense gas structures. Our results seem to deny the importance of shear and tides from the protocluster.
However, for a gas structure, it bears the tidal interactions
27 from all external material, not only the protocluster. To
fully consider the tidal interactions, we derived the tide field according to the surface density distribution. Then, weused the average strength of the external tidal field of a structure to measure the total tidal interactions that areexerted on it. For comparison, we also adopted an original pixel-by-pixel computation to estimate the average tidal
strength for each structure. Both methods give comparable results. After considering the total tidal interactions, theslope of the
N ⇤ R relation changes from 0.20 to 0.52, close to 0.5 of the pure free-fall gravitational collapse, andthe correlation also becomes stronger. Thus, the deformation due to the external tides can eﬀectively slow down thepure free-fall gravitational collapse of gas structures. The external tide tries to tear up the structure, but the externalpressure on the structure prevents this process. The counterbalance between the external tide and external pressure
hinders the free-fall gravitational collapse of the structure, which can also cause the pure free-fall gravitational collapse
to be slowed down. These mechanisms can be called "tide-regulated gravitational collapse.". The Multilayer Nature of Molecular Gas toward the Cygnus Region

24
Shiyu Zhang, Yang Su, Xuepeng Chen, Min Fang, Qingzeng
Yan, Shaobo Zhang, Yan Sun, Xiaolong Wang,pressure on the structure prevents this process. The counterbalance between the external tide and external pressure
hinders the free-fall gravitational collapse of the structure, which can also cause the pure free-fall gravitational collapse
to be slowed down. These mechanisms can be called "tide-regulated gravitational collapse."

The Multilayer Nature of Molecular Gas toward the Cygnus Region

Shiyu Zhang, Yang Su, Xuepeng Chen, Min Fang, Qingzeng Yan, Shaobo Zhang, Yan Sun, Xiaolong Wang,
Haoran Feng, Yuehui Ma, Miaomiao Zhang, Zi Zhuang, Xin Zhou, Zhiwei Chen, Ji Yang F We study thephysical properties and 3D distribution of molecular clouds (MCs) toward the Cygnus region using the MWISP CO
survey and Gaia DR3 data. Based on Gaussian decomposition and clustering for 13 CO lines, over 70% of the fluxes arerecovered. With the identification result of 13 CO structures, two models are designed to measure the distances of themolecular gas in velocity crowding regions. The distances of more than 200 large 13 CO structures are obtained toward
the 150 square degree region. Additionally, tens of the identified MC structures coincide well with masers and/or
intense mid-IR emission. We find multiple gas layers toward the region: (1) the extensive gas structures composing
the Cygnus Rift from 700 pc to 1 kpc across the whole region; (2) the ⇠ 1.3 kpc gas layer mainly in the Cygnus X
South region; and (3) the 1.5 kpc dense filament at the Cygnus X North region and many cometary clouds shaped by
Cygnus OB2. We also note that the spatial distribution of YSO candidates is generally consistent with the molecular
gas structures. The total molecular mass of the Cygnus region is estimated to be ⇠ 2.7 ⇥ 106 M assuming an X-factor
ratio XCO = 2 ⇥ 1020 cm 2 (K · km · s 1 ) 1 . The foreground Cygnus Rift contributes ⇠25% of the molecular mass inthe whole region. Our work presents a new 3D view of the MCs’ distribution toward the Cygnus X region, as well as
the exact molecular gas mass distribution in the foreground Cygnus Rift.

Surveys of clumps, cores, and condensations in Cygnus X: Temperature and nonthermal. velocity dispersion revealed by VLA NH3 observations
25

Xu Zhang, Keping Qiu, Qizhou Zhang, Yue Cao, Yu Cheng, Junhao Liu, Yuwei Wang, Xing Lu, Xing Pan

the whole region. Our work presents a new 3D view of the MCs’ distribution toward the Cygnus X region, as well as
the exact molecular gas mass distribution in the foreground Cygnus Rift.

Surveys of clumps, cores, and condensations in Cygnus X: Temperature and nonthermal. velocity dispersion revealed by VLA NH3 observations
Xu Zhang, Keping Qiu, Qizhou Zhang, Yue Cao, Yu Cheng, Junhao Liu, Yuwei Wang, Xing Lu, Xing Pan

F The physical properties, evolution, and fragmentation of massive dense cores (MDCs, ⇠ 0.1 pc) are fundamental
pieces in our understanding of high-mass star formation. We aim to characterize the temperature, velocity dispersion,and fragmentation of the MDCs in the Cygnus X giant molecular cloud and to investigate the stability and dynamics
of these cores. We present the Karl G. Jansky Very Large Array (VLA) observations of the NH3 (J,K) = (1,1)
and (2,2) inversion lines towards 35 MDCs in Cygnus X, from which we calculated the temperature and velocity
dispersion. We extracted 202 fragments (⇠ 0.02 pc) from the NH3 (1,1) moment-0 maps with the GAUSSCLUMPS
algorithm. We analyzed the stability of the MDCs and their NH3 fragments through evaluating the corresponding
kinetic, gravitational potential, and magnetic energies and the virial parameters. The MDCs in Cygnus X have atypical mean kinetic temperature TK of ⇠ 20 K. Our virial analysis shows that many MDCs are in subvirializedstates, indicating that the kinetic energy is insuﬃcient to support these MDCs against their gravity. The calculated
nonthermal velocity dispersions of most MDCs are at transonic to mildly supersonic levels, and the bulk motions makeonly a minor contribution to the velocity dispersion. Regarding the NH3 fragments, with TK ⇠ 19 K, their nonthermalvelocity dispersions are mostly trans-sonic to subsonic. Unless there is a strong magnetic field, most NH3 fragments
are probably not in virialized states. We also find that most of the NH3 fragments are dynamically quiescent, while
only a few are active due to star formation activity.

26