Star Formation NewsletterNo. 366 45-58
高橋実道（鹿児島大学/NAOJ）

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TaurusMC.
The
HOG
betweenthe 3D
dust andCO haverevealsa lowpattern
in existence
radial velocities
distancesthatis consistent
we fromreporttheExoplanet
analysesof theopticalandinfrared(OIR)
photometricmonitoring
observations
andvery
the high angular-resolution
X-Shooting
ULLYSES:
massivestars
atmetallicity.
I.and
Project
Descriptiontions
B-starAbundance
Study(BEAST)
illustrated
theof sub-stellar
companions
around4
3
fragmentation
of10
the
B213
filament.
is
10

↵

,
which
is
broadly
consistentwithobserved
value.
The
mechanismoftheformation,
streaming
instabilityorwe
directly
anddynamicallyconfirmthelong-standing
theoryontheoriginofspiralfeaturesin
protoplanetarydisks.
With
the
+1.5
with
converging
motions
of
the
gas
in
the
Taurus
MC,
with
the
near
side
of
the
cloud
movingathighervelocities
and
the
far
Jorick
S.
Vink
and
the
ULLYSESTeam
F
Observationsofindividual
massivestars,
super-luminous
supernovae,
gammacentimeterband
imagesofthelow-mass(M1
type)
pre-mainsequence
star,
DM
Tau.
We
found
that
the
OIR
photometric lighmassivestars.
In
this
paper,
we
present
thedetection
of
two
lower
mass
companions
toarelatively
nearby(148.7
pc),
The
role
of
magnetic
fieldsinthefragmentationofthe
Taurus
B213
filament
into
1.3 Sunmutual
collision,
depends
onthetimescaleofthestreaming
instability.
The
total
massRegionof planetesimals
also
dependsonthe↵ searchingandpatternmotionofcompanion-driven
spirals
being
independentofcompanion
mass,
here
we
establishafeasible
way
of
+3 at
ExcitedHydroxyl
OutflowintheHigh-Mass
Star-Forming
G34.26+0.15
side
movinglower
velocities.
This
convergence
of
flows
is
likelytriggeredbythelarge-scalegas
compression
causedbyrecombinationwere(V=6.632
detected,
wemag),
found
that
the
RMS
noise
stackedspectradecreases
followingtheradiometer
young
(17
bright
± but
0.006
2.58
± 0.06M
B9V
starofHIP
81208
residing
in theSco-Cenassociation,raybursts,andlines
gravitational-wave
eventsinvolving
spectacular
black-holemergers,
indicatethatthelow-metallicity
Universe
type
star-formingcores
4 Myr),
curvespresent
periodicvariations,which
isconsistent
with
that
the
host
young
star
is
rotating
in
the
same
direction
as
the
nata
is
about
30
100
M
if
the
planetarycore
hasalready
existedatthebeginning
and
grows
by
gas
accretion,butitdecreases
E
W.hiddenS.
E. LocalD. Araya,C.
Rigg,
P. Exoplanet
Hofner,S.
Kurtz,H.
Linz,
V.
RoseroG34.26+0.15
is a regionof behigh-massforplanetsthatareshell,beyondtheofbrighter
existing
ground-based
high-contrast
imagers.
interaction
ofspiral-arm-driving
theBubbleandthe
Per-Tauwith
Tauruslying
theintersection
of
the
two
bubblesurfaces.
using
theTan,Spectro-Polarimetric
High-contrast
REsearch(SPHERE)
instrument
atF
the
Very
Large
Telescope(VLT)
inequation.
Therefore,
detectingradio
recombinationlines
inadetection
sampleofat
free-freecontinuum
sourcesshouldpossible.
Anirudh
R.,
Chakali
Eswaraiah,
Sihan
Jiao,
Jessy
Jose
F
Fragmentation
is
a
key
step
in
the
processoftransformingisfundamentallydiﬀerent
from
our
own
Galaxy.
Manytransientphenomena
will
remainenigmatic
until
we
achieveafirm
A
panoptic
view
of
the
Taurusmolecular
cloud
I.
The
cloud
dynamics
revealed
by
gas
disk
and
is
hosting
at
least
one
giant
cold
spot.
In
addition,weresolvedthattheionized
gas
in
the
DM
Tau
disk
is localizedasthetimingoftheformationoftheplanetarycore
islater.
We
also
providesimpleapproximate
expressionsofthesurface+6+0.010star
formationthat
contains
a
broad
range
of
young
stellarobjects
indiﬀerentstagesofevolution,
includingahotmolecular
Chile.
Analysisofofthephotometry
obtained
gives massestimatesof 67intoM
the innercompanion
andspectral
0.135Space
M
forThis work
demonstrates
the potentialof broadband
VLA
observations
as thermal
low-resolutionline
scans.
J forclouds(and theirsubstructuressuch
as evolution
filaments,
clumps,andcontinuum
cores)
protostars.
Thegas Hubble
pressure
andgravitational
7 low
0.013
emission
and
3D
dust
understandingthephysics
andofmassivestars
atmetallicity(Z).
The
Telescopehasdevoteddensity
and
total
mass
of
the
planetesimals
and
find
that
the
total
mass
strongly
depends
on
the
dust
mass.
We
show
that
and
its
spatialdistribution
isvarying
with
time.
All
the
present
observations
canbecoherently
interpreted,
if
the
giant
cold
core,
hyper-compact
HII
regions
andaprototypical
cometary
ultra-compact
HII
region.
Previous
high-sensitivity
single
dish
the
outer
companion,
indicating
theformertobemost
likely
a
brown
dwarf
and
the
lattertobealow-mass
star.
The
systemcollapseare believed
to beSpectral
theprimary
agentsgoverning
thisprocess,referredas O.
thethermalJeans
fragmentation.
However,J.
D.orbits
Soler,
C.observe
Zucker,
J. E.
G.
Peek,
M.
Heyer,P.
F.
Goldsmith,
S.to
C.
Glover,S.massMolinari,
R. S.
Klessen,Broadband
VLA
Line
SurveyofaSampleof
IonizedJet
Candidates
500
to
250
massive
stars
at
low
Z
in
the
ultraviolet
(UV)
with
the
COS
and
STIS
spectrographs
under
the indicate
Directobservational
evidenceofthemulti-scale,dynamical
accretion
towardaplanetesimals
form
in
a
belt-likeregionbythecombination
of
the
dust
pile-upatthegaspressurebumpformedbyaplanetobservations
by
our
group
resultedinthedetection
of
broad
6035
MHz
OH
absorption
in
this
region;theline
showedasignificant
spot
is
the
dominant
anisotropic
UV
and/orX-raysourcethat
illuminates
theambient
cone-likeregion.
These
resultsiscompact
but unusual,asfactors
theorbitalplanesof thefields
two companions
arelikelyclose
toPezzuto,
orthogonal.
The
preliminary
orbital In
thecontributions
of
other
(such
as
magnetic
andturbulence)tothefragmentation
process
remainless
explored.
P.
Hennebelle,
L.
Testi,T.
Colman,M.
Benedettini,
D.
Elia,
C.
Mininni,S.
E.
Schisano,A.
Traficante
E.
Sanchez-Tovar,
E. formingD.
Araya,V.
Rosero,P.
Hofner,S.
Kurtz
Ffollowing
The
study companion
ofatheinteraction
betweenionizedjets,
ULLYSESprogram.
The
complementary“X-Shooting
ULLYSES”(XShootU)
project
providesenhancedlegacyvalue withhigh-massstar
hub-filament
systemandits
inwardmigration.
BEAST
detection
of
a
brown
dwarf
and
a
low-massstellararoundtheyoung
blue-shiftedasymmetry
indicativeofmoleculargas
expansion.
We
present
high-sensitivity
KarlG.
Jansky
Very
Large
Array
Planetesimalformation
at
the
gas
pressurebump
migratingplanetII.
Eﬀectssolutionswederivedforthesystemindicate
that
the
star
and
the
two
companions
arelikelyina
Kozai
resonance,
renderingthata detailed
theoreticalmodel
of isthehigh-energy
emission
isfromessential
ininter-core
theunderstandingof the space weathe
this
work,
we
have
testedpossiblefragmentation
mechanisms
by protostellar
estimating
the dust
mean
core
mass
and
mean
separationF
We
present
a studyoftheirthethree-dimensional(3D)
distributionof interstellar
derivedstellarextinction
observations
molecular
outflows
andenvironments
criticaltounderstanding
high-mass
star
formation,
especiallybecausejets
andhigh-quality
opticalandnear-infrared
spectraobtainedwiththewide-wavelength
coverage
X-shooter
spectrographat ESO’s
Dongting
Yang,
Hong-Li
Liu,
Anandmayee
Tej,
Tie
Liu,
Patricio
Sanhueza,
Sheng-Li
Qin,
Xing
Lu,
Ke
Wang,
bright
B
star
HIP
81208
(VLA)
observations
of
the
6035
MHz
OH
line
conducted
to
image
the
absorption
andinvestigate
its
originwithrespect
to
the
of
dust
growththesystemdynamicallyveryinterestingforfuturestudies.
ofthe B213
filament.
Webehaveusedthetransfer⇠14"
resolution
Clerk
Maxwell
Telescope(JCMT)
Submillimetre
Common-User
towardthe
Taurusmolecular
cloud
(MC)
and
its
relationJames
with
theneutralatomichydrogen(HI)emissionat 21 acm
wavelengtharoundtheextra-solar
planets
andtheoriginoflife.
outflows
arethought
to
key
in
the
of
angularmomentumoutwardsfromaccretion
disks.
We
reportlow-spectral
Gayathri
Viswanath,MarkusJanson,RaﬀaeleVito
Squicciarini,
Laetitia
Rodet,Simon
C.the
Ringqvist,
Very
Large
Telescope.
We
present
anoverview
ofGratton,
theJweXShootUproject,thatcombining
ULLYSESUV andandSirongPan,
Feng-Wei
Xu,
Enrique
Vazquez-Semadeni,Shanghuo
Li,
GilbertoC.
Gomez,
Aina
Palau,
diﬀerent
star
formation
sites
inand
the
region.
Industaddition,
reportdetectionofshowing
6030
MHz
OH
absorption
withVLA
12 Alibert
13
YuhitoShibaike,
Yann
F
Planetesimalformationis still
mysterious.
One
of
the
ways
to
form
planetesimals
is Guido
to XShootU
Bolometer
Array
2(SCUBA-2)/POL-2
850µm
continuummapandcombineditwithaPlanck
850
µm
map
and
HerschelandthecarbonmonoxideCOCOemission
in
the
=
1
!
0
transition.
We
used
the
histogramoforiented
gradients
resolution
VLA survey
for hydrogenradio recombinationlines,
OH,
NH3 , andCH3 OH linesSequence
toward a sample
of 58DM
high-mass
Anisotropic
Ionizing
IlluminationfromanM-typePre-main
Star,
Tau
Eric
E.
Mamajek,
SabineReﬀert,Gaël
Chauvin,
Philippe
Delorme,
ArthurVigan,
Mickaël
Bonnefoy,Nataliafurtherobservations
of
4.7
GHz
and
6.0
GHz
OH
lines
obtainedwith
theArecibo
Telescope.
The
6030
MHz
OH
line
shows
a
Garay,Paul
F.
Goldsmith,Mika
Juvela,Anindya
Saha,
Leonardo
Bronfman,
Chang
Won
Lee,
KenichiTatemopticalismatchcriticalfortheuniform
determination
ofof stellar
parameterssuch
aseﬀectivetemperature,surfacegravity,
invokeaspectragas
pressurebump
ina protoplanetarydisc.
In ourtheprevious
paper,
we propose
adust)
newfields
scenario
inbe
which
theof
piled-up
dust
data.
We
find
that
in
additiontothethermalcontribution,
presenceoforderedmagnetic
could
important
in
the
(HOG)
methodtothemorphology
ina
3D
reconstruction
thedust
density(3D
andthe
distribution
the
gas
star
forming
regions
that Baobab
containnumerous
ionizedjet candidates.
TheSai,observations
arefrom a Ing-Gueysurvey designed
to detect
Yuka
Terada,
Hauyu
Liu,
David
Mkrtichian,
Jinshi
MihokoKonishi,
Jiang,
Takayuki
Dynamical
detectionofacompanion
drivingaspiralarm
ina
protoplanetary
disk
Engler,SilvanoDesidera,ThomasHenning,
Janis
Hagelberg,
Maud
Langlois,
MichaelMeyer
F
Recentobservavery
similarabsorption
profile
as
the
6035
MHz
OH
line.
We
found
that
the
6035
MHz
OH
line
absorption
regionisspatially
at a gaspressurebump
createdbyHOG
a migrating
planetform
planetesimals
bybetweenstreaming
instability
in
aZ.
wide
regionofToth,
the
disc
as
atsu,
LokeshDewangan,
Jianwen
Zhou,
Yong
Zhang,
AmeliaStutz,
Chakali
Eswaraiah,L.
ViktorIsabelle
luminosity,andabundances,
as
well
as
wind
properties
suchasmass-loss
rates
infunctionofAs
uncertainties
instellar andfragmentation
of
the
B213
filament.
tracers’emission.
The
resultoftheanalysis
is
a
map
of
the
relationshipthedistancesandradialvelocities.
The
radio
continuum;
the
novel
aspect
of
this
work
is
to
searchforspectrallines
inbroadband
VLA
data
(we
providethescriptMuto,
Jun
Hashimoto,Motohide
TamuraF
The
powerful,
high-energy
magnetic
activities
of
young
stars
play
importantChenXie, B-starBin
B.Exoplanet
Ren,
Ruobing
Dong,
ÉlodieChoquet,ArthurVigan,
Jean-François
Gonzalez,
Kevin
Wagner,tions
fromAbundance
Study(BEAST)
have
illustrated
theexistenceof
sub-stellar
companions
aroundvery
unresolved
at⇠2"
scales,anditiscoincident
with
one
of
the
brightionized
cores
of
the
cometary
HII
region
that
shows
the
planetmigrates
inward.
In
this
work,
we
considertheglobaltime
evolution
of
dust
and
investigate
thedetailed
conditions
Ristorcelli,
Xianjin
Shen,
Anxu
Luo,
James
O.
ChibuezeF
There
isgrowing
evidencethathigh-mass
star
formationwindparameters
percolateintomany
adjacent
areasof
Astrophysics,
the
data
and
modellingofthe
XShootU
project
is expected
HOG
comparison
between
the
3D
dust
and
the
HI
emission
indicatesamorphological
match
at
the
distanceof
Taurusbut
developed
in
this
work
to
facilitate
explorationofotherdatasets).
We
reportdetection
of
25
GHz
CH
transitions
toward
3 OH
roles
in
the
magnetohydrodynamics
intheinnermost
parts
of
the
protoplanetarydisks.
In
addition,theassociatedUV
andTaotaoFang,
Maria
GiuliaUbeira-Gabellini
F
Radio
and
near-infraredobservations
haveobserved
dozensofprotoplan+1.5
IsabellaL.
Trierweiler,
Alexandra
E.
Doyle,
EdwardD.
Young
FA
persistentquestioninexoplanetdemographic
massivestars.
In
this
paper,
we
present
thedetection
of
two
lower
mass
companions
toarelatively
nearby(148.7
pc),
broad
radio
recombination
line
emission.
We
discussascenario
where
the
OH
absorptionistracingtheremnantsofapole-onandresultsoftheplanetesimalformationinourscenario.
We
use
a
1D
grid
single-sized
dust
evolutionmodel,
whichcanfollow
1.3
andhub-filament
systems(HFS)
areintricately
linked.
Thegaskinematics
along
the
filaments
andtheforminghigh-massananti-correlation
between
the
dust
and
the
HI
emission,which
uncoversa Z.
significant
amountofcoldwithinthe James Webbtobeaemission
game-changerforourphysicalunderstanding
ofthatmassive
stars
at
low
To
be
interprettensources;
fivehostof themalso
show
NHdensity
We
found
most
of
the
sources
detected
inableCH
OHconfidently
and
NHHI
been
3 emission.
3to3 have
etary
disks
that
spiralarm
features.
Numerical
simulations
have
shown
that
companions
may
excitespiraldensitywaves
X-ray
dictatesthephotochemistry;
moreover,thecoronaactivities
can
aﬀect
the
atmosphereofanewborn
extra-solar+3
A
panoptic
view
of
the
Taurusmolecular
cloud
I.
The
cloud
dynamics
by
gas
12by
young
(17
Myr),
bright
(V=6.632
± in
0.006
mag),
2.58
±
0.06
M
B9V
star
HIP
81208
residing
in revealedthe
Sco-Cenassociation,
molecular
outflow
that
is
being
ionizedinside-out
theultra-compact
HII
region.
iswhether
exoplanetarysystemsform
fromsimilarcompositionalbuilding
blockstoourown.
Polluted
white
dwarf
stars
oﬀe
the
growthoftheparticlesby
theirmutualcollision
andtheirradialdrift
anddiﬀusion.
We
calculatethetime-evolutionofthe4
ExcitedHydroxyl
OutflowtheHigh-Mass
Star-Forming
RegionG34.26+0.15
star(s)inthecentralhub
areinexcellentagreement
with
the
new
generationofglobalhierarchicalhigh-mass
star
formation
TaurusMC.
The
HOG
between
the
3D
dust
and
CO
revealsapatterninradialvelocities
anddistancesthatisconsistentclassified
as
ionizedjets
orjet
candidates
and
that
the
emissionlines
arecoincident
with,
or
very
near
(.
0.1
pc)
these
sources,Space
Telescope(JWST)
spectra
of
the
first
stellargenerations,theindividual
spectra
of
low
Z
stars
need
to
be
understood,
inprotoplanetary
via
companion-disk
However,the lack
direct observational
evidencefor spiral-driving
planet.
Howthedisks
UV
and
X-ray
photons interaction.
aregenerated,and howthey ofilluminate
the disks,
are not
wellunderstood.
Hereemission
and
3D
dust
using
the
Spectro-Polarimetric
High-contrast
Exoplanet
REsearch(SPHERE)
instrument
at
the
Very
Large
Telescope(VLT)
inradialdistribution
of
the
peak
mass
and
surfacedensity
of
the
dust
in
a
gas
disc
perturbed
byanembeddedmigratingplanet
W.
S.
Tan,
E.
D.
Araya,C.
Rigg,
P.
Hofner,S.
Kurtz,H.
Linz,
V.
RoseroF
G34.26+0.15
isaregionofhigh-massauniquewaytoaddress
thisquestionas
theyprovidemeasurements
of
the
bulk
compositionsofexoplanetary
material. We
withconverging
motions
of
the
gas
in
the
Taurus
MC,
with
the
near
side
of
the
cloud
movingathighervelocities
and
the
far
models.
In
thispaper,
we
present
anobservational
investigationofatypicalHFS
cloud,
G310.142+0.758(G310
hereafter)hence,
thesemolecular
lines
could
becan
used
as probesof theenvironment
near thelaunchingsite
of jets/outflows.
No radiocompanions
poses
challenges
tocurrent
theoriesofcompanion-disk
interaction.
Herewereportmulti-epoch
observations
of
which
is
exactly
where
XShootUdeliver.
wereporttheanalysesoftheopticalandinfrared(OIR)
photometricmonitoring
observations
and
the
high
angular-resolution+6+0.010J.
D.moving
Soler,
C.thatZucker,J. satisfies
E.broadG.obtained
Peek,
M.
Heyer,
P.
F.objects
Goldsmith,S.
C.
O.
Glover,S.planetesimals
Molinari,R.
S. 0.013
Klessen,Chile.
Analysisofthephotometry
gives
mass
estimates
of
67
M
for
the
inner
companion
and
0.135
M
for at theJ
andinvestigate
if
the
dust
the
conditionforplanetesimalformation.
We
find
that
form
in
a
belt-likestarformation
contains
a
range
of
young
stellarindiﬀerentstagesofevolution,
includingahotmolecular
7
side
at
lower
velocities.
This
convergence
of
flows
is
likelytriggeredbythelarge-scalegas
compression
causedbythewhich
revealsunambiguous
evidenceofmass
inflow
from
the
cloud
scale
via
the
filaments
onto
theforming
protostar(s)present
aband
statisticalanalysisofSpectro-Polarimetric
the
rocks
pollutingoxygen-bearing
white
dwarfsandcompareto rocks inthebinary system
HD100453withtheHigh-contrast
Exoplanet
REsearch(SPHERE)
facilityat Traficantethetheir
Very compositions
centimeter
imagesofthelow-mass(M1
type)
pre-mainsequence
star,
DM
Tau.
We
found
that
the
OIR
photometriclight
X-Shooting
ULLYSES:
massive
stars
at
low
metallicity.
I.
Project
Description
P.
Hennebelle,
L.
Testi,T.
Colman,M.
Benedettini,
D.
Elia,
C.
Mininni,S.
Pezzuto,E.
Schisano,
A.
the
outer
companion,
indicating
theformertobemost
likely
a
brown
dwarf
and
the
lattertobealow-mass
star.
The
systemregionbetweenthesnowline
andthepositionwheretheplanetreachesits
pebble-isolation
mass
when
the
strengthofturbulencecore,
hyper-compact
HII
regions
andaprototypical
cometary
ultra-compact
HII
region.
Previous
high-sensitivity
singledishinteraction
of
the
Local
Bubbleandthe
Per-Taushell,
with
Tauruslying
attheintersection
of
the
two
bubblesurfaces.
hub
conforming
with
the
model
predictions.
Continuumandmolecular
line
data
from
the
ATOMS
and
MALT90surveysare
Large
Telescope.
By
recoveringthespiralfeaturesvia
robustly
removing
starlight
contamination,
wemeasurespiralmotionthe
Solar
System.
We
find
that
the
majorityoftheextrasolar
rocks
are
consistentwith
thecompositionoftypicalchondrites
curvespresent
periodicvariations,which
isconsistent
with
that
the
host
young
star
is
rotating
in
the
same
direction
as
the
natal
Jorick
S.
Vink
and
the
ULLYSESTeam
F
Observationsofindividual
massivestars,
super-luminous
supernovae,
gamma4
3
F
We
present
a
study
of
the
three-dimensional(3D)
distributionofinterstellar
dust
derivedfromstellarextinction
observations
iscompactbut
unusual,astheorbitalplanesofthetwocompanions
arelikelyclose
toorthogonal.
The
preliminary
orbital
3 formation,observations
by
our
group
resultedintheconsistentdetection
ofThe
broad
6035
MHz
OH
absorption
in thisregion;theline
showedaconverging
significant
is 10↵perform
10, whichisextinction
broadly
withobserved
value.
The
mechanismof 10
thestreaming
instability
oracross4
yrtodynamical
motionanalyses.
spiralpatternmotionisconsistentwith
theorbitalmotion
of
the
used
that
cover
diﬀerent
spatialscales.
Threefilaments
(with
total
mass
5.7
±
1.1
⇥
M
)
are
identified
toward14
Ahigh-resolution
mappingtechniqueforface-ondisc
galaxies
disk
and
is
hosting
at
least
one
giant
cold
spot.
In
addition,weresolvedthattheionized
gas
in
the
DM
Tau
disk
is
localized,
raybursts,andgravitational-wave
eventsinvolving
spectacular
black-holemergers,
indicatethatthelow-metallicity
Universe
Measurement
uncertainties
prevent
distinguishing
betweenchondrites
andbulk
Earth,
butdopermitdetectingthe diﬀerence
towardthe
Taurusmolecular
cloud
(MC)
and
its
relationwiththeneutralatomichydrogen(HI)emissionat21
cm
wavelength
solutionswederivedforthesystemindicate
that
the
star
and
the
two
companions
arelikelyina
Kozai
resonance,
renderingblue-shiftedasymmetry
indicativeofmoleculargas
expansion.
We
present
high-sensitivity
KarlG.
Jansky
Very
Large
Array
mutualcollision,
depends
onthetimescaleofthestreaming
instability.
The
total
mass
of
planetesimals
also
depends
on↵andeccentric
companion.
With
this
first
observational
evidenceofa companion
drivingcan
ahave
spiralarm
among
protoplanetarydisks,
1213
thecentralhub
regionwhere
severalsignpostsofhigh-mass
star
formationbeen
observed.
The
hub
regioncontainsaHelenaFaustino
Vieira,Ana
Duarte-Cabral,
TimothyA.
Davis,
Nicolas
Peretto,Matthew
W.
L.
Smith,
Miguelandits
spatialdistribution
isvarying
with
time.
All
the
present
observations
becoherently
interpreted,
if
the
giant
cold
is
fundamentallydiﬀerent
from
our
own
Galaxy.
Manytransientphenomena
will
remainenigmatic
until
we
achieve
a
firm
and
the
carbonmonoxideCOandCOemission
in
the
J
=
1
!
0
transition.
We
used
the
histogramoforiented
gradients
Broadband
VLA
SpectralLine
SurveyofaSampleof
IonizedJet
Candidates
betweenchondritic
compositions
andbasalticorcontinental
crust.
Wefind
noby
evidenceof young
crust
amongstthe polluted whitethesystemdynamicallyveryinterestingforstudies.
BEAST
detection
of
a
brown
dwarf
and
a
low-massstellarcompanionaroundthe(VLA)
observationsofEthe6035
MHzOH
linefuture
conducted
to
image
the
absorption
andinvestigate
its
originwithrespect
to
the
is
about
30
100
M
if
the
planetarycore
hasalready
existedatthebeginning
and
grows
gas
accretion,butitdecreases
we
directly
anddynamicallyconfirmthelong-standing
theoryontheoriginofspiralfeaturesin
protoplanetarydisks.
With
the
massive
clump
±D.
260
M
)MichaelharbouringaP.
centralmassive
core.
Additionally,
five
outflowlobes
arewithassociated
with
the
spot
is methodthedominant
anisotropic
and/orX-raysourcethattheambient
cone-likeregion.
These
results
indicate
understandingof(1280thephysics
andUV
evolutionofmassivestars
atilluminates
lowmetallicity(Z).
The
HubbleSpace
TelescopehasdevotedQuerejeta,
Dario
Colombo,AndersonF
We
presentanew
dust
extinction
technique
which
we
are
able to
(HOG)
to
match
the
morphology
ina
3D
reconstruction
of
the
dust
density
(3D
dust)
and
the
distribution
of
the
gas
E.
Sanchez-Tovar,
E.
Araya,V.
Rosero,Hofner,
S.
Kurtz
F
The
study
of
the
interaction
betweenionizedjets,
bright
B
star
HIP
81208
large
disks.
Tentatively,
we
find
fewer
wide
gaps
in
intermediate-sized
disks
with
R
,90%
between
30
and
90
au.
We
perform
diﬀerent
star
formation
sites
in
the
region.
Inaddition,wereportdetection
of
6030
MHz
OH
absorption
with
the
VLA
and
as
the motion
timingofshow
the formation
ofchondritic
the planetary
core isoflater.
We alsorocks
providesimpleapproximate
expressionsof the surface
ef f isdwarfs.
Wethatthenatureextrasolar
also
supportedbythecompositionsof
localstars.
While
patternofcompanion-driven
spirals
being
independentofcompanion
mass,
here
we
establishafeasiblewayofsearchingcentralmassive
core
implyingaformingcluster.
Theobservedlarge-scale,smoothandcoherent
velocity
gradients
from
the
that
a of
detailed
theoretical
model
ofHOG
the high-energy
protostellar
emission
is withessential
intheunderstandingof
the space
weather500
orbitsto observe
250
massive
stars
atis
low
Zfor
the
(UV)
the the
COS
and
STIS
spectrographs
under
the in opticaltracers’emission.
The
resultofenvironments
theanalysisisain
map
ofultraviolettherelationshipbetweendistancesandanradialvelocities.
The
retrieveparsec-scalegassurfacedensitymaps
entirenearbygalaxies.
The
methodmeasuresthedust
attenuation
molecular
outflows
andtheircriticaltounderstanding
high-mass
star
formation,
especiallybecausejets
andGayathri
Viswanath,MarkusJanson,RaﬀaeleGratton,
Vito
Squicciarini,
Laetitia
Rodet,Simon
C.
Ringqvist,aseriesplanet-disk
interaction
simulations
toconstrainthesensitivityof
ourvisibility-fitting
approach.
Underassumption
furtherobservations
of
4.7
GHz
and
6.0
GHz
OH
lines
obtainedwith
theArecibo
Telescope.
The
6030
MHz
OH
line
shows
a
density
total massof theplanetesimals
and find
that
the
total
mass ground-basedstrongly
dependsonthe dust
mass.
We showthatforhiddenandspiral-arm-driving
planets
that areinbeyond
the detection
ofrelative
existing
high-contrast
imagers.
galactic
chemicalevolution
resultsvariations
intheabundancesofrock-forming
elements
spatially
andtemporally
aroundtheextra-solar
planets
andtheorigin
of
life.
cloud
down
to
the
core
scale,
andthesignaturesofinfallmotionseen
inthecentralmassive
clump
and
core,
clearly
unveila
ULLYSESprogram.
The
complementary“X-Shooting
ULLYSES”(XShootU)
project
providesenhancedlegacyvalue
withDynamical
detectionofacompanion
drivingaspiralarm
ina
protoplanetary
disk
HOG
comparison
between
the
3D
dust
and
the
HI
emission
indicatesamorphological
match
at
the
distanceof
Taurusbut
outflows
thought
to aprofilebekey
in thethetransferof OH
angularmomentumoutwardsfromaccretion
disks.
We
reportaNatalia
low-spectral
EricE.
Mamajek,
SabineReﬀert,Gaël
Chauvin,
Philippe
Delorme,
ArthurVigan,
Mickaël
Bonnefoy,
bands
onare
a pixel-by-pixel
basis
againstaMHzsmoothed,reconstructed
stellardistribution.
The
contribution
ofisforegroundlight alongofplanet-disk
interaction,
we
use
the
gap
widthsandcommondisk
tocalculatepotential
planetmasseswithintheverysimilarabsorption
as
6035
line.
We parameters
found
that
the
6035
MHz
OH
line
absorption
regionspatially
planetesimals
form
in
belt-likeregionbythecombination
of
the
dust
pile-upatthegaspressurebumpformedbyaplanet3
1
onanti-correlation
galaxy-wide
scales,thecurrent
sampleofratepolluted
white
dwarfsare
suﬃciently
young
and
close
tothe
Earth
that they
are nohigh-quality
opticalandnear-infrared
spectraobtainedwiththewide-wavelength
coverage
X-shooter
spectrograph
at
ESO’s
Chen
Xie,
Bin
B.
Ren,
Ruobing
Dong,
ÉlodieChoquet,ArthurVigan,
Jean-François
Gonzalez,
Kevin
Wagner,nearly-continuous,
multi-scale
massaccretion/transfer
process
atasimilarmass
infall
rate
of
⇠
10
M
yr
over
all
scales,an
betweenthe
dust
densityandtheHIemission,which
uncoversasignificant
amountofcoldHIwithinEngler,SilvanoDesidera,ThomasHenning,
Janis
Hagelberg,
Maud
Langlois,
MichaelMeyer
F
Recentobservaresolution
VLA
surveyforhydrogenradio
recombinationlines,
OH,
NH
,
and
CH
OH
lines
towardasampleof58
high-mass
Taurussample.
We
find
that
the
young
planetoccurrence
peaks
near
Neptunemasses,similartothe
DSHARP
sample.
For33
theline-of-sightiscalibrated
using
dust
emission
observations,assuming
that
the
dust
sits
in
a
layer
close
to
the
mid-planeofunresolved
at ⇠migration.
2" scales, and it is coincident with
one of the bright ionized cores of the cometary HII region that shows
and its inward
12
Very
Large
Telescope.
We
presentof F
the
XShootU
project,
showingthat
combining
ULLYSESUVand
XShootU
TaurusThe
between
the
3D
dust
and
CO
revealsawherepatterninvelocities
anddistancesthat
isof
consistent
0.01
Mfrom
/M
.
M
/Mprocess.
.Giulia
0.1
Mhigh-mass/M,antheoverview
rateis
17.4±8.3%;
forcompositions
0.1
M.
Mradial.
M, accretion
itcompanions
is
27.8±8.3%.
Both
TaotaoFang,
Maria
Ubeira-Gabellini
Radio
and
near-infraredobservations
haveobserved
dozensofprotoplantions
B-starExoplanet
Abundance
Study(BEAST)
have
illustrated
theexistenceof1 required
sub-stellar
aroundvery
aﬀectedby
thisconcludethat
exoticaretoexplainthemajorityof ofobservedrock typefeedingthecentralforming
protostar(s)
in
the
G310
HFS
cloud.
star
forming
regions
that
containnumerous
ionizedjetcandidates.
Theobservations
are
from
a
surveydesignedtodetect
J MC.
pHOG
⇤
JWe
J /M
p /M
⇤not
J /M
Directobservational
evidenceofthemulti-scale,dynamical
mass
toward
a
broad
radio
recombination
line
emission.
We
discussascenariotheOH
absorptionistracingtheremnantsapole-ontheface-ongalaxy.
Here,
we
apply
this
technique
to
M51
(NGC
5194)
as
a
proof-of-concept,
obtainingaresolution
0.14"
(5
+1.5
A
Chondritic
Solar
Neighborhood
of
them
are
consistentwithmicrolensing
surveys.
For
gas
giantsmore
massive
than
5
M
,
the
occurrencerate
is
4.2±4.2%,
massivestars.
In
this
paper,
we
present
thedetection
of
two
lower
mass
companions
toarelatively
nearby(148.7pc),
opticalspectraiscriticalfortheuniform
determinationofstellarparameterssuch
aseﬀectivetemperature,surfacegravity,withconverging
motions
of
the
gas
in
the
Taurus
MC,
with
the
near
side
of
the
cloud
movingathighervelocities
and
the
far
J
etary
disks
that
host
spiralarm
features.
Numerical
simulations
have
shown
that
companions
may
excitespiraldensitywaves
radio
continuum;
the
novel
aspectof andthisworkisvariations
tosystemsearchforspectral HII
linesregion.
in broadband
VLA data (weprovidethescripthigh-mass
star
forming
hub-filament
1.3
aroundpolluted
white
dwarfs,that
betweenexoplanetarycompositions
inthestellarneighborhood
are generally
molecular
outflow
that
is
being
ionizedinside-outbytheultra-compact
pc).
Our
dust
(and
gas)
surfacedensitymap
isconsistent
withindependent
dustandCO-basedstudiesatlowerresolution.
We+3
IsabellaL.
Trierweiler,
Alexandra
E.
Doyle,
EdwardD.
Young
FA
persistentquestioninexoplanetdemographics
consistent
directimagingsurveys.
young(17withMyr),bright
(V=6.632±convergence
0.006
mag),
2.58
±datasets).
0.06
M
B9V
star
HIP
81208
residing
inthe
Sco-Cenassociation,side
movinglower
velocities.
This
of
flows
isan
likelytriggeredbythelarge-scalegas
compression
causedby Tautheandluminosity,andabundances,
asIllumination
well
as
wind
properties
suchasmass-loss
rates
in function
ofGHz
Z.
As
uncertainties
instellarinprotoplanetary
disks
via
companion-disk
interaction.
However,
the
lack
of
directobservational
evidenceforspiral-driving
Dongting
Yang,
Hong-Li
Liu,
Anandmayee
Tej,
Tie
Liu,
Patricio
Sanhueza,
Sheng-Li
Qin,
Xing
Lu,
KeDM
Wang,
developed
in
this
work
to
facilitate
exploration
of
other
We
reportdetectionof25
CHtransitions
toward4at
3 OHStar,
Anisotropic
Ionizingfrom
M-typePre-main
Sequence
notdue
tosignificant
diﬀerencesintheinitialcompositionof
protoplanetarydisks.
Nonetheless,thereisevidencefromstellafindthatdiscrepancies
betweenourestimatesofsurfacedensityandotherstudiesstem
primarily
fromthechoice
of
dust
model
is
whether
exoplanetarysystemsform
fromsimilarcompositionalbuilding
blockstoourown.
Polluted
white
dwarf
stars
oﬀer
using
the
Spectro-Polarimetric
High-contrast
Exoplanet
REsearch(SPHERE)
instrument
at
the
Very
Large
Telescope(VLT)
Substructures
Compact
Disks
ofcompanion-disk
theTaurus
TaurusStar-forming
Regioninteraction
offivetheofHauyu
Local
Bubbleandthe
Per-Taushell,
withlying
thesourcesintersection
of
the
two
bubblesurfaces.
windparameters
percolateintomany
adjacent
areasof
Astrophysics,
the
data
and
modellingofthe
XShootU
project
isinTakayuki
expected
SirongPan,
Feng-Wei
Xu,
Enrique
Vazquez-Semadeni,Shanghuo
Li,
GilbertoC.
Gomez,
Palau,
Guido
companions
poses
challenges
tocurrent
theoriesofinteraction.
Herewereportmulti-epoch
observationstensources;theminalso
showNHemission.
We
found
that
most
ofat
the
detected
in
CH
OH
and
NH
been of
3
3Aina
3 haveYuka
Terada,BaobabLiu,David
Mkrtichian,
Jinshi
Sai,
MihokoKonishi,Ing-Guey
Jiang,+6+0.010observations
thatplanets
formedinthefirstseveralbillion
years
in
the
Galaxy
have
lower
metal
core
fractionscompared withauniquewaytoaddress
thisquestionas
theyprovidemeasurements
of
the
bulk
compositionsofexoplanetary
material.
WeLeon(i.e.
diﬀerent
dust
absorption
coeﬃcients).
Whenassuming
the
same
dust
opacitylaw,
ourtechniqueproduces
surfacedensities
Chile.
Analysisofthephotometry
obtained
gives
mass
estimates
of
67
M
for
the
inner
companion
and0.135
MTatemfor
J
Shangjia
Zhang,
Matt
Kalscheur,
Feng
Long,
Ke
Zhang,
Deryl
E.
Long,
Edwin
A.
Bergin,Zhaohuan
Zhu,
to
be
a
game-changerforourphysicalunderstandingof
massive
stars
low
Z.
To
be
able
to
confidently
interpret
James
Webb
7 at
0.013
Garay,Paul
F.
Goldsmith,Mika
Juvela,Anindya
Saha,
Leonardo
Bronfman,
Chang
Won
Lee,
Kenichi
X-Shooting
ULLYSES:
massive
stars
at
low
metallicity.
I.
Project
Description
classified
as
ionizedjets
orjet
candidates
and
that
the
emissionlines
arecoincident
with,
or
very
near
(.
0.1
pc)
these
sources,thebinarysystem
HD
100453withtheSpectro-Polarimetric
High-contrast
Exoplanet
REsearch(SPHERE)
facility
at
the
Very
PorousDust
ParticlesinProtoplanetary
Disks:
Application
to
the
HL
Tau
Muto, Jun
Hashimoto,Motohide
TamuraF The
powerful,
high-energy
magnetic
activities
ofDiskyoung
stars play
importantpresentastatisticalanalysis
of
the
rocks
pollutingoxygen-bearing
white
dwarfsandcomparetheir
compositions
torocks
inmapstheoutercompanion,
indicating
theformertoYongbemostlikelya brown
dwarf
and
the
latterto of
bea sitelow-mass
star.
The
systemthatareconsistent
withindependentstudies.
This
dust
extinction
techniqueprovides
us
with
gas
surfacedensity
at an
Earth
on
average.
atsu,
LokeshDewangan,
Jianwen
Zhou,
Zhang,
AmeliaStutz,
Chakali
Eswaraiah,L.
ViktorToth,Isabelle
Space
Telescope(JWST)
spectra
of
the
first
stellargenerations,theindividual
spectra
low
Z
stars
need
to
be
understood,
TrapmanF
Observationsofsubstructureinprotoplanetary
disks
have
largelybeen
limitedtothebrightest
andlargestdisks,
Jorick
S.
Vink
and
the
ULLYSESTeam
F
Observationsofindividual
massivestars,
super-luminous
supernovae,
gammahence,thesemolecular
lines
could
be
used
as
probesoftheenvironmentnear
thelaunchingofjets/outflows.
No
radio
Large
Telescope.
By
recoveringthespiralfeaturesvia
robustly
removing
starlight
contamination,
wemeasurespiralmotionShangjia
Zhang,
Zhaohuan
Zhu,
Takahiro
Ueda,
Akimasa
Kataoka,
AnibalSierra,CarlosCarrasco-González,rolesin themagnetohydrodynamics
inthe Survey
innermostparts
ofrocks
theareprotoplanetarydisks.
Incomposition
addition,theassociatedUV andBroadband
VLA
SpectralLineofa
Sampleof
IonizedJet
Candidates
iscompactbut
unusual,astheorbitalplanesofthetwocompanions
likelyclose
toorthogonal.
The
preliminary
orbitalthe
Solar
System.
We
find
that
the
majorityoftheextrasolarareconsistent
with
the
of
typicalchondrites.
Ristorcelli,
Xianjin
Shen,
Anxu
Luo,
James
O.disks
ChibuezeF
There
ismotiongrowing
evidencethathigh-mass
star
formation
unprecedented
resolution
for
full
disc
coveragestudiesofnearbygalaxies.
resultingwell-resolved
information
which
isyr
exactly
where
XShootUcandeliver.
raybursts,andgravitational-wave
eventsinvolving
spectacular
black-holemergers,
indicate
the thelow-metallicity
Universe
excludingtheabundant
populationof compact
which
are
likelysites
ofTheplanetformation.
Here,wespatial
reanalyze0.1”, 1.33opens
across4emission
toperform
dynamical
motionanalyses.
The
spiralpatternisconsistentorbitalmotionof theEnrique
MacíasF
Dustparticlesizes
constrained
from
dust
continuumandpolarization
observations
bywithradiointerferometry
X-ray
dictatesthephotochemistry;
moreover,thecoronaactivities
can
aﬀect
the
atmosphereofanewborn
extra-solar
E.
Sanchez-Tovar,
E. theD.
Araya,V.
Rosero,P.between
Hofner,S. kinematics
Kurtz
F The
study
of buttheinteraction
betweenrendering
ionizedjets,
solutionswederivedforsystemindicate
that
the
star
and
the
two
companions
arelikelyina
Kozai
resonance,
Measurement
uncertainties
prevent
distinguishingchondrites
andbulk
Earth,
dopermitdetectingthediﬀerences
andhub-filament
systems(HFS)
areintricately
linked.
The
gas
along
the
filaments
andtheforminghigh-mass
areinconsistent
byfor
atUV
least
anfromorderof photons
magnitude.
Motivatedbyporousdust
observed
in
small
Solar
Systembodies(e.g.,
fromisfundamentallydiﬀerent
ourown
Galaxy.
Manytransientphenomena
will
remainenigmatic
until
we understood.
achievea firmthepossibility
more
in-depth
examinationoftheinfluenceoflarge-scale
dynamics(andalso
stellarfeedback
mechanisms)
eccentric
companion.
With
this
first
observational
evidenceof ahow
companion
drivingathespiralarm
among
protoplanetarydisks,
mm
ALMA
continuum
observationsof
12compact
protoplanetary
disks
in
the
Taurusstar-forming
region.
Byfittingvisibilities
planet.
How
the
and
X-ray
are
generated,andthey
illuminate
disks,
are
not
well
Here
the Rosetta
systemdynamicallyveryinterestingforfuturestudies.
molecular
outflows
andtheirenvironmentsiscriticalto understanding
high-mass
star
formation,
especiallybecausejets andbetweenchondritic
compositions
andbasalticorcontinental
crust.
Wefind
noevidenceof
crust
amongstthepollutedwhite
star(s)inthecentralhub
areinexcellentagreement
with
the
new
generationofglobalhierarchicalhigh-mass
star
formationthemission),we
explore
how
the
dust
particle’s
porosity
aﬀectstheestimatedparticle
sizes
from
these
two
methods.
understandingofthephysics
andevolutionofmassive
stars
at
low
metallicity(Z).
The
HubbleSpace
Telescopehasdevotedwedirectly
anddynamicallyconfirmthelong-standing
theoryontheoriginofspiralfeaturesin
protoplanetarydisks.
With
theTaurusontheinterstellar
mediumatparsec-scales,
andconsequently
star
formationinnearbygalaxies.
14
directly,
weidentify
substructures
in
6
of
the
12
compact
disks.
Wethencomparethesubstructures
identified
in
the
full
we
reporttheanalysesoftheopticalandinfrared(OIR)
photometricmonitoring
observations
and
the
high
angular-resolution
outflows
arethought
towebekey
in thetransfer
ofof
angularmomentumoutwardsfromaccretion
disks.
We
reporta hereafter)
low-spectralAhigh-resolution
extinction
mappingtechniqueforface-ondisc
galaxies
dwarfs.
We
show
that
the
chondritic
natureextrasolar
rocks
is
also
supportedbythecompositions
of
local
While
Porousparticles
have
lower
refractive
indices,
which
aﬀect
both
opacityandpolarization
fraction.
With
weakerMieinterference
models.
In
thispaper,
present
anobservational
investigationofatypicalHFS
cloud,
G310.142+0.758(G310
500 orbits
to observe
250 massive stars
at being
low Z independent
in the ultraviolet(UV) withthehereCOSweand
STIS spectrographs
under
the
patternmotionof companion-driven
spiralsof companion
mass,establisha feasible way stars.
ofsearching

A Chondritic Solar Neighborhoodand its inward migration.

49 Anisotropic Ionizing Illumination from an M-type Pre-main Sequence Star, DM Tau

Yuka Terada, Hauyu Baobab Liu, David Mkrtichian, Jinshi Sai, Mihoko Konishi, Ing-Guey Jiang, Takayuki
Muto, Jun Hashimoto, Motohide Tamura F The powerful, high-energy magnetic activities of young stars play importantroles in the magnetohydrodynamics in the innermost parts of the protoplanetary disks. In addition, the associated UV and
X-ray emission dictates the photochemistry; moreover, the corona activities can aﬀect the atmosphere of a newborn extra-solar
planet. How the UV and X-ray photons are generated, and how they illuminate the disks, are not well understood. Here
we report the analyses of the optical and infrared (OIR) photometric monitoring observations and the high angular-resolution
centimeter band images of the low-mass (M1 type) pre-main sequence star, DM Tau. We found that the OIR photometric light
curves present periodic variations, which is consistent with that the host young star is rotating in the same direction as the natal
disk and is hosting at least one giant cold spot. In addition, we resolved that the ionized gas in the DM Tau disk is localized,
and its spatial distribution is varying with time. All the present observations can be coherently interpreted, if the giant cold
spot is the dominant anisotropic UV and/or X-ray source that illuminates the ambient cone-like region. These results indicatethat a detailed theoretical model of the high-energy protostellar emission is essential in the understanding of the space weather
around the extra-solar planets and the origin of life.
Anisotropic Ionizing Illumination from an M-type Pre-main Sequence StarA
Solar Neighborhood
DMChondritic
Tau の可視や近赤の明るさの時間変動と、cm波観

9Isabella L. Trierweiler, Alexandra E. Doyle, Edward D. Young F A persistent question in exoplanet demographics
測した円盤の明るさの非対称性、明るい領域の時間変
iswhether exoplanetary systems form from similar compositional building blocks to our own. Polluted white dwarf stars oﬀer
a化が、「中心星のcold
unique way to address thisquestionas they やx線で円盤がprovide measurements of the bulk compositions of exoplanetary material. We
spot
からのUV
present a statistical analysis of the rocks polluting oxygen-bearing white dwarfs and compare their compositions to rocks in炙られている」というモデルで説明できる。
the Solar System. We find that the majority of the extrasolar rocks are consistent with the composition of typical chondrites.
Measurement uncertainties prevent distinguishing between chondrites and bulk Earth, but do permit detecting the diﬀerences
between chondritic compositions and basaltic or continental crust. We find no evidence of crust amongst the polluted whitedwarfs. We show that the chondritic nature of extrasolar rocks is also supported by the compositions of local stars. Whilegalactic chemical evolution results in variations in the relativeFigure
abundancesof rock-forming
elements
temporally
5. Schematic model
for interpreting the observations
on DMspatiallyTau. Left andandright panels
indicate the configurations
during theare
X band(8–12 GHz) observations
andandthe third
epoch ofKu bandthat(12–18 theyGHz) observations,on galaxy-wide scales, the current sample of polluted white dwarfs
suﬃciently
young
close
toJVLAEarth
are notrespectively.
The blue arrow indicates the major axis of the DM Tau disk.

イントロ
前主系列星(PMS) :速い自転（数日）磁気活動が活発
magnetic loopの付け根にcold spot → 周期的な明るさの変化、x線放射
星表面の磁場と円盤内縁との相互作用やhigh-energy photonによる円盤蒸発など、
円盤進化の理解にも重要。蒸発がcm波の観測でわかる（？）
DM Tauに注目
M1 type PMS star, 0.5 Msun, d~144 pc
M type PMS はMagnetic dipole を持つ傾向、より大きい質量のPMSよりシンプル
PMSからのhigh-energy photon と円盤の関係の理解を進めたい。
観測
K2、0.6m PROMPT-8 望遠鏡 (V, R, I band)
JVLA(X 8-12 GHz, Ku12-18 GHz)

結果
K2で観測した時間変動

V,R,I AnisotropicとK2の比較
Ionizing Illumination from an M-type Pre-main Sequence Star

5

K2で見つかった~7日周期と合う。
それ以上の~20日の変動も見える。

Figure 2. Optical and near-infrared monitoring observations towards DM Tau. Green, orange, and cyan symbols present ourV, R, and I band monitoring observations that were taken in 2019 (Section 2.2). Left and right panels show the observations
were taken in early and late 2019, respectively, which were separated by a time period when DM Tau is not visible from ourobservatory at night time.
Gray curves show replications of the phase-folded K2 and 0.1-day boxcar-smoothed light curve (Section 3.1), which are verticallyo↵set to permit easier comparison with the V, R, and I bands data. The horizontal axis shows the Julian day o↵sets from reference
2458000. Three vertical lines in the left panel indicate the epochs of the JVLA observations which have been shifted by -28
periods for easier comparison with the optical monitoring.

左下：7.364日の周期で重ねた結果。オレンジは0.1日平均
右下：0.1日平均を引いたresidual.

where rraw is the rms of the light curve, and rresid is
the rms evaluated after subtracting a boxcar-smoothed
light curve from the phase-folded one (Figure 1, bottom
left). In our case, the thermal noise of the light curve( in Cody & Hillenbrand 2018) is negligibly small, andtherefore the error of Q is dominated by the uncertaintyof P̃ . We varied the value of P̃ from the aforementioned
initial identification to minimize Q. We found a minimum of Q=0.63 when using a period of 7.364 days,
which we regard as the best-fit variational period of
DM Tau. Our derived period is consistent with what
was reported in Rebull et al. (2020). We visually inspected the phase-folded light curves and the residuals
after subtracting the boxcar-smoothed light curves (Figure 1, bottom right) to ensure the correct convergenceof the period and Q. We note that in addition to the7.364±0.042 days periodic variations, the K2 light curveof DM Tau also occasionally presents flares of higher
fluxes and shorter duration.
The derived Q value indicates that DM Tau may be
regarded as a quasi-periodic variable at optical wave-of the phase-folded K2 light curve. The V, R, and I
magnitudes are clearly variable. During the Julian days
(JD) 2458490–2458508, the V band monitoring clearly
resolved the periodic variation of which the time andperiods are consistent with those of the K2 light curve.
At the same time, the R band shows a similar variation
to the V band, although the error bar is larger. In addition, DM Tau occasionally presents a variation of ⇠ ±0.5magnitudes on timescales shorter and longer than 7.364
days. For example, a long-term variation of &20 days
timescale can be seen from the right panel of Figure 2.
The observed OIR light curves can show o↵sets from aperfect periodic light curve due to stochastic flares (e.g.,
Chang et al. 2018; Hawley et al. 2014) or the switchingof accretion column (e.g., Čemeljić & Siwak 2020).
If the 7.364 days periodic variation of the DM Tau
is stationary, then our JVLA X band observations weretaken close to the minimum of this periodic optical modulation; the first epoch of Ku band observations weretaken slightly closer to the maximum while the second
Ku band observations were taken further closer to the8Terada et al.

there is a single dominant giant spot. We employed themethodology in the SOAP tool (Boisse et al. 2012). The
details are described in Appendix A.
A comparison between the synthetic optical light
curves produced from our model and our V and R bands
observations are presented in Figure 4. We found that
6
Teradaal.
theetperiodicmodulation of the V and R bands magnitudes can indeed be interpreted with a high latitude
giant cold spot that is ⇠1000 K cooler than the ambient
stellar surface (Figure 4, upper panel; Table 2). In ourbest-fit model, the spot covers ⇠50% of the stellar surface. Both the temperature and area of our spot model
are reasonable when compared to what were typicallyfound in the M dwarfs (Fang et al. 2016; Jackson et al.
2018; Flores et al. 2020). We note that the v sin i valueof the host protostar derived from the previous optical
spectroscopy (Hartmann & Stau↵er 1989) and the stellar radius we derived may imply that the host protostaris ⇠15 more inclined than the disk.
In our simplified spot model, we assumed a single circular spot although the spot may have a more complicated shape in reality. It can also be aggregation of multiple spots. To characterize how the spot is illuminating
the disk without being seriously biased by the assumption of the shape of the spot(s), we define a quantitythat is called spot phase. The unit of spot phase is degree. We define the spot phase to be zero when the spotis phasing the southwest, and when projected onto thedisk plane, is in the minor axis of the disk. The spot
phase increases counter-clockwisely by 2⇡ over a stellar rotational time period. The bottom panel of Figure
4 shows a comparison between the spot phase and thecentroids of the radio emission knots. There appears to
be a good correlation between these quantities. We notethat although our JVLA observations (Section 2.1) weretaken ⇠7 months after the OIR monitoring observations
carried out in 2019 January (Section 2.2). Nevertheless, our OIR monitoring observations were carried out
also about two years after the K2 observations while ourmonitoring observations still detected consistent periodicity and phase with those observed from the K2 data.
Therefore, we consider that it is fair to extrapolate thespot phase from the epochs of the K2 and OIR moniFigure 3. Left :- The JVLA images (color; Table 1), are overplotted with the ALMA 1.3 mm continuum image (Hashimoto00
toringobservaions
to make
et al. 2021). Contours are [200, 400] µJy beam 1 (✓maj ⇥ ✓min
=0.00 038⇥0.
026; P.A.=33). Fromcomparison
top to bottomwith
rows ourshowJVLAtheobservations.
Robust=2 weighted Ku band (12–18 GHz) image taken on August 4, the Robust=0 weighted X band (8–12 GHz) image takenthat there
one dominant
giant
cold
on August 6, and the Robust=2 weighted Ku band image takenWeon hypothesize
August 18. Color-codedarcsisindicate
the [10, 15,
20, 25,30] au radii. The lightblue line indicates the major axis of the
DM Taudisk. The
denotesthe JVLA
spot.
Duringthe filled
two ellipse
epochsof JVLA
Kusynthesizedband (12–beam. Right :- Azimuthal profiles of the radio intensity derived
the observations,images presented thisin thecold
left panel.
these plots,
18fromGHz)
spot In
centerfacedtheandzero position angle is defined along the major axis of the disk.illuminatedBlack lines indicate
3- detection
the southeastof limits.
the DM Tau disk (Figure
5, left). Between the first epoch of Ku band observaRobust=0 weighted 8–12 GHz (X band) and Robust=2
pact bright emission knot in the southwest and a di↵use
tions
and the X band (8–12 GHz) observations, the spot
weighted 12–18 GHz (Ku band) images. Each observaionized crescent that occupies the southwest side of therotatedcavity.
towardrightof (Figureleft)sig-andtion was performed on a di↵erent day (Table 1). The center
millimeter
Theupperfirst epoch
Ku band 5,
image
the UV/X-ray
regiontowardspatially resolved extended radio emission does not co- thus nificantly
detected photoionizeda knot in the south.
Themoved
third epoch結果

星表面にcold spot があるモデルの光度変化と観測の比較

JVLAのKu, X Band の輝度分布

Ku, X のピークとcold spot の位置が良く合う
Cold spot からのhigh-energy photon
で円盤が照らされるモデルでFigure 4. Top: A comparison of the magnitudes of the V,
R, and I bands monitoring observations with those given by
our photospheric model including a stellar spot (Appendix整合的に説明できる
A, Section 4). For clarity, the magnitudes were vertically

各半径の明るさのピークが時間とともに移動

Illumination
an M-type Pre-main Sequence Star
shifted in Anisotropic
the same way Ionizing
as in Figure
2. Similar tofrom
Figure2, the three vertical lines indicate the (-28 periods shifted)
time epochs of our successful JVLA observations. Bottom:
The mean position angle(s) derived based on the Gaussian
fittings to the azimuthal intensity profiles (Figure 3, right).
Downward triangles (H) show the brightest peaks and crossmarks show the second brightest peaks at each radius. The
black circle indicates the spot phase (for an explanation see
Section 4).

9tent with that of the disk rotation traced by CO velocities (redshifted in the northwest and blueshifted in thesoutheast; see Figure 5; Kudo et al. 2018).
There might be more than one cold spot on the surfaceof the host protostars, as the third epoch of Ku band observations (Figure 3, bottom) resolved more than one
emission ionized emission knot. There might be anFigure 5. Schematic model for interpreting the observations on DM Tau. Left and right panels indicate the configurations
other giant spot that is located at the far-side of theduring the X band (8–12 GHz) observations and the third epoch of JVLA Ku band (12–18 GHz) observations, respectively.
stellar surface and may illuminate the northeast with

55 Dynamical detection of a companion driving a spiral arm in a protoplanetary disk

Chen Xie, Bin B. Ren, Ruobing Dong, Élodie Choquet, Arthur Vigan, Jean-François Gonzalez, Kevin Wagner,
Taotao Fang, Maria Giulia Ubeira-Gabellini F Radio and near-infrared observations have observed dozens of protoplanetary disks that host spiral arm features. Numerical simulations have shown that companions may excite spiral density waves
in protoplanetary disks via companion-disk interaction. However, the lack of direct observational evidence for spiral-driving
companions poses challenges to current theories of companion-disk interaction. Here we report multi-epoch observations of
the binary system HD 100453 with the Spectro-Polarimetric High-contrast Exoplanet REsearch (SPHERE) facility at the Very
Large Telescope. By recovering the spiral features via robustly removing starlight contamination, we measure spiral motion
across 4 yr to perform dynamical motion analyses. The spiral pattern motion is consistent with the orbital motion of theeccentric companion. With this first observational evidence of a companion driving a spiral arm among protoplanetary disks,
we directly and dynamically confirm the long-standing theory on the origin of spiral features in protoplanetary disks. With thepattern motion of companion-driven spirals being independent of companion mass, here we establish a feasible way of searchingfor hidden spiral-arm-driving planets that are beyond the detection of existing ground-based high-contrast imagers.

Direct observational evidence of the multi-scale, dynamical mass accretion toward ahigh-mass star forming hub-filament system

Dongting Yang, Hong-Li Liu, Anandmayee Tej, Tie Liu, Patricio Sanhueza, Sheng-Li Qin, Xing Lu, Ke Wang,
Sirong Pan, Feng-Wei Xu, Enrique Vazquez-Semadeni, Shanghuo Li, Gilberto C. Gomez, Aina Palau, Guido
Garay, Paul F. Goldsmith, Mika Juvela, Anindya Saha, Leonardo Bronfman, Chang Won Lee, Kenichi Tatematsu, Lokesh Dewangan, Jianwen Zhou, Yong Zhang, Amelia Stutz, Chakali Eswaraiah, L. Viktor Toth, Isabelle
Ristorcelli, Xianjin Shen, Anxu Luo, James O. Chibueze F There is growing evidence that high-mass star formationand hub-filament systems (HFS) are intricately linked. The gas kinematics along the filaments and the forming high-massstar(s) in the central hub are in excellent agreement with the new generation of global hierarchical high-mass star formation
models. In this paper, we present an observational investigation of a typical HFS cloud, G310.142+0.758 (G310 hereafter)
which reveals unambiguous evidence of mass inflow from the cloud scale via the filaments onto the forming protostar(s) at the
hub conforming with the model predictions. Continuum and molecular line data from the ATOMS and MALT90 surveys areused that cover diﬀerent spatial scales. Three filaments (with total mass 5.7 ± 1.1 ⇥ 103 M ) are identified converging toward
the central hub region where several signposts of high-mass star formation have been observed. The hub region contains aイントロ
いくつかの円盤で渦状腕構造が検出されている。
起源：伴星の重力 or 自己重力不安定性（GI）？
A&A proofs: manuscript no. ms
渦状腕の回転角速度
HD 100453
A (hereafter
HD 100453) is a young Herbig A9Ve accurately recover the disk morphology with theoretically mini伴星→
伴星の軌道できまる。
star with a mass of 1.70 ± 0.09 M (Dominik et al. 2003). The mum post-processing artifacts, which is an essential requirement
protoplanetary
disk around the primary star was directly imaged for accurate measurement of the pattern motion of spiral feaGI→ 円盤半径でのケプラー回転
at near-infrared (NIR) and submillimeter wavelengths, showing tures.
a cavity, a ring, and two spiral arms from inside out (Benisty
et al. 2017; Wagner et al. 2018; van der Plas et al. 2019; Rosotti
et al. 連星、且つ渦状腕構造構造が見えているHD100453について、2020). NIR interferometric observations revealed the pres- 3. Dynamical analysis
ence of the inner disk (Menu et al. 2015; Kluska et al. 2020; 3.1. Pattern motion of the spiral arm S1
Bohn渦状腕の位置を2015年と2019年で比較。渦状腕の起源を検証
et al. 2022) inside the cavity that is misaligned with andshadows the outer spiral disk (Bohn et al. 2022; Benisty et al.
2017).
The secondary star HD 100453 B (hereafter the companion)
観測is an early M star with a mass of 0.2 ± 0.04 M (Collins et al.
2009), located at a projected distance of around 1.0500 (109 au).
SPHERE K1-band (λ=2.11um)
The HD 100453 system o↵ers a particularly decisive test of comotion between spirals and companions that might be driving
them. Numerical simulations suggest that such a companion can
リング構造と、そこから伸びる
truncatethe disk and excite two spiral arms in the remaining disk
as observed in the NIR (Dong et al. 2016b). The companiondriven２本の腕が見えている。
origin of the spiral arms was supported by one of the observed spiral arms in the 12 CO line that connects to the compan灰色線：伴星の軌道
ion position
by assuming a coplanar orbit (Rosotti et al. 2020).
However, the potential mutual inclination between the companion orbit and the spiral disk (van der Plas et al. 2019; Gonzalez et al. 2020) raised the possibility of a projection e↵ect. With
HD 100453 being the exemplary configuration of a companion–spiral system, we study the motions of the spiral(s) and the companion here.

解析

Xie et al.: Dynamical detection of a companion-driving spiral
A&A proofs: manuscript no. ms

3.2. Motion of the stellar companion

The companion HD 100453 B has over 15 years of astrometricdata. We adopt astrometric data from Collins et al. (2009), Wagner et al. (2018), and Gonzalez et al. (2020) (see Table F.1). A
linear fit to the PAs of the companion shows that the companion has an angular velocity of 0 .384 ± 0 .019 yr 1 in the sky
plane between 2003 and 2019 (Appendix F). Based on the PAs
only in 2015 and 2019, we also obtain an angular velocity of
0 .40 ± 0 .07 yr 1 for the companion, which is consistent with ourlinear fit. Hence, we adopt the fitting result as the angular velocity of the companion because it contains more independent measurements. To obtain the companion motion in the disk plane, we
deprojected the angular velocity of the companion from the sky
plane to the disk plane. In the deprojection, we adopt the disk
inclination, the disk position angle, and the companion position
angle to be 33 .81, 144 .35, and 133 .2, respectively. We obtain
Fig.the
3. Angularvelocityof the S1 spiralpatterncompanion
motion in HD 100453(blackdiskline). It
could follow
local Keplerian motion (green curve) or be
angularvelocityof thein theplane
to besmaller than the maximum value1of the companion orbital motion (blue curve), under gravitational instability (GI) or companion–disk interaction,
0 .455 ±0measured.023 yrspiral between
2015with
andthe2019.
二つの観測で渦状腕のピークの位置の比較
渦状腕の回転角速度とケプラー回転、伴星軌道の比較
The
motion is consistentcompanion motion in the system and is inconsistent with the local Keplerian
Fig. 2. Peak locations of spiral arm S1 in polar coordinates after correc- respectively.
motion, revealing the companion-driven origin of the spiral arm S1, while excluding the GI origin. The motions here adopt a central stellar mass
also estimate the probability density distribution of thetion for viewing geometry. The solid curves represent the best-fit model of 1.70 ±We
0.09 M . The colored shaded regions around each curve represent the corresponding uncertainties.
灰色線は2015年の渦状腕の位置から
ケプラー回転より明らかに遅く、伴星の角速度の範囲内に
angular velocity in the disk plane (Appendix G). We
spiral for the peak locations (dot points) between 2015 and 2019, as- companion
suming the companion-driven scenario. The derived angular velocities between
calculatethecompanion
angularvelocity
based
on
the
compancriminate
betweenthe scattered light from the dusty disk andthedisk
surfaceonthenearside
of
the
disk
(i.e.,
S2)
ケプラー回転した場合の位置→GIの場合の予想含まれる。
1of spiral pattern motion are 0 .88±0 .07 yr . The uncertainty estimation andion
the skyplane isparameterslarger than the disk
inclinationof 33the.8. Wethatfittingof the embedded
orbitaladoptedfromorbit
resultsplanetin (Rameau et al. 2017; Currie et al.
the disk inclination to be the angle between the flat disk 2019; Rich et al. 2019). H↵ surveys for the signal of planetaryis presented in Appendix D. The 2019 observations significantly deviate define
Gonzalez
etdynamicalal.plane.
(2020).
The derived
probability density distribumidplane and→the sky
Large viewingに伴星が作る腕が確認された最初の観測
angles (i.e., >30 .0) accretions mostly resulted in nondetections of planets (Cugno
from the gravitational instability prediction (dashed curve), adopting a preventtion ushas
a Gaussian
the companion
angularfromrestoring the profile;correct face-on
morphology viahas
et anal. 2019;
Zurlo velocet al. 2020; Xie et al. 2020), possibly caused
central star of 1.7 M .
+0 .023
1
theitydeprojection(Dong
et al.
2016a).
UnlikeS2, S1 interval)
locates on inby highextinction
or periodic
accretions if the forming planet
of
0
.457
yr
(1
credible
the
disk
plane
in
0 .023the far side of the disk
where the inclination of the disk surface is present. In summary, current instruments with conventional
2019.than
Thetheangularvelocity
derivedfrom tothe techniques
orbital parameters
is smaller
disk inclination.
Thus, itis more accurate
are inefficient in the search for planets embedded in
restorethe S1 arm backto face-on
morphology
thanfittheto
S2thearm.companion
disks.
is consistentwiththe direct
linearPAs. This
Therefore, we did not provide a motion measurement for the S2
Our dynamical
motionanalysis of the HD 100453 system
consistentangularvelocityand
its
Gaussiandistribution
areexarm.
validated the approach of mapping spiral arm motion to loment (Appendix A), we conclude that the o↵set is caused by the pected because the companion motion between
2003giant
andplanets
2019in protoplanetary disks, first proposed
cate hidden

57 Substructures in Compact Disks of the Taurus Star-forming Region

Shangjia Zhang, Matt Kalscheur, Feng Long, Ke Zhang, Deryl E. Long, Edwin A. Bergin, Zhaohuan Zhu, Leon
Trapman F Observations of substructure in protoplanetary disks have largely been limited to the brightest and largest disks,
excluding the abundant population of compact disks which are likely sites of planet formation. Here, we reanalyze 0.1”, 1.33
mm ALMA continuum observations of 12 compact protoplanetary disks in the Taurus star-forming region. By fitting visibilities
directly, we identify substructures in 6 of the 12 compact disks. We then compare the substructures identified in the full Taurus
sample of 24 disks in single star systems and the ALMA DSHARP survey, diﬀerentiating between compact (Ref f ,90% < 50 au)
and extended (Ref f ,90% > 50 au) disk sources. We find that substructures are detected at nearly all radii in both small andlarge disks. Tentatively, we find fewer wide gaps in intermediate-sized disks with Ref f ,90% between 30 and 90 au. We perform
a series of planet-disk interaction simulations to constrain the sensitivity of our visibility-fitting approach. Under an assumptionof planet-disk interaction, we use the gap widths and common17
disk parameters to calculate potential planet masses within the
Taurus sample. We find that the young planet occurrence rate peaks near Neptune masses, similar to the DSHARP sample. For
0.01 MJ /M . Mp /M⇤ . 0.1 MJ /M , the rate is 17.4±8.3%; for 0.1 MJ /M . Mp /M⇤ . 1 MJ /M , it is 27.8±8.3%. Bothof them are consistent with microlensing surveys. For gas giants more massive than 5 MJ , the occurrence rate is 4.2±4.2%,
consistent with direct imaging surveys.

Porous Dust Particles in Protoplanetary Disks: Application to the HL Tau Disk

Shangjia Zhang, Zhaohuan Zhu, Takahiro Ueda, Akimasa Kataoka, Anibal Sierra, Carlos Carrasco-González,Enrique Macías F Dust particle sizes constrained from dust continuum and polarization observations by radio interferometry
are inconsistent by at least an order of magnitude. Motivated by porous dust observed in small Solar System bodies (e.g., fromthe Rosetta mission), we explore how the dust particle’s porosity aﬀects the estimated particle sizes from these two methods.
Porous particles have lower refractive indices, which aﬀect both opacity and polarization fraction. With weaker Mie interference
patterns, the porous particles have lower opacity at mm wavelengths than the compact particles if the particle size exceeds
several hundred microns. Consequently, the inferred dust mass using porous particles can be up to a factor of six higher. The
most significant diﬀerence between compact and porous particles is their scattering properties. The porous particles have awider range of particle sizes with high linear polarization from dust self-scattering, allowing mm-cm-sized particles to explain
polarization observations. With a Bayesian approach, we use porous particles to fit HL Tau disk’s multi-wavelength continuumイントロ
DSHARPをはじめとして、多数の天体でring-gap構造が観測普遍的に存在？
コンパクトな円盤については十分な数の観測がない。
→ Taurus のコンパクト天体の構造を調べ、統計的な議論を行う。

観測
ALMA 1.33 mm, ~0.1”
Long et al 2019の32のサンプルのうち、12個の天体で構造が見つかっている。
過去の研究で構造が見つからなかった12の円盤の構造をvisibility から調べる。（残りの8天体は連星）

結果
12の天体のうち、構造が見つかったものが６個 5Figure 1. Deprojected visibility and radial intensity profiles for the six disks with identified substructure (a) and the six smoothdisks (b) following our fitting approach. Overlaid in blue on the visibility curves are our best-fit models, which are used to

8ring-gapの分布
円盤の大小によらず広い範囲に分布
60 au. No obvious correlation of gap width and location
Planet-disk interactions are proposed as one of the
ピークは小円盤が~20
au、大円盤が~40
otherwise
exists.
major causes of observedau（バイアス？）
disk substructure (e.g. Rice
Figure 3. Incidence of gaps and rings in 5 au radial location bins for the compact case (left-hand panels), and 15 au bins for theextended case (middle panels). Probability density functions (PDFs) of substructure locations (scaled to match the underlying
histograms) are overlaid in red and blue, respectively. These PDFs are plotted together in the right-hand panels for a more
direct comparison of gap and ring locations in compact and extended disks.

The story is much the same with gap depths. The
majority of gaps are shallow, with gap-ring intensity
variations below 30%, especially interior to 60 au. It
is tempting to link wider and deeper gaps at large radiiin the extended disks to a more massive planet population (more massive planets carve out larger gaps under
the assumption of planet-disk interaction), but this relationship largely disappears after correcting gap width togap location (Figure 5), a better indicator of planet mass
(Kanagawa et al. 2016; Zhang et al. 2018). It is worth

et al. 2006; Zhu et al. 2012), and we expect that gap
location should coincide with orbital location of the embedded planet. Additionally, more massive planets will
form steeper pressure gradients within the disk and create larger gap openings than are created by less massive
planets (Fung et al. 2014; Kanagawa et al. 2015; Rosotti
et al. 2016; Zhang et al. 2018).
In order to characterize the sensitivity of our modelfitting approach for detecting substructure induced byyoung planets, we combine a series of planet simulations

以下、gapの起源が惑星とした場合の解析
12

α=10^-3, a̲max=0.1mmを仮定してgapから見積もった惑星の位置と質量
これまでの観測で見えていない領域を見ている。

20­50au の領域や、円盤半径30-90 au の円盤にはwide gapは見られない。giant planet の存在に制限？
Figure 8. Potential young planets in the Taurus sample with detected exoplanets on the planet mass-semi-major axis diagram.
The planet mass is calculated as the mass assuming amax = 0.1 mm and ↵ = 10 3 (see Table 5 in the Appendix). The semi-major
axis is equivalent to the gap location. Compact disks are in red and extended disks are in blue. The number inside the circle
indicates the disk in which the planet resides. The error bar encompasses the uncertainties in the fitting and the disk viscosity.
Exoplanets detected by various methods are marked with di↵erent colors.

et al. 2019; Wang et al. 2020; Hashimoto et al. 2020)).
Compared to Zhang et al. (2018), we add the following
gaps to the DSHARP sample: D25 of Elias 20, D29 of
RU Lup, D98 of DoAr 25, and D117 of IM Lup, as their
gap widths are also > 0.12. Their masses are inferred using the fitting method, instead of by direct comparison
with simulations. Exoplanets detected by various methods are represented by scatter points of di↵erent colors.
The distribution of planets from the Taurus survey issimilar to the distribution from the DSHARP survey.
Interestingly, the giant planets (> 0.1 MJ ) between
20-50 au are fewer compared to smaller and larger separations. As planet masses are inferred from gap widths,
this echoes our finding in Figure 4, where wide gaps
are rarer between 20-50 au. Since the definition of the

gap width ( ) used to calculate planet mass is slightlydi↵erent from the one in Figure 4 (normalized by theouter gap edge instead of the gap location), we remake
the gap width-gap location plot in Figure 9’s top panel.
It is similar to Figure 8 and also to Figure 4 except thex-axis is shown in log-scale. We mark the region withfewer wide gaps in ellipse and question mark. Additionally, this dearth of wide gaps is even more evident if we
use the e↵ective radius Re↵,90% as the x-axis (bottom
panel of Figure 9). For Re↵,90% between 30-90 au, mostof the gap widths are below 0.2.
More disk surveys of high angular resolution observations are needed to test out whether this void of wide
gaps for intermediate sized disks (or gaps with intermediate separations) are statistically significant. If they15

惑星の軌道長半径、質量のoccurence rate
半径が大きく、質量が小さいほど多い傾向

Figure 9. The gap width vs. gap location (top panel) and
gap width vs. e↵ective disk radius (bottom panel) for Taurus and DSHARP samples. Gaps in compact disks are in
red and extended disks in blue. The gaps in the DSHARP
sample are marked in more transparent colors. For the bottom panel, each vertical line represents a disk radius. Points
threaded by the same vertical line belong to the same disk.
The intermediate regions with fewer wide gaps are marked
by ellipses and question marks.

are, it indicates that gaps at the inner and outer disks
may be a↵ected by di↵erent physical processes (e.g. different planet formation or evolution mechanisms).
In Figure 10, we expand on the analysis by counting
potential planets in mass-location bins among compact
and extended disks in the Taurus survey.6 The y-axes
are the planet-star mass ratios in units of Jupiter massover solar mass. We choose to present the planet-starmass ratio instead of the absolute planet mass since it
directly reflects the observable, gap width. Another ad-

Fi
sa
se
pa
ne
or
re
m
di
th

co
ve
32
Th
wi
of

結果まとめ1. 12のサンプルのうち、６個でsubstructure を観測構造があるコンパクト（<50au）円盤の数が２倍に。
構造は浅く、狭い < 5 au
6個の構造がない円盤は平均的に小さく暗い
2. Re ,90 < 23 au or <12mJy の円盤で構造なし→より高分解能が必要？
3. 先行研究と合わせると、コンパクト円盤の2/3に構造

6. α<10^-3 なら、gap は20­30au のNeptune massに対応。これまで見つからない領域を調べられる。
7. 今回のサンプルで、小さい円盤にも惑星が存在する可能性が明らかに。
8. 惑星の存在確率は、惑星が軽く、遠いほど大きくなる
Taurus とDSHARPで分布は1σで一致

9.Taurus での惑星の存在確率はmicrolensing の結果と小円盤では~20 au, 大円盤では~40 au で構造のピーク、整合的。
バイアス？構造の典型的な場所はない？
0.01Mj/Msun<Mp/Mstar<0.1Mj/Msunで17.4%
0.1Mj/Msun<Mp/Mstar<1Mj/Msunで27.8%
4. Taurus とDSHARP では、>5Mjで４.２％、直接撮像と整合的大きい円盤ほどgap幅や深さが大。
ギャップ半径で規格化した幅の違いはほぼない。
5. 20­50au の範囲や、円盤半径30-90 au の円盤には

ff

wide gapは見られない。giant planet の存在に制限？

The role of magnetic fields in the fragmentation of the Taurus B213 filament into Sun45
type star-forming cores

Anirudh R., Chakali Eswaraiah, Sihan Jiao, Jessy Jose F Fragmentation is a key step in the process of transforming
clouds (and their substructures such as filaments, clumps, and cores) into protostars. The thermal gas pressure and gravitational
collapse are believed to be the primary agents governing this process, referred to as the thermal Jeans fragmentation. However,the contributions of other factors (such as magnetic fields and turbulence) to the fragmentation process remain less explored. In
this work, we have tested possible fragmentation mechanisms by estimating the mean core mass and mean inter-core separationof the B213 filament. We have used the ⇠14" resolution James Clerk Maxwell Telescope (JCMT) Submillimetre Common-User
Bolometer Array 2 (SCUBA-2)/POL-2 850 µm dust continuum map and combined it with a Planck 850 µm map and Herscheldata. We find that in addition to the thermal contribution, the presence of ordered magnetic fields could be important in the
fragmentation of the B213 filament.

A panoptic view of the Taurus molecular cloud I. The cloud dynamics revealed by gas
emission and 3D dust

J. D. Soler, C. Zucker, J. E. G. Peek, M. Heyer, P. F. Goldsmith, S. C. O. Glover, S. Molinari, R. S. Klessen,
P. Hennebelle, L. Testi, T. Colman, M. Benedettini, D. Elia, C. Mininni, S. Pezzuto, E. Schisano, A. Traficante
F We present a study of the three-dimensional (3D) distribution of interstellar dust derived from stellar extinction observations
toward the Taurus molecular cloud (MC) and its relation with the neutral atomic hydrogen (HI) emission at 21 cm wavelength
1213
and the carbon monoxide CO and CO emission in the J = 1 ! 0 transition. We used the histogram of oriented gradients(HOG) method to match the morphology in a 3D reconstruction of the dust density (3D dust) and the distribution of the gas
tracers’ emission. The result of the HOG analysis is a map of the relationship between the distances and radial velocities. The
HOG comparison between the 3D dust and the HI emission indicates a morphological match at the distance of Taurus but
an anti-correlation between the dust density and the HI emission, which uncovers a significant amount of cold HI within the
Taurus MC. The HOG between the 3D dust and 12 CO reveals a pattern in radial velocities and distances that is consistent
with converging motions of the gas in the Taurus MC, with the near side of the cloud moving at higher velocities and the far
side moving at lower velocities. This convergence of flows is likely triggered by the large-scale gas compression caused by theinteraction of the Local Bubble and the Per-Tau shell, with Taurus lying at the intersection of the two bubble surfaces.

A
panoptic
view
of
the
Taurusmolecular
cloud
I.
The
cloud
dynamics
revealedbygas
46
emission and 3D dust

J. D. Soler, C. Zucker, J. E. G. Peek, M. Heyer, P. F. Goldsmith, S. C. O. Glover, S. Molinari, R. S. Klessen,
P. Hennebelle, L. Testi, T. Colman, M. Benedettini, D. Elia, C. Mininni, S. Pezzuto, E. Schisano, A. Traficante
F We present a study of the three-dimensional (3D) distribution of interstellar dust derived from stellar extinction observations
toward the Taurus molecular cloud (MC) and its relation with the neutral atomic hydrogen (HI) emission at 21 cm wavelengthand the carbon monoxide 12 CO and 13 CO emission in the J = 1 ! 0 transition. We used the histogram of oriented gradients(HOG) method to match the morphology in a 3D reconstruction of the dust density (3D dust) and the distribution of the gas
tracers’ emission. The result of the HOG analysis is a map of the relationship between the distances and radial velocities. The
HOG comparison between the 3D dust and the HI emission indicates a morphological match at the distance of Taurus but
an anti-correlation between the dust density and the HI emission, which uncovers a significant amount of cold HI within the
12
Taurus MC. The HOG between the 3D dust and CO reveals a pattern in radial velocities and distances that is consistent
with converging motions of the gas in the Taurus MC, with the near side of the cloud moving at higher velocities and the far
side moving at lower velocities. This convergence of flows is likely triggered by the large-scale gas compression caused by theinteraction of the Local Bubble and the Per-Tau shell, with Taurus lying at the intersection of the two bubble surfaces.

Broadband VLA Spectral Line Survey of a Sample of Ionized Jet Candidates

E. Sanchez-Tovar, E. D. Araya, V. Rosero, P. Hofner, S. Kurtz F The study of the interaction between ionized jets,
molecular outflows and their environments is critical to understanding high-mass star formation, especially because jets andoutflows are thought to be key in the transfer of angular momentum outwards from accretion disks. We report a low-spectral
resolution VLA survey for hydrogen radio recombination lines, OH, NH3 , and CH3 OH lines toward a sample of 58 high-massstar forming regions that contain numerous ionized jet candidates. The observations are from a survey designed to detect
radio continuum; the novel aspect of this work is to search for spectral lines in broadband VLA data (we provide the script
developed in this work to facilitate exploration of other datasets). We report detection of 25 GHz CH3 OH transitions toward
ten sources; five of them also show NH3 emission. We found that most of the sources detected in CH3 OH and NH3 have beenclassified as ionized jets or jet candidates and that the emission lines are coincident with, or very near (. 0.1 pc) these sources,
hence, these molecular lines could be used as probes of the environment near the launching site of jets/outflows. No radio47 Broadband VLA Spectral Line Survey of a Sample of Ionized Jet Candidates

E. Sanchez-Tovar, E. D. Araya, V. Rosero, P. Hofner, S. Kurtz F The study of the interaction between ionized jets,
molecular outflows and their environments is critical to understanding high-mass star formation, especially because jets andoutflows are thought to be key in the transfer of angular momentum outwards from accretion disks. We report a low-spectral
resolution VLA survey for hydrogen radio recombination lines, OH, NH3 , and CH3 OH lines toward a sample of 58 high-massstar forming regions that contain numerous ionized jet candidates. The observations are from a survey designed to detect
radio continuum; the novel aspect of this work is to search for spectral lines in broadband VLA data (we provide the script
developed in this work to facilitate exploration of other datasets). We report detection of 25 GHz CH3 OH transitions toward
ten sources; five of them also show NH3 emission. We found that most of the sources detected in CH3 OH and NH3 have beenclassified as ionized jets or jet candidates and that the emission lines are coincident with, or very near (. 0.1 pc) these sources,
hence, these molecular lines could be used as probes of the environment near the launching site of jets/outflows. No radio
recombination lines were detected, but we found that the RMS noise of stacked spectra decreases following the radiometerequation. Therefore, detecting radio recombination lines in a sample of brighter free-free continuum sources should be possible.
This work demonstrates the potential of broadband VLA continuum
observations as low-resolution spectral line scans.
14Planetesimal formation at the gas pressure bump following a migrating planet II. Eﬀects
of dust growth

Yuhito Shibaike, Yann Alibert F Planetesimal formation is still mysterious. One of the ways to form planetesimals is to
invoke a gas pressure bump in a protoplanetary disc. In our previous paper, we propose a new scenario in which the piled-up dust
at a gas pressure bump created by a migrating planet form planetesimals by streaming instability in a wide region of the disc as
the planet migrates inward. In this work, we consider the global time evolution of dust and investigate the detailed conditions
and results of the planetesimal formation in our scenario. We use a 1D grid single-sized dust evolution model, which can follow
the growth of the particles by their mutual collision and their radial drift and diﬀusion. We calculate the time-evolution of theradial distribution of the peak mass and surface density of the dust in a gas disc perturbed by an embedded migrating planet
and investigate if the dust satisfies the condition for planetesimal formation. We find that planetesimals form in a belt-likeregion between the snowline and the position where the planet reaches its pebble-isolation mass when the strength of turbulence
is 10 4  ↵  10 3 , which is broadly consistent with observed value. The mechanism of the formation, streaming instability or
mutual collision, depends on the timescale of the streaming instability. The total mass of planetesimals also depends on ↵ andThis work demonstrates the potential of broadband VLA continuum observations as low-resolution spectral line scans.

48 Planetesimal formation at the gas pressure bump following a migrating planet II. Eﬀects

of dust growth

Yuhito Shibaike, Yann Alibert F Planetesimal formation is still mysterious. One of the ways to form planetesimals is to
invoke a gas pressure bump in a protoplanetary disc. In our previous paper, we propose a new scenario in which the piled-up dust
at a gas pressure bump created by a migrating planet form planetesimals by streaming instability in a wide region of the disc as
the planet migrates inward. In this work, we consider the global time evolution of dust and investigate the detailed conditions
and results of the planetesimal formation in our scenario. We use a 1D grid single-sized dust evolution model, which can follow
the growth of the particles by their mutual collision and their radial drift and diﬀusion. We calculate the time-evolution of theradial distribution of the peak mass and surface density of the dust in a gas disc perturbed by an embedded migrating planet
and investigate if the dust satisfies the condition for planetesimal formation. We find that planetesimals form in a belt-likeregion between the snowline and the position where the planet reaches its pebble-isolation mass when the strength of turbulence
is 10 4  ↵  10 3 , which is broadly consistent with observed value. The mechanism of the formation, streaming instability or
mutual collision, depends on the timescale of the streaming instability. The total mass of planetesimals also depends on ↵ andis about 30 100 ME if the planetary core has already existed at the beginning and grows by gas accretion, but it decreases
as the timing of the formation of the planetary core is later. We also provide simple approximate expressions of the surface
density and total mass of the planetesimals and find that the total mass strongly depends on the dust mass. We show thatplanetesimals form in a belt-like region by the combination of the dust pile-up at the gas pressure bump formed by a planet
and its inward migration.

Anisotropic Ionizing Illumination from an M-type Pre-main Sequence Star, DM Tau

Yuka Terada, Hauyu Baobab Liu, David Mkrtichian, Jinshi Sai, Mihoko Konishi, Ing-Guey Jiang, Takayuki
Muto, Jun Hashimoto, Motohide Tamura F The powerful, high-energy magnetic activities of young stars play importantroles in the magnetohydrodynamics in the innermost parts of the protoplanetary disks. In addition, the associated UV and
X-ray emission dictates the photochemistry; moreover, the corona activities can aﬀect the atmosphere of a newborn extra-solar
planet. How the UV and X-ray photons are generated, and how they illuminate the disks, are not well understood. Here
we report the analyses of the optical and infrared (OIR) photometric monitoring observations and the high angular-resolution
centimeter band images of the low-mass (M1 type) pre-main sequence star, DM Tau. We found that the OIR photometric light50 A Chondritic Solar Neighborhood

Isabella L. Trierweiler, Alexandra E. Doyle, Edward D. Young F A persistent question in exoplanet demographics
is whether exoplanetary systems form from similar compositional building blocks to our own. Polluted white dwarf stars oﬀer
a unique way to address this question as they provide measurements of the bulk compositions of exoplanetary material. We
present a statistical analysis of the rocks polluting oxygen-bearing white dwarfs and compare their compositions to rocks in
the Solar System. We find that the majority of the extrasolar rocks are consistent with the composition of typical chondrites.
Measurement uncertainties prevent distinguishing between chondrites and bulk Earth, but do permit detecting the diﬀerences
between chondritic compositions and basaltic or continental crust. We find no evidence of crust amongst the polluted whitedwarfs. We show that the chondritic nature of extrasolar rocks is also supported by the compositions of local stars. Whilegalactic chemical evolution results in variations in the relative abundances of rock-forming elements spatially and temporally
on galaxy-wide scales, the current sample of polluted white dwarfs are suﬃciently young and close to Earth that they are notaﬀected by this process. We conclude that exotic compositions are not required to explain the majority of observed rock types
around polluted white dwarfs, and that variations between exoplanetary compositions in the stellar neighborhood are generally
not due to significant diﬀerences in the initial composition of protoplanetary disks. Nonetheless, there is evidence from stellar
observations that planets formed in the first several billion years in the Galaxy have lower metal core fractions compared with
Earth on average.

15

51 Excited Hydroxyl Outflow in the High-Mass Star-Forming Region G34.26+0.15

W. S. Tan, E. D. Araya, C. Rigg, P. Hofner, S. Kurtz, H. Linz, V. Rosero F G34.26+0.15 is a region of high-massstar formation that contains a broad range of young stellar objects in diﬀerent stages of evolution, including a hot molecularcore, hyper-compact HII regions and a prototypical cometary ultra-compact HII region. Previous high-sensitivity single dishobservations by our group resulted in the detection of broad 6035 MHz OH absorption in this region; the line showed a significant
blue-shifted asymmetry indicative of molecular gas expansion. We present high-sensitivity Karl G. Jansky Very Large Array(VLA) observations of the 6035 MHz OH line conducted to image the absorption and investigate its origin with respect to thediﬀerent star formation sites in the region. In addition, we report detection of 6030 MHz OH absorption with the VLA andfurther observations of 4.7 GHz and 6.0 GHz OH lines obtained with the Arecibo Telescope. The 6030 MHz OH line shows avery similar absorption profile as the 6035 MHz OH line. We found that the 6035 MHz OH line absorption region is spatiallyunresolved at ⇠ 2" scales, and it is coincident with one of the bright ionized cores of the cometary HII region that shows
broad radio recombination line emission. We discuss a scenario where the OH absorption is tracing the remnants of a pole-on
molecular outflow that is being ionized inside-out by the ultra-compact HII region.

X-Shooting ULLYSES: massive stars at low metallicity. I. Project Description

Jorick S. Vink and the ULLYSES Team F Observations of individual massive stars, super-luminous supernovae, gammaray bursts, and gravitational-wave events involving spectacular black-hole mergers, indicate that the low-metallicity Universe
is fundamentally diﬀerent from our own Galaxy. Many transient phenomena will remain enigmatic until we achieve a firm
understanding of the physics and evolution of massive stars at low metallicity (Z). The Hubble Space Telescope has devoted
500 orbits to observe 250 massive stars at low Z in the ultraviolet (UV) with the COS and STIS spectrographs under the
ULLYSES program. The complementary “X-Shooting ULLYSES” (XShootU) project provides enhanced legacy value withhigh-quality optical and near-infrared spectra obtained with the wide-wavelength coverage X-shooter spectrograph at ESO’s
Very Large Telescope. We present an overview of the XShootU project, showing that combining ULLYSES UV and XShootU
optical spectra is critical for the uniform determination of stellar parameters such as eﬀective temperature, surface gravity,
luminosity, and abundances, as well as wind properties such as mass-loss rates in function of Z. As uncertainties in stellar andwind parameters percolate into many adjacent areas of Astrophysics, the data and modelling of the XShootU project is expected
to be a game-changer for our physical understanding of massive stars at low Z. To be able to confidently interpret James Webb

molecular outflow that is being ionized inside-out by the ultra-compact HII region.

52 X-Shooting ULLYSES: massive stars at low metallicity. I. Project Description

Jorick S. Vink and the ULLYSES Team F Observations of individual massive stars, super-luminous supernovae, gammaray bursts, and gravitational-wave events involving spectacular black-hole mergers, indicate that the low-metallicity Universe
is fundamentally diﬀerent from our own Galaxy. Many transient phenomena will remain enigmatic until we achieve a firm
understanding of the physics and evolution of massive stars at low metallicity (Z). The Hubble Space Telescope has devoted
500 orbits to observe 250 massive stars at low Z in the ultraviolet (UV) with the COS and STIS spectrographs under the
ULLYSES program. The complementary “X-Shooting ULLYSES” (XShootU) project provides enhanced legacy value withhigh-quality optical and near-infrared spectra obtained with the wide-wavelength coverage X-shooter spectrograph at ESO’s
Very Large Telescope. We present an overview of the XShootU project, showing that combining ULLYSES UV and XShootU
optical spectra is critical for the uniform determination of stellar parameters such as eﬀective temperature, surface gravity,
luminosity, and abundances, as well as wind properties such as mass-loss rates in function of Z. As uncertainties in stellar andwind parameters percolate into many adjacent areas of Astrophysics, the data and modelling of the XShootU project is expected
to be a game-changer for our physical understanding of massive stars at low Z. To be able to confidently interpret James Webb
Space Telescope (JWST) spectra of the first stellar generations, the individual spectra of low Z stars need to be understood,
which is exactly where XShootU can deliver.

A high-resolution extinction mapping technique for face-on disc galaxies

Helena Faustino Vieira, Ana Duarte-Cabral, Timothy A. Davis, Nicolas Peretto, Matthew W. L. Smith, MiguelQuerejeta, Dario Colombo, Michael Anderson F We present a new dust extinction technique with which we are able toretrieve parsec-scale gas surface density maps for entire nearby galaxies. The method measures the dust attenuation in opticalbands on a pixel-by-pixel basis against a smoothed, reconstructed stellar distribution. The contribution of foreground light along
the line-of-sight is calibrated using dust emission observations, assuming that the dust sits in a layer close to the mid-plane of
the face-on galaxy. Here, we apply this technique to M51 (NGC 5194) as a proof-of-concept, obtaining a resolution of 0.14" (5pc). Our dust (and gas) surface density map is consistent with independent dust- and CO-based studies at lower resolution. We
find that discrepancies between our estimates of surface density and other studies stem primarily from the choice of dust model(i.e. diﬀerent dust absorption coeﬃcients). When assuming the same dust opacity law, our technique produces surface densities
that are consistent with independent studies. This dust extinction technique provides us with gas surface density maps at anwhich is exactly where XShootU can deliver.

53 A high-resolution extinction mapping technique for face-on disc galaxies

Helena Faustino Vieira, Ana Duarte-Cabral, Timothy A. Davis, Nicolas Peretto, Matthew W. L. Smith, MiguelQuerejeta, Dario Colombo, Michael Anderson F We present a new dust extinction technique with which we are able toretrieve parsec-scale gas surface density maps for entire nearby galaxies. The method measures the dust attenuation in opticalbands on a pixel-by-pixel basis against a smoothed, reconstructed stellar distribution. The contribution of foreground light along
the line-of-sight is calibrated using dust emission observations, assuming that the dust sits in a layer close to the mid-plane of
the face-on galaxy. Here, we apply this technique to M51 (NGC 5194) as a proof-of-concept, obtaining a resolution of 0.14" (5pc). Our dust (and gas) surface density map is consistent with independent dust- and CO-based studies at lower resolution. We
find that discrepancies between our estimates of surface density and other studies stem primarily from the choice of dust model(i.e. diﬀerent dust absorption coeﬃcients). When assuming the same dust opacity law, our technique produces surface densities
that are consistent with independent studies. This dust extinction technique provides us with gas surface density maps at an
unprecedented resolution for full disc coverage studies of nearby galaxies. The resulting well-resolved spatial information opens
the possibility for more in-depth examination of the influence of large-scale dynamics (and also stellar feedback mechanisms)
on the interstellar medium at parsec-scales, and consequently star formation in nearby galaxies.

54 BEAST detection of a brown dwarf and a low-mass stellar companion around the young

bright B star HIP 81208

Gayathri Viswanath, Markus Janson, Raﬀaele Gratton, Vito Squicciarini, Laetitia Rodet, Simon C. Ringqvist,
Eric E. Mamajek, Sabine Reﬀert, Gaël Chauvin, Philippe Delorme, Arthur Vigan, Mickaël Bonnefoy, Natalia
Engler, Silvano Desidera, Thomas Henning, Janis Hagelberg, Maud Langlois, Michael Meyer F Recent observations from B-star Exoplanet Abundance Study (BEAST) have illustrated the existence of sub-stellar companions around very
massive stars. In this paper, we present the detection of two lower mass companions to a relatively nearby (148.7+1.5
1.3 pc),young (17+34 Myr), bright (V=6.632 ± 0.006 mag), 2.58 ± 0.06 M B9V star HIP 81208 residing in the Sco-Cen association,using the Spectro-Polarimetric High-contrast Exoplanet REsearch (SPHERE) instrument at the Very Large Telescope (VLT) in+6+0.010Chile. Analysis of the photometry obtained gives mass estimates of 67 7 MJ for the inner companion and 0.135 0.013 M forthe outer companion, indicating the former to be most likely a brown dwarf and the latter to be a low-mass star. The system
is compact but unusual, as the orbital planes of the two companions are likely close to orthogonal. The preliminary orbital
solutions we derived for the system indicate that the star and the two companions are likely in a Kozai resonance, rendering
the system dynamically very interesting for future studies.

Dynamical detection of a companion driving a spiral arm in a protoplanetary disk

Chen Xie, Bin B. Ren, Ruobing Dong, Élodie Choquet, Arthur Vigan, Jean-François Gonzalez, Kevin Wagner,
Taotao Fang, Maria Giulia Ubeira-Gabellini F Radio and near-infrared observations have observed dozens of protoplanetary disks that host spiral arm features. Numerical simulations have shown that companions may excite spiral density waves
in protoplanetary disks via companion-disk interaction. However, the lack of direct observational evidence for spiral-driving
companions poses challenges to current theories of companion-disk interaction. Here we report multi-epoch observations of
the binary system HD 100453 with the Spectro-Polarimetric High-contrast Exoplanet REsearch (SPHERE) facility at the Very
Large Telescope. By recovering the spiral features via robustly removing starlight contamination, we measure spiral motion
across 4 yr to perform dynamical motion analyses. The spiral pattern motion is consistent with the orbital motion of theeccentric companion. With this first observational evidence of a companion driving a spiral arm among protoplanetary disks,
we directly and dynamically confirm the long-standing theory on the origin of spiral features in protoplanetary disks. With thefor hidden spiral-arm-driving planets that are beyond the detection of existing ground-based high-contrast imagers.

56 Direct observational evidence of the multi-scale, dynamical mass accretion toward ahigh-mass star forming hub-filament system

Dongting Yang, Hong-Li Liu, Anandmayee Tej, Tie Liu, Patricio Sanhueza, Sheng-Li Qin, Xing Lu, Ke Wang,
Sirong Pan, Feng-Wei Xu, Enrique Vazquez-Semadeni, Shanghuo Li, Gilberto C. Gomez, Aina Palau, Guido
Garay, Paul F. Goldsmith, Mika Juvela, Anindya Saha, Leonardo Bronfman, Chang Won Lee, Kenichi Tatematsu, Lokesh Dewangan, Jianwen Zhou, Yong Zhang, Amelia Stutz, Chakali Eswaraiah, L. Viktor Toth, Isabelle
Ristorcelli, Xianjin Shen, Anxu Luo, James O. Chibueze F There is growing evidence that high-mass star formationand hub-filament systems (HFS) are intricately linked. The gas kinematics along the filaments and the forming high-massstar(s) in the central hub are in excellent agreement with the new generation of global hierarchical high-mass star formation
models. In this paper, we present an observational investigation of a typical HFS cloud, G310.142+0.758 (G310 hereafter)
which reveals unambiguous evidence of mass inflow from the cloud scale via the filaments onto the forming protostar(s) at the
hub conforming with the model predictions. Continuum and molecular line data from the ATOMS and MALT90 surveys areused that cover diﬀerent spatial scales. Three filaments (with total mass 5.7 ± 1.1 ⇥ 103 M ) are identified converging toward
the central hub region where several signposts of high-mass star formation have been observed. The hub region contains a
massive clump (1280 ± 260 M ) harbouring a central massive core. Additionally, five outflow lobes are associated with thecentral massive core implying a forming cluster. The observed large-scale, smooth and coherent velocity gradients from thecloud down to the core scale, and the signatures of infall motion seen in the central massive clump and core, clearly unveil anearly-continuous, multi-scale mass accretion/transfer process at a similar mass infall rate of ⇠ 10 3 M yr 1 over all scales,feeding the central forming high-mass protostar(s) in the G310 HFS cloud.

Substructures in Compact Disks of the Taurus Star-forming Region

Shangjia Zhang, Matt Kalscheur, Feng Long, Ke Zhang, Deryl E. Long, Edwin A. Bergin, Zhaohuan Zhu, Leon
Trapman F Observations of substructure in protoplanetary disks have largely been limited to the brightest and largest disks,
excluding the abundant population of compact disks which are likely sites of planet formation. Here, we reanalyze 0.1”, 1.33
mm ALMA continuum observations of 12 compact protoplanetary disks in the Taurus star-forming region. By fitting visibilities
directly, we identify substructures in 6 of the 12 compact disks. We then compare the substructures identified in the full Taurus
sample of 24 disks in single star systems and the ALMA DSHARP survey, diﬀerentiating between compact (Ref f ,90% < 50 au)

58

Porous Dust Particles in Protoplanetary Disks: Application to the HL Tau Disk

Shangjia Zhang, Zhaohuan Zhu, Takahiro Ueda, Akimasa Kataoka, Anibal Sierra, Carlos Carrasco-González,Enrique Macías F Dust particle sizes constrained from dust continuum and polarization observations by radio interferometry
are inconsistent by at least an order of magnitude. Motivated by porous dust observed in small Solar System bodies (e.g., fromthe Rosetta mission), we explore how the dust particle’s porosity aﬀects the estimated particle sizes from these two methods.
Porous particles have lower refractive indices, which aﬀect both opacity and polarization fraction. With weaker Mie interference
patterns, the porous particles have lower opacity at mm wavelengths than the compact particles if the particle size exceeds
several hundred microns. Consequently, the inferred dust mass using porous particles can be up to a factor of six higher. The
most significant diﬀerence between compact and porous particles is their scattering properties. The porous particles have awider range of particle sizes with high linear polarization from dust self-scattering, allowing mm-cm-sized particles to explain
polarization observations. With a Bayesian approach, we use porous particles to fit HL Tau disk’s multi-wavelength continuum
and mm-polarization observations from ALMA and VLA. The moderately porous particles with sizes from 1 mm-1 m can explain
both continuum and polarization observations, especially in the region between 20-60 au. If the particles in HL Tau are porous,
the porosity should be from 70% to 97% from current polarization observations. We also predict that future observations of theself-scattering linear polarization at longer wavelengths (e.g., ALMA B1 and ngVLA) have the potential to further constrain
the particle’s porosity and size.