HD142527’s morphology
d=140pc, M=1.9+-0.3Msun
10-140AUにgap
outer disk : 140-300AU

SED (Acke and Ancker 2004)

UKAGAWA ET AL.

ferenceas thatach refer mask
n order
imagesxposureframe.
mes toFor thento one
tain theframes
xistencemaging,ce stars.
for 1!.0

F packd pixel
circum-H-band (Fukagawa et al. 2006)

Vol. 636

24.5μm (Fujiwara et al. 2006)

comparison between images of 24.5μm (Fujiwara
SK AROUND HD 142527
L135et al. 2006) and H-band (Fukagawa et al. 2006)

Fig. 3.—Central-component-subtracted 24.5 mm image of HD 142527(color) and H-band scattered light image with CIAO (contour). The color bar
to the right is in the units of Jy arcsec!2.

L136
WARA ET AL.

T AL.

orso

Disk model (Fujiwaraetal.
2006)
FUJIWARA ET AL.
Vol. 644
中間赤外(24.5μm)

Vol. 644

近赤外(H-band 1.65μm)

Vol. 644

高温度rimが隠れる
Fig. 4.—Colorview
and ofpositionof theeastern
and westernarcs.
Fig. 5.—Schematicthe modelof theHD 142527
system.
TheThegap color
profilescalculatedbyusing
theemissivityof
astronomicalsilicateare also
between the inner and outer disks exists at r p 80–170 AU.
plotted with the solid lines.

Fig. 5.—Schematic view of the model of the HD 142527 system. The gap
between the inner and outer disks exists at r p 80–170 AU.

scattering, resulting in the observed asymmetry in the NIR. An
scattering, resulting in the observed asymmetry in the NIR. An
axial symmetric disk inclined to the east-west direction is alsoof HD
142527 by CIAO show that the western side of the
高温度rimが見える
L154
FUKAGAWAET AL.the symmetric structure
636
axial symmetric disk inclined to the east-west
direction is also
後方散乱(暗い)consistentwithof theVol.
extendeddisk
前方散乱(明るい)heextended disk is brighter than the eastern side by 2.0 mag
consistent with the symmetric structure of the extended disk
tracedg(Fukagawa et al. 2006). The 850 neutral
mm density
continuum
observations
filters for theAO (both HD 142527 andreferenceby 850 mm radiation. It is not necessary to consider antracedby850mm
radiation.
Itisnotnecessarytoconsider
anwere istoo thoughtbright for thetoAO)
obtain similar PSFsas thataxial
asymmetric material distribution such as a circumbinary
nsby Submillimeter Array (SMA), stars
which
betotime
optiof
HD142527.
The
total
exposure
was660sfor
each
refaxial asymmetric material distribution such as a circumbinary
diskmask
to account for the observations.
ically thin to dust emission and a goodof theimages
totalwereamounterencetracer
star. The K-band
obtained with a smaller
disk to account for the observations. of 0!.6 diameter in addition to the images with a 1!.0 one, inDetails
orderof the appearance of a protoplanetary disk, including antof dust, show an east-west symmetricstructureof theextended
toconfirm
theinnerholethatwedetected
intheH-band
images
Details of the appearance of a protoplanetary disk, including a“peculiar horseshoe-like feature” for models with an inclinationed
disk (N. Ohashi et al. 2006, in preparation).
To explain
taken on the night before.
For the 1!.0thesemask images, the exposure“peculiar
horseshoe-likefeature”
formodelswithaninclination
timeinwaswhich
3 s, and two
exposures
wereco-addedinto ofone 30!,frame. were predicted in simulations of Kessel et al. (1998). A
seobservations, we propose a model
thedustdisk
isTheKessel
seeing condition
worse, Aand we chose 27 frames toof 30!, were predicted in simulations ofet al. was(1998).
model 12 mm intensity map in their paper shows a morphology
isgeometrically thick and inclined produce
as thetheeastern
final imagesideamongisthefarther
obtained 110 frames. For themodel 12 mm intensity map in their papershows
asixmorphology
strikingly
similar to our images of the outer disk of HD 142527.
0!.6 mask
images,exposuresofdisk
1 s wereco-added
into oneer
to us and the inner rim of the eastern
sideoftheouterwas
isIn order
frame,
anda
totalof60
framestaken.
toobtain
thestrikingly similar to our images of the outer disk of HD 142527.
NIR interferometric observations of LkHa 101 show that an asymis
exposed to us. Figure 5 shows a schematic
viewasofthatthe
modelsame spatial resolutionof theH band, only seven frames
NIR interferometric observations of LkHa
101showthatan asymusable.
It was,however,
to confirm themetric
existencearclike radiation component is present in addition to aelof the HD 142527 system. Sincewere
theinneredge
andsufficient
rimasareofpresent
the inner hole.
Inthe same manner
for the H-band imaging,
metricarclikeradiation
component
isinadditiontoa
central compact component (Tuthill et al. 2002). In the case ofre
hottest within the outer disk andwe affectthe137785
MIRandbrightness
observed HD
HD 145191 as PSF reference stars.
central images
compact(Tuthillet Theal.total2002).
Intimetheof caseofwas 240 and 840LkHaFig. 1.—Observedof HDcomponent
142527
panels)andcentral-componentss
exposure
PSF stars
s for 1!.0101, the asymmetric arclike structure is thought to be atmost strongly,
the (leftemittingregionof theouterdisk
appears
and0!
.
6
mask
imaging,
respectively.
btracted
imagesofHD
142527(rightpanels).
These
imagesarein
18.8mm(top)
LkHa 101, the asymmetric arclike structure is thought
to be attributed to the hot dust within the inner rim of the inner hole maders!2imageswe
likeThea narrow
ring.
Therefore,
the ofopticaldepthTheobtained
werementioned
first processed using the IRAF packd 24.5 mm tributed(bottom).
colorbars
totherightareintheunits
Jyarcsec.
to the hot dust within the inner rimof dark
the innerhole
made with sky flats,byed
agestofor
subtraction,flat-fielding
baddustpixelsublimation. Although the observed spatial scale and waveabove does not directly correspondthe verticaldepthof theGemini + FARGO (Casassus et al. 2012, ApJ)
The Astrophysical Journal Letters, 754:L31 (5pp), 2012 August 1

Casassus et al.

The Astrophysical Journal Letters, 754:L31 (5pp), 2012 August 1

1aaTpoc
Tt

1
41
3

22

Figure 2. Annotations on the H2 (1–0)S(1) image also shown on Figure 1. In red
we indicate the spiral arms we could identify, with red identification numbers.
The green numbers indicate the positions of the two intensity nulls, or gaps,along the ring. The blue box surrounds the position of the knot.
(A color version of this figure is available in the online journal.)

Figure 3. Upper limits on the Ks magnitude of HD 142527b. Axis labels are asfor Figure 1. In (a) we show the collapsed SINFONI data cube, as produced by
the pipeline, but divided by an azimuthal average chosen to highlight the PSF
pattern. In (b) we show the collapsed image of the spectrally deconvolved andPSF-subtracted data cube, with a linear intensity scale stretching from −0.75
to 0.57, in counts, where the maximum number of counts in the collapsed cube
(shown in (a)) is 548. The root-mean-square dispersion of the counts in anannulus from 0.2 to 0.3 arcsec is 9.610−2 , or a 3σ lower limit to the flux ratioof 1905. Using a separate PSF standard, this residual rms value is 0.19, givinga 3σ lower limit to the flux ratio of 966.

age, which would imply a mass of less than 12 Mjup given thisFigure the4. FARGOof aand
10 M
planet embedded
in a 0.1 M! disk.
jupmodelsMK limit. However,age of simulation
HD 142527
theareThe spatial axes are in AU. The color scale represents the surface density in
not precise enoughto ascertain this upper limit mass value. We
a logarithmic ramp in FARGO code units in which 10−5 equals 88 g cm−2 .
stress again thatthisthelimit
constrains
thetopresenceof ofmassive
Noticestellarshift relative
the position
the cavity centroid of ∼16 AU.
gaseous giants at stellocentric radii of 14–35 AU.
(A color version of this figure is available in the online journal.)!!

this source is located at a separation of 5. 44 from HD 142527,
and a P.A. of 220 deg (east of north).
The inner radius of the ring varies from 0.!! 7 to the north,to about 1.!! 0 to the south, and a projection effect is discardedsince the central star is clearly offset by 0.!! 17 ± 0.!! 02 fromthe center of this approximate ellipse. This offset was first
noted by Fukagawa et al. (2006), albeit at lower angularresolution.
In K band the west side of the rim we see is brighter, inagreement with Fukagawa et al. (2006). Fujiwara et al. (2006)
and Verhoeff et al. (2011) already noted that in the thermal IR,
N, and Q bands, it is the eastern side that is brightest, whichis consistent with a projection effect (Fujiwara et al. 2006).

4. ANALYSIS
4.1. Arguments in Favor of a Planet-createdGap for HD
142527 with FARGO. Our goal here is nothydrodynamicsimulations

90AUにおかれたM=10Mjup
でgapは説明可能
tofit
but to verifytoqualitatively
the tenability of thisThe contribution thefromdata
photoevaporation
cavity clearing
scenario
forcase.
HD 142527.
a dedicatedgrid-based twocan be neglectedin thisThe innerFARGO
disk, theislarge
gap,dimensional
availableon2006)
the web (Masset 2000),
and the vigorous
accretioncode
rate publicly(Garcia Lopezet al.
of 7 × 10−8 andM$ specificallyyr−1 argue against
photoevaporation.
designedfor planet–diskAninteractions. The run
X-ray-driven presented
wind can indeed
explaina subsetof the observedin thisLetter
corresponds
to a system evolution
accreting disksequivalent
with inner holes,
but
only
thosewithradii
smaller
to 1.7 Myr.
than 20 AU and We
accretion
ratescommon
less than fiducial
10−8 M$ parameters
yr−1 (Owen for the model, aspicked
et al. 2011).

etta&W
pooosclaoasta

00.1

0.20.32

Angular position north (arcsec)

2a10–1

b–22CO1100–1–1

Continuum–2
2–2c2d1

100–1

–1

2 μm

–22HCO+
10–1–2 2
1
Angular position east (arcsec)–20–1–2ALMACasassus
et al. 2013

00.1

0.2
0.3
345GHz(Casassuset al. 2013)
22ab

10–1

360 mJy/beam
1 mJy/beam

1→1mmのダスト面密度に300倍以上の比

0North-South specificintensity ratio = 28+-0.5–1–22Continuum

cdgap-crossing filament

COCO(3-2) (Casassus et al. 2013)
2b10–1–2COgapの内側でピーク

2 filament付近でピーク白コントア：intensity

RESEARCH SUPPLEMENTARY INFORMATION

10–1–22

色：速度HCO+(4-3) (Casassusetal.
2013)
0
Blueとredのピーク位置のズレ0.2” = inner disk の半径ぐらい
Blue : 奥から手前＝星に向かう方向–1

exposed rim (たぶん) 及びSUPPLEMENTARY INFORMATION
gap-crossingRESEARCH
filamentでHCO+が受かった。

–22d

奥

白コントア：intensity
10–1

手前
HCO+
–2 2–2
10–1–2

色：速度(右図)

HCO+(4-3) (Casassus et al. 2013)
dust continuumは非対称性が見えるがHCO+はリング状に見える

indicated by the exact overlap with the channel boundaries. Countours indicate
LSR velocity, with colour codes that match b). d: RGBSUPPLEMENTARY
intensity image,with theINFORMATIONRESEARCH

緑:Kepler回転

Keplerian velocities ( 1 ≤ v/km s−1 ≤ 5.9) in green, and the high velocity flows
in red (11.5 > v/km s−1 > 5.9) and blue (1 > v/km s−1 > −4). e: Peak intensity

igure S7 HCO+ (4-3) maps. Axis labels for images are in arcsec; North is up,

イメージ図0PROTOPLANETARY DISK AROUND
HD 142527–1 24.5μmとHCO+のintensityのピークはだいたい同じ位置→exposed rimだろう–22d

10–1

HCO+

21n east (arcsec)–20–1–2Fig. 3.—Central-component-subtracted 24.5 mm image of HD 1(color) and H-band scattered light image with CIAO (contour). The co
1 of Jy arcsec!2.
the right is inunits(4–3) line
upplementary Fig. 1 for an overlay with thetocontinuum.
d, theHCO

K AROUND HD 142527

L135–22d124.5μmとHCO+のintensityのピークはだ
いたい同じ位置

0–1

HCO+–2 2–2
10–1–2Fig. 3.—Central-component-subtracted 24.5 mm image of HD 142527(color) and H-band scattered light image with CIAO (contour). The color bar
to the right is in the units of Jy arcsec!2.

→exposed rimだろうへその緒East(HCO+で明るい、Blueshift)
ダストcontinuum

へその緒Westが超明るい(HCO+で明るい、Redshift)

奥inner disk

手前

exposed rim (MIRとHCO+で明るい)

前方散乱(NIR散乱
光で明るい)

回転

gas inflowの見積もり
下限値 : filamentのfluxから見積もったfilament mass
HCO+(4-3)のcritical density ~10^6 cm^-3
filament density >~10^6inflow velocity ~ 5km/s
filament area ~ 0.25*0.25 arcsec^2->Mdot > 7*10^-9 Msun/yr
上限値 : dust continuumから見積もったfilament mass
dust continuumで全体のフラックスに対してfilament fluxは1/1000→disk mass が0.1Msunなので、filament mass は10-^4Msun
characteristic radial velocity<1km/s (not observed), size 100AU →dynamical age offilament mass>474yr→Mdot<2*10^-7Msun

たぶん説明しなければならないこと
・円環内で30倍程度の1mmダスト面密度の差が必要
・gapをあけるメカニズム(本当に10木星一つでいいの？)
・惑星を介した降着流の理論