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

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 (FujiwaraSK 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

Disk model (Fujiwaraet al. 2006)
FUJIWARA ET AL.

Fig. 4.—Color and position of the eastern and western arcs. The color
profiles calculated by using the emissivity of astronomical silicate are alsoplotted with the solid lines.

of HD 142527 by CIAO show that the western side of theextended disk is brighter than the eastern side by 2.0 mag(Fukagawa et al. 2006). The 850 mm continuum observations
by Submillimeter Array (SMA), which is thought to be optically thin to dust emission and a good tracer of the total amountof dust, show an east-west symmetric structure of the extended
disk (N. Ohashi et al. 2006, in preparation). To explain theseobservations, we propose a model in which the dust disk isgeometrically thick and inclined as the eastern side is farther
to us and the inner rim of the eastern side of the outer disk isexposed to us. Figure 5 shows a schematic view of the modelof the HD 142527 system. Since the inner edge and rim arehottest within the outer disk and affect the MIR brightness
most strongly, the emitting region of the outer disk appears
like a narrow ring. Therefore, the optical depth we mentioned
above does not directly correspond to the vertical depth of theVol. 644

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
axial symmetric disk inclined to the east-west direction is also
consistent with the symmetric structure of the extended disk
traced by 850 mm radiation. It is not necessary to consider anaxial asymmetric material distribution such as a circumbinary
disk to account for the observations.
Details of the appearance of a protoplanetary disk, including a“peculiar horseshoe-like feature” for models with an inclinationof 30!, were predicted in simulations of Kessel et al. (1998). A
model 12 mm intensity map in their paper shows a morphology
strikingly similar to our images of the outer disk of HD 142527.
NIR interferometric observations of LkHa 101 show that an asymmetric arclike radiation component is present in addition to acentral compact component (Tuthill et al. 2002). In the case ofLkHa 101, the asymmetric arclike structure is thought to be attributed to the hot dust within the inner rim of the inner hole madeby dust sublimation. Although the observed spatial scale and wave-

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

1aaTpocTt

1
41322Figure 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 discarded
since 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
onlythosewithradiismaller
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

ALMA
Casassus
et al. 2013

CO(3-2) (Casassus et al. 2013)

HCO+(4-3) (Casassus et al. 2013)イメージ図PROTOPLANETARY DISK AROUND HD 142527

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

K AROUND HD 142527

L135

24.5μmとHCO+のintensityのピークはだ
いたい同じ位置→exposed rimだろう

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.

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