星形成ゼミ 2018-1-26 片岡
61.Probing the massive star forming environment - a multiwavelength investigation of the filamentary
IRDC G333.73+0.37, Veena et al., arXiv
62.Detection of non-thermal emission from the massive protostellar jet HH80-81 at low radio
frequencies using GMRT, Vig et al., arXiv
63.Star formation in a high-pressure environment: An SMA view of the Galactic centre dust ridge,
Walker et al., arXiv
64.Carbon Monoxide Observations Toward Star Forming Regions in the Outer Scutum-Centaurus SpiralArm, Wenger et al., arXiv
65.ALMA and VLA Observations of the HD 141569 System, White et al., arXiv
66.HST Scattered Light Imaging and Modeling of the Edge-on Protoplanetary Disk ESO-Hα 569,
Wolff et al., arXiv
67.GMC Collisions as Triggers of Star Formation. VI. Collision-Induced Turbulence, Wu et al., arXiv
68.Formation of Super-Earths by Tidally-Forced Turbulence, Yu, arXiv
69.High-mass Star Formation through Filamentary Collapse and Clump-fed Accretion in G22, Yuan etal., arXiv
70.ALMA Detection of Bipolar Outflows: Evidence for Low Mass Star Formation within 1pc of Sgr
A*, Yusef-Zadeh et al., arXiv
71.Mapping young stellar populations towards Orion with Gaia DR1, Zari et al., arXiv

Akimasa Kataoka (NAOJ)

ALMA Detection of Bipolar Outflows: Evidence
for Low Mass Star Formation within 1 pc of Sgr A*
F. Yusef-Zadeh1, M. Wardle2, D. Kunneriath3, M. Royster1, A. Wootten3, D.A. Roberts4•

概要：銀河系中心Sgr A*の周り1pc以内の狭い領域において、11天体のbipolar outflowを検出した。
The Astrophysical Journal Letters, 850:L30 (8pp), 2017 December 1
1天体の観測例

The Astrophysical Journal Letters, 850:L30 (8pp), 2017 December 1

Yusef-Zadeh et al.

全体像

白い棒がoutflowの方向を表す
Figure 1. Relative coordinates (0,0) in Figures 1–4 coincide with the position of Sgr A* at a, d (J 2000) = 17h 45m 40.s 038, −29°00′28 069. (a) The blueshifted andredshifted lobes are detected to the NE and SW, and the green color represents the intermediate velocity range. The intensity range is between −1 and 10 mJy beam−1.
The cross coincides with the position of a compact 226 GHz source (see (h)). (b) A color image of CS(5−4) emission at a velocity of 103 km s−1, channel width of

Akimasa Kataoka (NAOJ)

••

銀河中心BHは質量4×10^6Msunで、そのThe Astrophysical Journal Letters, 850:L30 (8pp), 2017 December 1

outflowの速度と長さから、平均的な年齢はYusef-Zadeh et al.

Table 1 6500年(+8100年-3600年)と推定。
周りでは当然潮汐力が強い→~10^7(r/Entries Give the Source Name, the Coordinates, the Flux Density, the Extent of the Blueshifted and Redshifted Lobes in Terms of the Beam Solid Angle, the Velocity
Difference of the Lobes, the Angular Separation of the Lobes in Arcseconds, the Center Velocity, and the Position Angle of the Source in Degreespc)^-3[cm^-3]以上の密度がないと、潮汐
SourceJ2000 CoordRed Lobe

Blue Lobe

R.A.(s)Decl.(″)
FΔv
Ω
力に負けて星ができないと思われている。
−1
h m

•

BP1
BP2
BP3
BP4
BP5
BP6
BP7
BP8H I
BP9
BP10
BP11

17 45

-29 00¢mJy km s

BeammJy km s−1

Beam

km s−1″km s−1deg.

38.91740.41740.49540.84039.86939.34339.44039.63840.41439.29640.553

30.72
15.48
29.11
21.03
22.24
44.27
32.82
31.28
30.41
29.39
16.62

215
1140
7.8
54
63
2489
22.2
6.2
155
171
42.7

2.9
3.6
1.5
1.5
1.4
6.5
2.9
1.2
2.9
1.2
1.5

135
450
10.3
L
•116
1198
L
5.1
510
170
44.7

2.4
1.9
1.1
L
1.6
5.1
L
1.1
2.1
1.2
1.35

2
4
1
1
4
V
5
1
13
2
3
1

1.45
1.29
0.74
0.17
0.41
1.01
1.80
0.81
3.28
0.44
0.39

113.0
97.0
163.5
197.5
−93.0
68.5
−199.5
−81.8
−59
−57
163.5

−42.1
26.6
51.3
54.3
−88.9
5.1
56.1
−50.7
−50.3
62.8
22.5

だが、実際には100個程度のOB型星が銀河
中心0.4pc以内で見つかってる(最近できた星)••FΔv結構lowΩ massのものが最近できたことを示PAΔvΔθvcenter

観測はALMAの13CO, H30α, SiO(5-4)

す。

銀河系中心はA が30等なので赤外ソースを見つけるのは難しい•

BH周りの星形成率とか結構高いかもね

Table 2
Physical Parameters of Molecular Outﬂows with Entries Giving the Source Name, the Mass and Hydrogen Number Density of Individual Lobes, the Total Mass of theLobes, the Jet Length, and the Outﬂow Force
Source

BP1
BP2
BP3
BP4
BP5
BP6
BP7
BP8H I
BP9
BP10
BP11

Red Lobe

Blue Lobe

Mass

nH

Mass

nH

Total
Mass

M:

cm−3

M:

cm−3

0.19
1.0
0.007
0.049
0.057
2.2
0.020
0.0056
0.14
0.15
0.039

2.6e+05
9.8e+05
2.5e+04
1.7e+05
2.2e+05
8.9e+05
2.6e+04
2.8e+04
1.8e+05
7.7e+05
1.4e+05

0.12
0.41
0.0093L
0.10
1.1
L
0.0046
0.46
0.15
0.04

2.1e+05
1.0e+06
5.3e+04L
3.4e+05
6.1e+05L
2.6e+04
9.9e+05
7.6e+05
1.7e+05

M:

Jet Length´(sin i )
1017 cmForce´(cos2 i sin i )L : /c

0.32
1.4
0.016
L
0.16
3.3
L
0.01
0.60
0.31
0.079

0.87
0.77
0.44
0.10
0.25
0.60
1.1
0.48
2.0
0.26
0.23

5.7e+02
1.1e+04
1.4e+01L
4.1e+03
5.4e+04L
1.4e+04
4.8e+02
4.1e+03
1.3e+02

We imaged the ALMA continuum data after self-calibration,
We identiﬁed 11 sources with physical characteristics (size,
Akimasa
Kataoka(NAOJ)
mass, age, energetics) of young star formation activity withinusing CASA version 4.7.2. After all spectral windows were

GMC Collisions as Triggers of Star
Formation. VI. Collision-Induced Turbulence
Benjamin Wu, Jonathan C. Tan, Fumitaka Nakamura, Duncan Christie, Qi Li

やったこと：２つのGMCがぶつかる場合とぶつからない場合のシミュレーションを行い、違いを比較した。
数値計算：Enzo code, 理想MHD, 自己重力あり、超音速乱流、heating/cooling,
AMRで一番高いところで0.0625pcの分解能計算セットアップ128pc^3の計算ボックス、GMCを２つ準備、RGMC=20pc, 個数密度100 cm^-3,
M=9.3×10^4 Msun、impact parameter= 0.5RGMC
周りは10 cm^-3のCold neutral medium,

non-colliding caseでは、GMCと

CNMはどちらも10km/sでconvergingしていると仮定。
B=10µG, uniform B-fields, θ=60度（衝突方向に対して）mass to flux ratio=4.3(supercritical)
T=15K (thermal-to-magnetic pressure ratio = 0.015)
Akimasa Kataoka (NAOJ)

Fig. 1. Row 1: Time evolution of projected mass surface density for the non-colliding model. Row 2: Connected extractions (CEs), the largest spatiallyconnected sub-structures for each density threshold are shown plotted over the corresponding grayscale mass surface density map. Blue, green, red,ncncnc
and cyan correspond to CEnc
2 , CE3 , CE4 , and CE5 , respectively (see text). Rows 3–4: Same as rows 1–2 except for the colliding model. Snapshots at
t = 1, 2, 3, and 4 Myr are shown. The visualizations adopt the rotated coordinate system (x′ , y′ , z′ ) (i.e., the simulation coordinates (x, y, z) transformed
by a (θ, φ) = (15◦ , 15◦ ) rotation used throughout this paper series. (Color online)

Blue, green, red, and cyan correspond to CEnc2, CEnc3, CEnc4, and CEnc5,*CE: connected extractions, clump-finding algorithm finding the largest structure*CEnc2は個数密度10^2個以上の領域で、ひと塊とみなせるもの
Akimasa Kataoka (NAOJ)

localized within the collisional interface and grow over time

where s ≡ ln (ρ/ρ ), and the mean (s) and variance (σ ) of

Publications of the Astronomical Society of Japan (2017), Vol. 00, No. 07

速度分散の時間発展

Fig. 4. Velocity dispersions as functions of density. Each panel represents a different snapshot in time, from t = 1 to 4.5 Myr. The non-colliding caseis represented by dashed lines, while the colliding case is represented by solid lines. For each model, σ v (averaged over the x, y, and z lines-of-sight)
for the total gas content (black), CE2 (blue), CE3 (green), CE4 (red), and CE5 (cyan) is plotted. (Color online)of a few and were in agreement with observed velocity dispersions of ∼ a few km s−1 (Hernandez & Tan 2015).
Figure 3 shows p–v diagrams of the gas density in the
non-colliding and colliding simulations, measured alonglines of sight for the collision axis (vx ) and for a side view(vz ). Results for vy are not displayed, but are in generalsimilar to those along vz .
n are shown. PDFs for the total gas (black), CE2 (blue), CE3 (green), CE4 (red),In the non-colliding model at 2 Myr, the overall gas disse, while solid lines represent the colliding case. Power laws are fitted toeachtribution shows turbulent kinematic structures that are genweighted PDFs. (Color online)
erally within ±5 km s−1 . The individual GMCs can be distinguished in the x direction. CEnc
2 , which traces GMC 2
at this time (see subsection 3.1), shows similar kinematicnc
structure. CEnc
3 and CE4 can also be seen, with relatively
narrow velocity spreads of at most a few km s−1 .
At 2 Myr, the colliding model has formed a more spathe collision-inducing increased turbulence in the GMC–otially compact structure and exhibits much stronger kine6
GMC system. In this time, the turbulent driving modeb
matic signatures.
Portions of the GMCs exceed ± 10 km s−1 ,to the bulk flow velocity combined with initially turbuhas increased to 0.26 and 0.24 for the non-collidingdueand
lent gas. This gas has not yet interacted with the incoming
Akimasa(NAOJ)
colliding models, respectively. We note, with caveatsGMC.
thatCEc2 , Kataokadwhich contains
the combined GMC gas, showsmass-weighted PDF.

マッハ数

2Myr

4Myr

無衝突

10.9

9.73

衝突

13.05

15.22

much higher, although CEc s at successively higher densities similarly form with lower relative velocity dispersions.
The cloud collision is less apparent along vz , but higher
velocity dispersions relative to the non-colliding case canbe seen at the interface.
At 4 Myr, p–v diagrams for the non-colliding model
reveal the presence of higher density structures via the total
projected cell mass values, but overall velocity dispersionnc
is similar. CEnc
2 now includes both GMCs, and CE3 tracks
nc
the majority of GMC 2. CEnc
4 and CE5 , which have now
formed, contain gas with relatively low velocity dispersions.
The colliding case at 4 Myr reveals very different
behavior, exhibiting much higher velocities and more compact gas structures. CEs at this stage of evolution now
include gas with much higher velocity dispersions, withhigher-density CEs showing large amounts of disruption.
Compared to the colliding case at 2 Myr, the gas kinematics
are now dominated by post-collisional gas located in thecentral structure rather than the pre-collisional gas fromthe original GMCs.

結論：GMC衝突によって作られたクランプ

は、高いマッハ数・大きな速度分散・（ビリアル平衡を長時間維持）

HST Scattered Light Imaging andModeling of the Edge-on
Protoplanetary Disk ESO-Hα 569
Schuyler G. Wolff, Marshall D. Perrin, Karl Stapelfeldt, Gaspard Duchene, Francois
Menard,Deborah Padgett, Christophe Pinte, Laurent Pueyo, William J. Fischer•

HSTのプログラムで、WISEとSpitzerのサーベイで新たに判明した
エッジオン原始惑星系円盤のうち19天体をサーチするプログラムのうちの１点体の解析を示した論文
ターゲット：ESO Hα 569 (a low-mass T Tauri star in the Cha I star forming region)
カメレオン領域：160±15 pc 、1-2Myr,

Akimasa Kataoka (NAOJ)

Tranfer Modeling3

ESO H↵ 569 Radiative Tranfer Modeling
西の方が東より20倍明るい

5

2MASS, Spitzer, WISE, Herschel, ALMA, and the
赤い（814の方が606より明る HST,LABOCA instrument on the APEX telescope (see Figure 4). Table 1 provides the SED values with photometい）ric errors and references for each value. The SED shows
the characteristic double-peaked shape of edge-on disks
円盤はざっくり125au
with contributions from both the scattered light fromthe central star peaking at about 1.5 µm and the thermal
814画像を606画像から引くと emission from the surrounding optically thick disk peaking at roughly 70 µm. Data at similar wavelengths fromdi↵erent epochs show variability at the 10 20% level,
ジェット成分が見える
consistent
with3.variability
in jetother
young(EsFigure
An image seenof thecreatedby disks
subtracting
F814W
from theF606W
image.
Contoursareet al.
2011;image
Flahertyet al.
2012;
Muzerolle
et al.
SEDは一般論としてedge-on円paillat the22009). drawn from2 0.01 to 0.19 mJy/arcsec in intervals of 0.03

mJy/arcsec . The 100 au scale bar corresponds to an angular scale of 0.62500 .

盤っぽい（1.5µmに散乱光、Figure 2. A wider F606W filter image displaying the di↵use
nebula extending outward from the disk. The direction of theH↵ filament HH919 is shown by the arrow. The jet lines up
well with the reported position of HH 919, consistent withESO H↵ 569 being the origin of this outflow. The 500 au
scale bar corresponds to an angular scale of 3.12500 .

70µmに光学的に厚い円盤がみえるはず）

814(0.8µm)画像をモデル
フィットした。

2.3. Spectral Energy Distribution
A spectral energy distribution (SED) for the disk
was compiled from the literature, including data from

Figure 4. Spectral energy distribution for ESO-H↵ 569 withupper limits indicated by triangles. The SED exhibits the
double peaked structure typical of an optically thick, edgeon disk. The values were compiled from the literature withmore information given in Table 1. The stellar spectrum foran M2.5 star with Tef f = 3500 K is overplotted.

Figure 1. HST images of the protoplanetary disk ESOH↵569. Top: F814W. Bottom: F606W. Both images show
the dark dust lane and asymmetries between the top andbottom of the disk, while only F606W establishes the presence of an outflow jet. The 100 au scale bar corresponds toan angular scale of 0.62500 .

background noise. The measured flux density is 0.058 ±compared to the flux in 9 neighboring pixels with nojet signature. The peak surface brightness of the jet is⇠ 0.19 mJy/arcsec2 . The ability to measure color variations in the shape of the disk and width of the darklane between the F606W and F814W bands is hinderedby the presence of this bright jet.

Akimasa Kataoka (NAOJ)

cc(Pinte et al. 2006, 2009) was used to construct
SEDs andnentthe( ),disk
surfacedensitytemperature
exponent (↵),
disk edge
2Dof theinternal
asand
amap
byproductof
0.8 µm scattered light images for each of the models.
typeMCMC(sharp orradiative
tapered). transfer
For the maximum
particlesize,
The 0.6Forµm scattered
lightBest
imageswere
not modelledcalculation,andthe resTable
3. MCMCParamters
observed
image
this
work,
Rfit
=
R
.
This
exponential
taper
is
c
out
the grain population is described by a single species of
because the strong jet signature required masking 50%
are fairly
consistent:a Modelingcalculated disk midplane
ESO H↵ 569
Radiative Tranfer
2al. 21 t
amorphous
dustof
Olivinecomposition(Dorschneretfor the inwards
value
predicted
by physical models of viscousperatureaccretion
disks
of the integrated
disk flux.
of
10
K
at
100
AU,
increasingt
Parameters
Best-fit
Values1995)
withaparticle
size
distribution
followinga-3.5
The selectedmodel assumes
axisymmetricdisk
theobservation(Hartmann
et al.an1998),
but observations
senK law
atwere5extending
AU.notThelargersourceofpotential
system
power
from
0.03
µm
up
to
the
free
paramwith a surface
density,by+2.6a power law disInclination( )⌃, described
83.0
4.8
theassume
diskuntil
mass
is dustthusistotheassumeddustoeterbias
amaxin. fall-o↵Wethat thewellthe
mixed
with
↵
total
obs
sitiveenoughthisoutergradualtribution
in radius
given by to⌃ =detect⌃0 (R/R)
where↵+1.7 0Dunham etdustcombinaopacity cha
Scale
Height(au)
16.2
the ity.
gas, irrespectiveof al.
the (2016)
particle use
size.aThis
2.0and R0 is theis termed
thesurfacedensityexponent
pared
to
the
dat
Hughes et al. (2008)+0.00017
used this form tion
toteristic
modelboth (withgasdustof
dust
properties
a
=
100
µm)
results
inofcoagulated
grains
with
thin
icy
man
max
reference Dust
radiusMassof 100“sharp-edged”
model(Mau.) In this
0.00057
0.000222
mean
scattering
phase
asymmetryfactor1994).
of Focalculation.
dusttruncatedcontinuum
observations ina theIt( millimeter.
=
0.23, cm
/g function
Ossenkopf& Henningthe diskand
is abruptly
at an outer+0.94 radius Rout .
Surface Density ↵1.77 0.14
g =model0.54. uses
Dust olivine
porositydust
is modeled
simplyasa frac-3.2, w
as described
inMcCabesectionIn orderistoexpected
achieve a good
fit tothe smalldi↵use emission
and
et
that
the
dust
grainsseen
inscattered
+0.09
tion
between0
and1ofvacuum
that
is
mixed
with
the
above theFlaring
disk and the disk mass 1.19
and inclination
simul0.08
yields a similar opacity at 2.8 mm within a factor
silicates
theBruggeman e↵ective
mixingrule. poi
each
model
light
should be disk
wellmodel
coupledwith
forfollowing
young
disks,
taneously,a “tapered-edged”
was tested,in the gas
But
other
resultscaneasilybeobtained.
For insta
Note—Best fit values for the covariFor
comparison
withtheobserved
0.8µm
scattered
which thedensity ⌃ falls o↵ use
exponentiallywithsome density
tovarylawfromAsuggesting
thissurface
distribution
if images,
weinsteadadoptisthe dust
opacityfromBance likelihoodthe
estimation ofmodeof the
light
each
model
image
was
convolved
witha1
critical radius Rc of material outside of the disk:
2
with
et
al.
(1990)
(
=
0.03
cm
µm)
MCMC.
⌫
Tiny
Tim simulated
PSF (Krist 1995).extinction
The/g
0.8at
µm870
ob-valujustified
here.
(See
also
recent
work
by
Guidi
et
al.
2016;
✓ ◆↵
✓
◆2+↵
use T=20
then tothat
yieldsservations
were K,
maskedselectonlyantheestimatedpixels withdisk m
RR
2
residuals
isA choF⌫ D
Pohl
etc al. 2017,
and Tflux
Charespectively).
⌃=⌃
exp for HD 163296(1)
M
(gas
+
dust)
=
=
0.0055M,afactorofvalues3
above
thebackgroundnoiselevel.
⌫ B⌫ (T )
Rc
Rc
While
the
rob
2D
map ofofthenoise
was generated
by convertingtheThe scale height is also defined
as13. Wea show
power
law
radiuslower(againgas
tor
Figurethe evolution
theshapeinof theassuming
image and SED for thedi↵erentstandard
dust masses. Our best
fitp
model
isdustshown
in blue. The other models use the same parameter values except for the mass, which is some fraction of the best fit dust massobserved
image
toelectrons,
and assigning= peakNinethe SEDpro
For this work, Rc = Rout . This exponential taper
isBetterconstraints
thedust
as indicated in the legend. ofFor a100).
fixed inclination,
decreasing
the dust mass moves onphotonsfrom thethermalparticle
vided
by
MCF
by
H(R)
=
H
(R/R
)
where
is
the
flaring
exponent
2 the mass00
to the scattered light peak. Decreasing
by a factor of 10 generates a flat SED without the double peaked structure.
forthevalues.
The
model
imageswerealignedwithpredicted by physical models of viscous accretion disks
Likewise, if the dust mass ties
is one tenth
the best
fit value,
double nebula shape begins
to disappear couldin the scattered
light cla
andthusthethe millimeter
opacities
help
3.7. Dust Mass
image, and is not seen
at
all
in
the
1.9
⇥
10
M
model.
disks, itithe observations via a cross correlationthickand normalized(Hartmann et al. 1998), but observations were not senthe
true
mass
of
this
disk.
Some
disagreement
betw+0.00017–M
The best
disk themass oftotal
0.057 Mobserved
is abnormallyflux.two.
But naturally
a separate
to each individualThe
modelswerefit thencom- obThe
disk
dust
mass
is
0.00057, fit tositivebest-fit
enoughtodetectthis
outer
gradualfall-o↵until
面白い点：円盤質量が大きい。ガスダスト比を100とすると、0.057Msunで、円盤0.00022asinglemodel
servableiscapableofyieldingabetterfit
tothatcontinu
one,large, especially considering
the
small
centralobpredictions
fromthe
2.8 mm and870 µm
2 at
pared
to
the
data
via
an
error-weighted
pixel-by-pixel
1
Hughesetal.
(2008)
used
this
form
to
model
both
gas
hich corresponds
a disksome
mass authorsof 0.057 M(assuming
though multiple mm continuum observations
the cost of an inferior fit to the other. This is likely due
Notetothat
give
this ject,equationusing
the notation
measurementsmaybe(1) seeunsurprisingsincederivedsupport this estimate.
Assuming a gas to dust rato:
Limitationsin the parameterizationofthe comtop
CPU
time,
calculation.
Forsimilarwork
Duchêneetal.
(2010)
anddust
continuum
observations
inthemillimeter.
It
質量が中心星の16%にもなる。
he standard=ISM↵.gas to dust ratio of 100). This is 16%
tio of 100, the disk mass is 16% the mass of theplex physical processes ongoing in protoplanetary disks.
massesfrom
sub-mmdata
be analytic
biaseddownward
centralstar,
establishing
the
ESO
H↵
569
disk
as
work,
amay
fairlysimplestructure forand McCabe et al. (2011).In this
For
the
SEDs,
whendiskfitting
is expectedthat thedust
scatteredthestellar mass
forsmalla 0.35
M grains
star seen
like inESO
H↵ 569,a clear outlier in the Cha I SFR. Despite the highmalism with a single grain population was used. (2) The
thecasepoint,
ofstableEODs
if they
begin
toto become
optically
だが、これはALMAによる2.8mm
連続は観測の結果（0.057Msun）とよく一致。
each
model
the
issomeallowedlight should
be well coupled with the gas for young disks,mass, the disk
appears
gravitationallyat
all foregroundinability of
our extinction
datasetconstrain
aspects of rel- t
surprisingly high disk to star mass ratio.
physics and processes (e.g. neither the SED nor
to vary
fromwavelength.
AV = 0 evant
10
with
Rimage=provide
3.1,
andthe onat that
That
said,
good
agreementsuggesting the use of this surface density distribution isradii.
V the
the
scattered
light
much
information
In the grid
fit
and
the
initial
MCMC
run
using
the
– The
vertical structure of the disk as defined by thethe innermostthe
regionsobservedof the disk). - model
extinction
thatis minimizes
justified ＃ただし、ALMAの結果は、小さいオパシティ、高い温度を仮定すれば下がる
here. (See also recent work by Guidi et al. 2016;scale height andthe exponent
Dunhametal. (2016)
millimeter-continu
thetweenpower law value
flaring
2
Using a combination of di↵erent observables (specestimator,
the
fit
to
the
disk
mass
reliedheavilyonwellconstrained. The best fit model has a masstral data, images in scattered light, and thermal emisis chosen.
Pohl et al. 2017, for HD 163296 and T Cha respectively).averaged diskresiduals
derivedmass
andresultfromdataour
fit tograin
thefull S
temperatureof ⇠ 23
K, similar
to thesion,
andpolarimetry
toconstrain
proper実は、double-peaked
SEDは、相当質量の高いedge-on円盤を見てるかも？
heThe
870scaleµm
measurement.
Given
surprisinglyhighother disk observations.
The
scalerobustheight is selfWhilethetreatment
oflighttransfer
proheight
is also defined
as athepower
law in radiusties) helps
toradiative
break degeneracies
betweenvarious
andthe
HSTprofile,scattered
image
seems
tomodelindi
consistent with the modeled temperatureparameters.
However,
care
must
be
taken
to
determineass
estimate,
we
speculated
that
the
870
µm
photombymodel
MCFOSTis essential
for modeling opticallyby H(R) = H0 (R/R0 ) where is the flaring exponent
Akimasa
Kataoka(NAOJ)
supporting
avidedflareddisk
in which the gas
the correct approach for the relative weighting of observ5