星形成ゼミ
SFN #296 46-50
2017/10/27
東大/国立天文台 辰馬 未沙子
46. Alignment Between Protostellar Outflows and Filamentary Structure
47. 13C isotopic fractionation of HC3N in two starless cores: L1521B and L134N (L183)
48. Physical properties of dusty protoplanetary disks in Lupus: evidence for viscous evolution?
49. Dust properties of the cometary globule Barnard 207 (LDN 1489)
50. Constraining accretion signatures of exoplanets in the TW Hya transitional disk1

Alignment Between Protostellar Outflows and Filamentary Structure
Ian W. Stephens1 , Michael M. Dunham2,1 , Philip C. Myers1 , Riwaj Pokhrel1,3 , Sarah I. Sadavoy1 ,Eduard I. Vorobyov4,5,6 , John J. Tobin7,8 , Jaime E. Pineda9 , Stella S.R. Oﬀner3 , Katherine I. Lee1 ,Lars E. Kristensen10 , Jes K. Jørgensen11 , Alyssa A. Goodman1 , Tyler L. Bourke12 , Héctor G. Arce13 ,Adele L. Plunkett14
3
1

Harvard-Smithsonian Center for Astrophysics, 60 Garden Street, Cambridge, MA, USA
ペルセウス座分子雲の原始星57個に関2
Department of Physics, State University of New York at Fredonia, 280 Central Ave, Fredonia, NY 14063, USA
3
Department of Astronomy, University of Massachusetts, Amherst, MA
01003, USA
してSMAのCO(2-1)観測をし、アウトフ
4Institute of Fluid Mechanics and Heat Transfer, TU Wien, Vienna, 1060, Austria
ローとフィラメントの向きの関係につい5Research Institute of Physics, Southern Federal University, Stachki Ave.
194, Rostov-on-Don, 344090, Russia
6
University of Vienna, Department of Astrophysics, Vienna, 1180, Austriaて調べた。
7
Homer L. Dodge Department of Physics and Astronomy, University of Oklahoma, 440 W. Brooks Street, Norman,
OK 73019, USA
フィラメントの方向はHerschelのoptical
8
Leiden Observatory, Leiden University, P.O. Box 9513, 2300-RA Leiden, The Netherlands
mapを元に調べた。
9Max-Planck-Institut für extraterrestrische Physik, D-85748 Garching,depth
Germany
10Centre for Star and Planet Formation, Niels Bohr Institute and Natural History Museum of Denmark, Universityof Copenhagen, Øster Voldgade 5-7, DK-1350 Copenhagen K, Denmarkアウトフロー/フィラメント間の角度は
11
Niels Bohr Institute and Center for Star and Planet Formation, Copenhagen
University, DK-1350 Copenhagen K.,
ランダムか、平行(22%)と垂直(78%)のDenmark
12
混合のどちらかと一致した。
SKA Organization, Jodrell Bank Observatory, Lower Withington, Macclesfield,
Cheshire SK11 9DL, UK
Figuremap of the Perseus molecular cloud (Zari et al. 2016), with magenta lines showing the directions of the outflows
13 1. ⌧
Department
Astronomy,
Yale
Haven,
06520, USA
measuredin this study. The sizeofof thelines only represents the
directionUniversity,of the outflow and notNew
the angularextent. Thin CT
blue contours
are shown for ⌧= 0.0002. These contours roughly show the boundaries of each labeled clump and correspond to a column density
原始星の性質(multiplicity,
14of
N (HEuropean) ⇡ 5 ⇥10 cm(Sadavoy
et al. 2014).
Southern
Observatory, Av. Alonso de Cordova 3107, Vitacura,Santiago de Chile, Chile 温度, opacity)•••

353 GHz2

353 GHz21•

2

where PAOut and PAFil are the PAs of the outflow andfilament, respectively. MIN indicates that we are interested in the minimum of the two values in the brackets.
Table 3 lists the measured PAs for all outflows and filaments in this study.

line emission obviously traces the outflow cavity walls
rather than the outflow centroid, we connect the continuum peak to a local CO maximum near the continuum
rather than the absolute maximum. In cases where there
are no clear local outflow maxima for one lobe, we use
the PA measured by the other lobe. If no local maxima
exists for both lobes and the CO only traces cavity walls,
we manually measure the PA by eye. We indicate in the“Ref/Info” column of Table 3 which outflow measuringmethod we used. For the angles measured in this paper,a crude approximation of the uncertainty can be foundby subtracting the blue outflow PA from the red outflow
PA. With such an approximation, the uncertainty in theoutflow PA is typically less than 10 .
Frequently, the observed field about a MASSES target overlaps with other protostellar sources, which cancause significant confusion in assigning which emission
comes from which protostar. To disentangle
2 which emission belongs to which source, we used SAOImage DS9 toに関わらず、同じような角度の分布を持っていた。

E-mail contact: ian.stephens at cfa.harvard.edu(上図) Herschelの353 GHz optical depth mapに

τ353GHz=0.0002のコントアを青で表している。マ
3.1. Outflow
Position Angles

We present the outflow PAs in Table 3. We independently measure the outflow PAs for both the blue- andred-shifted outflows (henceforth, called the blue and red
lobes). The range of the PA measurements are from–180 to +180 ; both positive and negative values allow
one to assign the appropriate quadrant for the outflow.
We also provide the combined PA, PAOut , which is simply the average of the two outflows after adding 180 tothe lobe with the negative PA. Some entries only provide measurements for one lobe because the other lobe
was undetected.
In many cases (about half of the sources) we used out-

35
ゼンダの線はアウトフローの方向を示しており、長さに意味はない。

•

原始星の角運動量の軸の方向は周りの構造に依存していないのかもしれない。

•

赤線、黒線: 観測からわかったアウトフロー/フィラメント間の角度。

•

点線: 3Dモンテカルロシミュレーションを2Dに投影。平行を020°、垂直を70-90°と定義した。

Figure 10. Cumulative distribution function of the projected angles between outflows and filaments, , with the red step curveshowing the empirical distribution, F . Black dashed lines showdi↵erent mixes of projected outflow-filament angles that are 3dimensionally parallel and perpendicular in increments of 10% (i.e.,
the top line is 100% parallel and 0% perpendicular, the next line
is 90% parallel and 10% perpendicular, and so on). Parallel angles
are defined as 3-dimensional angles drawn from a distribution between 0 and 20 , while perpendicular angles are defined as angles
drawn from a distribution between 70 and 90 (see Appendix A
for details). The blue line shows a random distribution of projected
angles, while the magenta line shows the best bimodal fit to thedata of 22% parallel and 78% perpendicular.

•

青線: 0-90°でランダムに存在しているとき。

•

下の3図はmultiplicity(左), 温度(中), opacity(右)への依存性を調べたもの。multiplicityは10,000au以内に別の原始星があるかどうか。温度とopacityについては、ちょうど半分ずつ分布する境目が50Kと0.016だった。
11

Figure 13. CDFs of , binning data based on multiplicity (left), bolometric temperature (middle, an indicator of age), and optical depth(right). All CDFs use filament measurements from the FILFINDER algorithm.

Tilley & Pudritz (2004) show that cores within filaments 3 tions of 3-dimensionally random and mostly perpendic-

13

C isotopic fractionation of HC3 N in two starless cores: L1521B and L134N (L183)

12
1,3
KotomiTaniguchi,
Hiroyuki
Ozeki
and
Masao
Saito
6
1

8

Departmentof Astronomical Science, School of Physical Science, SOKENDAI (The Graduate University for Advance
Table 1. Spectral line parameters of HC3 N and its three 13 C isotopologues in L1521B and L134N
CCH
Studies), Osawa, Mitaka, Tokyo 181-8588, Japan+ HNC, - H
2
L1521B
L134N
Department of Environmental
Science, Faculty of Science, Toho
University, Miyama, Funabashi, Chiba 274-8510!
!
SpeciesFrequency
T
∆v
T dv
V
rms
T
∆v
T dv
V
rms
+ CN, - H
Japan
C2H2
HC3N
(GHz)
(mK)
(km s ) (K km s ) (km s ) (mK)(mK)
(km s ) (K km s ) (km s ) (mK)3
+ HCNH ,+ HCN,
National Astronomical Observatory of Japan, Osawa, Mitaka, Tokyo 181-8588, Japan
C2H2+
a

∗
A

b

∗
A

−1

c

LSR

−1

∗
A

−1

d

∗
A

−1

c

LSR

−1

−1

+

HC3 N

45.49031

2456 (82)0.73 (3)1.89 (10)

6.3

7.9

E-mail contact: kotomi.taniguchi at nao.ac.jp

H

13

990 (26)

0.71 (2)0.75 (3)

2.7

3.4

CCCN

44.08416

68 (7)

0.67 (6)0.049 (7)

6.3

6.5

21 (2)

0.67 (7)0.015(2)

2.0

2.3

13

45.29733

61 (6)

0.78 (8)0.051 (7)

6.3

7.5

12 (2)

0.78 (17)0.010 (3)

2.6

3.0

HC

CCN

13
2.6

- H2

-H

+ e-, -H

HC3NH+++ N,
C3Hn
45.30171 the102J(8)= 50.71
0.077 (8)6.3
27 (4)
0.71 (9)0.020 (4)4.0
WeCN
observed− (5)4 rotationallines
of 8.5the normal
speciesandthree C isotopologues- Hof/- HHC3 N at the 45 GH(n = 3-5)
band toward
two represent
low-massstarless
cores,
L1521B
and L134N(L183),
using
the Nobeyama 45 m radio telescope in orde
Note—Numbers
in parentheses
the standard
deviationin the Gaussian
fit, expressedin units of thelast significant
digits.
a Taken from the Cologne Database for Molecular Spectroscopy (CDMS) (Müller et al. 2005).
to study the main formation pathways of HC3 N in each core. The abundance ratios of the three 13 C13 isotopologue
Table 2. Column densities of HC3 N and its three C isotopologues
b The errors are approximately 0.2 km s , which correspond13
to the velocity resolution.
in L1521B are derived to be [H13 CCCN]:[HCCCN]:[HCC13 CN] =and0.98: 1.00: 1.52the 12(0.14)
C/13 C ratios
in L1521B
and (0.16)
L134N (1 sigma). Th
c The rms noises in emission-free regions.
fractionation pattern is consistent with that at the cyanopolyyne peak in Taurus Molecular Cloud-1. This fractionatiod The errors are 0.5 km s
at most due to smoothing in the velocity direction.
L1521B
L134N
pattern suggeststhat the main formation pathway of HC3 N is the neutral-neutral
reaction between C
2 H2 and CN
Species
Column density
ColumnC/ C
13
13 C/ C
13 density
On the other hand, their abundance ratios in L134N are found to be [H
CCCN]:[HCCCN]:[HCC
CN]= 1.5(0.2)(×10 cm )ratio(×10 cm )ratio
1.0 : 2.1 (0.4) (1 sigma), which are diﬀerent from those in L1521B. From thisfractionation
pattern,
we proposetha
HC N(5.5 ± 0.3)×100−(8.6 ± 0.3)×10−!
" formation pathway
the reaction between HNC and CCH
is a possible
main
of
HC
N
in
L134N.
We
find
out
that
th
∗
3
TA
H CCCN
4.7 ± 0.6
117 ± 161.4 ± 0.2
61 ± 9−ln same
1 − molecule are not, common even in the similar(1)
main formation pathways ofτ =theWe
HC CCN
4.7 ± 0.7 physical
115 ± 16 conditions.
0.9 ± 0.2
94 ±discus
26
f ηB {J(Tex ) − J(Tbg )}星のない2つの低質量コアを野辺山45mの45GHz帯で•whereHCC CNL134N
7.2 ±and0.8
76 ± 61.9 ± 0.3
46 ± 9the possible factors to make a diﬀerence
pattern between
L1521B/TMC-1.
# in$ fractionation
%
&−1
13

HCC

2

−1

−2

12

11

−2

13

12

11

13

−2

3

13

13

13

hν
hν
13
J(T
)
=
exp
−1
,
Note—Errors represent(2)the standard deviation.
観測し、HCkkT
Acceptedby ApJ3Nの3つの C同位体置換体の比率を調べた。
and'Figure 3. Possible main formation pathways leading to HC3 N.
%#$ hν %&−1$E
π3h∆v
1 13 1
https://arxiv.org/pdf/1707.08267
lower1313
L1521Bでは[HCCN]:[HCCCN]= −0.98(±0.14):1.00:1.52(±0.16)であった。
N = τ CCCN]:[HC1 − exp
Q
exp
.
(3)
8π 3
4ln2 µ2 Jlower + 1
kTex
kTex
2. L134N : the main formation pathway of HC3 N is the reaction of CCH + HNC (Patbeam filling
factor,In Equation (1), τ denotes the optical depth, TA∗ the antenna peak temperature (Table 1), f theAccording
4. DISCUSSION
to Figure
6 in Furuya
et al. (2011), the both CCH/13 CCH and CCH/C13 CH
at theandearlyL134N,
stage around 103 yr, and the ratios are almost constant by ∼ 105 yr.
3Nが主にC
2H2とCNの反応で形成されることを示している。
and ηこれはHC
eﬃciency, respectively.
We used 1 for the beam filling factor in bothdecrease
L1521B
B the main beam
4.1.
Main
formation
pathways
HC3withN in
L1521B
L134N
2 agreetheirmodel at andjust before
105 y
of HC
summarizedin Table of
3 N in L134N
arelargerthan
thebecause the emission region sizes in L1521B (Hirota et al. 2004) and L134N (Dickens et al. 2000)
13
CCH/C13 CH ∼ 60). The C13 CH/
in Furuya et al. 2011) is app
13 CCH ratio 5(Figure 3 (b)1′′
5
13HC3 N, namely
13
The
diﬀerencesinabundance
among
the
three
C
isotopologues
of
the
and
10
yr
and
startstoincrease
just
before10yr.
The
H
CCCN/HCCCN ratio
is debeam size of the Z45 receiver (37 , Section
2).
The
main
beam
eﬃciency
was
0.71(Section
2).
T
and
T
are
the
ex
bg
13
13
13
一方、L134Nでは[H
CCCN]:[HC CCN]:[HCCCN]= assumed
1.5(±0.2):1.0:2.1(±0.4)であった。
mainthatformation
pathwayof HC3 N is as
the neutral-neutral
reactionof CCH
HNC,
the excannot be
isotopeexchange
reactions,discussed by
Takanoet+al.
excitation temperature
microwave background(≃brought
2.73 6
K).by
Wethe
the
1,2,3and the cosmic 2,3,4
4,5temperature
7 excitation
4,6calculated
8 (1998)
Furuyaetal.
(2011).
is
1.5
±
0.2,
which
is
consistent
with
1.6
by
M. Tazzari, L. Testi, A. Natta , M.
Ansdell, J. Carpenter
G.is Guidi, M. Hogerheijde , C.F
showedthatthe reaction
between
HC3 N ,and
the 13 C
isotopologues.
J(T) in Equation(2) carbon
the atom is eﬃcient at the temperature as low
temperature is 6.5 K (Suzuki et al. 1992) for the normal species and
9
8
6
8,10
6 in main formation pathway between L134N
4.2.
What
factorcontributes
the 13
diﬀerences
ManaraA.Equation
Miotello, theN.column
van density,
der Marel
E.F.
van
,athe
J.P.
Williams
thereactionofDishoeck“13 CTable
+ HC
may
form
various
C isotopologuesof HC3 N. However, i∆v is thatthe, line
width(FWHM,
1),3 N”
Q ispartition
Planckfunction., In(3), N is
これはHNCとCCHの反応で形成されることを示している。
13
13
Taniguchi
et al. (2016b)
compared theof CHC
isotopic
fractionation of HC3 N in various sourthereactioncontributes
to theCrotational
isotopic
fractionation
function,µ is the permanent electric dipole moment of HC3 N, andEloweris theenergy of thelowerenergy3 N, because their results did n1
tohigh-mass
star-forming
cores.
They
found
that
the
fractionation patterns in all of theof Astronomy,of Cambridge,
MadingleyRoad,
CB3
Cambridge,
UKlevel.Institute
We used 3.73172
D for µ of HCUniversity
isotopologue
is selectively
formed.
We 0HA,thenwill
not formationconsiderpathway
theeﬀectstheon the3 N (Deleon & Muenter 1985).
4
and suggested
that theprimaryof HC3 Nofmay
be reactioncommon in various
ph2The derived column densities are summarized in Table 2. The optical depths are derived to bereactions
13
dependon the physical C
conditions
suchfractionationas temperature andof
density.
3.01Garching,±significantly
0.15,
0.0267±observed
European Southern Observatory, Karl-Schwarzschild-Str.
2, D-85748
of HC N in the following
discussion.
Hence,
theGermany
isotopicHC•• Physical properties of dusty protoplanetary disks in Lupus: evidence for viscous evolu
tion?
•
•

above. The 14 red dots represent disks that were initially part ofPhysicalthepropertiesof butdusty
36 analyzed objects,
resultedprotoplanetaryin having a signal-to-noisedisks in Lupus: evidence for viscous evoluratiotheatdust
longbaselines
toosmall
to allowfora robust
estimate
ofderived with very di↵erent
tion?
Fig.
7. (left): Ratio between
massesderived in thiswork
and thosederived by
Ansdell
et al. (2016).
Although
1.Comparison(top): distribution of stellar masses for the full Lupus sample
methods (for a detailed theirdescription,
the text), the masses
are within a withfactor ofbeing
2 (gray area)
for the vast majorityof disks.Fig.
(right):diskseestructure,compatible
unresolved.
An ex1,2,3
4,5
8
between the disk inclinationsi (along the line of sight)2,3,4
obtained in this work and thosederived by Ansdell et al. (2016).
both
plots,Ansdell
the disks arefrom
et al. 7(2016)bars)4,6
and
for theHogerheijde
sub-sample analyzed
ceptionthe reddots
is J16102955-3922144(marked 6in,In J.
M.fromTazzari, among
L.
Testi
, A.
Natta
, M.
Carpenter, G.(white
Guidi
, M.
, C.F.
sortedleft to right by increasingstellarmass and the circled
dots highlightsources with
0.7 § Ansdell
M‹ {Md § 1.
in
this
work
(blue
bars).
(bottom):
observed
integrated
continuum
flux
8
6
8,10
6
on whose structure
havederbeenMarelable to obtaina marginal
Manara9 , blue)
A. Miotello, N. wevan, E.F.
van Dishoeck, J.P.
Williams
at890µm(Ansdell
et
al.
2016)
as
a
functionof stellar mass. Blue dots
constraint.
Table 4. Summary of fit results for disks with cavities.
represent sources whose analysis is presented in this work. Red dots

1

Institute of Astronomy, University of Cambridge,Previously
Madingley
Road, CB3 0HA, Cambridge, UK
known TDs represent sources that appear unresolved and have been discarded in the2Name ALMAの890µmで22の円盤を空間分解し、ダスト表面密度、円盤R
reasonref.
restof the analysis
due low signal-to-noise
European Southern Observatory, Karl-Schwarzschild-Str.
2,
D-85748
Garching,
Germany ratio. In this and subsequent(au)
3. Modelingplots, the circled
dots highlight sources in the 0.7 ´ 1 Md mass bin. We
3
MY Lup´0.59 ˘ 0.01 34
1
Excellence Cluster Universe, Boltzmannstr.
2,
D-85748
Garching,
GermanySz 100´1.5 ˘ 0.1
462
also report transition
disks (“x” symbols), sources with irregular shapeSz
84 fit質量、円盤サイズ、赤道面温度プロファイルを求めた。
´1.0 ˘ 0.2
41
3
4
To
study
the
structure
of
the
disks
we
their
continuum
emisINAF-Osservatorio Astrofisico di Arcetri,
Largo´0.5E.
Fermi
5, (hexagons),
I-50125 Firenze,
Italy and the sources with integrated flux
binaries(diamonds),
J16102955-3922144
˘ 0.64
31
4
sion
with
a
disk
model
that
is
based
on
the
two-layer
approxi5
Fcont † 431
mJyFitzwilliams
that we excluded Place,from our analysis(emptyIreland
circles).
School of mation
CosmicPhysics,
DublinInstitutefor
Advanced
Studies,2
Dublin,Disks
withtentatively new evidenceof a cavity(Chiang & Goldreich 1997;SzDullemondetal.˘2001).
a
129 ダストガス比=0.01、表面:´0.33
0.02 22 In
5
min=10nm、amax=1µm、n(a)∝a-3.5、6
J16000236-4222145´0.20
˘ 0.02
6
Institute thefor following
Astronomy,
UniversityofHawaiiat
Manoa,
2680 Woodlawn
dr., Honolulu, HI, 96822, USA
we introduce
the fundamental
quantities
that30are
7
1974; Hartmann
et al. 1998), using
the parametrization:
Not fitted Vitacura,neededto compute theAv.
disk Alonsoemission deandfor morea3107,
details
we Pringle Santiago,-3.0、
Joint ALMA
Observatory,
CrdovaChile
赤道面:
min=10nm、a
max=1.023cm、n(a)∝aJ16083070-3828268
large cavity2« ˆ ˙ ff
to Tazzari etal. (2016).
8 8. Mass-averaged refer˙´ TheRY Luplarge cavity
7ˆ
Fig.
midplane temperatureLeiden
as a functionUniversity,of stellar
2´
LeidenObservatory,
Niels
Bohrweg2,
NL-2333
CA
Leiden,Netherlands
Sz 111large cavity
2
R
R
mass (left) and luminosity (right) for the disks for which we derive a
Sz 123Aダスト表面密度:9⌃g pRq “⌃02, 4
exp Technology´,(1)reliabledisk structure. Error
bars on the Oﬃce,y-axis reflect Directorate
the distribution
ScientificSupportof Science, Europeanbinary
Space
ResearchandCentre(ESA/ESTEC),
J16070854-3914075
edge-on2, 4 R0
Rc
A&A proofs: manuscript
no. main

•

hole

•

of models obtained fromthe fits.
In morethan half disks we find a disk
3.1.
Disk
model
temperature smaller than T d “ 20 K used by Ansdell et al. (2016).

Sz 112
J16011549-4152351
exhibita similar size-mass correlation:
J16081497-3857145•

F890µm † 4 mJy
no stellar parameters
unresolved

5
5
(4)

Under the basic assumptions that, at each(上図)radius, thedisk is ver- where ⌃0 is a normalization factor, R0 is a characteristic radius
赤道面平均温度と中心星質量、光度に相関はなかった。
thatis the power-law slope and Rc is
Notes
For“fourpreviously
known
and, fortwo wediskskeepfor
F890equilibrium,p0.8
˘ 0.2qthelog
Rtwo-layerp0.7(top)
˘ 0.3q(8) fixed to 10 au,µm
c `TDstically
isothermal
in disks.
hydrostatic
In Table 4 we report
the findingsof the fitsandof these
As logwhich we found new evidence of a cavity (middle)thewe reporttheradialexponential
cut-o↵ radius. The dust surface density is given
explained in Section approximation2, we do not fit the threedisks us
withtoclearly
36
allowscomputethediskcoefficient
continuumwith
0.73 emis˘ as
0.15
standard
deslopecorrelation, the holeradiusRhole of(estimatedthe andthe ⌃ad pRqpeak radius).
resolved gaps since the huge density depletion and the consid- viation(下図)
sub-mmの積分フラックス(=円盤質量)と指数関数のカット
We alsooflist
the ˘
disks
we havenot offittedwith correlathe reason
0.12
0.05.
The
slopesthe(bottom)
twoby:
linearsionis givenof the centralstar,
a thatsurfacedensityerable size of such gaps
likely tothe
haveproperties
changed the heating
for whichwe havewithin
been unable
to fit them. both suggesting thattions
are similar
the uncertainties,of the dust in the remainder
the a
disk,
which
cannotbe exprofile ofand
dust
grain
size
distribution.
AtRomeromm
References(1)
etwavelengths,
al. and(2012),(2) Merínal.pRq(2008),(3)⇣ ⌃ pRq ,largerdisks appear
brightersmallerdiskset⌃appear“Marel(2)dvan derfainter.
gplained with a simplemost
modelof
based
on
the
two-layer
approximaMerínetal.
(2010),(4)
Bustamanteetal.
(2015)(5),
オフ半径(=円盤サイズ)には相関があった。
The
Lupus
correlation
results
systematically
below
the
Taurusthe disk emission originates from the dust grains residet al. (2016), (7) see
discussionin Ansdell
et al.
(2016).
tion. These disks will be analyzed in detail in van der Marel et Auriga/Ophiuchus
one,
confirmingthat theLupus
disks tend to
ingweinapply
the denseand geometricallythin anddiskfaintermidplane.
Based
on
where
⇣ isIn the dust-to-gas mass ratio, assumed to be constantal., in prep. Conversely,
our modelingto all the disks be larger
than the Taurus-Auriga/Ophiuchus
ones.
in the sample for which
gap is not observed
the synthesized
thea conservation
ofintheenergy delivered
byassumed
the stara distanceonto thedisk
this study weof 200pc for andthe disks
in theto the typical ISM value ⇣ “ 0.01. The choice of the
equal
(下図)
LupusはTaurus-Auriga/Ophiuchusと比べて暗く(=質量が小maps: among these disks,
five
of
them
are
found
to
have
surface
Lupus
III
cloud,
howeverrecentmeasurements
of
the
Gaia
surface and on its propagation to the disk midplane, the two- profile spacein Eq. (1) and of a constant dust-to-gas ratio are a clear
densities inwardly decreasing that are compatible with partially telescopesuggestcould
at a distance„ 150 pc, atclear hole
( “they´1.0andbe closer,“ ´0.8)locatedofrespectively
layer approximation is thus appropriate
reproducing
simplification
which
them
even
depleted gaps.
Rhole would« for
41makeauandRhole« fainter.
34theau, disk
for J16102955-3922144
the of reality, in which we expect ⇣ to change acrossさく)大きい円盤を持つ傾向にある。1-2Myrの差(Lupusの方が古
In
order
to
test
whether
the
Lupus
disks
are
e↵ectively
lessemission
at mmwithwavelengths(Isellaal. 2009;
Ricci
et al. 2010;For Sz 100, one of
the three sources
possible cavities,
fit etis moreuncertain(uncertainty
on is large),a marginal
thewithdisk
from both observational (de Gregorio-Monsalvo et al.
massiveandofmore
extendedthantheTaurus-Auriga/Ophiuchus
we obtain a robust fitTrottawith “et´1.5
that
confirms
thepresence
evidenceacavity
at
R
«
31
au).
The
findings
of
our
fits
hole
al. 2013; Testi et al. 2016). we need to check whether
2013)
and theoretical(Birnstiel & Andrews 2014) arguments.
the twosamplesare distinguishof an inner hole with radius Rhole « 46 au, where we defined ones,
are confirmed
from
the
fact
that
all
these
disks
exhibitvisibilい)を考慮すると、これは粘性進化を表しているかもしれない。
able
aet
direction
perpendicular
toettheinferred
averagecorprevious studies (Andrews
al. deprojected2009;
Trottaal.
However,sinceRhole as the radius where ⌃Following
ity alongprofiles(cfr.
visibility
plots
in in
AppendixA) in this study we are only analyzing the dust cond pRq peaks. Unlike Sz 100, the otherrelation.
To
do
that,
we
proceedasfollows.
First,
weconsidertwo sources with possible
Sz et
123A
and J16070854whose realthepart gas
tendssurface
toward (andin some cases
reaches)nega2013;cavities
Tazzarial. 2016),
we parametrize
densitytinuumemission,
we cannot pose any constraint on the actual
thetwosamples
as a single
sampleand webrightness
perform a oflinearre-with3914075 were excluded
fromoursample,theformerbecausetive
values,compatiblewiththesurfaceadiskwith a self-similar solution for an accretion(Lynden-Bell& gas-to-dust(same disk
Bayesianalgorithm used above),finding a corre- variations in the disks. These choices are useful as
it is a binary, the latter because it is edge-on. Finally, four out gression
a centralcavity.
The othertwo disks classified
as TD (Sz 112
太陽系から導かれる円盤のダスト表面密度よりも、Lupusは浅い•••

lation:of the six disks classified as TD but with no evidence of cav- and J16011549-4152351) were excluded from our sample due
ities in the continuum maps were included in our sample: for log
to Fa890low
integrated flux (below 4 mJy) and due to the lack(9) ofµm “ p0.8 ˘ 0.2q log Rc ` p0.8 ˘ 0.2q ,Fig. 11. 890µm integrated flux (normalized to a common distance of
Sz15084pc)and
MY
Lup
we
deriveasurfacedensity
profilewithastellarparameters,
respectively.
as a function of exponential cut-o↵ radius, constrained by fitting spatially resolved observations with angular resolution better than with correlation coefficient of 0.80 ˘ 0.06 and a standard deviArticle
10theof 890µm
390.75”. number,
For somepage
disks,
flux was extrapolated from the mea- ation of 0.08 ˘ 0.02. As expected, the correlation results paralsured 1.3 mm flux assuming an average spectral index ↵ “ 3.0. Yel- lel to those derived for the two samples considered separately
low elements are Taurus-Auriga/Ophiuchus disks from the Andrews and with a vertical o↵set intermediate between them. Then, for(2015) compilation; blue elements are Lupus disks analyzed in this pa- each disk, we computed the distance from the fit f it , which isper. Gray lines represent the correlations found by the Bayesian linear defined to be positive for disks more massive and smaller thanregression for the Taurus-Auriga/Ophiuchus disks (dash-dotted), for the the linear relationship in Eq. 9, and negative for disks that are5
Lupus disks (dashed), and for both the samples taken together (solid).
less massive and larger. In Fig. 12 (upper panels) , we show the

Article number, page 3 of 39

プロファイルと大きなサイズを持つ。これは太陽系の惑星/微惑星が形成後に外部から内側へ移動したことを示唆しているのかもしれない。

Dust properties of the cometary globule Barnard 207 (LDN 1489)
Aditya Togi1,2 , A.N. Witt1 , Demi St.John3,4

Ritter Astrophysical Research
centre,University of Toledo, 2825 West Bancroft Stree(左上図)ClassTheI 原始星であるB207を多波長観測した。
•
2
Department of Physics and Astronomy, The University of Texas at San Antonio, One U• (左下図) 温度9.4-11.1K、コア密度5.6×105cm-3、コア質量5.6MsunはTX 78249, USA
3
典型的なglobuleと似ていた。
Institute of Engineering, MurrayState University, Murray, KY 42071, USA
4
Department of Physics, Montana State University, P. O. Box 173840, Bozeman, MT 5971
1

Togi, Witt & St.John: Dust properties in B207

Dec (J2000)

30′00′′

25′00′′•

20′00′′(右下図) ダストのアルベドは0.54(Uバンド)から0.84(Iバンド)まで波長

E-mail contact: aditya.togi atutoledo.edu
と共に増加しており、ISMより大きなダストの存在が示唆される。
asdf+26◦15′00′′

Barnard 207 (B207, LDN 1489, LBN 777), also known as the Vulture Head nebula, is a
NIR, MIR, FIRの観測から大きなダストがglobule全体に分布している•
Taurus-Auriga-Perseus molecular cloud region. B207 is known to host a Class I protostar, I
ことがわかった。
at a projected distance of ∼8,400
au from the dense core centre. Using imaging and photome
range, from UV to sub-mm,
we study the physical properties of B207 and the dust grains c• コアで形成された大きなダストが乱流によりリムまで拡散したと考themass
optical depth areτ = typical. The column density,
can be globules found in the Milky Way intersdensity, temperature, andobtainedof N(H),other
えられるが、その場形成の可能性は除外できなかった。
fromτ increasingM
increasein thewith
opticalwavelengths, along with the detection
Region160µm 250µm
350µm dust
500µm
Talbedo
N(H)N(H) =M(H)N , (H)×T(1)
κK × mMJy/sr MJy/sr MJy/sr MJy/sr
K
10 cm
MM
10 cm
1(south)
1.75
2.66
1.97
1.01
–
–
–
infrared,
indicates
thepresenceof larger dust grains in B207. The measured optical, ne
2
0.30
3.28
2.21
1.36
–
– where – = 110 is the adopted hydrogen gas-to-dust mass ra3
9.21
15.3
9.54
5.00
14.1
2.46tio in the
0.04
4.01 (Sodroski et al. 1997) and κ issolar 11.6
neighbourhood
intensities
agreement
with
CMM+AMMdust
grain type oFilterτ 2.85 a andτ
I CMM+AMMI
SB
a
4
28.7
45.6 are31.3 in15.1
13.6
8.13the dust0.15
11.1
13.7We used
opacity
at 500theµm.
thevalueISRF
for κ
=
5
47.8
79.5
57.6
28.9
13.0
17.3cm g 0.32
10.6 et al.29.9
U for AMM
4.77 and
0.721
1.338
0.259
0.273
0.54±0.05
from Köhler
(2015), average
AMMI0.625 0.135
6
63.8
121
101
49.1
35.9type dust
0.66
10.1
58.5
B
5.55 0.624 0.648 0.110
1.497
0.839
0.361
0.65±0.05
grains.
Evolution
for12.0
Solids(THEMIS),suggesting
mantleformationon the d7
69.8
151Model
136
78.2
11.1Interstellar
71.6 The1.31
117 box is 50
V0.485 0.671 0.080
1.528
1.811
0.468
0.74±0.05
spatial 9.40
width of each×100 6.41= 0.034×0.068
8(core)
117
201
170
89.4
11.7
69.6pc for 1.27
10.1 distance
107of 140 pc. After
R estimating
6.80 0.402
1.425
2.361
0.511
0.77±0.03
an assumed
the col-0.676 0.065
9
115
182
135
63.9
12.9
38.5
0.70
10.6
66.0
Iturbulence
0.045
0.911responsible
3.272
0.625
0.84±0.03
globule.
We
investigate
thepossibilityoffor
diﬀusing dust gr
umn density,
we calculated the massof thegas6.37
column0.259
in each0.656 being
10
58.5
99.8
74.0
34.4
13.0
20.6region. 0.38
11.1
31.2temperature,
The FIR
intensities,
density,a. Thecolumn
values of
ISRF, and
DGL, and SB
are in units of 10 erg/s/cm /A/sr. The ISRF for diﬀerent wavelengths are from
44.1
78.1
54.8
25.6
13.4
14.1mass of0.26
20.5 are listed
the gas11.6of each region
Summing
Porterin&Table
Strong1.(2005).
to1112 externallayersofHowever,in
situ
formation of large dust grains cannot be
27.4
57.3 outer
39.9
18.9
13.3
10.6up B207.
0.19
12.7
12.0
the mass estimates, thetotal gas b.
mass
is about
5.6 extinction
M (not optical depth and albedo of the dust in the sky adjacent to B207 assuming R = 3.1. The albedo
τ anda are the05m00s40s

20s
04m00s 4h03m40s
RA (J2000)

Fig. 2. Overlay of our rectangular cut region on the core of B207 on
a SPIRE-Herschel dust emission map at 500 µm. The rectangular box
towards the lower right in the image measures the background intensity.

Fig. 4. Temperature profile of B207 obtained by fitting the SED at the
FIR wavelengths. The temperature decreases to about 11 K in the corecompared to the surrounding medium of 14 K. We used these estimatedtemperatures in Planck’s function to calculate optical depths at 500 µm
to estimate column densities. The column density, N(H), at the core isabout 7.2×1022 cm−2 , causing an extinction of about AV = 48, assuming
RV = 5.5 for molecular clouds, and assuming the aggregate (AMM and
AMMI type) dust grain opacity from Köhler et al. (2015).

A&A proofs: manuscript no. aa_rev6_revised

500

I500
B500µmTable 1. Measured FIR intensities of B207 and derived physical properties

H

21

−2

⊙d

Abel 500

500

Abel
21
H

−2

A&A proofs: manuscript no. aa_rev6_revised

MH
Md

Table 4. Dust characteristics
500

2

500

−1

′′

abs

DGL,sky(0.78×IDGL,sky +S Bmax )
IS RF

max

c

′′

2

Fig. 3. Measured background subtracted integrated FIR intensities foreach rectangular region as a function of core distance. The zeroth posi⊙tion is 13
the centre 20.3of the central
rectangularequatorial
41.5
27.6box with
13.3
13.7coordi-7.01including
0.13
13.3
7.50
valuesarefromDraine(2003a).
heavy
element
correction).
Figure4showsthetempers′′nates RA, Dec =32.7+26◦ 19′ 3221.1.
14 = 4h 4m 47
13.4
10.1
13.8
5.20
0.09
–
–

max

−8

2

V

is theaverageabsorption optical depth of photons after their first scattering, τ = 0.5(1 − a)τ
ature and the column density profile c.
forτ B207
over
our selected15(north)
11.7
28.2
18.2
8.48
13.8
4.35regions.0.08–
d. aboutI
diﬀusegalactic light adjacent to B207, derived by using aI(1 − e )eAcceptedby
A&A
The temperature
at– the core is
11isKtheandthe peakTemperature, column density and mass for regions 1 and 2 were not column
estimatedsince they
the peakintensity
density,
N(H), is 7.2×10 cme. S. B
This iscolumndensity
is of the globule after subtracting the nearby background sky intensity.
abs

22

DGL,sky

−2

IS RF

abs
−τ

−τabs

max
erage
individual
intensities
are outsideof thebackground-subtracted
globule in ′′the diﬀuse
sky
region. over the strip equivalent to an extinction of A = 48,
′′
f.
The
quantityR(0.78×DGL+SB
assumingmax)/ISRF is the ratio of the maximum intensity at the rim of the globule to the intensity of theV
V = 5.5 forofThe
15 column
boxes, eachof size
50 and×100. Thesemeasuredvaluesforof each region using thedensity,
N(H),
mass,
M(H),
are calculated
illuminatinginterstellar
radiation
field.
renormalized
case
A
from
Weingartner&
Draine(2001);
DraineFIR
intensities
at 160,and at500
plottedin Fig.
AMM
and AMMI
dust250,
mass350,
opacity
500µm
µmare
from
Köhleret al. (2015).
g.
The
albedoofthecloud,a,evaluatedfrom the corresponding ratio (0.78×IDGL +SBmax )/ISRF assuming the forward scattering(2003a).
Whenconsideringanalternate
dust
mass
opacity
κ
c
500
3.The
Thetemperature,core centre Tis at, thezeroth spatial position in the plot
Abel and column density, NAbel (H), are the temperature2 and theasymmetryparameter,
0.6
≤
g
≤
0.9
from
Fig. 6, Witt & Stephens (1974).
=
5.04
cm
/g
at
500
µm
for
dust
grains
with
thin
ice
mantlesatwithnegative andpositiveoﬀsetssignifyingestimatedthe direction
corresponding
columndensity,respectively,from fromthe Abel inversion method.6−3
centraldensity
10cm(Ossenkopf&
Henning1994),
thecolsoutheast to northwest.
6 by a factor
density and mass in each region was reduced
Spectral energy distributions (SEDs) were constructed and umn
Table 5. DGL and optical-IR-submm sky-subtracted intensities forwavelengths
the3.2conversion
5.04=1.77 and the total mass reduces from 5.6 toM⊙ . Thisfrom DN to Jy units is adopted fromhttp://arxiv.org/pdf/1707.07925

Fig. 9. Core+DGL (red circles) and rim+fDGL (blue squares) intensities
of B207 as a function of wavelength. The solid and dashed lines in thenear-to-MIR and FIR are the scattering and emission spectra of dust, reAS spectively. Diﬀerent line colours (black, green, red, and blue) represent
re- Dust
John:
properties
in B207
CM, CMM,
CMM+AMM,and CMM+AMMI grains, respectively.
star
the
core
ine
Simi- the V band and scaled this value to applicable optical depths forThen(R)that the other bands by using the dust model of RV = 5.5. The values
rence
in- of DGL and fDGL for the direction of B207 are listed in Table 5

EMIS for wavelengths from the optical to MIR. In Fig. 9 we plot our, this intensities after having added the DGL and the fDGL for the cores that and rim, respectively, along with the THEMIS model values of−2
ma pro- CM, CMM, CMM+AMM, and CMM+AMMI from Ysard et al.
er- in (2016).
ult
M,
This
the
sence
al.
f the 4. Results and discussions
ual
proer- 4.1. Physical properties of the globuled-IR,
al. 4.1.1. Temperature
6
ar-IR
10
outerins Assuming a single temperature black body to fit the SED at FIR
the dust temperature at the core position is estin the wavelengths,
acFig. 10. Our derived rim dust albedos (black circles) are calculated
to be about 11 K. The core temperature is about 3 K lesstype. mated16)
using the ratio (0.78×IDGL + SBmax )/ISRF and plotted along with thethe dust
temperature
thefullouter
regionsofofCM,
the globnical thanenTHEMIS
model
values forinthe
sizewarm
distribution
CMM,
ule.
With
the
Abel
Inversiontechniquethemeasured
dust
tempared AMM, and AMMI grains. The grey circles are dust albedos estimatedobat thecore is foundto (using
be aboutthe)/ISRF).
SEDrrema- peratureassuming
no reductionin DGLthe 1.7
ratioK(Iless+ SBmax
DGL thanA reductionof 13% and 7%
in albedo
valuesisarein U andwith
B bands,
bility measured
temperatures.
Thisdiﬀerencein seenagreementtherespectively,
withbyinsignificant
for a and22%
opti- results
obtained
Roy et al.changes(2014)at higher
for thewavelengths
globule B68
ndreductionin
DGL
intensity.
eringm- L1689. The SED technique uses the measured FIR intensities
outerlist averaged over the line of sight. The outer area of the projected•(上図) SEDをモデルと比較すると、コア(赤点)とリム(青点)の両方において、CMM+AMMI、CMM+AMMダ
ストモデルと一致した。

•

つまり、globule全体でダストへのマントル形成が起
きている。

•
•

CM (core mantle): 成長していないISMダストモデル。
CMM (core mantle mantle): 分子雲の端に存在するような、2番目のH-rich carbon mantleを持つダストモデ
ル。

•

CMM+AMM (+aggregates): 分子コアの外側にあるよ
うな、CMM粒子が集まってアグリゲイトを形成するモデル。

•

CMM+AMMI (with ice): 高密度コア領域にあるような、CMM+AMMのアグリゲイトに氷マントルが形成されたモデル。

•(下図) ダストのアルベドの波長依存性を見ても、少なくともISMのダスト(CM)は除外されている。
7

Constraining accretion signatures of exoplanets in the TW Hya transitional disk
Taichi Uyama1 , Takayuki Tanigawa2 , Jun Hashimoto3 , Motohide Tamura1,3,4 , Yuhiko Aoyama5 , Timothy D.Brandt6 , and Masato Ishizuka1
1

Department of Astronomy, The University of Tokyo, 7-3-1, Hongo, Bunkyo-ku, Tokyo 113-0033, Japan
2
National Institute of Technology, Ichinoseki
College, Hagisho Takanashi, Ichinoseki
021-8511, Japan
多重リング円盤が見つかっているTW
HyaをNIRで直接撮像し、原始•惑星への降着があるかどうか調べた。

•

37

原始惑星へ降着しているとPaβ (1.282µm)で明るくなり、それは黒体
輻射よりも高い強度を持つ。

Figure 1. FOV arrangement for observations. Each rectangle
represents a separate FOV. The red circle indicates the central star.
The vertical and horizontal axes represent the angular distancefrom the central star. These settings avoid the central star together
with an inner square of 0.5′′ ×0.5′′ , which allows suﬃcient exposure
time without saturation.

the pipeline usually removes hydrogen, which means Paβ
in our data cube is not aﬀected by telluric correction.
To achieve high contrast, we used a spectral diﬀerential
imaging technique (SDI; Smith 1987). We selected sevenchannels around the Paβ wavelength as a science channel with a width of 1.05 nm and other 24 channels between 1.278 and 1.285 µm as continuum (reference) channels. We avoided the OH airglow region (Maihara et al.
1993) when selecting reference channels. The airglow skylines remain in the data cube because they are used forwavelength references in the pipeline. We made reference
PSFs for each FOV using linear combinations of the reference frames based on equations (2)–(4) in Artigau et al.
(2008) to determine the coeﬃcients of the reference images.
In 2.
thisPaβ
process,
dividedthe FOV
into 12annu- with
Figureimage weof thefirst FOV.
The imageis alignedlarin a1.similarmannertonearthe thelocally
optimized
thatregionsin FigureThe blacksquareupper-rightvertex is
combinationof images (LOCI) method (Lafrenière et al.
a badpixel cluster.
2007).
Following SDI data reduction, no point sources weredetected in any of the FOVs. Figure 2 shows the Paβ
image that was produced by combining the seven channels of the science frames, and Figure 3 shows the final
SDI-reduced image for the first FOV. In the Paβ image,
because of low AO performance, a stellar halo is evident
near the central star where there is expected to be remnants of subtraction in the SDI-reduced image due toPoisson noise. We then normalized all of the images bydividing by their integration time, and convolved themwith an aperture with a radius equal to half the FWHM
of the central star. The FWHM was measured in theunsaturated frames to be ∼60 mas. We calculated thestandard deviation for each FOV and produced a radialnoise profile. We masked badpixels in this process and
they
do 3.
notSDI-reduced
aﬀect on calculating
thefirst
noise.
Figureimage of the
FOV.The
Thetypicalalignment is
the same as in Figure 2.

noise was compared to photometric results for the central•••(上図) 中心星を避けて4つの領域に分割したField of view。
(中図) 1st FOVのPaβ画像。
3(下図) spectral diﬀerential imaging (SDI)では降着なしだったが、Paβ

calculated based on the J-band flux of TW Hya, we define the error in the detection limit as 5%.
3. DISCUSSION

放射の5σ検出限界を0.”4で5.8×10-18, 1.”6で1.5×10-18 erg/s/cm2と導We investigate the presence of potential protoplanets
within TW Hya’s disk in two diﬀerent ways. Section 3.1
presents a conventional approach that assumes mass accretion from circumstellar disk onto the central star andignores the inability to distinguish between the mass andmass accretion rate. Section 3.2 proposes a new method
for interpreting the detection limit by considering circumplanetary disk mechanisms. We focus on the two
notable gaps at 0.′′ 4 and 1.′′ 6. We assume that these locations represent ∼25 AU and ∼95 AU using the distancedata (59±1 pc) published by Gaia Collaboration
et al.
J(2016), whereas previous studies have assumed that thegaps are at ∼20 AU and ∼80 AU based on data publishedby van Leeuwen (2007). We assume that extinction of
the Paβ line by the circumstellar disk is negligible. TW
Hya’s disk is almost face-on (Qi et al. 2004, 2008). The
vertical direction from the jovian-mass protoplanet canbe estimated locally clear for Paβ (Tanigawa et al. 2012;
Aoyama et al. 2017).

出できた。

•

円盤と水素放射のシミュレーションから原始惑星質量も求められ、25auに1.45±0.04M , 95auに2.29(+0.03 -0.04)MJがあることがわかり、これは以前の惑星検出限界とも一致している。

3.1. Using the Empirical Relationship

The Paβ luminosity of YSOs has been reported to havean empirical correlation with the accretion luminosity(Natta et al. 2004, 2006) for objects down to ∼10 MJ(e.g. GSC 06214-00210 b and FW Tau b; Bowler et al.
2011, 2014). The relationship is given by
log(

Lacc
LPaβ
) = 1.36 × log(
) + 4,
L⊙
L⊙
8

(1)

where Lacc is the accretion luminosity and LPaβ is the