星形成ゼミ
SFN #301 (15-21本目)
百瀬宗武（茨城大・理）ハイライトは以下の３本（特に最後の）• #16: Robo-AO Discovery and Basic Characterization of Wide Multiple Star Systems in the
Pleiades, Praesepe, and NGC 2264 Clusters (Hillenbrand et al. AJ, 155:51 (15pp))• #18: A search for pre- and proto-brown dwarfs in the dark cloud Barnard 30 with ALMA
(Huélamo et al., A&A 597, A17)
• #19: The ALMA-PILS survey: 3D modeling of the envelope, disks and dust ﬁlament of IRAS
16293‒2422 (Jacobsen et al. A&A in press)

16. Robo-AO Discovery and Basic Characterization of Wide
Multiple Star Systems in the Pleiades, Praesepe, and NGC
2264 Clusters

The Astronomical Journal, 155:51 (15pp), 2018 February
・イメージングの実際

stacked image

Hillenbrand et al.

PSF

PSF subtracted

L. Hillenbrand et al. (AJ, 155, 51)
http://ads.nao.ac.jp/abs/2018AJ....155...51H【背景】(1) バイナリーの頻度分布については，様々な依存性が議論され
The Astronomical Journal, 155:51 (15pp), 2018 Februaryている（Field stars vs. YSO clusters や Open clusters；中心星質量依存性など）。(2) 装置面では，小口径用望遠鏡に開発されたフルオートのlaser ガイド付き Robo-AOを開発，多天体サーベイに威力発揮。

Pleiades, Praescepe, NGC2264の全構成メンバーの約10%（J等級=1013.5）について，波長600nmイメージングによるbinary探査を実施。
距離年齢

Pleiades

136 1
pc

125 8
Myr

Praescepe

179 2
pc

757 36Myr

740pc
NGC 2264 あるいは
913pc

~ 3Myr

構成
メンバー
数

今回の
バイナリー 対象のSp.
観測
検出※
Type
ターゲット

~1500

32

K&
early M

8

K&
early M

~1000

~1500

212

108

120

34

Table 2
(Continued)
Cluster

BinaryFGK(YSOs)※ 以前から知られていたのは10%のみ

Signiﬁcanceσ

Projected Separation(arcsec)

Position Angle(degrees)

Optical Brightness Ratio(Δmag)

Mass Ratio[q = m 2 m1]

Figure 1. Shown here are the stacked image cutout (left), CSIMon-1573
the PSF image assembled
from images 0.82
surrounding the leftmost(center), and the PSF- L
5.1
175.0 image in time
4.05±0.13
CSIMon-1824
4.5
0.89
205.1
0.96±0.05
L
subtracted remainder image (right) that isolates the secondary star for AK IV-314, a binary system having separation 1 0. North is up and east is to the right.
CSIMon-6975【研究内容】パロマー60インチ(1.5m)望遠鏡 + Robo-AOを組み合わせ，Hillenbrand et al.

10.3

2.37

51.3

1.08±0.12

L・コントラスト
カーブの例(左) stacked image上(右) PSF差引後※ 0.2” = 2λ/D 以内の
5. Contrast curves for three stars of varying image quality; raw contrast is on the left and PSF-subtracted contrast on the right. The stars illustrated are: AK IV伴星検出は不可能 Figure314, which was one of the most well-imaged stars, but is a binary system with separation of 1 03; the secondary has been subtracted before generating the contrast
curves (resulting in the artifact discontinuity around 1 6). HCG-156 is representative of the mean performance, and is a single star. HHJ-407 is about one standard
deviation away from the mean performance. As illustrated in the right panel, PSF subtraction improves the contrast by several magnitudes, though companion
detection is still not possible below ∼0 2 (roughly 2 ´ l D ). The broad bump for AK IV-314 is the residual of the seeing halo of the subtracted companion.

Figure 2. Example PSF models, evaluated at whole pixel values and matched to cuts across Robo-AO image data. Left: 2D Moffat model of source BPL 167. Because
The Astronomical Journal, 155:51 (15pp), 2018 February
Hillenbrand et athe peak of the model is not located at the centerofapixel,
andpartialpixel
valuesareinterpolated
in
the
plot,
the
peak
is
not
well-represented
graphicallybutisbetterthe binaries, just ﬁve, two, and zero in the three respective
binaries in the 30–500 au range in the Pleiades and Praesepe
estimated numerically. This model matches theimagewerewings,
but slightly
overestimatestheasFWHM
the imagesamples,core. Right:
Gaussianmodel
sourceCSIMonand to2D
highercontrast
levelsofthan
in NGC
2264.
clusters
revealed
in a literaturesearchhavingintheir
0722. Relative to the Moffat model, the Gaussianmodel
bettermatches
the
FWHM
in
the
image
core,
but
is
worse
in
the
image
wings.
Notably,
there
are
many
imagesonwhichbinaries
arecompanions previously known. These conﬁrmations (10% of
detected at magnitude differences exceeding the individual
our reported binary sample) provide conﬁdence in our methods“raw” contrast values
listed inTable 1 and/or
more thethan threeand detections
overall. Furthermore,
the ﬁrst
consideraused to determine multiplicity and measure
the propertiesof the they allowWeﬁt two-dimensional
Moffatfunctions,using
standard deviations better than the nominal contrast at a givention of color information because the previously identiﬁed
secondary.
form
separation (left panel of Figure 5). These high contrast outliers
binaries had been observed at infrared wavelengths. We expect
are due to the use of PSF-subtracted images, which were
the separations to be about the same, given the large cluster-a
2 + images.
⎛
generated(xfor- allxo)ﬁnal( y - yoThe)2 ⎞ PSF-subtracted data
distances, but our reported magnitude differences will be larger
x , y) = Anaturally
better contrast,⎟ ,down to less than
⎜1 + have signiﬁcantly
the optical than in the infrared, due to the expectedf (redder
2
3.3. Image QualityinAnalysis⎝g
5 mag for most targets, as illustrated in⎠the right panel for thecolor of the fainter companions, relative to their primaries.
three examples shown in Figure 5. Five binary systems have
8 presents theofimage
Image quality was used to assess theFigure
performancethe gallery
AO of our Robo-AO detected
brightness
ratiosof moreposition,
than four magnitudes.
Twotheof these,
where
x
and
y
describe
thecentroid
x
and
y
are
binary systems. There were 78 images containing
candidateoosystem and to determine the signiﬁcanceof the point sources
including the most signiﬁcant outlier at the smallest separabinaries, with 70 unique sources—excluding
repeats coordinatesand poor
spatialon theand inA,theγ,initial
andimage
α arefreebut are
tions,
couldimage,not be seen
cutouts,
detected in an observation.
quality images. Figure 9 illustrates the magnitude differences asclearlyin the(and wereas
detected
parameters.
Following
thepresent
proﬁleﬁt,PSF-subtracted
its FWHM images
was deﬁned
a functionof pair
Sources detected
at higher contrast
We modeled the primary PSF on eachimage
toseparation.
assess image
in that manner). The other high-brightness-ratio systems werethan the thenominallimitsfrom better-than-average quality
quality and monitor its variation acrossdata
set.come
Highidentiﬁed in the non-PSF-subtracted
data in observations with
1 a - 1)0.5.
=
2
g
(
2
images or from the PSF-subtracted images; we note that this FWHM
exceptionally good contrast curves.
quality images have smaller FWHMs
and are produced whensubset of high-contrast companions is located within ∼1″–1 5,Results for the individual clusters are presented below. The
the AO correction delivers a diffraction-limited
PSF.
Largersuggesting that they
are truebound companions.
medianimage,In anyThegiven
numberfractionof pixels
at threeessentiallytherawthemultiplicity
across theclusters, countingaseparation
1 1, with the bypeak between ∼0 5–1 0, andFWHM images occur when thepairPSF
is isdominated
total
of
70
visualbinarysystemsamong
441
distinctly
imagedbackgroundsky level far exceeds the number of pixels withdeclinetoward aDueﬂat distribution
beyond∼2″. Beyond
targets with good Robo-AO imaging, is thus 15.9%±1.9% (oruncorrected atmospheric turbulence,continued
or poorseeing.
to・separation
vs. ΔMagThe Astronomical Journal, 155:51 (15pp), 2018 February

Hillenbrand et al.

• プレアデスとプレセペの質量比分布
The Astronomical Journal, 155:51 (15pp), 2018 February

プレア
デス

プレセ
ペ

NGC
2264

※ 0.2-0.9の範囲に分布

Hillenbrand et al

Figure 10. Magnitude difference as a function of system composite color (left) and corresponding inferred mass ratio as a function of primary mass (right) for the
Pleiades (red, with upper limits indicated by inverted triangles set by the lowest masses available from the adopted evolutionary tracks) and Praesepe (blue) binary
samples. As the distributions are dominated by small-number statistics, no conclusions can be drawn beyond illustration of the range in q of the detected binaries

・水色：観測しなかった天体
・黄色：観測，単独星
・赤色：観測，バイナリー
・黒線はisochrone 理論モデルから期待される色等級図のライン

Praesepe, previous similar work (notably by Bouvier et al.
solar neighborhood ﬁeld stars. Our observations also targeted
only a narrow magnitude range, which corresponds to differen
1997 in the Pleiades, and by Bouvier et al. 2001 and Patience
primary mass ranges and secondary mass sensitivities at theet al. 2002 in Praesepe) has been conducted at infrareddifferent cluster distances. Thus, we can not make meaningfu
wavelengths, though in sum covering a comparable number ofcomparisons to the features of the ﬁeld star distributions instars to our study.
either separation or mass ratio.
We identiﬁed 66 unique binary systems, only seven of
Nevertheless, the results of our work broadly sample mass
which were previously known. Given the small contrast ratios
ratios q = m 2 m1 = 0.2–0.9 around primary stars withand close separations, the majority of the newly identiﬁed~0.4–0.9 M:. The measured parameters for individual objects
companions are likely to be physically bound. Toward thewill be valuable for future studies aimed at placing the
low-contrast widest pairs, and the highest-contrast close
multiplicity results for single-age clusters in the context of ﬁeld
pairs, boundedness becomes less likely. We can assess thestar samples with diverse ages, though better characterized
likelihood of chance superpositionof faint foreground全体としてのBinaryor検出率はmultiplicity properties. Additional high spatial resolution
background objects using a simulation of galactic stellar
survey work that would complete our multiplicity census for
populations. We queried the TRILEGAL (Girardi et al. 2005,
these important clusters should be carried out.
2012) V1.6 model9 over 1 deg2 ﬁelds toward each of theclusters, so as to establish a representative sampling of theWe acknowledge the Caltech SURF (Summer Undercontamination on scales of a few arcsec. The raw star counts
graduate Research Fellowship) program for partially supportingbrighter than i=17 mag (see Figure 4) were scaled down to
the work of C. Zhang. Russ Laher provided appreciatedRobo-AOʼs 8 6 by 8 6 ﬁeld of view, to arrive at a respective
guidance on use of the APT. Luisa Rebull provided the catalog
0.0025, 0.0181, 0.0087 contaminating stars per observation
photometry used in creating Figure 7. We thank Emma
toward the Pleiades, Praesepe, and NGC 2264 clusters, as
Hovanec for literature research on the targets of this study
expected. Multiplying by the number of sources observed in
The Robo-AO system at Palomar was supported by theeach cluster results in 0.5, 2.0, and 1.0 expected interlopers

15.5 ± 2 %18. A search for pre- and proto-brown dwarfs in the darkcloud Barnard 30 with ALMA

【観測・解析】• Baseline = (15-395) kλ，0.95” × 0.50”，検出できる最大サイズ ~ 6”

S. K. Huélamo et al., A&A 597, A17
http://ads.nao.ac.jp/abs/2017A%26A...597A..17H• 30のコア中ALMAの検出は5個(Fig1)，全てλOri の電離領域中に存在
A&A 597, A17 (2017)【目的・内容】褐色矮星の起源を探る一環として，Lambda Orionis 中に

LB08

LB14

LB10

LB19

LB31

ある暗黒星雲 B30中のコアの小質量側を探査。APEX/LABOCA の870μm
ダスト連続波広域マップをもとに同定された30のコアを，ALMA
880μm
N. Huélamo et al.: A search for pre- and proto-brown dwarfs in the dark cloud Barnard 30 with
ALMA
で観測（Cycle 1）。APEX/SABOCA 350μmデータも補助的に使用。
B30

5"Spitzer MIPS/24 microns image

2

λ Ori

Table 1. ALMA 880 µm detections in the B30 region.

3

4

Fig. 2. The five sources detected at 880 µm with ALMA in B30. North is up and east to the left. The ALMA beam size is displayed at the bottom
right corner of each image. The white dashed circles represent the ALMA beam (1800 diameter), and are centered at the pointing coordinates (phasecenters) for each source.

2ºIRAS 25 microns

LABOCA 870 microns
ALMA pointings

5

ALMA detection coordinates
RA(J2000)Dec(J2000)[h m s][ 0 00 ]05:31:22.97 +12:11:34.7
05:31:09.29 +12:11:08.8
05:31:19.46 +12:09:15.1
05:31:27.81 +12:05:30.9
05:31:15.32 +12:03:38.2

Separation fromphase center[arcsec]
8.7
6.8
4.5
4.2
0.6

LABOCA
sourcea
B30-LB08
B30-LB10
B30-LB14⇤
B30-LB19⇤
B30-LB31

S⌫
[mJy]
5.70
2.20
44.0
10.7
0.60

rms
[mJy/beam]
0.26
0.23
0.25
0.20
0.13

Mass
(ALMA)⇤⇤[MJup ]
9
3
67
16
0.9

Mass
(LABOCA)b,⇤⇤[MJup ]
106
46
51
182
82

Missing
fluxc
[%]
87
93
0
86
99

Av d

[mag ]
2.5
1.2
2.0
2.8
2.4

Tentative
natureVeLLO/pre-BD
pre-BDYSO
YSO
pre-BD

6

LB08 97
12

Notes. (a) LABOCA designation number (see BGH16); (b) From BGH16; (c) Percentage of missing flux between ALMA and LABOCA data;(d)
From the 2MASS extinction map; (⇤) Sources with gas emission detected with ALMA; (⇤⇤) Derived for a dust temperature of 15 K.

LB10

13

11

成分も検出

SABOCA 350 microns
LABOCA

15

17
14

18

1

7 8
2

1'

15

20 9
27 13
16 17
251026 12

23LB19
21 22
6
5
24
3 4

11
30

LB31

beginning of each observation. Flux calibration was performed
using Mars and Uranus as primary calibrators, and HL Tau,
V883 Ori, VY CMa and CRL618 as secondary calibrators. The
absolute flux calibration uncertainty is estimated to be ⇠30%.
Our map was centered at RA = 05:31:20.5, Dec = +12:05:45,
comprising a region of ⇠800 ⇥400 . For processing the data we used
the Bolometer Array Analysis Software (BOA2 ) and CRUSH3(see Kovács 2008) software packages. Data reduction processing
included flat-fielding, calibration, opacity correction, correlated
noise removal and de-spiking. Every scan was visually inspected
in order to identify corrupted data. We used and optimized dataprocessing to detect faint point-like sources (options -faint -deepin CRUSH). The final image was smoothed to a resolution of
10.6 arcsec. The total on-source observing time was 4.5 h andthe rms reached was ⇠50 mJy at the central areas of the map.
We detected a total of 17 sources in the SABOCA map (seeFigure 1) with SNR between 3.0 and 4.6. Their coordinates cor-

• ALMA観測のボーナスとして広がったCO(3-2)に埋もれたコンパクト

LB14

16

mainly resolved out, in the primary beam of most of the positions observed in the southern region of B30, and very faint gas
emission inside the primary beam of some of the positions surveyed in the northern part of the cloud. The vlsr of the CO(3–2)
cloud emission is ⇠11 km s 1 , consistent with one of the velocity components derived by Lang et al. (2000, 9.43 km s 1 ) in the
average spectrum of the region. The analysis of the ALMA datashows that we have detected gas emission in only two sourcesthat are also detected in the continuum (see Table 1). They are
discussed in detail in Sect. 3.
Finally, we have estimated the relative positional accuracy ofthe observations using Eq. (1) from Reid et al. (1988). Considering the beam major axis (⇠0.900 ), we derive relative positional
accuracies between 0.200 for SNR of 4.6 (LB31) and ⇠5 mas fora SNR of 176 (LB14). The absolute position accuracy is smaller
than the synthesized beam width.

SABOCA• APEX/SABOCAでは 8’ x 4’ (と思う)の領域をマッピング（左図），

ALMA

28
N

29
E

350μm，7.8”ビームで17個のコアを検出

【ALMA検出と赤外線画像との比較】
N. Huélamo et al.: A search for pre- and proto-brown dwarfs in the dark cloud Barnard 30 with ALMA
シアン円：APEX beam

λ Fλ [erg/s/

λ Fλ [erg/s/

緑＋：ALMA検出，黄円：ALMA FOV，

10-11
10-12

検出率 5/30，大部分のLABOCA Coreは6”（2400au）以上に広がった構造

J-band#d

3.6 microns

5.7 microns

24 microns←対応天体なし（CO検出なし）

#b

10-12

10-13

10-13

10-14

10-14

1

LB08

10-11

10
λ [µm]

100

1000

1

10
λ [µm]

100

100

Fig. 5. Observed SEDs of the five ALMA detections. In all the panels, the open triangles andfluxes, respectively, while the asterisks represent the APEX/SABOCA data. Left and middle
LB19. The red circles represent optical to mid-IR data from all our catalogues whenever availa
panel represent IRAS data. Right panel: three ALMA detections with no infrared counterparts:
ALMA detections are color-coded for each source. We have included the limiting magnitudes

APEX/LABOCAで広がっている

CO(3-2)検出(deconvolved size = 27”)#a
5"

ALMA beam

LB10

J-band

3.6 microns

5.7 microns

24 microns

A&A 597, A17 (2017)
#b

-9

10-9

LB19

10-10

0.06

ALMA beam

LB14

J-band

3.6 microns

5.7 microns

24 microns

10-10
10-11
10-12

10-13

-14

10-14
1

#a

10-12

10-13

←対応天体 (Class II)？
10

#c

10-11

10
λ [µm]

星周円盤 (APEXとALMAで同等のFlux)

100

1000

LB14

10-12
10-13
10-14
10-15

0.02

10-16
10.00

LB31
LB08
0.4
LB10

10-11

0.04

Flux [Jy/beam]

5"

λ Fλ [erg/s/cm2]

λ Fλ [erg/s/cm2]

#c

10-10

10
λ [µm]

100

1000

LB19

0.3

Flux [Jy/beam]

10-8

λ Fλ [erg/s/cm2]

10-8←対応天体なし（CO検出なし）
LB14
10

#a

(compact)

0.2
0.1

1

10
λ [µm]

0.0

100

1000

Fig. 5. Observed SEDs of the five ALMA detections. In all the-0.02
panels, the open triangles and squares represent -0.1
the APEX/LABOCA and ALMA
-10
0
10
20
30
-5
0
5
10
15
20
25
fluxes, respectively, while the asterisks represent the APEX/SABOCA data. Leftand [Km/s]
middle panels: we show the complete
SEDs
of
LB14
and
Velocity
Velocity[Km/s]
LB19. The red circles represent optical to mid-IR data from all our catalogues whenever available (see Sect. 2.3). The purple crosses in the LB19
Fig. with
6. Topnopanels:
ALMA
CO(3–2)LB08,
intensity
weighted
velocity(first order moment,
panel represent IRAS data. Right panel: three ALMA detections
infraredcounterparts:
LB10
and LB31.
The field
APEX/LABOCA
and coemissionover-plottedincontours.
The
left
panel
corresponds
to
LB14,
while
the
middleand ri
ALMA detections are color-coded for each source. We have included the limiting magnitudes (black diamonds) of our infrared data.
emission of LB19, respectively. For LB14, contours are 5, 10, 20, 40, 80, and 120 times thecontours are 5, 10, 20, and 30 times the rms noise of the map, 0.20 mJy/beam. Ellipses at thecontinuum and for the CO(3–2) maps. In the case of LB19, the beam for the CO(3–2) image cand <60 K (right panel). Bottom panels: CO(3–2) spectrum in the region of emission of LB1(right) regions of emission of LB19. In the last panel both the compact (dotted line) and excomparison.

M = 24-43 MJ (20-30Kを仮定)
ALMA beam

5"

#b

LB19

J-band

5.7 microns

APEX/LABOCAで広がっている#a#c(deconvolved size = 24”)
M(ALMA) ~16 MJ (15Kを仮定)

5"
ALMA beam#e#d3.1.3. LB08, LB10, and LB31
J-band

3.6 microns

5.7 microns

24 microns

#b

0.06

#a

LB30g

#c
#g

5"

Fig. 4. Infrared (CAHA/O2000 and Spitzer/IRAC and MIPS) images centered on the ALMA detection coordinates. North is up and east to theleft. We have included in all the J-band images (left panels) the position of the ALMA detections (green crosses), and the possible infrared
counterparts to the APEX/LABOCA detections identified by BGH16 (green labels). The cyan diamonds represent the APEX/LABOCA peakintensity coordinates (ALMA phase center coordinates). We have also plotted the APEX/LABOCA beam of 13.800 radius (cyan dashed circle),
the ALMA FOV of ⇠1800 diameter (yellow dashed circle), and the ALMA beam at the bottom left corner (yellow solid ellipse).

Flux [Jy/beam]

0.04←対応天体なし（CO検出も）

ALMA beam

infalling at 400 AU scales near the central protostar. The extended component does not show a clear infalling pattern.

LB14

-0.1

A17, page 8 of 15

0.3

0.02

赤外線の対応天体がないのは，
0.00
VeLLOs（低質量原始星）か
-0.02
-10

0.0

LB08, 10, and 31 are the weakest sources detected with
1.2 at their positions,
ALMA. There is no presence of gas emission
with an rms per channel of 13 mJy/beam,
mJy/beam, and
LB19
1.0 11LB19
18 mJy/beam, respectively.
(extended)(compact)
0.8
While LB08 and LB10 lie in the northern region of B30,
0.6 cloud, well within
LB31 is located in the southern part of thethe ionization front seen in the 24 µm image
0.4 (see Fig. 1). While
LB08 shows extended emission in the APEX/LABOCA map,
0.2
LB08 and LB10 are detected as point-likesources. None of

0.4

0

10
20
Velocity [Km/s]Starless Cores（BDのprecursors)？

30

0.2
0.1

Flux [Jy/beam]

LB31←対応天体 (Class I)？

24 microns

Flux [Jy/beam]#b

3.6 microns

-5

0

5
10
15
Velocity [Km/s]these ALMA dete
regime (Fig. 4).

LB08 shows
APEX/LABOCA
fied an infrared cobeam: LB08a (sesitional accuracy
source is unrelated
is a detection wit
a separation of 2
name 0531239+1
four di↵erent ban
with a positional a
The Spitzer/MIPS

0.0
-0.2
20

25

-5

0

5
10
15
Velocity [Km/s]

20

25

Fig. 6. Top panels: ALMA CO(3–2) intensity weighted velocity field (first order moment, color scale) with the ALMA 880 micron continuum

A&A 597, A17(2017)【SABOCA検出（コントア）とIRAC
3.6μm画像，8μm(SB14)との比較】

SB06

SB02
SB01

SB03 SB04

#a
#b

#b?

LB22f

SB05

LB22a

#c
5"

LB23a
5"

5"

5"

SB12

SB09
SB08

SB07

SB11

SB10

#a

#b
LB19d

LB19b

10"

LB19a

10"

5"

5"

SB14

SB13

SB15

SB17
SB16

#a

#a
#a

LB28a
5"

5"

5"

10"

Fig. 8. Spitzer IRAC 3.6 µm finding charts with the APEX/SABOCA detections, except for SB14 (IRAC 8 µm image). North is up and east to
the left. The green crosses represent the coordinates of the peak emission of the APEX/SABOCA detections. The white contours represent the
APEX/SABOCA emission at 2.5, 3, 4 and 5 level. The infrared counterparts within a radius of 500. 3 (half of the APEX/SABOCA beam) arerepresented by yellow crosses. If previously discussed by BGH16, they are named with the APEX/LABOCA designation. If not, they are namedwith low-case letters. The magenta circles represent WISE detections, the cyan diamonds represent the position of the APEX/LABOCA cores
peak intensity, and the blue circles indicate AKARI detections. The orange square represents a Planck detection (see text).

source LB23a, which is classified as a probable member by
BGH16. Its SED shows a clear IR excess starting at ⇠6 µm. We
also detect a source with WISE slightly further away (5.600 fromevidence pointing towards an extragalactic nature according to
the NED database. As seen in Fig. 10, the object is resolved into
two sources in our CAHA/O2000 near-IR infrared images, andSEDも含めて個々の天体の性質を簡単に議論しているlogarithmically from 0.5 to 7.3 Jy beam 1 km s 1 . The RA and DEC o↵sets are relative to the phase center of the observations.

19. The ALMA-PILS survey: 3D modeling of the envelope,
COの積分強度マップ
S. K. Jacobsen et al.: The ALMA-PILS survey: 3D modeling of the envelope, disks and dust filament of IRAS 16293–2422
to resolve
inner gap and nearby structure prop- 3.4. Dust envelope model
disks and dust refinements,
filament of
IRAS the16293–2422
erly, as etgeometric
such as self-shadowing onto the outer
S. K. Jacobsen
al. (A&A,e↵ects
in press)
disk became important.
http://ads.nao.ac.jp/abs/2017arXiv171206984J

The dust envelope was modeled with a 1D radial density powerlaw density distribution, as the envelope has been well-fitted previously by such models (e.g., Schöier et al. 2002). More compli【内容】PILS(Protostellar InterferometricLine
Survey)で観測している
3.3. Dust opacity& temperaturecated circumbinary envelope structures, such as an infalling, rotating circumbinary envelope were not considered, as we focused
13CO/C17O/C18O(3-2)データを3D輻射
Protobinary (IRAS16293-2422)のWe used dust opacities from Ossenkopf & Henning (1994), on the innermost region of IRAS 16293 in this work. Recent obwhich are good approximations for dense cores (van der Tak servations of GG Tau (Dutrey et al. 2014), as well as simulations
輸送計算で解析 → 星周円盤の構造，それぞれのLuminosityなど議論
et al. 1999; Shirley et al. 2002, 2011). Opacity tables of dust of the same system (Nelson & Marzari 2016) suggest that binary
with thin ice-mantles and another with bare dust grains were star formation results in partial clearing of the material in the inused,assuming
coagulated
dust
grainswithanambientgas
num3つの主要なトピックス
nermost region where the protostellar binary resides. Based on
63
ber density of 10 cm . These dust opacity tables are generally the 868 µm continuum observation, we do not expect the inte131817(i) 2つ中心星がある時の原始星周辺領域の温度構造(特に1Dとの違い)
Fig. 2:・C
Zeroth
maps
of
the
CO,
C
O,
and
C
O isotopologues from the PILS observations. Contour levels are diviused for models of dust around deeply embedded protostars,
in-17moment
Oがもっともダスト連続波と類似(arc構造)：光学的に薄い
rior
to
be
completely
evacuatedofo↵sets
dustarebetween
thedisks,but
1
1
logarithmically
from
0.5
to
7.3
Jy
beam
km
s
.
The
RA
and
DEC
relative
to
the
phase
centerofthe observations.
cluding IRAS 16293 (e.g., Schöier et al. 2002; Jørgensen et al. depleted instead, due to accretion into the two protostars and(ii) I16293 に対するダスト温度構造モデリング(SEDとimageを制限に)・B方向で強い吸収(ダスト連続波を背景に)
2005b; Crimier et al. 2010). The dust opacity was allocated in dynamical e↵ects, as described by Nelson & Marzari (2016). A
refinements, to resolve the inner gap and nearby structure prop- 3.4. Dust envelope model
the cells in a self-consistent manner, with the first RADMC-3D(iii) CO isotoplogues データを使った円盤構造等の議論
plateau was
erly, as geometricduste↵ectsdensity
such as self-shadowing
onto used
the outerto imitate the mass depletion inThe dust envelope was modeled with a 1D radial density pow
disk became
thermal Monte Carlo photon propagation done in a modelof important.
side a given radius rplat , meaning
that
we useda constant,ratherlaw density
distribution,
as the envelope
has been well-fitted(i)
一般的な設定によるdust
温度分布（詳細次ページ）
purely icy-dust opacities. Grid cells with temperatures above than a radial power-law, density distribution
viously by such inmodels(e.g.,
Schöier
et al. 2002). More com
this
inner
region,3.3.
Dust opacity& temperaturecated circumbinary envelope structures, such as an infalling,
S. K. Jacobsen
et al.:temperature
The ALMA-PILS survey:
3D modelingthe envelope,disks anddust filament of IRAS 16293–2422
the assumed water
sublimation
were
then ofallocated868μm
ダスト連続波イメージ
while3Dを使用，適当なdust
keeping the dust density distribution
in theouterwereenvelope
tating circumbinary
envelope
not considered, as we focu
・RADMCmodelを仮定(温度構造を反映)
We
used
dust
opacities
from
Ossenkopf&
Henning(1994),
bare-grain dust opacities for the next photon propagation.eledWe
did the as
on the innermost region of IRAS 16293 in this work. Recent
with
model
protoplanetary(PP-disk)structure
a power-law:which
arebothgood approximations
for diskdensecores (vander Tak servations of GG Tau (Dutrey et al. 2014), as well as simulati
Class 0に分類，過去の研究により‥・エンベロープ
PPDISK
構造，エンベロープは2つのパート
known
from Class
II sources(e.g.,+
Andrews
et al. 2012)
and thenot change the sublimation temperature to account for etthe
al. local
1999;
Shirley
et al. 2002,2011). Opacity
tablesof dust of the same system (Nelson & Marzari 2016) suggest that bin
density solution from the angularmomentumconservation
of
an
8
with
thin
ice-mantles
andanother
with
bare
dust
grainswere star formation results in partial clearing of the material in the!
environment
in
terms
of
pressurebutinsteadusedasinglesubinfalling,rotating
collapse(Terebeyetal.
1984).
This
infalling,p・ d = 120pcを採用>
used,
assuming
coagulated
dust
grainswith anreferredambient
gas
num- nermost region where the protostellar binary resides. Based>r>rotating
collapsedensity
structureishereafter
to
as
a
>
3
limation temperature of 90 K (Sandford & Allamandola1993).
>⇢dust, ifgenerally
rat rplatthe 868Power-law,
p=1.7
ber
densityof model,106 cmbased. Theseopacitytablesare>rotating
toroidon theshapeappearing0 toroidalµm
continuum
observation,
we do not expect the i>>・16293A : highly active As the cell opacities were redefined, the cell dust equilibrium
r
used
for
modelsof
dustarounddeeplyembedded
protostars,
in<the centrifugal radius (Terebey et al. 1984),
0 which is the radiusrior to be completely evacuated of dust between the disks,
⇢(r)
=
(1)
!
cludingIRAS
16293(e.g., >Schöier
et
al.
2002;
Jørgensenetal.
where theinfallingmaterialwiththelargestangularmomenpdepleted
instead,duetoaccretion
into
the two protostars>
temperatures after the next photon propagation will be di↵erent,r>tum impacts
the etmidplane.
In>
terms
of
luminosity,allmodels,2005b;
Crimieral. 2010).
The
dust
opacitywasallocatedin(色々なアウトフロー現象付随）
plat>
dynamical e↵ects, as described by Nelson & Marzari (2016>>whether
they
used
one
or
two
radiation
sources,
werelimitedPlateau,
600au
⇢
,
if
r
<
r
. density
the
cells
in
a
self-consistentmanner,
with
the
first
RADMC-3Dwith some dust cells shifting from below to above 90 K and vice>0
platdust
plateau wasrplat
used =
to imitate
the mass depletion:
to a totalMonteluminosityof photon
21 L . Thisluminosity
is
based
on
inr
thermalCarlo
propagation
done
in
a
model
of
0
・16293B : more quiescentside a given radius rplat , meaning that we used a constant, raversa, that is, an opacity allocation error. For both diskpurely
compotegration
of
the
SED
using
data
from
Spitzer,
ISO-LWS, Hericy-dust opacities. Grid cells with temperatures
above than a radial power-law, density distribution in this inner reg
schel/SPIRE
andsubmillimeter(Chandler et
al. 2005;
Cortheassumedwater
sublimationdata
temperature
werethen allocated
nent
model
types,
this
error
was
found
to
be
negligible
after
two
while keeping the dust density distribution in the outer envel
・separation = 5.3”, or 636 au
reia et al. 2004; Makiwa 2014; Schöier et al. 2002),重要な結果
where the
Where
⇢
is
dust
density,r
isthebare-grain dust opacities
for the next
photonpropagation.
We
did
as adistancepower-law:to the model center,luminosity
is estimated to be 21 ± 5 L (Jørgensen et al. 2016).
recursions (5 and 0.1 % relative to the total bare-grain dust
mass,
not
changethe sublimation
temperaturetoaccount
forrecentthe localThisluminosity
assumesadistance
of
120
pc,
based
on
⇢
is
the
densityatdistancer0suband r90K以上の領域の体積）がof the density
・total luminosity = 21 5 at
L⦿1 , for the PP-disk model and the rotating toroid model,
8 the radius
0 of pressure but instead used a single
plat isエンベロープ温度構造（30K,
50K,!
environment
in
terms
rep
>
distance estimates of the bulk of the ⇢ Oph cloud from extinc>r>>plateau.
r
was
fixed
to
600
AU
in
all
models,welimation
temperatureof
90
K(Sandford&
Allamandola1993).
>⇢0,aif distancer rplattion
measurements(Knude & Hog
1998; Lombardi et al. 2008)
plat>
spectively). The higher error in the PP-disk model, evenAs
with
ten
>
>
r0
<
cellparallax
opacities
wereredefined,
the
cell
dust
equilibrium
輻射源が1つか2つかで大きく変わる（2ページ後）
andtheVLBI(Loinardetal.
2008).
The
interbinarydischosetoensurethattheentiredust
structure
resided in⇢(r)filament=>! p>times more photon packages than the rotating toroid model(Tatemperatures
after
the next
photonpropagation
willthebeangudi↵erent,>tance wasfixed
to 636
AU forall models,
based on
r
>
plat
>
00
>
Fig. 1: Dust continuum at 868 µm, in log-scale. Contour levels with>⇢r < rplat . et al.
thisdensityplateau.
We
fixed
p
=
1.7,
taken
lar distanceof ⇠5.3peaksof the868 µmsome dust
cells between
shifting the
from
below
to above
90ALMAK and vice>
: 0 r0 from, ifSchöier1
ble 1), came from
the
very
high
dust
densities
necessary
tomatch
are logarithmically divided between 0.02 and 2 Jy beam . The

r, out

A&A proofs: manuscript no. IRAS16293_3DMOD

nr, in⇢0, env
r0, env
penv
MA
MB
†
T e↵
LA
r0, diskrinner disk
rdisk,A
rdisk,B

Description

Value
8⇥103 AU
5 AU
600 AU
131
131

Fpeak, A
Fpeak, B
Disk A aspect ratio
NH2 , B

Number of grid cells in the outer radial region (r > 600 AU)
Number of grid cells in the inner radial region (r  600 AU)
Number of photons used in thermal Monte Carlo process
Luminosity of source A

88
110
5⇥107
3 – 20 L⌃A⌃B

Octree refinement radius around source
Octree refinement number

400 AU
1

Octree refinement radius around each source
Octree refinement number

250 AU
2

Envelope radius
Grid start radius
Radius of the density plateau
Number of grid cells in the polar range
Number of grid cells in the azimuthal range

p
H0,A
H0,B
iA
nlev, disk
nlev, in disk
nphotons

Grid cells in the outer radial region (r > 600 AU)
Grid cells in the inner radial region (r  600 AU)
Envelope reference density at r0, env
Envelope reference radius
Envelope density power-law exponent
Source A stellar mass
Source B stellar mass
Star surface temperature
Source A luminosity
PP-disk reference radius
Disk inner radius
Disk A radius
Disk B radius

22
110
2.5⇥10 14 g cm 3
1 AU
1.7
1M
0.1 M
5000 K3 – 20 L
10 AU
1 AU
150 AU
50 AU

Disk constraints
Fpeak, A
Fpeak, B
Disk A aspect ratio
NH2 , B

1

Peak flux density toward source A
Peak flux density toward source B...
Disk B column density

1.0 Jy beam
2.0 Jy beam 1
1.64
1.2⇥ 1025 cm 2

Parameter space for reference surface density of PP-disk A at 10 AU
Parameter space for reference surface density of PP-disk B at 10 AU

0.1 – 5.0 g cm 2
1.0 – 12.0 g cm 2

PP-disk models⌃A⌃B

Parameter space for reference surface density of PP-disk A at 10 AU
Parameter space for reference surface density of PP-disk B at 10 AU
Parameter space of the PP-disks flaring constants
Parameter space of the PP-disks dust density radial power-law exponents
Parameter space of PP-disk A scale-height at 10 AU
Parameter space of PP-disk B scale-height at 10 AU
Parameter space of PP-disk A inclination, 90 is edge-on
Octree refinement level of entire disk
Octree refinement level in innermost region
Number of photons used in thermal Monte Carlo process

0.1 – 5.0 g cm 2
1.0 – 12.0 g cm 20 – 0.25
0.5 – 1.5
0.85 – 2.0 AU
0.85 – 3.0 AU
30 – 902
4
107

Parameter space of the centrifugal radius of rotating toroid A
Parameter space of the centrifugal radius of rotating toroid A
Parameter space of the mass accretion rate into source A
Parameter space of the mass accretion rate into source B
Octree refinement level of entire disk
Octree refinement level in innermost region
Number of photons used in thermal Monte Carlo process

50 – 100 AU
5 – 40 AU
1.0⇥10 6 – 5.5⇥10 6 M yr 1
1.0⇥10 6 – 5.5⇥10 6 M yr 1
2
2
106

Reference density
Filament radius from filament center...
...

2.5 ⇥10 17 g cm 3
130 AU
170 AU
300 AU

Rotating toroid models

IRAS 16293 modelnr, out
nr, in⇢0, env
r0, env
penv
MA
MB
†
T e↵
LA
r0, diskrinner disk
rdisk,A
rdisk,B

1.0 Jy beam 1
2.0 Jy beam 1
1.64
1.2⇥ 1025 cm 2

PP-disk models

Temperature analysis
nr, out
nr, innphotonsLA
One radiation source
roctnoctree levels
Two radiation sources
roct
noctree levels

Peak flux density toward source A
Peak flux density toward source B...
Disk B column density

Disk constraints

Grid
rout
rin
rplat
n✓
n

110
2.5⇥10 14 g cm 3
1 AU
1.7
1M
0.1 M
5000 K3 – 20 L
10 AU
1 AU
150 AU
50 AU

モデルパラメーターle 1: RADMC-3D model parameters
Parameter

Grid cells in the inner radial region (r  600 AU)
Envelope reference density at r0, env
Envelope reference radius
Envelope density power-law exponent
Source A stellar mass
Source B stellar mass
Star surface temperature
Source A luminosity
PP-disk reference radius
Disk inner radius
Disk A radius
Disk B radius

rc, A
rc, B
ṀA
ṀB
nlev, disk
nlev, in disk
nphotons
Dust arc⇢0
rout
Filament semi-minor axis
Filament semi-major axis

Notes. Model parameters for each setup. LB is always defined as LB = 21.0 L - LA . † The radiation spectra of both source A and B are treate
blackbodies with a temperature of 5000 K, following Schöier et al. (2002).
Article number, page 4 of 20

連星系と単独星のある温度以上の領域の相対的な差

Total Luminosity 一定の下ではBinaryの方がSingleよりより低温領域が広くなる↓
ガス化学に大きな影響あり低い <——

中心密度30K: CO
50K: H2CO のsublimation T.
——> 高い 90K; H2O

Fig. 3: Relative di↵erences in volumes of dust above di↵erent temperatures. The volume di↵erence between the single star temperature volume, V1 , and binary star temperature volume, V2 , is shown, normalized to V1 , i.e. ⌧ 0.2 means that the total temperaturevolume is 20 % lower if there are two stars compared to one. The envelope mass range is 0.7 – 24 M , consistent with the dense coremass range observed in (Alves et al. 2007). The relevant mass range for IRAS 16293 is 2.4 – 4.8 M , (our IRAS 16293 envelopemodel has a mass of ⇠4 M ). There is a clear tendency for a single star to result in more dust heated above ⇠ 50 K.

to the degeneracy between H0 and i, only models with inclina- together with the given dust density model, the molecular hytions below 55 could be excluded. The peak flux values were drogen number density nH was found. The gas line emission
2
degenerate with di↵erent ⌃0 , H0 , L⇤ and i values and the col- depends on the number density of the molecule undergoing(ii) Dust
umn放射モデリングdensity toward source B did not o↵er any constraints ei- a rotational transition, the CO isotopologue in our case, the・MAther,= 1.0M（過去の速度場の解析から）,rplatの内側に
⦿，MallB≤0.1M
as almostof our⦿investigatedparameter space satisfied
number density of the other molecules in the gas which excite
the NH2 column density condition. Due to previous observations50auで固定）
the molecule collisionally and the kinetic temperature which
diskコンポーネント，２つのダスト密度モデル（半径は150au,
of infall toward both sources (Caux et al. 2011; Chandler et al. changes the collisional rates (Brinch & Hogerheijde 2010) and・静水圧平衡で記述されるPPDisk=DM。Bはface
2005; Pineda et al. 2012; Zapata et al. 2013; Oya on仮定，Aの傾き角は
et al. 2016), thus the excitation of the CO isotopologue. In LIME, the number
freeweparameter，イメージに加えSEDも制約として使う
considered the rotating toroid model. The dust density distri- density of the colliders is approximated as nH , as H2 is by far
2bution of this model can be foundsemi-analyticallyby defining
the 2009:
most abundant species in the dense molecular cores where・回転トロイドモデル”rotating
toroidmodel” = RTM(Hartmann
discrete streamlines from the rotating envelope, which spiral in- star formation takes place (e.g., Genzel & Stutzki 1989). LIME
元はHartmann,
Calvet,Bossstreamlines
1996)：角運動量保存で落下する流線の無限
wards and impact
opposing
in the midplane, creating performs non-LTE (Local Thermodynamic Equilibrium) line ra遠方で，シート形状平衡解の重みをつけた密度モデル
a disk structure. From Hartmann (2009),
diative transfer modeling, where the rotational level populations
are found iteratively. The CO isotopologue data files contain⇣⌘ 1/2 01
ing collisional rate coefficients (Yang et al. 2010) were downcos✓
1
2
Ṁ 1 + cos✓
BBB cos✓
2cos ✓0 CCC
20loaded
from
the
LAMDA
database (Schöier et al. 2005). The
B@
CA ,⇢(r, ✓) =+(5)q
rc: centrifugal
radiuscos✓0r/rc
3
collisional
rate coefficients of the CO isotopologues with H2 in
4⇡ GM⇤ rthese files include collisions with both ortho- and para-H2 .
DMに比べて In this work, we assumed that the dust and gas tempera・arc構造については柱密度一定の形で入れる
where Ṁ is the mass accretion rate onto the central object, ✓0 is tures are coupled, which is usually a good approximation in the
RTMは鉛直方向に
the starting polar angle of the streamline in question
and rc is the dense inner environments of the envelope (Schöier et al. 2002),
centrifugal radius. The
densityin each no.
grid
cell
in our model was that were modeled here. The radius of the LIME model was set
A&A
proofs: manuscript
IRAS16293_3DMOD
広がり，赤道面へのopticalfound by predefining nstream streamlines with discrete ✓0 values to 2 ⇥ 103 AU, as more distant, cold regions in the envelope will
Table 2: Example dust model parameters.
depthが小さくなり，dust温度高い
and evaluating them at nr radial points,
along the streamline. A not contribute much emission due to freeze-out of CO.
nearest-neighbor search was performed,
with the dust
density of22
the absorption features around each source andPP-disk model
LA [L ] LB [L ] ⌃0,A [g cm ] ⌃0,B [g cm ] H0,A [AU] H0,B [AU]Optimally,iA [ ]
the RADMC-3D grid cell defined to be that of the nearest defined the major features of the interbinary CO isotopologue emission
DM 1
18.0
3.0
1.0
3.0
1.25
1.5
55
DM 2
DM 3

14.0
10.5

7.0
10.5

1.0
1.0

0.05
0.05

0.85
1.25

Rotating toroid model

LA [L ]

LB [L ]ṀA [M yr 1 ]ṀB [M yr 1 ]rc,A [AU]

RTM 1
RTM 2
RTM 3
RTM 4
RTM 5

Article number, page 8 of 20
18.0
10.5
20.0
7.0
3.0

3.0
10.5
1.0
14.0
18.0

6

3.75⇥102.1⇥10 6
3.8⇥10 6
3.0⇥10 6
3.0⇥10 6

gas emission maps, with the largest di↵erence in the disk regions.

Fig. 4: Observed and synthetic dust continuum emission at 868 µm for the di↵erent physical models summarized in 2. Image is in

2.0
50
2
log-scale and the contours are logarithmically divided between 0.02 and 2 Jy beam 1 . DM denotes the PP-disk model, while RTM
http://home.strw.leidenuniv.nl/~moldata/
2.0
60
denotes the rotating toroid model.

rc,B [AU]seen in Fig. 2 were recreated in the synthetic moment zero maps,
2.75 ⇥ 1075
20which would imply that our dust density model is consistent withthe observed gas line emission. We did not attempt to match the
2.1 ⇥ 10 650
20exact absorption level as it depends not only on the molecule
4.6 ⇥ 10 675
20abundance but also on the gas-to-dust mass ratio and dust opac6
ity, neither of which were constrained in this work.
2.0 ⇥ 1075
20
In the case of a PP-disk model, the velocity in the disk around2.0 ⇥ 10 675
20each source was modeled as Keplerian rotation. Here the central
stellar mass becomes important if there is any disk inclination
toward the observer, as radial velocities cause spectral broadentroducing more material in our filament model toward sourceing,
A reducing the line optical depth. This, in turn, will result inhigher integrated emission if there is any line self-absorption,
6

as simple free-fall,pGMtot /r,(6)
２つのダストピークの値を合わせることは
where r is the distance to the model center, G is the gravitaどのモデルでもある程度可能
tional constant and M is the combined mass of source A andshould require L to be even higher than we currently find inv(r) =

tot

B. This approximation is valid at kAU scales but breaks down in
the innermost region. The dust in the interbinary region should
arguably be drifting toward either source, in accordance withthe local gravitational field. Since only one dust opacity model
can be set in LIME (v. 1.5), bare-grain dust opacities were usedin the entire model, as the dust grains in the disk regions are

S. K. Jacobsen et al.: The ALMA-PILS survey: 3D modeling of the envelope, disks and dust filament of IRAS 16293–2422

IME model parameters(iii) CO 放射モデリングParameter
Description
Value
・LIMEを使って計算，g/d=100とする
Grid outer radius...
2 ⇥ 103 AU
Grid start・non-LTE，ただしガス温度＝ダスト温度は仮定
radius...
30 AU
nnodesNumber of grid nodes in the LIME calculations 7 ⇥ 104
・DMの場合はケプラー回転，RTMの場合は回転自由落下(Tereby,4 Shu, Cassen 1984)
CO/H2
Standard ISM abundance of CO
1013
アバンダンス比を振った例もappendixにはあり
CO/H2・CO isotopologues
Standard
ISM
abundanceof 13 CO1.30⇥10 6
S. K. Jacobsen et al.: The ALMA-PILS survey: 3Dmodeling of theenvelope,
disks and dust filamentof IRAS 16293–2422
C18 O/H2
Table 3: LIME model parameters
17
C O/H2Freeze out factor Parameter
Grid outer radius
Gas-to-dust-mass ratio
Grid start radiusStandard ISM abundance of C18 O
Standard ISM abundance of C17 O
Value. . . Description
3. . . for all conversions from dust 2to⇥ 10
AUmass
Used
gas
...
30 AU

1.79⇥10 7
5.58⇥10 80.01
100nnodes
CO isotopologues abundancesof all models
CO/H2
13
X13 CO
CO/H2
18
C O/H2
XC18 O
C17 O/H2Freeze out factor
XC17 O

Number of grid nodes in the LIME calculations
13 Standard ISM abundance of COCOabundance
Standard
ISM abundance of 13 CO
18Standard ISM abundance of C18 O
C Standard
O abundance
ISM abundance of C17 O
17. . .
C O abundance
Used for all conversions from dust to gas mass

2.6⇥10 7
3.58⇥10 8
1.12⇥10 8

Gas-to-dust-mass ratio

CO isotopologues abundances of all models

13
en abundances assume that
into CO.
X COC and O atoms maximally combine
CO abundance

2.6⇥10 7
3.58⇥10 8
1.12⇥10 8

13

C18 O abundance
C17 O abundance

XC18 O
XC17 O7 ⇥ 104
10 4
1.30⇥10 6
1.79⇥10 7
5.58⇥10 80.01
100

RTMの方がA の「放射」をよく再現
A&A proofs: manuscript no. IRAS16293_3DMOD「スケールハイトが大きい必要あり」

IME model parametersof Fig.assume
5. that C and O atoms maximally combine into CO.
Notes. Given abundances
Table 4: LIME model parameters of Fig. 5.

Parameter

Description

Value

Description
Value
Rotating toroidParameter
model
Rotating toroid modelLA
Luminosity
source18 L
LALuminosity ofof source
A A
18 L
LB
Luminosity ofof source
B B
3L
LB
Luminosity
source
3L
ṀA
Mass accretion rate
3.75 ⇥ 10 6 M yr 1
6
6
ṀA
Mass
accretion
M yr 1ṀB
Mass
accretion raterate 2.75 ⇥ 10 3.75
M yr⇥1 10
rc,ACentrifugal radius
75 AU
6
1
ṀB
Mass
accretion
rate
2.75
⇥
10
M
yr
rc,B
Centrifugal radius
20 AU
rc,A
Centrifugal radius
75 AU
PP-disk modelLA
Luminosity of source
A
14 L
rc,B
Centrifugal
radius
20 AU
LLuminosity of source B
7L
B

PP-disk model⌃⌃0,A
0,B
LA
H0,A
H0,B
LB
iA

Dust surface density at 10 AU
Dust surface density at 10 AU
Luminosity
ofat source
A
Scale-height
10 AU
Scale-heightat source
10 AU
LuminosityofB
Disk A inclination

RTM

0.6 g cm 2
5.0 g cm 2
1.5 AU
2.0 AU
60

14 L
7L
⌃0,A
Dust surface density at 10 AU
0.6 g cm 2
DM
2
Table
5:
LIME
model
parameters
of
Fig.
6.
⌃0,B
Dust surface density
at cannot
10 AU
5.0 gthatcm
model, we
exclude the possibility
the disk-like emission structure around source A could be from a flat disk, based
H0,A
Scale-heightatour10AUand observations alone.1.5
AUpossible that the
1
1
on
model
It
is
also
ṀA [M yr ] ṀB [M yr ]presence
material in front of disk 2.0
A could
allow the rotating
Hが小さいと
H0,BModel
Scale-heightat 10ofAU
AU
6
6
9.0⇥101.3⇥10toroid models to use the standard ISM CO abundance and still
iA LLA == 37 LL
Disk
A
inclination
6
6
qualitatively match the observations. 60
5.5⇥101.4⇥10A

LA = 10.5 L
LA = 14 L
LA = 18 L

4.6⇥10 6
4.2⇥10 6
3.75⇥10 6

IME model parameters of Fig. 6.

6

1.6⇥10 6
1.85⇥10 6
2.75⇥10 66

吸収しすぎ

6. Discussion

Fig. 5: Zeroth moment maps of the observed and synthetic CO isotopologue gas line emission. Contour levels are divided logarithThe
combinedthe dustthe
continuum
and CO that the disk-like emismodel,
weconstraints
cannot fromexcludepossibility
11PP-disk model
LA
LB
⌃0,A
⌃0,B
H0,A
H0,B
iA

Luminosity of source A
14 L
Luminosity of source B
7L
Dust surface density at 10 AU
0.6 g cm 2
Dust surface density at 10 AU
5.0 g cm 2
RTM（ダストピークを再現する）の場合でLuminosity比を変えた場合のScale-height at 10 AU
1.5 AU
Scale-height at 10 AU
2.0 AUC17Oシミュレーション，L
18L⦿ 必要A
Disk A inclination
60 et al.: The ALMA-PILS survey: 3D modeling of the envelope, disks and dust filament of IRAS 16293–2422
S. K. Jacobsen

Table 5: LIME model parameters of Fig. 6.
Model

ṀA [M yr 1 ]ṀB [M yr 1 ]LA = 3 L
LA = 7 L
LA = 10.5 L
LA = 14 L
LA = 18 L
LA = 20 L

9.0⇥10 6
5.5⇥10 6
4.6⇥10 6
4.2⇥10 6
3.75⇥10 6
3.8⇥10 6

1.3⇥10 6
1.4⇥10 6
1.6⇥10 6
1.85⇥10 6
2.75⇥10 6
4.6⇥10 6

Notes. All models are rotating toroids, using rc,A = 75 AU and rc,B = 20
AU.

However, if larger amounts of CO are in front of disk A, on
similar spatial scales, then it could explain the extra line emisがsion in the observations comparedto the PP-disk model emission. Since the continuum emission is consistent with a PP-disk

model, we cannot exclude the possibility that the disk-like emission structure around source A could be from a flat disk, basedon our model and observations alone. It is also possible that thepresence of material in front of disk A could allow the rotating
toroid models to use the standard ISM CO abundance and still
qualitatively match the observations.

6. Discussion
The combined constraints from the dust continuum and CO
isotopologue emission, necessitate very high PP-disk model
scale-heights around source B, H0 > 3.0 AU at 10 AU, which
is suggestive of a nonsettled disk with a large vertical distribution, meaning that it is indicative of a structure similar to that of the di↵use, rotating toroid model. These scaleheights are unprecedented for Class II disks, but similar to the
one reported by Tobin et al. (2013), who find a best-fit PP-disk
model to the Class 0 disk around L1527 with a scale-height of
48 AU at 100 AU. In comparison, when converting H0 to thescale-height at 100 AU, the PP-disk model around source B

まあまあ
あっているかなというモデル（CO，dustとも）

Article number, page 11 of 20

Fig. 6: Observed and modeled C17 O zeroth moment maps, contour levels are divided logarithmically from 0.5 to 7.3
Jy beam 1 km s 1 . All models are rotating toroid models matching the dust continuum peak flux densities for disk A and B.

DMでBの吸収を合わせようとすると，
due to trapping in the water-ice, which would allow higher abundances in the gas model for regions with Tdust 90 K than re極端に大きなHが必要 H > 3.0au @ r=10au（原始星ではよくある）
gions with 30 K  Tdust < 90 K. This should lead to an emission

regions where the temperatures exceed 90 K. At the scales of1000 –1500 used by Schöier et al. (2002), spherically symmetricaldensity models are good approximations of the outer envelope

Accepted by ApJL

15 http://arxiv.org/pdf/1712.07193
History of Globulettes in the Milky Way
Tiia Grenman1 , Erik Elfgren1 and Hans Weber1
1Luleå University of Technology, Sweden

E-mail contact: tiia.grenman at ltu.se
Globulettes are small (radii < 10 kAU) dark dust clouds, seen against the background of bright nebulae. A majorityof the objects have planetary mass. These objects may be a source of brown dwarfs and free floating planetary mass
objects in the galaxy. In this paper we investigate how many globulettes could have formed in the Milky Way andhow they could contribute to the total population of free floating planets. In order to do that we examine H-alphaimages of 27 H II regions. In these images, we find 778 globulettes.
We find that a conservative value of the number of globulettes formed is 5.7 × 1010. If 10 % of the globulettes form free
floating planets then they have contributed with 5.7 × 109 free floating planets in the Milky Way. A less conservative
number of globulettes would mean that the globulettes could contribute 2.0 × 1010 free floating planets. Thus theglobulettes could represent a non-negligible source of free floating planets in the Milky Way.
Accepted by Astrophysics and Space Science
http://urn.kb.se/resolve?urn=urn:nbn:se:ltu:diva-67161
http://arxiv.org/pdf/1801.01355
HII領域の画像を丹念に調べて，Globulettes のサイズ分布や銀河系内の総数を見積もり。
フリーフローティングプラネットの起源（母胎）か？
12
画像があれば良かったのだが。。。

Accepted by AJ

17

http://arxiv.org/pdf/1712.01468

Detection of a centrifugal magnetosphere in one of the most massive stars in the ρ Oph
star-forming cloud
S. Hubrig1 , M. Schöller2 , S. P. Järvinen1 , M. Küker1 , A. F. Kholtygin3 and P. Steinbrunner4
1

AIP, Germany, 2 ESO, Germany, 3 Saint-Petersburg State University, Russia, 4 FU Berlin, Germany

E-mail contact: shubrig at aip.de
Recent XMM-Newton observations of the B2 type star ρ Oph A indicated a periodicity of 1.205 d, which was ascribedto rotational modulation. Since variability of X-ray emission in massive stars is frequently the signature of a magnetic
field, we investigated whether the presence of a magnetic field can indeed be invoked to explain the observed Xray peculiarity. Two FORS 2 spectropolarimetric observations in diﬀerent rotation phases revealed the presence ofa negative (⟨Bz ⟩all = −419 ± 101 G) and positive (⟨Bz ⟩all = 538 ± 69 G) longitudinal magnetic field, respectively.
We estimate a lower limit for the dipole strength as Bd = 1.9 ± 0.2 kG. Our calculations of the Kepler and Alfvénradii imply the presence of a centrifugally supported, magnetically confined plasma around ρ Oph A. The study of thespectral variability indicates a behaviour similar to that observed in typical magnetic early-type Bp stars.
Accepted by AN
https://arxiv.org/pdf/1712.05939

A search
for pre- and proto-brown dwarfs in ρOphthe dark
Barnard 30 with ALMA
X線変光から1.2日で自転しているらしいことがわかった
A中のcloudB2型星のZeeman観測による磁場調査。
1
異なる自転フェーズ角の測定から，磁場強度やDipole成分を見積もり。
N. Huélamo, I. de Gregorio-Monsalvo2,3, A. Palau4 , D. Barrado1 , A. Bayo5,6 , M.T. Ruiz7 , L. Zapata4 ,H. Bouy1 , O. Morata8 , M. Morales-Calderón1 , C. Eiroa9 , and F. Ménard10
1Dpto. Astrofı́sica, Centro de Astrobiologı́a (INTA-CSIC); ESAC campus, Camino bajo del Castillo s/n, Urb.
Villafranca del Castillo, E-28692 Villanueva de la Cañada, Spain; 2 European Southern Observatory, Alonso de20Charlottesville, VA 22904, USA; 11 National Radio Astronomy Observatory, 520 Edgemont Road, Charlottesville, VA
12
1322903,
USA;
Sterrewacht
Leiden,
LeidenUniversity,
PO
Box
9513,
2300
RA
Leiden,The
Netherlands;
SpaceFirst Results from the Herschel and ALMA Spectroscopic Surveys
of
the
SMC:
14
Telescope
Science
Institute,
3700
San
MartinDr.,
Baltimore,MD
21218,
USA;
Lennard-Jones
Laboratories, Keele
The Relationship Between [C ii]-brightGas
andCO-bright
Gas
at
Low
Metallicity
University, Staﬀordshire ST5 5BG, UK; 15 National Astronomical Observatory of Japan, Chile Observatory, 2-21-1
1,2
16 Bolatto1 , Mark Wolfire1 , Steven R. Warren3 , Rodrigo HerreraKatherine
E.
Jameson,
AlbertoD.
Osawa, Mitaka,Tokyo
181-8588,
Japan;
The
Joint
ALMA
Observatory,
AlonsodeCrdova3107,
Vitacura,
Santiago,
174 , Kevin Croxall5,6 , Eric Pellegrini7 , John-David Smith8 , Monica Rubio9 , Remy Indebetouw10,11 ,Camus
Chile; SOFIA Science
Center,Deutsches
SOFIA
Institut,NASA
Ames
ResearchCenter,MoﬀettField,
CA,
94035,
18P. Israel12 , Margaret Meixner13 , Julia Roman-Duval13 , Jacco Th. van Loon14 , Erik Muller15 ,
Frank
USA;
I. Physikalisches Institut der Universität zu Köln, Zülpicher Straße 77, 50937, Köln, Germany
Celia Verdugo16 , Hans Zinnecker17 and Yoko Okada18
E-mail contact: katie.jameson at anu.edu.au
1
Astronomy Department and Laboratory for Millimeter-wave Astronomy, University of Maryland, College Park, MD
The
Small
providesand
theAstrophysics,
only laboratory
to study
the structureof molecular
at 2611,high
220742,
USA;Magellanic
ResearchCloud
School(SMC)of Astronomy
Australian
National
University,
Canberragas
ACT
3
resolution
andlowmetallicity.
We
present
results
fromthe
HerschelSpectroscopic
Survey
of
the
SMC
(HS
),
which
3
Australia; Cray, Inc., 380 Jackson Street, Suite 210, St. Paul, MN 55101, USA
mappedthe key far-IRfürcoolinglines [C ii], [Oi], [N ii],and [O iii] in D-85748
five star-forming
regions,
and 5new
ALMA 7m4
Max-Planck-Institut
extraterrestrische
Physik,Giessenbachstr.,
Garching,
Germany;
Department
of
12
13
3
array
maps of(2 − 1) withoverlapping
four140of thefive18th
HS Avenue,
regions.Columbus,
We detectOH[C ii]
andAstronomy,
The CO
OhioandStateCO
University,
4051coverage
McPherson
Laboratory,
West
43210,[Oi]throughout
all
of
the
regions
mapped.
The
data
allow
us
to
comparethestructureof6
7 the molecular clouds andUSA; Illumination Works LLC, 5650 Blazer
Parkway,
Suite 152, Dublin OH 43017; Zentrum für Astronomie,
13
12<
surrounding
photodissociation
regions
using
CO,
CO,
[C
ii],
and
[O
i]
emissionat(< 3 pc) scales.
We8∼10 arcsec
Institut für Theoretische Astrophysik, Universität Heidelberg, D-69120 Heidelberg, Germany;
Departmentof Physics
estimateA
using
far-IR
thermalcontinuum
emission
from
dust
and
find
the
CO/CII
ratios
reach
the
Milky
Way
value
9
V
& Astronomy, University of Toledo, 2801 W Bancroft St, Toledo, OH 43606, USA; Departamento de Astronomı́a,athigh AV indetheChile,
centersof the36-D,
cloudsChile;and fall
10 to ∼ 1/5 − 1/10× the Milky Way value in the outskirts, indicating the
Universidad
CasillaDepartment12of Astronomy, University of Virginia, PO Box 400325,
presenceof translucent
molecular
not traced
byAstronomy
bright COemission. We
estimate
theRoad,amountof molecular VA
gasCharlottesville,
VA 22904,
USA; 11gas
National
Radio
Observatory,
520
Edgemont
Charlottesville,
12
tracedbybright[C
ii]emission
at
low
A
and
brightCOemission
at
high
A
.
We
find
that
most
of
the
molecular
12
VV
22903, USA;
Sterrewacht Leiden, Leiden University, PO Box 9513,122300 RA Leiden, The Netherlands; 13 Spacegas
is at low
AV andtraced3700
by bright[C ii] emission,
but thatemission
appears to extend
to wherewe14
Telescope
Science
Institute,
San MartinDr., Baltimore,
MDfaint
21218,COUSA;
Lennard-Jones
Laboratories,
Keele
estimate
theStaﬀordshire
H2 -to-HI transition
occurs.
15 converting our H2 gas estimates to a CO-to-H2 conversion factor (XCO ),University,
ST5 5BG,
UK; ByNational Astronomical Observatory of Japan, Chile Observatory, 2-21-1
we
show
that
X
is
primarilyafunction
16 of AV , consistent with simulations and models of low metallicity molecularCO
Osawa, Mitaka, Tokyo 181-8588, Japan; The Joint ALMA Observatory, Alonso de Crdova 3107, Vitacura, Santiago,
clouds.
Chile; 17 SOFIA Science Center, Deutsches SOFIA Institut, NASA Ames Research Center, Moﬀett Field, CA, 94035,
USA; 18 I.by
Physikalisches
Institut derLow-metal環境であるSMCに含まれている星間物質（分子雲成分）を対象にUniversität zu Köln, Zülpicher Straße 77, 50937, Köln, Germany
Accepted
ApJ
遠赤外禁制線{CII],{OI],{NII],[OIII]（Herschel）とCO(ALMA/ACA)を組みE-mailcontact: katie.jameson atanu.edu.au
http://www.mso.anu.edu.au/
kjameson/SMC_HS3_ALMA_preprint.pdf~
合わせて解析。分子雲のLow
Av領域はCOが解離していて放射は見えず，[CII]で
The Small Magellanic Cloud (SMC) provides the only laboratory to study the structure of molecular gas at high3
トレースされている。
resolution and low metallicity. We present
results from the
HerschelSpectroscopic
Survey
of
the
SMC
(HS
), which15
mapped the key far-IR cooling lines [C ii], [O i], [N ii], and [O iii] in five star-forming regions, and new ALMA 7m-

21
Dynamics of magnetic flux tubes and IR-variability of Young Stellar Objects
Sergey Khaibrakhmanov1,2 , Alexander Dudorov2 , Andrey Sobolev1
1

Kourovka astronomical observatory, Ural Federal University, Ekaterinburg 620000, Russia
2
Theoretical physics department, Chelyabinsk state university, Chelyabinsk 454001, Russia
E-mail contact: khaibrakhmanov at csu.ru
We simulate the dynamics of slender magnetic flux tubes (MFTs) in the accretion disks of T Tauri stars. The dynamical
equations of our model take into account the aerodynamic and turbulent drag forces, and the radiative heat exchange
between the MFT and ambient gas. The structure of the disk is calculated with the help of our MHD model of theaccretion disks. We consider the MFTs formed at the distances 0.027–0.8 au from the star with various initial radii andplasma betas β0 . The simulations show that the MFT with weak magnetic field (β0 = 10) rise slowly with speeds lessthan the sound speed. The MFTs with β0 = 1 form outflowing magnetized corona of the disk. Strongly magnetized
MFTs (β0 = 0.1) can cause the outflows with velocities 20–50 km s−1 . The tubes rise periodically over times fromseveral days to several months according to our simulations. We propose that periodically rising MFTs can absorb
stellar radiation and contribute to the IR-variability of Young Stellar Objects.
Accepted by RAA
http://arxiv.org/pdf/1712.09094
円盤内縁部の理論的構造解析に基づき，YSOsが示す赤外変光と関連させて議論。

The evolution of young HII regions
P.D. Klaassen1 , K.G. Johnston2 , J.S. Urquhart3 , J.C. Mottram4 , T. Peters5 , R. Kuiper6,4 , H. Beuther4 ,F.F.S. van der Tak7,8 , C. Goddi9,10