SF newsletter 349 #11-15
M. Momose (Ibaraki Univ.)#11, 13, 14のポイントを紹介＃12,15 は アブストラクトと一言メモ11.

suggests that LkHa225 South is another case of a source with episodically enhanced accretion that causes brightening by ordersof magnitude, and development of a hot absorption spectrum and warm wind. It is similar to Gaia 19ajj, but also reminiscentin its long brightening time and brightness oscillation near peak, to the embedded sources L1634 IRS7 and ESO Ha 99.

Expected FU Ori Outburst Amplitudes from the Optical to the Mid-Infrared

Lynne A. Hillenbrand, Antonio C. Rodriguez F Disks around young stellar objects (YSOs) consist of material that
thermally emits the energy provided by a combination of passive heating from the central star, and active, viscous heating due
to mass accretion. FU Ori stars are YSOs with substantially enhanced accretion rates in their inner disk regions. As a disk
transitions from standard low-state, to FU Ori-like high-state accretion, the outburst manifests through photometric brightening
over a broad range of wavelengths. We present results for the expected amplitudes of the brightening between ⇠4000 Å and 8µm – the wavelength range where FU Ori type outburst events are most commonly detected. Our model consists of an opticallythick passive + active steady-state accretion disk with low and high accretion states.

Self-absorption in [CII], 12 CO, and HI in RCW120. Building up a geometrical and• 簡単なDisk
modelによって，FU
physicalmodelof the region Ori Outburstが起こった時の可視から中間赤外線での増光量を予言

S.•Kabanovic,
Schneider,
V. Ossenkopf-Okada,F. Falasca, R. Güsten, J. Stutzki, R. Simon, C.
Buchbender,
近年のTimeN.Domain
surveyから，大きな変動が検出されフォローアップ分光観測でFU
Ori的な天体と
L. Anderson, L. Bonne, C. Guevara, R. Higgins, B. Koribalski, M. Luisi, M. Mertens, Y. Okada, M. Röllig, D.
同定されたものが複数あり
Seifried,
M. Tiwari, F. Wyrowski, A. Zavagno, A. G. G. M. Tielens F Revealing the 3D dynamics of HII regions andtheirassociatedmolecular
cloudsisimportantforunderstandingthelongstanding
problemastohowstellarfeedback
aﬀects• nIR（e.g., VVV）やmIR (NEOWISE) のTime Domain survey dataからもoutburst candidatesが多数見
the density structure and kinematics of the interstellar medium. We employed observations of the HII region RCW 120 in
12
13[CII],
observed
withinthe
SOFIA
legacyprogram
FEEDBACK,
and
the
CO
and
CO (3!2) lines, obtained with APEX. In
つかっているが，フォローアップ分光（他波長での）は限定的。NEOWISEデータはuniformだが，addition we used HI data from the Southern Galactic Plane Survey. Two radiative transfer models were used to fit the observed
opticalでの増光(~x100)に比べて増光量が小さい(~x5) code SimLine proves that the CO emission cannot stemdata.
A line profile analysis
with the 1D non-LTE radiative transfer
froma spherically symmetricmolecular cloud configuration. With a two-layer multicomponent model, we then quantified the• ここでは，FU
Oriと他のタイプの変動現象を区別できるcriteriaが必要，簡単な円盤モデルを構築
amount of warm background and cold foreground gas. There is a deficit of CO emission along the line-of-sight toward thecenter of the HII region which indicates that the HII region is associated with a flattened molecular cloud. Self-absorption in
the CO line may hide signatures of infalling and expanding molecular gas. The [CII] emission arises from an expanding [CII]
bubble and from the PDRs. A significant part of [CII] emission is absorbed in a cool ( 60-100 K), low-density (<500 cm 3 )enough outburst accretion rates, the entire ultraviolet, optical, near-infrared, and potentially mid-infrared (dependingon the radial extent of the outbursting region) wavelengths should be disk-dominated. Far-infrared and millimeter
wavelengths are sensitive to reprocessed emission from the high-accretion zone.
The experiment we perform here is to contrast hypothetical low-state accretion disks, with a stereotypical high-state
disk, and quantify expected outburst amplitudes as a function of wavelength.

モデルの概要PREDICTED OUTBURST AMPLITUDES
Our toy model consists in the low state of:• A progenitor low-mass pre-main sequence star, with assumed values of Tef f,⇤ = 3800 K and R⇤ = 1.5 R for its
4
temperature and radius. The SED is specified by a NextGen photosphere having luminosity L⇤ = 4⇡R⇤2 Teff,⇤ ;• A dust disk with inner radius corresponding to an assumed temperature of dust destruction, Tmax, dust = 1400
K. The SED is modelled under the optically thick assumption, as a summation of blackbodies from the di↵erent
radial annuli. The passive disk luminosity is Ldust = 0.25L⇤ ;• A gaseous accretion disk with inner radius fixed at 2 R . Although the magnetospherically defined innertruncation radius would vary as a function of accretion rate, we keep this value constant for simplicity. The total
accretion luminosity is given by Lgas, acc = GM⇤ Ṁ /R⇤ with a fraction up to 1/2 of this radiated by the disk,
depending on the accretion flow geometry.
Our model in the high state consists of:• A pure accretion disk as presented in Rodriguez & Hillenbrand (2021). The fiducial case here is a disk withmaximum temperature Tgas, max = 7000 K and accretion rate of Ṁ = 10 5 M /yr. As above, 1/2 of theaccretion luminosity is assumed to be radiated by the disk1 .
Contributions to the pre-outburst total source luminosity are L⇤ = 0.42 L , Ldust = 0.10 L , and Lgas, acc =結果

3

Low stateの質量降着率が10-8, 10-7, 10-6M⦿/yr の場合のHigh state (10-5M⦿/yr)に変化した
とき(magenta)との変化量（下）変化量の波長依存性は，
Low state時の質量降着率に依存する（元々，高いアクリーションレー
トだったものは中間赤外での増効率は小さい）

Figure 1. Top panels: Bright-state spectral energy distribution for an accretion disk-dominated FU Ori type system, accretingat Ṁ = 10 5 M /yr (magenta), compared to composite spectral energy distributions (green) for passive + accretion disk systems
having low-state accretion rates of Ṁ = 10 8 , 10 7 , 10 6 M /yr. In each panel, the same underlying stellar photosphere (navyblue), and passive dust reprocessing disk (cyan) are shown, along with the active gaseous accretion disk (orange); the assumed
distance is d = 800 pc. Bottom panels: Expected wavelength-dependent amplitude of an accretion outburst, calculated simply
as the flux ratio of the magenta and the green curves, converted to magnitudes. As the low-state accretion rate increases, theoutburst amplitudes decrease, and the wavelength dependence of the brightening steepens.

of low-mass T Tauri stars in the Class II phase. The amplitudes steepen towards the highest Ṁ case, which is more

13.

around the spherically expanding HII bubble. This scenario can possibly be generalized for other HII bubbles and would explain
the observed “flat" structure of molecular clouds associated with HII bubbles. We suggest that the [CII] absorption observed inmany star-forming regions is at least partly caused by low-density, cool, HI-envelopes surrounding the molecular clouds.

A rich population of free-floating planets in the Upper Scorpius young stellar association

Núria Miret-Roig, Hervé Bouy, Sean N. Raymond, Motohide Tamura, Emmanuel Bertin, David Barrado, Javier
Olivares, Phillip A. B. Galli, Jean-Charles Cuillandre, Luis Manuel Sarro, Angel Berihuete, Nuria Huélamo
F The nature and origin of free-floating planets (FFPs) are still largely unconstrained because of a lack of large homogeneous
samples to enable a statistical analysis of their properties. So far, most FFPs have been discovered using indirect methods;
microlensing surveys have proved particularly successful to detect these objects down to a few Earth masses. However, theephemeral nature of microlensing events prevents any follow-up observations and individual characterization. Several studies
have identified FFPs in young stellar clusters and the Galactic field but their samples are small or heterogeneous in age and5 (depending on the assumed age) in the region encompassing
origin. Here we report the discovery of between 70 and 170 FFPs
Upper Scorpius and Ophiuchus, the closest young OB association to the Sun. We found an excess of FFPs by a factor of up
to seven compared with core-collapse model predictions, demonstrating that other formation mechanisms may be at work. We
estimate that ejection from planetary systems might have a contribution comparable to that of core-collapse in the formation of
FFPs. Therefore, ejections due to dynamical instabilities in giant exoplanet systems must be frequent within the first 10 Myr
of a system’s life.

FAUST III. Misaligned rotations of the envelope, outflow, and disks in the multiple
protostellar system of VLA 1623 2417
• Upper
Sco・Ophiuchus領域（1-10Myrの若い星団領域）でFree-floating
planetsを多数(70-170)
FAUST
III, Satoshi Ohashi et al. F We report a study of the low-mass Class-0 multiple
system VLA 1623AB in theOphiuchus star-forming region, using H13 CO+ (J = 3 2), CS (J = 5 4), and CCH (N = 3 2) lines as part of the ALMA同定
Large Program FAUST. The analysis of the velocity fields revealed the rotation motion in the envelope and the velocity gradientsin the outflows(about 2000
au down toによる予言に比べて50 au). We further investigatedof the circum-binary VLA 1623A disk as• 単純なcorecollapse(星形成的)
最大 thex7 rotation
多い，他の過程の寄与を示唆
well as the VLA 1623B disk. We found that the minor axis of the circum-binary disk of VLA 1623A is misaligned by about 12
degrees with respect to the large-scale
outflow and the rotation axis of the envelope. In contrast, the minor axis of the circum• 若い惑星系からのejectionが結構重要な過程か？
binary disk is parallel to the large-scale magnetic field according to previous dust polarization observations, suggesting that themisalignment may be caused by the diﬀerent directions of the envelope rotation and the magnetic field. If the velocity gradientof the outflow is caused by rotation, the outflow has a constant angular momentum and the launching radius is estimated tobe 5 16 au, although it cannot be ruled out that the velocity gradient is driven by entrainments of the two high-velocity

Free-Floating Planets(FFPs)とは• 13 MJup以下の，主系列星やBrown dwarfに重力的に束縛されていない天体• 重力レンズによる検出を除き，急激に暗くなるので若い時以外は検出困難• 4つの形成機構：以下の全てが働いている証拠はあるが，相対的な寄与は不明‣ Scale-down version of star formation via core collapse‣ 原始惑星系円盤中での形成‣ Aborted stellar embryos ejected from a stellar nursery‣ Photo-erosion of prestellar core by stellar winds of OB stars

解析の流れと結果

LETTERSLETTERS• Upper Sco・Ophiuchus領域（1-10Myrの若い

NATURE ASTRONOMY

NATURE AS

星が黄色，青がBDs，赤がFFPs−20星団領域）で過去20年に渡りoptical/nIRで撮り溜められたデータ（Dynamical Analysis of−20

出された星々の位置・固有運動・マルチバンド
−25
測光データ

Dec. (°)

Dec. (°)

Nearby Clusters = DANCe catalogue) から抽• GaiaやHippercosからUSC/Ophメンバーを特定−25→3,455の high probability candidates を特定−30• その中で70-170 のFFPs（数は，年齢の仮定に
よる）

250

245
RA(°)

−30

240
250

250
245
RA(°)

245
240

RA(°)

240
250

245

240

RA(°)

Fig. 1 | Sky distribution of stars, brown dwarfs and FFPs discovered in this study and classified assuming an age of 5!Myr. Stars are shown as yellow| Sky distribution of stars, brown dwarfs and FFPs discovered in this study and classified assuming an age of 5!Myr. Stars are show
triangles, brown dwarfs as blue squares Fig.
and1FFPs
as red dots. The dashed ellipses indicate the area analysed with the DANCe catalogue (Methods).
triangles, brown dwarfs as blue squares and FFPs as red dots. The dashed ellipses indicate the area analysed with the DANCe catalogue (The distributions are overlaid on backgroundimagestaken
inoptical(left)
andradio(right,at
857!GHz)wavelengths.
Backgroundimagesadaptedwith
The distributions are overlaid on background images taken in optical (left) and radio (right, at 857!GHz) wavelengths. Background images
96
permission from: left, Mario Cogo (http://galaxlux.com);right,!ref.
Sciences.
permission from: left, Mario Cogo, EDP(http://galaxlux.com); right,!ref. 96, EDP Sciences.

The distributions are overlaid on background images taken in optical (left) and radio (right, at 857!GHz) wavelengths. Background images adapted withpermission from: left, Mario Cogo (http://galaxlux.com); right,!ref. 96, EDP
Sciences.
グレーが以前から知られていたメンバー

色等級図

黒が今回同定したメンバー

アイソクロン
12

赤：3Myr

実線と破線は異なるモデル↓
質量分布関数

0.5 MҰ

16

Av = 1.0 mag

6

0.1 MҰ
8

0.1 MҰ

18
20

0.02 MҰ

0.02 MҰ

0.015 MҰ

0.015 MҰ

0.01 MҰ

22
24

J (mag)i (mag)1012
14

0.5 MҰ

0.5 MҰ

0.1 MҰ
0.1 MҰ
0.02 MҰ
0.015 MҰ
0.01 MҰ

0.02 MҰ

16 0.015 MҰ
0.01 MҰ

0.006 MҰ

0.006 MҰFFPsの形成機構

4

Av = 1.0 mag

14

青：10Myr

統計的な相対的光度関数

0.5MҰ

2

4

i‫ݦ‬K s (mag)

6

8

18
0.01 MҰ
0.006 MҰ
20
00.006 MҰ
1

2

J‫ݦ‬K s (mag)34Fig. 2 | Colour–magnitude diagrams of the members of USC and Oph identified in this work. The left panel indicates the (i, i-Ks) colour-magnitude
diagram and the right panel the (J, J-Ks) colour-magnitude diagram. Previously known members are shown as grey symbols and new members as black
symbols. Error bars represent the uncertainty in the photometry reported in the Gaia DR2 and DANCe catalogues. The isochrones from the BHAC1547(solid lines) and the PARSEC-COLIBRI48 models (dashed lines) at 3!Myr (red) and 10!Myr (blue) (as well as the extinction vector) are superimposed.

Number of obje

103

実視等級分布，質量分布関数
102
101

Number of objects

100

2

4

6

8

10
12
J (mag)5Myrを仮定したMF

Stars

103

High-mass側
Salpeter的
102
1.0

objects

Stars

直接的な観測量

103

0.5

0

−0.5
−1.0
log(M/M⊙)

BDの範囲まではlog-normal
Stars
Haugbølle et al. (2018)7
FFPsはそこからexcess
Bate(2019)83

LETTERS

0.5
0
−0.5
−1.0
−1.5
−2.0
−2.5
近傍の系外惑星統計でもlog(M/M⊙)
指摘されているgiant stars and background Galaxies,
using
two different
BD
FFPs
Stars
BD methods.
FFPs
7
Haugbølle etal.
(2018)First, using synthetic data518 , we estimated a contamination rate in
Bate (2019)
Dip！：7-13Mjup
the planetary-mass domain smaller than 4%. Second, using sources
3
for which10both
DANCe and Gaia DR2 measurements are available (in the range 9 < J < 14 mag, hence above the planetary-mass
regime) and assuming that the Gaia DR2 sample represents theground truth, we estimated a contamination rate of approximately
8%. The real
102 contamination rate of FFPs is probably between these
14
16
18
1.0
0.5
0
−0.5
−1.0
−1.5
−2.0
−2.5
two values and should be confirmed by follow-up spectroscopiclog(M/M⊙)
observations. The number of FFPs reported in our analysis must
constitute a lower limit of the true total number of FFPs as ourBD
FFPs
Fig. 3 | J apparent magnitude distribution and mass functions of theanalysisis expected to miss the objects most affected by extincmembers of USC and Oph. Top: apparent magnitude distribution. Middle:tion (AV ≳ 3 mag), as well as objects displaying a large near-infrared
結構多く残るfunction. Bottom: observational mass function (theexcess observational
related to themasspresenceof circumstellar
material.
7,8functions from simulations are overlaid). The shaded regions
Themass
fractionof FFPs in our sample, meaning the relative proindicate the 1 and 3σ uncertainties from a bootstrap (top)and the+0.023
portion of FFPs to stars and brown dwarfs, is 0.045−0.029, where
dispersion due to the age (3–10!Myr, middle and bottom). All of thethe uncertainties
come from the uncertainty in individual ages
mass functions are normalized in the mass range 0.004–10!M⊙. The(between 3 and 10 Myr). We estimated this fraction by first inte−1.5
−2.0
−2.5
(75!MJup) and deuterium (13!MJup) burning limits, which indicate
gratinghydrogenthe observational
mass function (middle panel of Fig. 3) inthe boundary between stars and brown dwarfs (BD) and BD and FFPs
Stars + BDに対し
the FFP(4–13 MJup), brown dwarf (13–75 MJup) and stellar (0.075–
respectively, are indicated by the vertical dotted lines according to the＋0.023-0.029
10 M⊙, where M⊙ is the mass of47the Sun) mass regimes and thenBD 0.045
FFPs
BHAC15 evolutionary models and assuming an age of 5!Myr.
computingthe ratio between FFPs and brown dwarfs plus stars.
Whereas previous studies reported a similar fraction of FFPs3,4, our

Number of objects

Number of objects

NATURE ASTRONOMY

102
1.0

The conservative ranges we provide include both the uncertainties from our observations and currentbmass (q). Our observations are not sensitive to masses between 1 and 4!MJup and thus, the planet occu

それぞれのFFPs形成機構の寄与
惑星円盤からのeject

コアコラプス

その他の過程fFFP observed = fFFP ejected + fFFP core collapse + fFFP other= fgiant × funstable × nejected
不安定に
ガス巨大惑星放出個数!
13 MJup なる確率
伴う確率
+ 4M
ξcore collapse (m) dm + fFFP other

(1)

Jup

↑
↑
系外惑星の
↑
観測された
The valueoffisconstrainedbytheobserveddemographics
of
≈
1
giant
統計から見積もる> 75%
量の 10-130%
iant exoplanetsmeasured by (惑星軌道の離心率)
radial velocity, direct imaging, tran（次ページ）

t and microlensing surveys. The planetary occurrence rate

11,12,55–62

fgiant，fejectedの見積り

LETTERS

NATURE ASTRONOMY

Table 1 | Planetary occurrence rate for different studies
Planetary detection method

Planetoccurrence rate(%)

Mass range of theplanets (MJup)

Separation orsemi-major axis

Spectral type of
the primary bodyf_{FFP
ejected}c

Radial velocity12,55

2.1!±!0.5

4–13

0.1–100!au

Solar

0.016–0.021

23–130

Direct imaging57

0.7
0.6+
−0.5

5–13

30–300!au

BAFGKM

0.005–0.006

7–38

Direct imaging94

5.76
1.83+
−0.62

5–13

30–300!au

BAFGKM

0.014–0.018

20–115Microlensing58

1–2

0.007–0.02a

0.2–5!ΘEall

0.008–0.02

11–125

Combination (radial
velocity!+!direct
imaging!+!microlensing)95

~4

1–13b

2–1,000!auall

0.03–0.04

44–250f

FFP ejectedf
FFP observed(%)

The conservative ranges we provide include both the uncertainties from our observations and current knowledge of planetary systems. ΘE = angular Einstein radius. aMass ratio between the planet and starmass (q). bOur observations are not sensitive to masses between 1 and 4!MJup and thus, the planet occurrence rate is overestimated with respect to our observations. cAssuming funstable!=!0.75−1 and nejected!=!1.

観測された
fFFP observed = fFFP ejected + fFFP core collapse + fFFP other= fgiant × funstable × nejected! 13 MJup+ 4Mξcore collapse (m) dm + fFFP other
Jup

(1)

instabilities64–66,69. Our results suggest that giant planet systems must
量の10-130%form and become dynamically unstable within an observed lifetime of the region of 3–10 Myr to contribute to the population of
FFPs. Although the instability among the Solar System’s giant planets70 was much less violent than those for the mass range of FFPs

14.

to seven compared with core-collapse model predictions, demonstrating that other formation mechanisms may be at work. We
estimate that ejection from planetary systems might have a contribution comparable to that of core-collapse in the formation of
FFPs. Therefore, ejections due to dynamical instabilities in giant exoplanet systems must be frequent within the first 10 Myr
of a system’s life.

FAUST III. Misaligned rotations of the envelope, outflow, and disks in the multiple
protostellar system of VLA 1623 2417

FAUST III, Satoshi Ohashi et al. F We report a study of the low-mass Class-0 multiple system VLA 1623AB in theOphiuchus star-forming region, using H13 CO+ (J = 3 2), CS (J = 5 4), and CCH (N = 3 2) lines as part of the ALMA
Large Program FAUST. The analysis of the velocity fields revealed the rotation motion in the envelope and the velocity gradientsin the outflows (about 2000 au down to 50 au). We further investigated the rotation of the circum-binary VLA 1623A disk aswell as the VLA 1623B disk. We found that the minor axis of the circum-binary disk of VLA 1623A is misaligned by about 12
degrees with respect to the large-scale outflow and the rotation axis of the envelope. In contrast, the minor axis of the circumbinary disk is parallel to the large-scale magnetic field according to previous dust polarization observations, suggesting that themisalignment may be caused by the diﬀerent directions of the envelope rotation and the magnetic field. If the velocity gradientof the outflow is caused by rotation, the outflow has a constant angular momentum and the launching radius is estimated tobe 5 16 au, although it cannot be ruled out that the velocity gradient is driven by entrainments of the two high-velocity
outflows. Furthermore, we detected for the first time a velocity gradient associated with rotation toward the VLA 16293B disk.
The velocity gradient is opposite to the one from the large-scale envelope, outflow, and circum-binary disk. The origin of its
opposite gradient is also discussed.

• ALMACosmic
Large Project“FAUST”で取得したProto-multiple
system
VLA1623データの論文，
rays in molecular clouds probed by H2 rovibrational lines – Perspectives for the
James
Space
Telescope+(3-2),Webb
H13CO
CS(5-4),
CCH(N=3-2)を対象にした解析。

Marco Padovani, Shmuel Bialy, Daniele Galli, Alexei V. Ivlev, Tommaso Grassi, Liam H. Scarlett, Una S.
Rehill, MarkC. Zammit, Dmitry V. Fursa, Igor
Bray F Cosmic
rays (CRs)at sub-TeV
energies play a fundamental• Protobinary
VLA1623Aを囲むCicum-binary
diskの短軸‖ (Large
Scale
B-field)だが，Outflow軸やエrole in the chemical and dynamical evolution of molecular clouds, as they control the ionisation, dissociation, and excitationof H2 . Their characterisation is important both for the interpretation of observations and for the development of theoretical
ンベロープ回転軸とは12°ズレあり。初期にクラウド回転と磁場の向きがずれていた？
models. The methods used so far for estimating the CR ionisation rate (⇣) in molecular clouds have several limitations due
to uncertainties in the adopted chemical networks. We refine and extend the method proposed by Bialy (2020) to estimate ⇣• Outflow短軸方向(?)の速度勾配，アウトフローの回転，もしくは2本の高速jetにentrainされた成分
by observing rovibrational transitions of H2 at near-infrared wavelengths, which are mainly excited by secondary CR electrons.
• VLA 1623B
円盤の回転も初検出，大きなスケールのエンベロープの回転方向と逆
Combiningmodels of interstellar CR propagation and attenuation with the calculation of the expected secondary electron
spectrum and updated H2 excitation cross sections by electron collisions, we derive the intensity of the four H2 rovibrationalλ=0.87mm連続波のマップ
FAUST III. Misaligned rotations of the envelope, outflow, and disks

3

Figure 1. Images of the 0.87 mm dust continuum emission observed toward the VLA 1623 region with ALMA. The data istaken from the ALMA archive and details of the observation are described by Harris et al. (2018). The class 0 source, VLA
1623A, is resolved into two sources, VLA 1623A1 and VLA 1623A2. The beam size is shown in the left bottom corner of theright panel. The contours are 0.93, 2.7, 10, and 50 mJy beam 1 (1 = 0.12 mJy beam 1 ) to indicate the circum-binary disk
around VLA 1623A and circum-stellar disk around VLA 1623B.

Note—a
The rotation is seen in H13 CO+ .
b
The rotation is seen in CS.
c
The position angle and inclination are derived by Harris et al. (2018).

考えられる状況のまとめ

Figure 21. A schematic view of the various rotation motions in the VLA 1623 region studied in this work.

A2 protostars may be formed in high-density inner re-of VLA 1623A1 (or A2) is aligned with the rotation of

6

解析したライン強度分布の全景
Ohashi et al.

H13CO+: 赤道面付近に広がり＝エンベロープ
CCH, CS: アウトフロー

Figure 2. A three color image of the integrated intensities of H13 C
VLA 1623 region. The velocity range for integration is VLSR = 6
continuum emission presented by Harris et al. (2018) and shown in

下のプロファイルも参照

Figure 2. A three color image of the integrated intensities of H13 CO+ (blue), CCH (green), and CS (red) emission toward theVLA 1623 region. The velocity range for integration is VLSR = 6 to 10 km s 1 . The white contour shows the 0.87 mm dust
continuum emission presented by Harris et al. (2018) and shown in Figure 1 to indicate the disk and protostellar positions.

Figure 3. H13 CO+ (J = 3 2) and CS (J = 5 4) spectra
toward the protostellar positions of the VLA 1623A1 and B
are shown as the black and red lines, respectively. Verticaldashed lines stand for the source systemic velocity (3.8 km
s 1 ).

13+
Integrated intensity: H CO
FAUST III. Misaligned rotations of the envelope, outflow, and disks

7

Figure 5. Integrated intensity maps of the H13 CO+ emission toward the VLA 1623 region. The velocity range for integrationis 1.4 6.0 km s 1 . The 1-sigma noise level is 2.9 ⇥ 10 3 Jy beam 1 km s 1 . The black contours show the 0.87 mm dust
continuum emission presented by Harris et al. (2018) and shown in Figure 1, to indicate the disk and protostellar positions.
The beam size of the H13 CO+ emission is shown in the bottom left corner of each panel.

Figure 5. Integrated intensity maps of the H13 CO+ emission toward the VLA 1623 region. The velocity range for integrationis 1.4 6.0 km s 1 . The 1-sigma noise level is 2.9 ⇥ 10 3 Jy beam 1 km s 1 . The black contours show the 0.87 mm dust
continuum emission presented by Harris et al. (2018) and shown in Figure 1, to indicate the disk and protostellar positions.
The beam size of the H13 CO+ emission is shown in the bottom left corner of each panel.

Integrated intensity: CS & CCH

Figure 6. Integrated intensity maps of the CS emission in color scale and the CCH emission in black contours toward the VLA
1623 region. The velocity range for integration is 6 to +10 km s 1 . The contours of the CCH emission are 0.02, 0.05, 0.1, and
0.2 Jy beam 1 km s 1 , where 1 = 0.0025 Jy beam 1 km s 1 . The blue thick contours show the 0.87 mm dust continuum
emission (Harris et al. 2018) to indicate the circum-binary disk and protostellar positions. The beam size of the CS emission isshown in the bottom-left corners.

H13CO+
Channel maps

FAUST III. Misaligned rotations of the envelope, outflow, and disks

FAUST III. Misaligned rotations of the envelope, outflow, and disks

99Figure 7. Channel maps of the H13 CO+ (J = 3 2) emission, overlaid with the 0.87 mm dust continuum emission (Harris
et al. 2018) as black contours. The contour is 0.93 mJy beam 1 , indicating the disks of VLA 1623A, B, and W. The channel
1
13 channel
width
and 7.
stepChannel
are 0.6 km
s of
, and
the
labeledat thecentereach panel.emission
The 1-sigma
Figuremaps
the3H
CO+ (J1 centroid= 3 12)velocities
emission,areoverlaid
withthe upper
0.87 mmdustof continuum(Harris
13
+
1
noise
level
for
H
CO
is
1.2
⇥
10
Jy
beam
km
s
in
each
panel.
The
beam
size
is
shown
in
the
bottom-leftcorners.
et al. 2018) as black contours. The contour is 0.93 mJy beam , indicating the disks of VLA 1623A, B, and W. The channel
1width and step are 0.6 km s , and the channel centroid velocities are labeled at the upper center of each panel. The 1-sigma
noise level for H13 CO+ is 1.2 ⇥ 10 3 Jy beam 1 km s 1 in each panel. The beam size is shown in the bottom-left corners.

Figure 8. The same channel maps of the H13 CO+ (J = 3 2) emission as Figure 7, but zoomed-in views around the protostars.
The black contours indicate the 0.87 mm dust continuum emission (Harris et al. 2018) to indicate the disks and stellar positions.
13 TheThe
contour
are thesame maps
as in ofFigureshown inasthebottom-leftcorners. views around the protostars.
Figure8. levels
The samechannelthe H1.
CO+ beam(J = 3size2)is emission
Figure7, but zoomed-in

H13CO+では，ダストのコンパクトな円盤中(下)でも，
Large scaleのマップ(上)と整合的な回転運動が見える

The black contours indicate the 0.87 mm dust continuum emission (Harris et al. 2018) to indicate the disks and stellar positions.
The contour levels are the same as in Figure 1. The beam size is shown in the bottom-left corners.

CS
Channel maps

矢印はFigure 9. Channel maps of the CS emission, overlaid with the 0.87 mm continuum emission (Harris et al. 2018) as black
contours. The contourr level is 0.93 mJy beam , indicating the disks of VLA 1623A,
W. The blue and(Hara+
red arrows
COB, and
Outflow2021)
1

indicate the directions of the CO outflows observed by Hara et al. (2021).
The channel width and step are 0.6 km s 1 , and the channel centroid velocities are labeled at the upper center of each panel.
The 1-sigma noise level for each panel is 0.0012 Jy beam 1 km s 1 . The beam size is shown in the bottom-left corners.

Moment 1 of H13CO+

FAUST III. Misaligned rotations of the envelope, outflow, and disks

13

Protobinary VLA1623Aを囲むCicum-binary diskの
短軸・回転軸とエンベロー
プ回転軸は少しずれている

Figure 11. Intensity-weighted mean velocity (moment 1) maps of the H13 CO+ line toward the VLA 1623 region. The rightpanel is the zoomed-in view around the protostars. The mean velocity is derived using a velocity range of 1.2 6.2 km s 1with an intensity of > 0.015 Jy beam 1 (6 ). The black contour indicates the 0.87 mm dust continuum emission (Harris etal. 2018) with an intensity of 0.93 mJy beam 1 . Magenta dashed lines indicate the minor axis of the circum-binary disk. The
protostellar positions are shown as the star markers. The beam size is shown in the bottom-left corners.

Outflow axisや回転を示唆する速度勾配
Mom0：Outflowの軸はエンMom1：Outflowの軸と垂直方向

ベロープ回転軸とほぼ一致にも速度勾配あり，回転？

FAUST III. Misaligned rotations of the envelope, outflow, and disks

18

17

Ohashi et al.

Figure 15. Integrated intensity maps of the (a) CS and (b) CCH emission overlaid with the 0.87 mm dust continuum emission
Figure(Harris et al. 2018) in blue thick contours. The velocity range for integration is 3.4 4.2 km s 1 . Thin black contoursof the 16. Mean velocity (moment 1) maps of the CS (a) and CCH (b) emission. The mean velocity of the CS emission is11
derivedCS emission start from 5 and have intervals of 15 , where 1 = 1.2 mJy beam 1 km s 1 . Thin black contours of the
CCHby using a velocity range of 0.6 5.4 km s with an intensity of > 0.05 Jy beam , while that of the CCH emission isderivedemission start from 5 and have intervals of 7 , where 1 = 1.4 mJy beam 1 km s 1 . Thick black contours of the CS and
CCHby using a velocity range of 2.6 6.2km s 1 with an intensity of > 0.02 Jy beam 1 to avoid the contamination from theemission encompass the outflow cavity structure and are 25 and 7 , respectively. The 0.87 mm dust continuum contours
are emission. Magenta contours indicate 25 and 7 of the CS and CCH integrated-intensity emission, respectively. Black
hyperfineat a level of 0.93 mJy beam 1 . The magenta dashed, black dotted, and grey lines indicate the minor axis of the circum-binarylines indicate the outflow directions. The dashed lines perpendicular to the outflow axis indicate the cuts for the position-velocity

12.

Self-absorption in [CII], 12 CO, and HI in RCW120. Building up a geometrical andphysical model of the region

S. Kabanovic, N. Schneider, V. Ossenkopf-Okada, F. Falasca, R. Güsten, J. Stutzki, R. Simon, C. Buchbender,
L. Anderson, L. Bonne, C. Guevara, R. Higgins, B. Koribalski, M. Luisi, M. Mertens, Y. Okada, M. Röllig, D.
Seifried, M. Tiwari, F. Wyrowski, A. Zavagno, A. G. G. M. Tielens F Revealing the 3D dynamics of HII regions andtheir associated molecular clouds is important for understanding the longstanding problem as to how stellar feedback aﬀects
the density structure and kinematics of the interstellar medium. We employed observations of the HII region RCW 120 in[CII], observed within the SOFIA legacy program FEEDBACK, and the 12 CO and 13 CO (3!2) lines, obtained with APEX. In
addition we used HI data from the Southern Galactic Plane Survey. Two radiative transfer models were used to fit the observed
data. A line profile analysis with the 1D non-LTE radiative transfer code SimLine proves that the CO emission cannot stemfrom a spherically symmetric molecular cloud configuration. With a two-layer multicomponent model, we then quantified theamount of warm background and cold foreground gas. There is a deficit of CO emission along the line-of-sight toward thecenter of the HII region which indicates that the HII region is associated with a flattened molecular cloud. Self-absorption in
the CO line may hide signatures of infalling and expanding molecular gas. The [CII] emission arises from an expanding [CII]
bubble and from the PDRs. A significant part of [CII] emission is absorbed in a cool ( 60-100 K), low-density (<500 cm 3 )atomic foreground layer with a thickness of a few parsec. We propose that the RCW 120 HII region formed in a flattenedmolecular cloud and is now bursting out of its parental cloud. The compressed surrounding molecular layer formed a torus
around the spherically expanding HII bubble. This scenario can possibly be generalized for other HII bubbles and would explain
the observed “flat" structure of molecular clouds associated with HII bubbles. We suggest that the [CII] absorption observed inmany star-forming regions is at least partly caused by low-density, cool, HI-envelopes surrounding the molecular clouds.

A rich population of free-floating planets in the Upper Scorpius young stellar association
Núria Miret-Roig, Hervé Bouy, Sean N. Raymond, Motohide Tamura, Emmanuel Bertin, David Barrado, Javier• Olivares,
HII領域 Phillip
RCW 120に向けたSOFIA[CII]観測，APEX
12CO(3-2),
dataを組み合わせてモデル化
A. B. Galli, Jean-Charles
Cuillandre, Luis ManuelSarro, HI
Angel
Berihuete, Nuria Huélamo
F
The nature and origin of free-floating planets (FFPs) are still largely unconstrained because of a lack of large homogeneous
することにより，その構造を議論
samples to enable a statistical analysis of their properties. So far, most FFPs have been discovered using indirect methods;
surveys have proved particularly successful to detect these objects down to a few Earth masses. However, the• microlensing
星形成を抑制するフィードバックに対する知見を得たい5

A&A proofs: manuscript no. Self-absorption_in_RCW120_Kabanovic

A&A proofs: manuscript no. Self-absorption_in_RCW120_Kabanovic
A&A proofs: manuscript no. Self-absorption_in_RCW120_Kabanovic

モデルを簡略化したCartoon

観測データ

Galactic( warm(background(HI(Galactic( warm(background(HI(embedding(low6density(
cloud((T<20K),(HI(+(H2embedding(low6density(
cloud((T<20K),(HI(+(H2molecular(
fragmented(shell(molecular(
fragmented(shell(cool(C+cool(C+exciting(star(with(spherical(HII(
region,(UV6radiation(and(X6rays(escape(exciting(star(with(spherical(HII(
region,(UV6radiation(and(X6rays(escape(cool,(low(density(HI(enveloping(the(molecular(
cloud,(carbon(ionized(by(CR(and(X6ray((HISA(cloud)1

expanding(C+(bubble((warm(C+cool,(low(density(HI(enveloping(the(molecular(
cloud,(carbon(ionized(by(CO6clump(with(CII(emitting(CR(and(X6ray((HISA(cloud)
PDR(surfaces

2
3

1

warm(C+A&A proofs: manuscript no. Self-absorption_in_RCW120_Kabanovic

expanding(C+(bubble((Fig. 21: Cartoon of the RCW 120 region where the observer is located on the right and sees a circular sha
2 by a molecular ring that is(which is a 3D bubble in reality), and an expanding C+ shell (red), surrounded
3 of the H II region, this be(blue). The sketch represents a ’cut’, there is also molecular material in front
CO6clump(with(CII(emitting(
CO emission arises from the clump interiors and [C II] from the UV-illuminated clump surfaces and the exradiation and X-rays leak into the surrounding molecular cloud and into the enveloping H I cloud (green). T
PDR(surfaces
cloud in which carbon is mostly ionized by cosmic rays. The Galactic background (green arrows on the lef
HI .

ible because the H II region created a
Fig. 21: Cartoon of the RCW 120 region where the observer is located on the right and seesa circularshapedHgeometr
II reggeneralit is observedthat the+flattened orfilament-like(e.g., Bally e(which is a 3D bubble in reality), and an expanding C shell (red), surrounded by a molecularringthat is fragmented
Heiles & Troland 2003; Molinar(blue). The sketch represents a ’cut’, there is also molecular material in front of the H 1990;
II region, this becomes cleare2010). Though there are di↵erent view
CO emission arises from the clump interiors and [C II] from the UV-illuminated clump surfaces
andthe expandingC+
are forming(quasi-static
vs dynamic
in both cases.
In Ithequa
radiation and X-rays leak into the surrounding molecular cloud and into the enveloping Hscenarios
I cloud fit(green).
This Hlayer
cloud onwould
contract
along itcloud in which carbon is mostly ionized by cosmic rays. The Galactic background (greening
arrowsthefirst
left)
is responsi
sheet-like geometry and then further cHI .
shape (Lin et al. 1965). Since the freecloud is much larger than the one of(Toalá et al. 2012; Pon et al. 2012), clu
will collapse faster than the globible because the H II ament
regioncreated a hole in theing to star formation inside sheet-like
general it is observedbulent,that magneto-hydrodynamic
the geometry of molecu
simulanebelle2005;Bally
Banerjee
et al.
2009; dVflattened or filament-like(e.g.,
et al.
1989;
2006),
sheetsandfilaments
form
natura1990; Heiles & Troland 2003; Molinari et al. 2010
sion in colliding atomic flows.
2010).
Thoughtherearedi↵erent views of how den
Fig. 22: 3D visualization of the RCW120 region to show theit is important
to note thao
are(quasi-staticHowever,vs dynamic
scenarios),
oblate geometry of the molecular cloud.
Theforming
observers perspecstrongly biased towards sheet-like geo
tive is from the right and the line integrated[C II] map
scenarios
fit inis proboth tures
cases.
thequasi-staticview
are Inmore
likelyto be observedorjected on the left side. The spherical ing
H II cloud
region (red)is surwould
firstmolecular
contractclouds
along
its
shortestax
due to the enhanced crounded by the flat, low-density cloud (green). The clumpy PDR
sion
from
the
surrounding
torus and the
sheet-likegeometry(golden clumps) and the expanding C+ bubble(purple)are found and then further collapse to ables embedded in molecular clouds suffi
in the interface region between H II region
and molecular
cloud.
shape(Lin et al.
1965).
Since
themolecular
free falltime
oft
tensionof thecloudin allcloud is much larger larger
thanthanthetheoneof a sphericalc
H II region)
are more diffi
columnalong
the line insideof sight oa(Toalá et al. 2012; Ponet al.density2012),
clumps
Article number, page 22 of 27

ament will collapse faster than the global molecular

15.

The velocity gradient is opposite to the one from the large-scale envelope, outflow, and circum-binary disk. The origin of its
opposite gradient is also discussed.

Cosmic rays in molecular clouds probed by H2 rovibrational lines – Perspectives for theJames Webb Space Telescope

Marco Padovani, Shmuel Bialy, Daniele Galli, Alexei V. Ivlev, Tommaso Grassi, Liam H. Scarlett, Una S.
Rehill, Mark C. Zammit, Dmitry V. Fursa, Igor Bray F Cosmic rays (CRs) at sub-TeV energies play a fundamentalrole in the chemical and dynamical evolution of molecular clouds, as they control the ionisation, dissociation, and excitationof H2 . Their characterisation is important both for the interpretation of observations and for the development of theoreticalmodels. The methods used so far for estimating the CR ionisation rate (⇣) in molecular clouds have several limitations due
to uncertainties in the adopted chemical networks. We refine and extend the method proposed by Bialy (2020) to estimate ⇣by observing rovibrational transitions of H2 at near-infrared wavelengths, which are mainly excited by secondary CR electrons.
Combining models of interstellar CR propagation and attenuation with the calculation of the expected secondary electron
spectrum and updated H2 excitation cross sections by electron collisions, we derive the intensity of the four H2 rovibrationaltransitions observable in dense, cold gas: (1-0)O(2), (1-0)Q(2), (1-0)S(0), and (1-0)O(4). The proposed method allows theestimation of ⇣ for a given observed line intensity and H2 column density. We are also able to deduce the shape of the lowenergy CR proton spectrum impinging upon the molecular cloud. We present a look-up plot and a web-based application thatcan be used to constrain the low-energy spectral slope of the interstellar CR proton spectrum. We comment on the capabilityof the James Webb Space Telescope to detect these near-infrared H2 lines, making it possible to derive for the first time spatial
variation of ⇣ in dense gas. Besides the implications for the interpretation of the chemical-dynamic evolution of a molecular
cloud, it will be possible to test competing models of CR propagation and attenuation in the interstellar medium, as well ascompare CR spectra in diﬀerent Galactic regions.

Application of a Steady-State Accretion Disk Model to Spectrophotometry and HighResolution Spectra of Two Recent FU Ori Outbursts

Antonio C. Rodriguez, Lynne A. Hillenbrand F We apply a conventional accretion disk model to the FU Ori-type
objects HBC 722 and Gaia 17bpi. Our base model is a steady-state, thin Keplerian disk featuring a modified Shakura• H2rovibrationallinesを観測することで宇宙線のionisation
rateを推定する方法に関する理論
Sunyaev temperature profile, with each annulus radiating as an area-weighted spectrum given by a NextGen atmosphere at
the appropriate temperature. We explore departures from the standard model by altering the temperature distribution in the• JWSTを想定した観測可能性についても議論
innermost region of the disk to account for "boundary region"-like eﬀects. We consider the overall spectral energy distribution(SED) as well as medium- and high-resolution spectra in evaluating best-fit models to the data. Parameter degeneracies arestudied via a Markov Chain Monte Carlo (MCMC) parameter estimation technique. Allowing all parameters to vary, we find
6.70
1 +0.46
accretion rates for HBC 722 of Ṁ = 10 4.90 M yr 1 +0.99
dex
and
for
Gaia
17bpi
of
Ṁ
=
10
M
yr
0.40
0.36 dex; the+900
corresponding maximum disk temperatures are 7100+300
K
and
7900
500
400 K, respectively. While the accretion rate of HBC 722
is on the same order as other FU Ori-type objects, Gaia 17bpi has a lower rate than previously reported as typical, commensurate