Star Formation Newsletter Seminar
4/15
古屋 #350 23-28

HII領域の進化を正しく捉えるために必要な半径の計算分解能はいくらだろうか？ 適切に設定しないと,

23

物理量を1桁過大/過小評価する恐れがある.

https://arxiv.org/abs/2112.09013v1

Warpとnon-coplanar円盤構造があれば, 円盤形成の初期に見られたであろう, 大局的構造は消え, リングとギャップが形成されることを3D SPH計算で示した.

24

https://arxiv.org/abs/2110.06227v2

重水素化メタンをclass 0/I褐色矮星で初検出 ⇨ 存在比と重水素濃縮領域の密度を推定 ⇨ CH4&CH3Dを気相に戻す過程が重要/WCC化学的描像と整合する.

25

https://arxiv.org/abs/2201.07064v1

IRAM 30mで褐色矮星前駆天体で重水素化合物探査 ⇨ 低温イオン分子反応＆塵表面反応化学からの存在比と整合的だが, D/H比と強い相関を示す物理量はなかった

26

https://arxiv.org/abs/2201.07315v1

SMAでCyg.Xでの分子流探査 ⇨ 分子流の運動量率と光度やMenvとの相関解析からlow-massとhigh-massでは関連性は低そうだが, 前者と系外銀河では関連!?

27

https://arxiv.org/abs/2202.04676v1

TW Hydraで過去に取得された, すべての長基線データを2つの方法で像合成 ⇨ 求められたβの空間分布はmmサイズのダストがギャップ内ではみられないことと整合

28

https://arxiv.org/abs/2202.00376v1

ALMA High-resolution Multiband Analysis for the Protoplanetary Disk around TW
Hya

Takashi Tsukagoshi, Hideko Nomura, Takayuki Muto, Ryohei Kawabe, Kazuhiro D. Kanagawa, Satoshi Okuzumi,
Shigeru Ida, Catherine Walsh, Tom J. Millar, Sanemichi Z. Takahashi, Jun Hashimoto, Taichi Uyama, Motohide Tamura F We present a high-resolution (2.5 au) multiband analysis of the protoplanetary disk around TW Hya using
ALMA long baseline data at Bands 3, 4, 6, and 7. We aim to reconstruct a high-sensitivity millimeter continuum image
and revisit the spectral index distribution. The imaging is performed by combining new ALMA data at Bands 4 and 6 withavailable archive data. Two methods are employed to reconstruct the images; multi-frequency synthesis (MFS) and the fiducial
image-oriented method, where each band is imaged separately and the frequency dependence is fitted pixel by pixel. We findthat the MFS imaging with the second order of Taylor expansion can reproduce the frequency dependence of the continuum
emission between Bands 3 and 7 in a manner consistent with previous studies and is a reasonable method to reconstruct the
spectral index map. The image-oriented method provides a spectral index map consistent with the MFS imaging, but witha two times lower resolution. Mock observations of an intensity model were conducted to validate the images from the two
methods. We find that the MFS imaging provides a high-resolution spectral index distribution with an uncertainty of < 10 %.
Using the submillimeter spectrum reproduced from our MFS images, we directly calculated the optical depth, power-law index
of the dust opacity coeﬃcient ( ), and dust temperature. The derived parameters are consistent with previous works, and theenhancement of within the intensity gaps is also confirmed, supporting a deficit of millimeter-sized grains within the gaps.
TW Hydraで過去に取得された, すべての長基線データを2つの方法で像合成 ⇨ 求められたβの空間分布はmmサイズのダストがギャップ内ではみられないことと整合

A 16 au Binary in the Class 0 Protostar L1157 MMS

John J. Tobin, Erin G. Cox, Leslie W. Looney F We present VLA observations toward the Class 0 protostar L1157
MMS at 6.8 mm and 9 mm with a resolution of 0.04" (14 au). We detect two sources within L1157 MMS and interpret thesesources as a binary protostar with a separation of 16 au. The material directly surrounding the binary system within the inner
50 au radius of the system has an estimated mass of 0.11 M , calculated from the observed dust emission. We interpret theobserved binary system in the context of previous observations of its flattened envelope structure, low rates of envelope rotationfrom 5000 to 200 au scales, and an ordered, poloidal magnetic field aligned with the outflow. Thus, L1157 MMS is a prototype
system for magnetically-regulated collapse
and the presence of a compact binary within L1157 MMS demonstrates that multiple
https://arxiv.org/abs/2202.00376v1

28

ALMA High-resolution Multiband Analysis for the Protoplanetary Disk around TW Hya
1

1

2

1

shi Tsukagoshi, Hideko Nomura, Takayuki Muto, Ryohei Kawabe, Kazuhiro D. Kanagaw
4
5
6
7
1
uzumi, Shigeru Ida, Catherine Walsh, Tom J. Millar, Sanemichi Z. Takahashi, Jun Has
9, 108, 11, 12
Taichi Uyama,and Motohide Tamura

vision of Science, National Astronomical Observatory of Japan, Osawa 2-21-1, Mitaka, Tokyo 181-8588, Japan
Division of Liberal Arts, Kogakuin University, 1-24-2 Nishi-Shinjuku, Shinjuku-ku, Tokyo, 163-8677, Japan
3 College of Science, Ibaraki University, Bunkyo 2-1-1, Mito, Ibaraki, 310-8512, Japant of Earth and Planetary Sciences, Tokyo Institute of Technology, 2-12-1 Ookayama, Meguro, Tokyo, 152-8551
arth-Life Science Institute, Tokyo Institute of Technology, 2-12-1 Ookayama, Meguro, Tokyo 152-8550, Japan
6 School of Physics and Astronomy, University of Leeds, Leeds, LS2 9JT, UK
Research Centre, School of Mathematics and Physics, Queen’s University Belfast, University Road, Belfast BT7
8 Astrobiology Center, 2-21-1 Osawa, Mitaka, Tokyo 181-8588, Japan
9 Infrared Processing and Analysis Center, California Institute of Technology, Pasadena, CA 91125, USA
10 NASA Exoplanet Science Institute, California Institute of Technology, Pasadena, CA 91125, USAubaru Telescope, National Astronomical Observatory of Japan, Osawa 2-21-1, Mitaka, Tokyo 181-8588, Japan
12 Department of Astronomy, School of Science, University of Tokyo, Bunkyo, Tokyo 113-0033, Japan

28

TW Hydraで過去に取得された, すべての長基線データを2つの方法で像合成 ⇨ 求められたβの空間分布はmmサイズのダストがギャップ内ではみられないことと整合(Received Mar 15, 2021; Revised January 28, 2022; Accepted February 2, 2022)

https://arxiv.org/abs/2202.00376v1

Tsukagoshi
al.
ALMA4 High-resolution Multiband Analysis
for theetProtoplanetary
Disk around TW Hya
1

1

2

1

shi Tsukagoshi, Hideko Nomura, Takayuki Muto, Ryohei Kawabe, Kazuhiro D. Kanagaw
4
5
6
7
1
uzumi, Shigeru Ida, Catherine Walsh, Tom J. Millar, Sanemichi Z. Takahashi, Jun Has
9, 108, 11, 12
Taichi Uyama,and Motohide Tamura

vision of Science, National Astronomical Observatory of Japan, Osawa 2-21-1, Mitaka, Tokyo 181-8588, Japan
Division of Liberal Arts, Kogakuin University, 1-24-2 Nishi-Shinjuku, Shinjuku-ku, Tokyo, 163-8677, Japan
3 College of Science, Ibaraki University, Bunkyo 2-1-1, Mito, Ibaraki, 310-8512, Japant of Earth and Planetary Sciences, Tokyo Institute of Technology, 2-12-1 Ookayama, Meguro, Tokyo, 152-8551
arth-Life Science Institute, Tokyo Institute of Technology, 2-12-1 Ookayama, Meguro, Tokyo 152-8550, Japan
6 School of Physics and Astronomy, University of Leeds, Leeds, LS2 9JT, UK
Research Centre, School of Mathematics and Physics, Queen’s University Belfast, University Road, Belfast BT7
8 Astrobiology Center, 2-21-1 Osawa, Mitaka, Tokyo 181-8588, Japan
9 Infrared Processing and Analysis Center, California Institute of Technology, Pasadena, CA 91125, USA
10 NASA Exoplanet Science Institute, California Institute of Technology, Pasadena, CA 91125, USAubaru Telescope, National Astronomical Observatory of Japan, Osawa 2-21-1, Mitaka, Tokyo 181-8588, Japan
12 Department of Astronomy, School of Science, University of Tokyo, Bunkyo, Tokyo 113-0033, Japan
Figure 1. Whole view of the UV coverage of the combined data of Bands 3, 4, 6 and 7 from left to right (top). Close-up viewof the UV coverage inside ±1000 k (bottom).

28(Received Mar 15, 2021; Revised January 28, 2022; Accepted February 2, 2022)

https://arxiv.org/abs/2202.00376v1
weighting with a robust parameter of 0. We employed
for the shorter baseline data and from 6000 to 900 sec

ALMA High-resolution Multiband Analysis for the Protoplanetary Disk around TW Hya
1

1

2

1

shi Tsukagoshi, Hideko Nomura, Takayuki Muto, Ryohei Kawabe, Kazuhiro D. Kanagaw
4
5
6
7
1
uzumi, Shigeru Ida, Catherine Walsh, Tom J. Millar, Sanemichi Z. Takahashi, Jun Has
9, 108, 11, 12
Taichi Uyama,and Motohide Tamura

vision of Science, National Astronomical Observatory of Japan, Osawa 2-21-1, Mitaka, Tokyo 181-8588, Japan
Division of Liberal Arts, Kogakuin University, 1-24-2 Nishi-Shinjuku, Shinjuku-ku, Tokyo, 163-8677, Japan
3 College of Science, Ibaraki University, Bunkyo 2-1-1, Mito, Ibaraki, 310-8512, Japant of Earth and Planetary Sciences, Tokyo Institute of Technology, 2-12-1 Ookayama, Meguro, Tokyo, 152-8551
arth-Life Science Institute, Tokyo Institute of Technology, 2-12-1 Ookayama, Meguro, Tokyo 152-8550, Japan
6 School of Physics and Astronomy, University of Leeds, Leeds, LS2 9JT, UK
Research Centre, School of Mathematics and Physics, Queen’s University Belfast, University Road, Belfast BT7
8 Astrobiology Center, 2-21-1 Osawa, Mitaka, Tokyo 181-8588, Japan
9 Infrared Processing and Analysis Center, California Institute of Technology, Pasadena, CA 91125, USA
10 NASA Exoplanet Science Institute, California Institute of Technology, Pasadena, CA 91125, USAubaru Telescope, National Astronomical Observatory of Japan, Osawa 2-21-1, Mitaka, Tokyo 181-8588, Japan
12 Department of Astronomy, School of Science, University of Tokyo, Bunkyo, Tokyo 113-0033, Japan(Received Mar 15, 2021; Revised January 28, 2022; Accepted February 2, 2022)

https://arxiv.org/abs/2202.00376v1

Warping Away Gravitational Instabilities in Protoplanetary Discs

Sahl Rowther, Rebecca Nealon, Farzana Meru F We perform 3D SPH simulations of warped, non-coplanar gravitationally unstable discs to show that as the warp propagates through the self-gravitating disc, it heats up the disc rendering it
gravitationally stable. Thus losing their spiral structure and appearing completely axisymmetric. In their youth, protoplanetary
discs are expected to be massive and self-gravitating, which results in non-axisymmetric spiral structures. However recent observations of young protoplanetary discs with ALMA have revealed that discs with large-scale spiral structure are rarely observedin the midplane. Instead, axisymmetric discs with some also having ring & gap structures are more commonly observed. Our
work invloving warps, non-coplanar disc structures that are expected to commonly occur in young discs, potentially resolves thisdiscrepancy between observations and theoretical predictions. We demonstrate that they are able to suppress the large-scale
spiral structure of self-gravitating protoplanetary discs.

First CH3 D detection in Class 0/I proto-brown dwarfs: constraints on CH4 abundances

B. Riaz, W. -F. Thi F We report the first detection in the JK = 10 - 00 rotational transition line of CH3 D towards three Class
0/I proto-brown dwarfs (proto-BDs) from IRAM 30 m observations. Assuming a rotational temperature of 25 K, the CH3 D
7abundances (relative to H2 ) are in the range of (2.3–14.5) ⇥ 10 . The CH4 abundances derived from the CH3 D abundances++
5+
and assuming the DCO /HCO ratios are in the range of (0.05–4.8) ⇥10 . The gas-phase formation of CH3 D via CH2 D
8
10
3
is enhanced at high densities of 10 –10 cm and our observations are likely probing the innermost dense and warm regionsin proto-BDs. Thermal and/or non-thermal desorption can return the CH3 D and CH4 molecules formed at an early stage on
grain surfaces to the gas-phase. The gas phase abundances are indicative of warm carbon-chain chemistry in proto-BDs wherecarbon-chain molecules are synthesized in a lukewarm (⇠20-30 K) region close to the central source.

24
Deuterium chemistry and D/H ratios in Class 0/I proto-brown dwarfs

B.Warpとnon-coplanar円盤構造があれば,Riaz, W. -F. Thi F We haveconducted the first extensive
observational
survey of several deuterated species
in 16 Class
円盤形成の初期に見られたであろう,
大局的構造は消え,
リングとギャップが形成されることを3D
SPH計算で示した.
0/I proto-brown dwarfs (proto-BDs) https://arxiv.org/abs/2110.06227v2
and 4 Class Flat/Class II brown dwarfs. Observations were obtained with the IRAM
+

+

+

13

+

13

24

Warpとnon-coplanar円盤構造があれば, 円盤形成の初期に見られたであろう, 大局的構造は消え, リングとギャップが形成されることを3D SPH計算で示した.

https://arxiv.org/abs/2110.06227v2

https://arxiv.org/abs/2110.06227v2

24
https://arxiv.org/abs/2110.06227v2

https://arxiv.org/abs/2110.06227v2

24
https://arxiv.org/abs/2110.06227v2

https://arxiv.org/abs/2110.06227v2

Connecting Galactic and extragalactic outflows: From the Cygnus-X cluster to active
galaxies

I. M. Skretas, L. E. Kristensen F Molecular outflows are often detected originating from both protostellar and extragalactic
sources. Studies of low-mass, isolated high-mass, and extragalactic sources reveal scaling relations connecting the force carriedby an outflow and the properties of the source that drives it. The aim of this work is to examine the eﬀects of clustered starformation on the protostellar outflows and their scaling relations and to explore the possibility that outflows varying greatly
scale and energetics are consistent with being launched by the same physical processes. High-angular resolution CO J = 3-2
observations were used of ten high-mass protostars in the Cygnus-X molecular cloud, obtained at the SMA as part of the
PILS-Cygnus survey. From these data, the outflow force was measured. In addition, an extended sample of protostellar andextragalactic outflow-force measurements was assembled from existing literature to allow for a direct comparison of the scaling
relations of the two types of outflows. Molecular outflows were detected originating from all ten sources of the PILS-Cygnus
survey, and their outflow forces are found in close agreement with measurements from the literature. The comparison of the
protostellar and extragalactic sources reveals, with 95% confidence, that Class 0 protostars and extragalactic sources follow thesame outflow force–bolometric luminosity correlation. The close agreement between the Cygnus-X sources and sources of similarenvelope mass and bolometric luminosity suggests that clustered star formation has no significant eﬀect on protostellar outflows.
We find a strong indication that protostellar and extragalactic outflows are consistent with having a similar launch mechanism.
The existence of such a mechanism would enable the development of a single universal outflow launch model, although more
observations are required in order to verify this connection.

ALMA High-resolution Multiband Analysis for the Protoplanetary Disk around TW
Hya

Takashi Tsukagoshi, Hideko Nomura, Takayuki Muto, Ryohei Kawabe, Kazuhiro D. Kanagawa, Satoshi Okuzumi,
Shigeru Ida, Catherine Walsh, Tom J. Millar, Sanemichi Z. Takahashi, Jun Hashimoto, Taichi Uyama, MotoSMAでCyg.Xでの分子流探査
分子流の運動量率と光度やMenvとの相関解析からlow-massとhigh-massでは関連性は低そうだが,前者と系外銀河では関連!?
hide Tamura F We ⇨present
a high-resolution (2.5 au) multiband analysis of the protoplanetary disk around
TW Hya using
ALMA long baseline data at Bands 3, 4, 6, and 7. We aim to reconstruct a high-sensitivity millimeter continuum image
and revisit the spectral index distribution.
The
imagingisperformedbycombining
new
ALMA
data
at
Bands
4
and
6
with
https://arxiv.org/abs/2202.04676v1

27

SMAでCyg.Xでの分子流探査 ⇨ 分子流の運動量率と光度やMenvとの相関解析からlow-massとhigh-massでは関連性は低そうだが, 前者と系外銀河では関連!?

https://arxiv.org/abs/2202.04676v1

A&A proofs: manuscript no. main

Fig. 1. Continuum emission of the sources of the PILS-Cygnus survey (Pitts et al. 2022) plotted in gray-scale ranging from –0.1 to 0.5 Jy beam 1
in all maps. Displayed in red contours is the red-shifted CO emission, in blue contours is the blue-shifted CO emission, and in green contours is theintegrated SiO emission, when detected. All contour levels are set at 3,6,9,12,15 rms noise of the corresponding integrated emission.The yellow
star marks the assumed origin of the outflow and the light blue and orange lines mark the extend of the outflow lobes. Finally, the beam is marked
with the black contour at the bottom left.

Article number, page 4 of 37

https://arxiv.org/abs/2202.04676v1

In Fig. 7 the same characteristics displayed in Fig. 6 (i.e., Table 7. Best-fit parameters for the various subsamples.
「low-massとhigh-massでは関連性は低そう
good
agreement between the Cygnus-X and the Maud et al.
Sources
Slope (a)Intercept (b)(2015b) sources and a clear separation between the low- andだが,前者と系外銀河では関連!?」
Extragalactic 0.93 ± 0.11
6.7 ± 1.3
high-mass
sample)can be seen. We note though that the sepAGN
0.86 ± 0.14
5.9 ± 1.6
aration between the low- and high-mass samples appears moreSB
1.08 ± 0.20
8.6 ± 2.3
pronounced in the FCO - Lの根拠は, bol correlation (Fig. 7) than in the F CO
High-mass
0.69 ± 0.08
5.5 ± 0.3
- それぞれの天体種ごとに求められた相関同士
Menv correlation (Fig. 6). Therefore, overall this comparison
Low-mass
0.89 ± 0.20
4.7 ± 0.2
reinforces the points made in Sec. 4.1.1.
Class I
0.52 ± 0.24
5.1 ± 0.2
The most
important questions arising from Fig. 7 is how wellの関連性の強弱(右の3つの表)
Class 01.02 ± 0.26
4.3 ± 0.2
the FCO - Lbol correlations for the di↵erent object types compare,A&A proofs: manus
and if it is at all possible to assume a common correlation for all
The best fit is of the form log(FCO ) = a log(Lbol ) + b
three (low-mass, high-mass and extragalactic) samples. In order Notes.
Table 8. F-values for the best-fit variances comparisons and the degrees of f
A&A proofs: manuscript no. main
to address these questions, we calculated the best-fit of the FCO Lbol correlation for each of the samples.Table
In8.addition
these,
we comparisons and the degrees of freedom for each sample. Class 0 Class I Low-mass
F-values for to
the best-fit
variances
Extragalactic
1.11
1.85
2.11
also examined the AGN- and SB-driven outflows separately, as
a
Class
0
Class
I
Low-mass
High-mass
Starburst
AGN
DF
where s1 and s2 are thevariances to1.01
be compared,
with
AGN
1.69
1.93s1
well as the Class 0 and Class I sources. The least-squares
method 1.11
Extragalactic
1.85
2.11
2.28
1.51
1.09
49
Starburst 1.66 with
1.67
2.81 value3.19
s2 . The(Fcrit1.01
1.69 F-value
1.93 is then
2.49compared- a critical33
is used to find the best-fits, which are of the form: AGN
High-mass
2.52
4.80
Starburst
1.67
3.19on the degrees
1.50- (DF)
15 4.22
which2.81
depends
of- freedomof both sample
Low-mass
1.91
High-mass
2.52
4.22
4.80
84 1.14
These1.14
are calculatedasN 1 foreach
sample,with N - beinlog(FCO ) = a log(Lbol ) + b.
Low-mass (6) 1.91
66
Class I
1.67
the number
of- sourcesClass
in
If
Class I
1.67
- the sample.
- the34F-value calculate0-Class 0-is smaller
31
than Fcrit , then the two variances are consistent wit
The a and b parameters describing the fits for the various subNotes.
comparisonsareequivalentandcompared.
therefore
nottheshown.
Value
Mirrored comparisonsare equivalent andtherefore
not Mirrored
shown.
Valuesin boldface
arestatisticallysignificant
meaning thattwo
populabeing
similarandthetwo samples
can
be
In
this
wor
samples are shown in Table 7 and theNotes.
correlations
themselves
tions are comparable. (a) DF = N 1 for the F-test tions are comparable. (a) DF = N 1 for the F-test
we use the F-table for ↵ = 0.05, which corresponds to a 95%
are shown in Fig. D.1 in the Appendix.
confidence
level.
To properly compare the various fitsa statistical
is of theTable
9. P-values and approach
DF for comparison
intercept and slopeofto the dominancehigh-massand
protostellar
Table 9. P-valueseasily
and attributed
DF for comparisonof theofintercept
slope ofout- ea
samples with matching variances.
flows when averaging over a large number of clusters in the toneeded. As a first step, we performed an F-test on the variances
samples
withmatching
variances.
For
the
pairs
with
comparable
variancesthenperforme
tal outflow
activity of starburst
galaxies,weunlessthe initial
mass flaof the samples, comparing them in pairs. Briefly, to perform an
Pslope Pinter DF
functionissignificantly
more
top-heavyinthesegalaxies.
two-tailed
t-tests in order to examine if the parametersof thetaaExtragalactic
0.72 0.69
80
F-test we need to calculate the F-value, which
is given- AGN
as:Pslope Pinter DF
fu
Extragalactic - SB
0.53 best-fit,
0.49
62
the slope (a) and the intercept(b), are similar or not. Fo- AGN
0.72 0.6980
5. Summaryand conclusions
Extragalactic - Class 0 0.75 0.07
78 Extragalacticat-testtheinitialhypothesis
is
that
the
parameters
are equal (i
s1
SB
0.53
0.49
62
AGN - Starburst
0.40 0.35
46 Extragalactic
This
paper
presents
interferometricobservationsof
CO J = 3–
(7)
F= ,
this
case
the
intercept,
H
:
b
=
b
)
and
we
calculate
the t-valu
AGN
Class
I
0.21
0.65
65
0
1
2
Extragalactic
Class
0
0.75
0.07
78
2 and SiO J = 8–7 emission lines of ten high-mass protostellar 5s2
0.61 0.33
62
AGN - Class 0
Article number, page 10 of 37

in the Cygnus-X 0.40
molecular0.35
cloud, taken
AGN - sources
Starburst
46from the PILS- T
out withthe SubMillimeter
Array.
AGN - Cygnus
Class Isurvey and carried
0.21
0.65
65
addition, an extended sample of low-mass protostellar, high- 2
0.61 0.33
62
AGN - InClass
0mass protostellar and extragalactic outflows with measured out- so
Starburst
Classwas
0 gathered0.87
44 these data, C
flow-forces,from the0.07
literature. Using
Starburst- High-mass
0.08from this
0.19work, are97as follows: In
the mainconclusions arising
Notes. (a) DF = N1 + N2 4 for the two-tailed t-test . Pairs marked in
Low-mass- ClassI
0.23maps0.10
boldface can be considered to follow the same FCO - Lbol correlation– Using
integrated
intensityof the CO J98= 3–2 line emis- m
Class I - Class00.15were 0.003
63
sion, molecular
outflows
detected originatingfrom all flStarburst - Class 0
Starburst - High-mass
Low-mass - Class I
Class I - Class 0

0.87
0.08
0.23
0.15

0.07
0.19
0.10
0.003

44
97
98
63

ten sources of the PILS-Cygnus survey, and their respectivethwhether this correlation will lead to the same conclusion.
(a) Pitts
outflowwere
successfullymeasured
both
Notes. DF = N1 +N2 4forces
for thetwo-tailed
t-test. Pairs using
markedin theet al. (2022) compared envelope masses and bolometric lumiseparation,
the hvi, andthe vmaxF methods.
boldfacecanbeconsideredtofollowthesame
CO - Lbol correlation
nosities for protostars with luminosities in the range of < 1 L– The close agreement found between
the FCO , measured for5
to > 10 L , and found that they correlate with envelope mass as
the ten Cygnus-X sources, with results from the literature
1.2
Lbol / Menv
. Thus, since the power-law index is shallower thanfor sources with similar Menv and Lbol , indicate that clusteredthat of the IMF at M > 0.5 M , we would also conclude
thatthestar formation
has noto
significante↵ect
on the outflow
behavwhether this correlation
will leadthe same
conclusion.
Pitts
low-mass protostars drive the outflow contribution.
ior of protostars. As the outflow activity is tied to the accreet al. (2022) comparedenvelope masses and bolometric lumition process, this result suggests that protostellar accretion
The correlations are based on observations of a number of
nosities
luminosities
inthe
thesurrounding
range ofenvironment,<1L
is not withsignificantlya↵ected byhigh-mass star-forming regions, which likely containboth5 forhigh-protostars
to > 10
L ,aand foundtheywith envelope
mass
but it isthatrathertiedcorrelate
to local processes,
determinedby theasproand low-mass protostars. In these cases, the regions
contain
1.2
tostar itself.
single dominant outflow that is driven by the high-mass
protoLbol / M
env . Thus, since the power-law index is shallower than–of the FCO - Menv and FCO - Lbol correlations forstar, a result that is common to other studies (e.g.,
Beutheret IMFal.
thatof theat Examination
M
>
0.5
M
, we would also conclude that thethe protostellar sources, reveals clear di↵erences between the2002). This would suggests that the outflows from high-mass
low-mass
protostars
drive
the outflow
contribution.
lowand high-mass
protostellar
sources both in the correlaprotostars dominate the output from clusters, incontradiction
tionareitselfbased
as wellon
as in
the observed scatter.
with the result above. However, the time over whichThehigh-mass
correlations
observationsof a number of–Thestatisticalcomparison
ofthebest-fits
to the FCO - Lbol
sources accrete and drive outflows is significantly shorter thanhttps://arxiv.org/abs/2202.04676v1

https://arxiv.org/abs/2202.04676v1

Deuterium chemistry and D/H ratios in Class 0/I proto-brown dwarfs

B. Riaz, W. -F. Thi F We have conducted the first extensive observational survey of several deuterated species in 16 Class
0/I proto-brown dwarfs (proto-BDs) and 4 Class Flat/Class II brown dwarfs. Observations were obtained with the IRAM
30m telescope in the DCO+ (3-2), DCN (3-2), DNC (3-2), and N2 D+ (3-2) lines. The DCO+ /H13 CO+ , DCN/H13 CN, and
DNC/HN13 C ratios are comparatively higher and show a narrower range than the DCO+ /HCO+ , DCN/HCN, and DNC/HNC
ratios, respectively. The mean D/H ratios for the proto-BDs derived from these molecules are in the range of ⇠0.02-3. Both
low-temperature gas-phase ion-molecule deuteron transfer and grain surface reactions are required to explain the enhanced
deuterium fractionation. The very dense and cold (nH2 106 cm 3 , T 10 K) interior of the proto-BDs provide the suitableconditions for eﬃcient deuterium fractionation in these cores. There is no correlation between the D/H ratios and the CO
depletion factor, with the exception of the DCN/HCN ratios that show a strong anti-correlation possibly due to the diﬀerencein the peak emitting regions of the DCN and HCN molecules. Over a wide range in the bolometric luminosities spanning⇠0.002–40 L , we find a trend of higher DCO+ /HCO+ (r = -0.7) and DCN/HCN (r = -0.6) ratios, nearly constant DNC/HNC(r = -0.4) and DNC/HN13 C (r = -0.1) ratios, lower N2 D+ /N92 H+ ratios (r = 0.6) in the proto-BDs compared to protostars.
+
Only one Class II brown dwarf shows emission in the DCO (3-2) line. No correlation is seen between the D/H ratios and theevolutionary stage.

Connecting Galactic and extragalactic outflows: From the Cygnus-X cluster to active
galaxies

I. M. Skretas, L. E. Kristensen F Molecular outflows are often detected originating from both protostellar and extragalactic
sources. Studies of low-mass, isolated high-mass, and extragalactic sources reveal scaling relations connecting the force carriedby an outflow and the properties of the source that drives it. The aim of this work is to examine the eﬀects of clustered starformation on the protostellar outflows and their scaling relations and to explore the possibility that outflows varying greatly
scale30mで褐色矮星前駆天体で重水素化合物探査
and energetics are consistent with being
launched by the same physical processes. High-angularresolution CO J = 3-2
IRAM⇨ 低温イオン分子反応＆塵表面反応化学からの存在比と整合的だが,D/H比と強い相関を示す物理量はなかった
observations were used of ten high-mass protostars in the Cygnus-X molecular cloud, obtained at the SMA as part of the
PILS-Cygnus survey. From these data,
the outflow force was measured. In addition, an extended sample of protostellar andhttps://arxiv.org/abs/2201.07315v1

26

26

IRAM 30mで褐色矮星前駆天体で重水素化合物探査 ⇨ 低温イオン分子反応＆塵表面反応化学からの存在比と整合的だが, D/H比と強い相関を示す物理量はなかった

https://arxiv.org/abs/2201.07315v1

IRAM 30mで褐色矮星前駆天体で重水素化合物探査 ⇨ 低温イオン分子反応＆塵表面反応化学からの存在比と整合的だが, D/H比と強い相関を示す物理量はなかった

https://arxiv.org/abs/2201.07315v1

26

IRAM 30mで褐色矮星前駆天体で重水素化合物探査 ⇨ 低温イオン分子反応＆塵表面反応化学からの存在比と整合的だが, D/H比と強い相関を示す物理量はなかった

https://arxiv.org/abs/2201.07315v1

First CH3 D detection in Class 0/I proto-brown dwarfs: constraints on CH4 abundances

B. Riaz, W. -F. Thi F We report the first detection in the JK = 10 - 00 rotational transition line of CH3 D towards three Class
0/I proto-brown dwarfs (proto-BDs) from IRAM 30 m observations. Assuming a rotational temperature of 25 K, the CH3 D
abundances (relative to H2 ) are in the range of (2.3–14.5) ⇥ 10 7 . The CH4 abundances derived from the CH3 D abundances
and assuming the DCO+ /HCO+ ratios are in the range of (0.05–4.8) ⇥10 5 . The gas-phase formation of CH3 D via CH2 D+
is enhanced at high densities of 108 –1010 cm 3 and our observations are likely probing the innermost dense and warm regionsin proto-BDs. Thermal and/or non-thermal desorption can return the CH3 D and CH4 molecules formed at an early stage on
grain surfaces to the gas-phase. The gas phase abundances are indicative of warm carbon-chain chemistry in proto-BDs wherecarbon-chain molecules are synthesized in a lukewarm (⇠20-30 K) region close to the central source.

Deuterium chemistry and D/H ratios in Class 0/I proto-brown dwarfs

B. Riaz, W. -F. Thi F We have conducted the first extensive observational survey of several deuterated species in 16 Class
0/I proto-brown dwarfs (proto-BDs) and 4 Class Flat/Class II brown dwarfs. Observations were obtained with the IRAM
+
+
+
13
+
13
30m telescope in the DCO (3-2), DCN (3-2), DNC (3-2), and N2 D (3-2) lines. The DCO /H CO , DCN/H CN, and13++
DNC/HN C ratios are comparatively higher and show a narrower range than the DCO /HCO , DCN/HCN, and DNC/HNC
ratios, respectively. The mean D/H ratios for the proto-BDs derived from these molecules are in the range of ⇠0.02-3. Both
low-temperature gas-phase ion-molecule deuteron transfer and grain surface reactions are required to explain the enhanced
63
deuterium fractionation. The very dense and cold (nH2 10 cm , T 10 K) interior of the proto-BDs provide the suitableconditions for eﬃcient deuterium fractionation in these cores. There is no correlation between the D/H ratios and the CO
depletion factor, with the exception of the DCN/HCN ratios that show a strong anti-correlation possibly due to the diﬀerencein the peak emitting regions of the DCN and HCN molecules. Over a wide range in the bolometric luminosities spanning25

重水素化メタンをclass 0/I褐色矮星で初検出 ⇨ 存在比と重水素濃縮領域の密度を推定 ⇨ CH4&CH3Dを気相に戻す過程が重要/WCC化学的描像と整合する.

9

https://arxiv.org/abs/2201.07064v1

25

重水素化メタンをclass 0/I褐色矮星で初検出 ⇨ 存在比と重水素濃縮領域の密度を推定 ⇨ CH4&CH3Dを気相に戻す過程が重要/WCC化学的描像と整合する.

https://arxiv.org/abs/2201.07064v1

https://arxiv.org/abs/2201.07064v1

How D-type HII region expansion depends on numerical resolution

J. M. Pittard, M. M. Kupilas, C. J. Wareing F We investigate the resolution dependence of HII regions expanding pasttheir Strömgren spheres. We find that their structure and size, and the radial momentum that they attain at a given time, isin good agreement with analytical expectations if the Strömgren radius is resolved with dr  0.3 Rst . If this is not satisfied,
the radial momentum may be over- or under-estimated by factors up to 10 or more. Our work has significance for the amountof radial momentum that a HII region can impart to the ambient medium in numerical simulations, and thus on the relative
importance of ionizing feedback from massive stars.

Warping Away Gravitational Instabilities in Protoplanetary Discs

Sahl Rowther, Rebecca Nealon, Farzana Meru F We perform 3D SPH simulations of warped, non-coplanar gravitationally unstable discs to show that as the warp propagates through the self-gravitating disc, it heats up the disc rendering it
gravitationally stable. Thus losing their spiral structure and appearing completely axisymmetric. In their youth, protoplanetary
discs are expected to be massive and self-gravitating, which results in non-axisymmetric spiral structures. However recent observations of young protoplanetary discs with ALMA have revealed that discs with large-scale spiral structure are rarely observedin the midplane. Instead, axisymmetric discs with some also having ring & gap structures are more commonly observed. Our
work invloving warps, non-coplanar disc structures that are expected to commonly occur in young discs, potentially resolves thisdiscrepancy between observations and theoretical predictions. We demonstrate that they are able to suppress the large-scale
spiral structure of self-gravitating protoplanetary discs.

First CH3 D detection in Class 0/I proto-brown dwarfs: constraints on CH4 abundances

B. Riaz, W. -F. Thi F We report the first detection in the JK = 10 - 00 rotational transition line of CH3 D towards three Class
0/I proto-brown dwarfs (proto-BDs) from IRAM 30 m observations. Assuming a rotational temperature of 25 K, the CH3 D
HII領域の進化を正しく捉えるために必要な半径の計算分解能はいくらだろうか？
適切に設定しないと,物理量を1桁過大/過小評価する恐れがある.
abundances(relative to H2 ) are in the range of (2.3–14.5) ⇥ 10 7 . The
CH4 abundances
derived from the CH3 D abundances
and assuming the DCO+ /HCO+ ratios are in the range of (0.05–4.8) ⇥10 5 . The gas-phase formation of CH3 D via CH2 D+
10https://arxiv.org/abs/2112.09013v1
is enhanced at high densities of 108 –10
cm 3 and our observations are likely probing the innermost dense and warm regions

23

How D-type H region expansion depends on numerical resolution¢
J. M. Pittard , M. M. Kupilas and C. J. Wareing

School of Physics and Astronomy, University of Leeds, Woodhouse Lane, Leeds LS2 9JT, UK

Accepted 2021 December 16. Received 2021 December 16; in original form 2021 November 25

ABSTRACT

We investigate the resolution dependence of H regions expanding past their Strömgren spheres. We find that their structur
size, and the radial momentum that they attain at a given time, is in good agreement with analytical expectations if the Ström
radius is resolved with 3A  0.3 'st . If this is not satisfied, the radial momentum may be over- or under-estimated by factors
10 or more. Our work has significance for the amount of radial momentum that a H region can impart to the ambient mein numerical simulations, and thus on the relative importance of ionizing feedback from massive stars.

Key words: hydrodynamics – methods: numerical – ISM: bubbles – H regions – ISM: kinematics and dynamics – gal
ISM23