sources or ⇠ 1.00 5 Gaussian sources.
nents toward the southeast and west from the SMM4B
We ofalsotwo
performed
self-calibration
for the continposition. Main
The peakSMM4
intensity, total flux density, and de2. The Distinct Evolutionary NatureClass
0 Protostars
in Serpens
uum data using tasks in CASA (clean, gaincal, andconvolved size of the SMM4B continuum emission are
Yusuke Aso, Hirano Naomi, Yuri Aikawa,
et al.
25 mJy beam 1 , 173 mJy, and 0.00 70 ⇥ 0.00 53 (P.A.=95 ),applycal). Only
the phase was calibrated first with thetime bin of 3 scans (⇠ 18s). Then, using the derived
respectively. The peak intensity corresponds to a brighttable, the amplitude and the phase were calibrated toness temperature of Tb = 2.0 K. The total flux density
Serpens MainのSMM4をALMAで観測
gether. The self-calibration improved the rms noise level
corresponds to a gas mass of 0.29 M , while the peakof the continuum
maps by a factor of ⇠ 2. The obtained18
intensity corresponds to a gas mass column density of（Cycle 3、分解能~0.55ʼʼ(240 au)＠1.3
mm, 12CO
J=2-1, SO JN=65-54, C O J=2-1）
calibration tables for the continuum data were also ap0.04 M beam 1 under the same assumptions as above.
plied to the line data. The noise level of the line maps
were measured in emission-free channels. The parameT (K)● 1.3 mm continuum emission mapters of our observations mentioned above and others are
summarized in Table 1.
b

2つのコンパクトソース（SMM4A, SMM4B）、SMM4B周辺の広がった構造
3. RESULTS
輝度温度3.1. 1.3 mm continuum

Figure 1 shows a map of the 1.3 mm continuum emisSMM4A： 18 Kと高い
sion in the SMM4 condensation. The emission has two
local peaks. We label the stronger and the weaker
SMM4B： 2 Kと低い
peaks as SMM4A and SMM4B, respectively, in thispaper. SMM4A shows a size of ⇠ 200 (860 AU) at
the 3 noise level, while SMM4B shows a ⇠ 500 (2100
見た目からAU) size at the same noise level. The peak positionsof SMM4A and SMM4B measured by Gaussian fitting
SMM4A： r~240 auにシャープなエッジを持つ、disk状構造の存在
were ↵(J2000) = 18h 29m 56.s 718, (J2000) = 1 130 15.00 58
SMM4B： コンパクトな成分 or
and半径56↵(J2000) =auの小さなdisk?
18h 29m 56.s 526, (J2000) = 1 130 11.00 50,
respectively. The fitting uses emission within the 3
contour enclosing each peak after primary beam correction, providing peak intensities and deconvolved sizes(FWHM), as well as the positions. Total flux densities● 12COof the sources were measured by integrating the flux in6
the regions enclosed by the 3 contours after primary
SMM4A： ファン状のblueshiftした単極アウロフロー
beam correction.
The emission around SMM4A shows a compact strucSMM4B： アウトフローは双極でcollimateしている
ture with extensions to the east and the south. Its
peak intensity, total flux density, and deconvolved
blueshiftとredshiftの軸は30ほどmisalignsize are 205 mJybeam 1 , 492 mJy, and 0.00 75 ⇥ 0.00 46(P.A.=145 ), respectively. The peak intensity corresponds to a brightness temperature of Tb = 18 K. The
dust temperature in Serpens Main was estimated by
Lee et al. (2014) to be ⇠ 20 K. Thus, the continuum
emission in SMM4A is thought to be optically thick.
A lower limit to the gas mass can be calculated fromthe total flux density to be 0.83 M by assuming optical thinness, a dust temperature Tdust = 20 K, opacity
coefficient (850 µm) = 0.035 cm2 g 1 (Andrews &

SMM4A

SMM4B

1000 auFigure 1. Continuum emission map of SMM4A and
SMM4B. Contour levels are 3, 6, 12, 24, . . . ⇥ , where 1
corresponds to 0.1 mJy beam 1 . The color map showsbrightness temperature in the unit of K. Yellow plus signs
and lines denote two peak positions and major axes derived
from 2D Gaussian fitting. Yellow circle denotes ALMA primary beam (FWHM⇠ 2700 ). A blue-filled ellipse at thebottom-left corner denotes the ALMA synthesized beam;
0.00 57 ⇥ 0.00 46, P.A. = 85 .
Aso et al.

3.2. Spectral Energy Distribution
Figure 2a and 2b show Spitzer 24 µm and Herschel
70 µm images of the SMM4 region. SMM4A and
SMM4B are not detected by Spitzer and only marginallywith Herschel where they are much fainter than a neighboring Class 0 protostar. Figure 2c shows the SED of
the overall submillimeter condensation SMM4 as definedby the JCMT and derived from Spizter IRAC (3.6, 4.5,
5.8, 8.0 µm), Spizter MIPS 24 µm, Herschel PACS
70 µm observations, ALMA 1.3 mm (this work), andthe literature: CSO SHARK-II 350 µm (Suresh et al.
2016), JCMT SCUBA 450 µm and 850 µm (Davis et al.
1999), and CARMA 3 mm (Lee et al. 2014). The upper
limits in the SED, which are set to be the flux densities

SO
SMM4B：アウトフローの端と、SMM4B付近のショック領域

12COのlobeに沿ったPV図：

線状の2つのペア

これらのペアが同じmomentを持っていると仮定

blueやred lobesの傾きは、ib ~36 とir ~70
3Dでのそれらのずれは、~40● SMM4Bアフトフローが曲がっている原因i) 0.1 pcスケールのアウトフローとの力学的相互作用ii) アフトフローと磁場（mGのオーダー）に起因する電流での、電磁相互作用iii) より小スケール構造（ゆがんだdisk?）←空間分解できていない● C18O

SMM4 in Serpens Main

SMM4A：

SMM4B：

7

連続放射に対する吸収放射として観測

SMM4B周辺：

落ち込み、回転するenvelope

・SMM4Bの連続波ピークでのC18Oの存在量：

典型的なISMよりも約50倍小さい

・~1500 auスケールでの存在量：より広いスケールでの観測値と矛盾しない● SMM4A、SMM4B、SMM11（Class 0）と進化フェーズを比較
SMM4B（collimateしたアウトフロー、コンパクトな連続波源、SO輝線でトレースされる質量降着）：
SMM4A（高い輝度温度、fan型アウトフロー、大きなdisk状構造）よりも若い進化段階と考えられる
SMM11：

放射温度、放射光度、内部光度がSMM4AやSMM4Bよりも小さい
C18Oの存在量：数十倍ほどSMM4Bよりも小さい

連続放射：

球状エンベロープ（diskやコンパクト成分なし）

SMM4Aが最も進化したフェーズにあり、SMM4B、SMM11と続く

SMM4Bよりも更に若いtions and the production of synthetic observations. In Section 3 we present
the results of the simulations and the syn5. Synthetic
CO18observations.
O observations
ofdiscussﬁbrousthetic C18
In Section 4, we
the sig-ﬁlaments: the problems of mapping from PPV to PPP
nificance of the results and compare to previous work andS. D. Clarke,
A. P. Whitworth, R. L. Spowage, et al.
observations. In Section 5, we summarise our conclusions.

● フィラメント形成と分裂は複合プロセス：2

もつれ相互接続しているサブ構造と、複雑な運動で示される

NUMERICAL SETUP

PPP空間での密度構造は、分裂と星形成を反映する
2.1 Simulations

一方、分子線観測はPPV空間での特徴を明らかにするのみ
The simulations presented in this paper1 have been per-formed using the moving-mesh code Arepo (Springel 2010).
The code uses self-gravitating hydrodynamics, with time・PPV空間からPPP空間へのマッピングは、視線方向での重なりで難しい
dependent coupled chemistry and thermodynamics. The
boundary conditions are periodic
for coherence）の同定基準
the hydrodynamics,
・PPV空間での特徴（i.e.
velocity
but not for self-gravity. Ten simulations are performed withdi↵erent random seeds (labelled Sim01 to Sim10).
そのような特徴が、PPP空間において物理的に連続的で確かなものかどうかはわからない
The computational domain is defined by Cartesian coordinates (x, y, z), with |x| < 3.0 pc, |y| < 3.0 pc and |z| <● Simulation
2.5 pc. The initial density field is cylindrically symmetric
about the z axis, so we also introduce a radius variable w =(x2 + y 2 )1/2 , and put⇢
15 M pc 3 (w/pc) 1 , w < 3.0 pc, |z| < 1.5 pc;⇢(w, z)=(1)0.015 M pc 3 ,elsewhere.
Here the low-density gas is simply a filler in the outer regionsof the computational domain, and plays no significant role
18O観測
4 S. D.
et al.
inClarke
the evolutionof the filament; it constitutes⇠ 0.01% of● シミュレートされたフィラメントのC
the total mass. The initial density field is set up and settledwith ⇠ 106 cells all having approximately the same mass.
The initial velocity field is given by⇢
0.75 r̂ km s 1 +vturb , w < 3.0 pc, |z| < 1.5 pc;v(w, z)=(2)
0 km s 1 ,elsewhere.
Without the turbulent component, vturb , this gives a cylindrically symmetric inflow of 70 M Myr 1 pc 1 towards thez axis. The dense gas initially at w ⇠ 3 pc takes ⇠ 4 Myr
to reach the z axis. Since the simulations are only run for⇠ 0.45 Myr, the low-density filler gas outside w ⇠ 3 pc does
not have time to influence the dynamics near the z axis
1

The preliminary results from these simulations werepreviously presented in the thesis of Seamus Clarke(http://orca.cf.ac.uk/102784/)
Figure 2. On the left, the integrated intensity map of the C18 O emission, with black dots showing the location of the five spectra
displayed on the right. Four of the five spectra show multiple velocity components (as shown in Section 4.1 and Fig. 5).

0.04 pc, and finally adding noise. For each voxel, the noise

As with the first moment map, only velocity channels with

視線方向において様々な速度成分を持ち、複雑なスペクトルを示す

実際の観測と似ている

速度成分の多くは ~0.4 km s-1以下の線幅
遷音速 limit ＠~10 K↑観測結果（sub-sonic or trans-sonic）と一致

● Fibre：

今回のsimulationで多く見られる（長さ~3pcのフィラメント中に、平均で22のFibre）

PPV空間でvelocity coherent構造として定義 by Hacar et al. (2013)
Figure 7. A 3D plot showing the velocity centroids of the velocity components in PPV space, colour coded to show the individual groups
identified using the friends-of-friends algorithm. The structures are generally filamentary and resemble the fibres in Hacar et al. (2013)
それらFibreは、高密度でのCO
freezeoutが含まれていようがいまいが、強く影響を受けない
8 S. D. Clarke et al.

Figure 7. A 3D plot showing the velocity centroids of the velocity components in PPV space, colour coded to show the individual groups
identified using the friends-of-friends algorithm. The structures are generally filamentary and resemble the fibres in Hacar et al. (2013)

Figure 8. The lefthand frames display the same five spectra presented in Fig. 2, and the righthand frames display the density profiles along
the corresponding lines-of-sight. The coloured bars identify the ranges contributing to the di↵erent velocity components (vc ± 1.15 c ).

● フィラメント中の速度coherentなFibreの同定

c 2002 RAS, MNRAS 000, 1–18

Fibreは別々の構造であり、フィラメントにおいて building blockとなる
The problems of mapping from PPV to PPP
個々のFibreやFibreのグループを調べることで、フィラメントの内部構造が推測できる

しかしながら、

PPV空間からPPP空間へのマッピングは視線方向の重なりで難しい

Fibreの約50%が物理的に離れているガスからのコンタミあり
PPV空間での特徴が、PPP空間で繋がっている50%なのかを知ることは、
Figure 8. The lefthand frames display the same five spectra presented in Fig. 2, and the righthand frames display the density profiles along
the corresponding lines-of-sight. The coloured bars identify the ranges contributing to the di↵erent velocity components (vc ± 1.15 c ).

観測者は不可能c 2002 RAS, MNRAS 000, 1–18

Figure 9. A 3D plot showing the fibres identified in Fig. 7 mapped into PPP space, using the same colour code.

9● PPVで同定されるFibreは、PPPで同定されるsubフィラメントには関係しないが、

the three ‘spectra’ displayed on the right, showing multiple velocity components, separated by ⇠ 1 km s .
二次元に投影されたFibreとsubフィラメントの形は似ている
The problems of mapping from PPV to PPP 11

Figure 12. The lefthand frame displays the column density of the sub-filament from Fig. 11, and the black dots show the positions of1(2013). NH has also been used by Williams et al. (2018) to
多くの視線方向において、

how these features relate to fibres as defined by Hacar et al.
3

study the more massive filaments (aka spokes) in the huband-spoke system SDC13. However, they find no evidence
for fibres; each of the four filaments (spokes) shows only asingle velocity component.
It will be important to understand better how fragmenting filaments appear when observed with nitrogen bearing
molecules. These molecules trace di↵erent gas from C18 O,
and therefore mapping from PPV space to PPP space may
be more straightforward. Synthetic N2 H+ and NH3 observations are outside the scope of this paper, but will be thefocus of future work.

subフィラメントも重なっており、同定は難しい？

5
Figure 13. A map of the number of di↵erent sub-filaments alongeach line-of-sight. Over 30% of lines-of-sight intercept more than
one sub-filament.

14

S. D. Clarke et al.

actually be classified as sub-filaments. N2 H+ should be abetter tracer of sub-filaments, since N2 H+ emission is lessinfluenced by shocks than C18 O, and the volume-filling factor of N2 H+ -bright gas is much lower than C18 O-bright gas,leading to less line-of-sight confusion.
Ammonia (NH3 ) is also a dense gas tracer, and isthought to trace similar gas to N2 H+ (Johnstone et al. 2010;
Hacar, Tafalla & Alves 2017). NH3 has been used to detect
elongated features in the TMC-1 cloud in Taurus, using the
NbClust algorithm (Fehér et al. 2016), but it is unclear

CONCLUSIONSFilament formation and fragmentation is a complex process, characterised by tangled, interconnected sub-structuresand complicated kinematics, on both large and small scales.
While it is the real density structures in PPP space that
ultimately reflect the process of fragmentation and starformation, molecular-line observations only reveal featuresin PPV space. Unfortunately, the mapping from PPV space
to PPP space is compromised by confusion along the lineof-sight, and the identification criteria for features in PPV
space (i.e. velocity coherence) do not guarantee that suchfeatures are physically continuous and distinct in PPP space.
Synthetic C18 O observations of simulated filaments
show complex spectra, with multiple velocity components on
many lines-of-sight, similar to real observations of filaments

c 2002 RAS, MNRAS 000, 1–18

Figure 10. A 3D plot showing the sub-filaments found using DisPerSE. In the top panel, the di↵erent sub-filaments are colour coded.
In the bottom panel the colour shows the line-of-sight velocity from the simulation at that position.
c 2002 RAS, MNRAS 000, 1–18

Figure 14. J moments of the sub-filaments (lefthand plot) and fibres (righthand plot) from Sim02, confirming that at all levels they areelongated. The square represents the trunk of the dendrogram, circles the branches, and triangles the leaves.

Jプロット（Jaﬀa et al. 2018）を用いると、Fibreは平均的にはsubフィラメントよりも、やや狭く、時折より曲がっている6. Water and interstellar complex organics associated with the HH 212 protostellar disc
C. Codella, E. Bianchi, B. Tabone, et al.

Orion BのHH 212 (Class 0)に対して、HDOとCH3CHOで観測(Cycle 1 & Cycle 4 ALMA Band 7)● 14のCH3CHO輝線と1つのHDO輝線を検出
Codella et al.: Water and iCOMs around HH 212 mm

放射領域は垂直方向に~0.ʼʼ18 (73au)広がっている
全てのプロファイルのピーク：系速度の付近で、幅5-7 kms-1

Codella et al.: Water and iCOMs around H● 赤道面に沿ったCH3CHOとHCOのPV図
Codella et al.: Water and iCOMs around HH 212 mm
原始星から離れるにつれて速度↑

化学的に豊富なwarm gasのedge-onリングからの放射の可能性が高い

半径：~0ʼʼ.15 (60 au)で、以下の結果とよく一致(i) 別のiCOMs（NH2CHOとか）で測られた以前の結果(ii) 連続光で観測された光学的に厚いdiskの半径(iii) HCO＋の落下運動から推測される遠心力バリアの場所
今回の観測は、化学的に豊富なガスを見ている
そこで、落ち込むenvelopeが回転円盤に当たり、低速度のショックを作っている？

Fig. 7. Position-velocity cut of HDO(33,1 –42,2 ) (colour scale,magenta contours) along (left panels) and perpendicular (rightpanels) to the equatorial plane (PA = 112 , see Fig. 1) overlaid with the CH3 CHO(180,18 –170,17 )-E (upper panels) andCH3 CHO(180,18 –170,17 )-A (lower panels), drawn as white contours. The first contours and steps correspond to 3 (3.1 K kms 1 ). Dashed lines mark the position of the HH 212 mm protostar and the cloud VLSR (+1.7 km s 1 ; Lee et al. 2014). The error
bars are drawn in the bottom right corners.

Fig.（低速度ショックによる化学の研究には、正確なモデリングが必要）
7. Position-velocity cut of HDO(33,1 –42,2 ) (colour scale,magenta contours) along (left panels) and perpendicular (rightpanels) to the equatorial plane (PA = 112 , see Fig. 1) overlaid with the CH3 CHO(180,18 –170,17 )-E (upper panels) andCH3 CHO(180,18 –170,17 )-A (lower panels), drawn as white contours. The first contours and steps correspond to 3 (3.1 K km
● 円盤面の上下40-50
au以下で、低速度の放射（系速度から
1 km s-1）がCH3CHOとHDOで見られるs 1 ). Dashed lines markthe position of the HH 212 mm protostar and the cloud VLSR (+1.7 km s 1 ; Lee et al. 2014). The error
より進化した原始星L1527で最近発見された（Sakai
et al. 2017）ような、遠心力バリアの垂直構造を示唆
bars are drawn in the bottom right corners.

Fig. 8. Cartoon (not to scale) illustrating the scenario expectedin the inner 60 au region around the protostar for low-velocity
emission ( 1 km s 1 with respect to vsys ) in case of outflowing(left) or infalling (right) chemically enriched gas (see text).

観測による空間分布
光学的に厚い円盤面の上下の、.

流れ出し、広がって、回転する2つのリングの証拠？

Fig. 8. Cartoon (not to scale) illustrating the scenario expectedin the inner 60 au region around the protostar for low-velocity
emission ( 1 km s 1 with respect to vsys ) in case of outflowing(left) or infalling (right) chemically enriched gas (see text).
.

更なるALMA観測が必要

1

3

Sternwarte, University of Hamburg, Gojenbergsweg 112, 21029, Hamburg, Germany; 6 School of Physics, Astronomy& Mathematics, University of Hertfordshire, College Lane, Hatfield, Hertfordshire, AL10 9AB, UK; 7 Department ofDiﬀuseX-ray emission in the Cygnus OB2 association
Physics and Astronomy, University College London, Gower Street, London WC1E 6BT, UK; 8 I. Physik. Institut,
1
2
4
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Albacete of
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Flaccomio9 3Armagh, N.J. Wright, V. and
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Odiﬀerent
fractional
abundancein
SMM4B
is ∼. 50times
thanandthatof the angles
E-mailcontact:
albacete.facundo
at conicet.gov.ar◦ stellar◦ is more◦bythanband
energyemission
likelyarisesfrom
O-typewinds
thermalized
wind-windcollisions
in
the
most
populatedinterstellar
medium.
These
resultssuggestthat
SMM4A
evolvedSMM4B.
Our
studiesin
Serpens
Main shockedin the 3D space are estimated at ib ∼ 36 , ir ∼ 70 , and α ∼ 40 , respectively. The SO emission traces
We demonstratepresent
a oflarge-scale
studyof
diﬀuseX-ray
emissioninthenearbymassivestellarassociation
CygnusOB2
aspart
regionstheassociation,
while
the
soft
band
emissionprobablyarisesfrom
lessenergetic
termination
shocksagainst18
continuum
line observations
at millimeter
wavelengths
us to diﬀerentiate
evolutionary
regions, such as thatcavitywalls of andoutflows
and the vicinityof SMM4B.
The C allow
O emission
mainly traces
2 an infalling andof theChandraCygnusOB2
LegacyProgram.
We used40 Soft
ChandraX-rayACIS-I
observations
covering∼1.0 deg. intensethesurrounding
Interstellar-Medium.
Super-soft
anddiﬀuseemission
appears
more widelydispersedand18phasesofprotostars
withintheClass0phase.
rotating
envelope
aroundSMM4B.
The
C in
O our
fractional
abundancein SMM4B
is emission,∼ 50 times
smallerthan that of theAfterthanremoving
7924
point-likesources
detectedsurvey,background-corrected
X-ray
the
adaptivethe medium band emission. The diﬀuse X-ray emission is generally spatially coincident with low-extinction
AcceptedbyThe
AstrophysicalJournalinterstellar
medium.
Thesediﬀuse
resultssuggestthatDiﬀuse
SMM4A
is morethan
SMM4B.
studiesin Serpens Mainsmoothinglarge-scale
emission.
emission
was evolved
detectedin themassive
sub-bandsSoft
regionsreveals
that weattributetothe X-rayubiquitous
influenceof powerfulstellarwinds fromstarsOurand[0.5
their: 1.2]
interaction
demonstratethat
continuumandline
observationsatmillimeter
wavelengths
allow
us
to
diﬀerentiate
evolutionary
andhttps://arxiv.org/pdf/1806.10743
Mediumand marginally inDiﬀuse
the Hard[2.5emission: 7.0] keVband. From X-ray
analysis of stacked
with the[1.2local: 2.5],
Interstellar-Medium.
X-ray
is volume-filling,ratherspectral
than edge-brightened,
oppositely
diﬀ
34
−1
spectrawecomputea total[0.5–7.0
diﬀuseX-ray
luminosityof Lx evidence≈4.2×10erg s haloes, characterized
withevolved
plasmamassive
phasesprotostars
withinthekeV]Class
0 phase.
to of
other
star-forming
regions.
We
revealthefirstobservationalof X-rayaround sometemperaturestars. components at kT≈0.11, 0.40 and 1.18 keV, respectively. The Hi absorption column density corresponding
Accepted
byofTheAstrophysicalJournal22
Eﬀect
stochastic
grain
heatingchemistry
to thesetemperatures
has a distribution
consistent on
withcold
NH = dense
0.43, 0.80clouds
and 1.39×10
cm−2 . The extended medium
Accepted
by
ApJS
1
2,3
band
energy emission
likelyarises Changfrom O-type
stellar winds
by wind-wind collisions in the most populated
https://arxiv.org/pdf/1806.10743
Long-Fei
Chen1,2, Qiang, Hong-Wei
Xithermalized
http://arxiv.org/pdf/1806.01231
regionsoftheassociation,
while
the
soft
band
emissionprobablyarisesfromless energetic termination shocks against
1
2
Xinjiang Astronomical
Observatory,
ChineseSciences,
150 Science
1-Street,
Urumqithe surrounding
Interstellar-Medium.
Super-softand Academy
Soft diﬀuseofemission
appears
more widelydispersed
and830011,
intenseChina;
3of Chinese
AcademyTheof Sciences,
Beijing
100049,China; spatially
Nationalcoincident
Astronomical
thanUniversity
the ofmediumband emission.
diﬀuse X-ray
emission
isdensegenerally
with Observatories,
low-extinction ChineseEﬀect
stochastic
grain
heatingon
coldClassclouds chemistry
The
Distinct
Evolutionary
Natureoftwo
0Protostars
inSerpens
SMM4
Academyof
Sciences,
Beijing
100101,
China
regions that we attribute to the ubiquitous influence of powerful stellar winds from massive stars and theirMain
interaction
1,2
1
2,3
1
1
2
3
1,4
Long-Fei
Chen,HiranoQiangNaomi, Hong-Wei
withE-mailthe local
Interstellar-Medium.
DiﬀuseX-ray
emissionis volume-filling,rather thanedge-brightened,
oppositely
YusukeAso,chenlongf, YuriAikawa, Xi
Masahiro
N. Machida, Shigehisa
Takakuwa, Hsi-Weicontact:
atChang
xao.ac.cn
5
6 first observational evidence of X-ray haloes around some evolved massivetootherstar-forming
regions.
We
revealthe
Yen
andJonathanP.
Williams
1
2
Xinjiang
Astronomical
Observatory,of Sciences,
150 Science
1-Street,clouds.
Urumqi
830011,
The temperaturesof dustgrains play Chinese
importantAcademy
roles in thechemical evolutionof molecular
UnlikelargeChina;
stars.
1
2
3
Academia
Sinica Instituteof of
Astronomy
andAstrophysics/P.O.
Box 23-141,
Taipei106, Taiwan;
Departmentof Chinese
grains,thetemperaturefluctuationsof smallgrainsinducedbyChina;
photonsmaybesignificant.
Therefore,
if the grain
Universityof Chinese
AcademySciences,
Beijing
100049,National
Astronomical
Observatories,
Acceptedby
ApJS
Astronomy,
Graduate
Schoolof
Science,
The
UniversityofTokyo,
7-3-1
Hongo,
Bunkyo-ku,
Tokyo
113-0033,
Japan;
size distribution
is included
astrochemical
Academyof Sciences,
Beijing in
100101,China models, the temperatures of small dust grains may not be assumed 4to3
DepartmentWeof simulate
Earth and
Planetary
Sciences,
Facultyof Sciences
University,
Fukuoka
Japan;
http://arxiv.org/pdf/1806.01231
be constant.
a fullgas-grain
reaction
networkwith a Kyushu
set of dust
grain radii
using812-8581,
the classicalMRN
E-mailcontact:
chenlongf
atxao.ac.cn
DepartmentofPhysics
andAstronomy,
Graduate
Schoolof
ScienceandEngineering,Kagoshima
University,
grain size distribution and include the temperature fluctuations of small dust grains. Monte Carlo method1-21-35
is used5
Kagoshima,890-0065,
Japan;Southern
Observatory,Karl-Schwarzschild-Str.
2,
toKorimoto,simulate thereal-time
dust
grain’stemperaturefluctuations
is causedby the ofexternal
low energy
photonsTheof dustKagoshima
grainsplay
importantrolesEuropean
in Protostars
thewhichchemicalmolecular
clouds.
Unlikelarge
6NatureThetemperatures
Distinct
Evolutionary
of
two
Class
0
inevolution
Serpens
Main
SMM4
D-85748
Garching,
Germany;
Institutefor
Astronomy,
UniversityofHawaiiat
Manoa,
Honolulu,
Hawaii,USA
andtheinternal
cosmicray
inducedsecondaryphotons.
The
increaseof
dust
grainsradii
asice
mantles
accumulate
grains, the temperaturefluctuationsof smallmay be significant.
Therefore, if the grain
1
1
2 grains induced by photons
3
1,4
YusukeAsocontact:, Hirano
Naomi, Yuri, Masahiro
N. thatMachidaShigehisa
Takakuwa, Hsi-Weiongrain
surfacesis alsoincludedin Aikawa
our models.
We foundsurface, CO
inmodelswithnotgrain
E-mailyaso
at asiaa.sinica.edu.tw
2 abundances
size
distribution
isincludedinastrochemical
models,thetemperatures
of
small
dust
grainsmay
be size
assumed to5
6
Yendistribution
and Jonathan
P. Williams
andtemperaturefluctuations
are
more
than
one
order
of
magnitudelarger
than
those
with
singlegrain
We have observed
the submillimeter
continuum
condensation
Main grainusing theAtacamaMilbe
We simulatea full gas-grain
reaction
networkSMM4
with ina Serpens
set of dust
radii
using Largethe classicalMRN
1 constant.
size. Small
amountsof terrestrial
complexorganic moleculesBox(COMs)
canalso 106,
be formed
on2 smallgrains due
Academia
SinicaInstituteof Astronomy
and Astrophysics/P.O.
23-141,
TaipeiTaiwan;Departmentof to thegrain
size distribution
andofinclude
thetemperaturefluctuations
ofcosmic
small
dust
grains.
MontephotonsCarlomethod is used
Astronomy,
Graduate
Science,
Thelow
Universityof Tokyo,7-3-1 Hongo,
Bunkyo-ku,
Tokyo
113-0033,
Japan;overheattemperature
spikesSchool
inducedby externalenergy photons.
However,ray
inducedsecondary
3 simulate the real-time dust grain’s temperature fluctuations which is caused by the external low4 energy photons
toDepartment
of so
Earth
Planetary
Sciences,of Sciences
KyushuFukuoka
Japan; of surface
10 formed
small grainsthat andsurface
CO sublime
andFacultyless radicals
areonUniversity,
grains surfaces,thus812-8581,
the production
andtheinternal
cosmicray
inducedsecondaryphotons.
The
increaseof
dust
grainsradii
asice
mantles
accumulate
DepartmentofPhysics
andAstronomy,
Graduate
Schoolof
ScienceandEngineering,Kagoshima
University,
1-21-35
CO2 and COMs decreases by about one order of magnitude. The overheating of small grains can beoﬀset
by grain
5
Korimoto,
Kagoshima,
Kagoshima890-0065,
Japan;
EuropeanSouthern
Observatory,Karl-Schwarzschild-Str.
2,
on grainis alsoincludedin ourCO
models.
We foundthat
surface
CO2 abundances in models with grain size
growthsurfaces
so that theformationof surface
becomesmore
eﬃcient.
2 and COMs
D-85748 Garching,
Germany; 6 Institutefor Astronomy,
Universityof HawaiiatManoa,
Honolulu,
Hawaii,
distribution
andtemperaturefluctuations
are
more
than
one
order
of
magnitudelargerthanUSA
those with single grain
Accepted by MNRAS

3 2

2

1

8

University of Hawaii at Manoa, Institute for Astronomy, 640 North Aohoku Place, Hilo, HI 96720, USA; 2 Staﬀ Astronomer at the Infrared Telescope Facility, which is operated by the University of Hawaii under contract NNH14CK55B
A Near-IR
Spectroscopic
Surveyof FU Orionis Objects
with the National
Aeronautics and Space
Administration
1,2
MichaelConnelley
and Bo Reipurth1
E-mailS.
contact:
msc at ifa.hawaii.edu

We have conducted
homogenous
spectroscopic
survey of640
33 objects
varying
degreesof similarity
to USA; 2 Staﬀ AsUniversityof Hawaiia at
Manoa, near-IR
Institutefor Astronomy,
North with
AohokuPlace,
Hilo,
HI 96720,
FU
Orionis. Common
featuresthat are characteristic
the threeclassical
FUors FUtotal
Ori, atomic
V1057 Cyg,
ice formation
followed spectroscopic
by non-distructive
photodesorption
from theofdust
grains.
The two-sided
mass
tronomerat theInfrared
Telescope
Facility,
whichis operated
bythatthe
University
ofthe
Hawaiiundercontract
NNH14CK55B−6 absorption,
−1
and
V1515
Cyg
are:
strongCOabsorption,
weak
metal
strongwater
bands,
low
gravity,strongblue
shiftedflux
estimated
from
the
[OI]
jet
sums
to
1.65
×10
M
yr
,
a
value
is
very
close
to
mass
flux
previously⊙
ice formation followed by non-distructive photodesorption
from the dust grains. The two-sided total atomic mass
with He
theI absorption,
National
andAdministration(if
emissioncriteria,
33
objects
for theAeronautics
SiOfew
andany)the
H2 Space
outflow.
WeBasedconclude
theof classify
the coolingfromCO, OHand [OI]
is−6on these−1 bulk weflux estimatedestimatedfromandthejet[OI]jetsums
tolines.
1.65
×10
Mthat
, a value
thattheis very
closeastoeither
the bona
mass
flux previously
⊙ yr
fide
FUors with(eruptionobserved),
FUor-like
objects(eruptionnotobserved),
or peculiar
objectswith
someFUor-like
associatedgas
excitedinoutflow
shocks,withtheblue-shifted(SE)
outflow
showing
evidenceofashock-induced
E-mailcontact:
msc
at
ifa.hawaii.edu
estimatedtheandSiO
the HatlasWe
conclude
the objects,
bulk
the
from
2 outflow.
characteristics,
present
aOH
spectralof 14linesbona-fide
FUors,
10thatFUor-likeand9 cooling
peculiar objects.
All OH and [OI] is
UV fieldfor
responsible
forjettheandemission.
Wateraroundthe protostar
reveala veryoflow
ortho-to-pararatio CO,that
associatedwithwegas
excitedin formation
outflow
shocks,withblue-shifted(SE)
outflow
showing
evidenceofobjects
thatclassify
as FUors
or FUor-likeverythesimilarnear-IRWe
useFinally
this
spectralsimilarity
to a shock-induced
can beconductedinterpreted
inoffrom ahave
primordialgas
reservoir
theenvelope.
comparisonsof theWe
havea terms
homogenous
near-IR
spectroscopic
surveyinspectra.
of33
objectswithvarying
degreesof similarity todeterminetheextinctiontoeachsource,andcorrelatetheextinction
to
the
depth
of
the
3
µm
ice
band.
All
bona
fide
[OI]
jet
mass-flux
to
the
mass
fluxesderived
for
SiO
and
H
renders
HH
211
the
first
embeddedsystem
where
an
UV
field
responsible
for
the
OH
emission.
Water
lines
aroundtheprotostar
revealavery
lowortho-to-pararatio that
FU Orionis. Common spectroscopic features that are 2characteristic of the three classical FUors FU Ori, V1057
Cyg,
FUors
still
today
maintainthespectrumofaFUor,
despitetheeruption
occurring
up
to
80
years
ago.
Most
FUors
atomicjet is demonstrably
shown
to possess fromenougha momentum
to gasdrivereservoir
the observed
molecular
jets andlarge scalecanbeinterpreted
in
terms
of
formation
primordial
intheenvelope.
Finally
comparisonsoftheand V1515
Cyg are:strongCOabsorption,
weak
metal
absorption,strong waterbands,
lowthegravity,andFUor-like
objects
occupya uniquespace ona plotof Na+Ca
vs. CO equivalent
widths,whereaspeculiarstrong blue shifted
outflows.
[OI]I objects
jetmass-flux
to themass
fluxesderivedfor SiOandrenders
HH 211wethe
first theembeddedsystemwhere bonaanHeabsorption,
few mostly(if any)
emission
Based
onH2athesecriteria,classify
objects
as eithertend to andbe foundelsewhere.
Sincelines.
most FUors
show
reflection
nebula,wealso present
an33atlasofAcceptedby
Astronomy&
Astrophysics
atomicjet isdemonstrably
shown
to possessenough(eruption
momentumdrive
observed
molecular
jets and
large
scale
K-bandimagesof eachtarget.
We foundthat theobjects
near-IR
spectraof FUors
andyoungthebrown
dwarfscanbe extremely
fide
FUors
(eruptionobserved),
FUor-likenotto
observed),orpeculiar
objectswith
someFUor-like
https://arxiv.org/pdf/1806.00311
outflows.
similar, a distinguishingfeaturebeing the Paschen
in theFUors,
spectra of
AlthoughV1647 Ori,
6a,characteristics,
and present
a spectral
atlas ofβ absorption
14 bona-fide
10FUors.
FUor-like
objects,andAR
9 peculiar
objects. All
and V346 Normae had been previously classified as candidate FUors, we classify them as peculiar objects with some
objectsthat
weclassifyFUorsor now
FUor-likehave very
similarnear-IR
this spectral similarity to
Acceptedby properties
Astronomy&theirAstrophysics
FUor-likesinceasspectradiﬀer significantly
frombona fide
FUors. spectra.
We confirmWe
two usenew FUor-like
SpiralArms
inDisks:
Planets
orGravitational
Instability?
determineeach source,
and correlatethenear-IR
extinction
to the depth of the 3 µm ice band. All bona fide10
objects thethat extinction
were initiallyto
identified
as candidates
based on theirmorphology.
https://arxiv.org/pdf/1806.00311
1
2
3,2
Ruobing
Dongmaintain, Joan R. theNajitaand SeanFUorsstill today
spectrumof aBrittain
FUor, despite the eruption occurring up to 80 years ago. Most FUors
Acceptedby Astron.
J.
1
Steward Observatory,
Universityof Arizona,933on
N aCherry
Tucson, vs.
AZ 85721,
USA; 2 National
Opticaland FUor-likeobjects occupy
a uniquespaceplot Ave,of Na+Ca
CO equivalent
widths,whereas the peculiar
http://arxiv.org/pdf/1806.08880
3
Astronomical
Observatory,
950
North
CherryAvenue,Tucson,AZ
85719,
USA;
DepartmentofPhysics&
Astronomy,
Spiraltend
Arms
Disks:
Planets
or Gravitational
objects
to beinfoundmostlyelsewhere.
Since most FUors Instability?
show a reflection nebula, we also present an atlas of
118 Kinard Laboratory, Clemson University, Clemson, SC 29634, USA
K-bandimagesof1 ,eachtarget.
We foundthat
the Brittainnear-IR spectraof FUors and young brown dwarfs can be extremely
2
3,2
Ruobing
Dong
Joan
R.
NajitaSean
Herschel
spectral-line
mappingandof the
HH211 protostellar system
E-mailcontact:
rbdongat
gmail.com
9similar,a distinguishingfeature being
the Paschen β 1absorption in the spectra of FUors. Although
V1647 Ori, AR 6a,12
1
2
Odysseas
Dionatos
,seen
Tom
Ray
and
ManuelGüdelSteward
Observatory,
UniversityofArizona,933
N
CherryAve,
Tucson,AZ
85721,
USA;
OpticalSpiralarm
structuresinscatteredlightobservations
ofprotoplanetary
disks
can
potentiallyserve
assignposts
and V346
Normae had been previously classified as candidate FUors, we classify
them as peculiar National
objects with
some
3
1
of
planetarycompanions.
They
can
also
lend
uniqueinsights
intodisk
masses,which
arecriticalinsettingthemass
Astronomical
Observatory,
950
North
CherryAvenue,Tucson,AZ
85719,
USA;
DepartmentofPhysics&
Astronomy,
Institute for
Astronomy (IfA),
Universityof Vienna,Türkenschanzstrasse
17, A-1180
Vienna;FUor-like
properties
since theirspectranow
diﬀer significantly
from bonafide FUors.
We
confirm2
budgetforLaboratory,
planetformationbut
arediﬃcult
determine
AStudies,
surprisingly
high fractionof disks
that2,
havebeentwo new FUor-like
Astronomy& Astrophysics
Section,Dublin to
Institutefor directly.
Advanced
31 Fitzwilliam
Place,
DublinIreland118
KinardClemson
University,
Clemson,SC
29634,
USA
objects
that were
initiallylight
identified
asarmscandidates
based
onastheirnear-IR
morphology.
well-studiedin scattered
have spiralof some kind
(8/29),
do a highfraction(6/11) of well-studied Herbig
E-mail contact: odysseas.dionatos at univie.ac.atintermediate
mass
stars at(i.e.,
Herbig stars > 1.5M⊙ ). Here we explore the origin of spiral arms in Herbig systems by
E-mailcontact:
rbdonggmail.com
Accepted by Astron. J.
1

10Midand their
far-infraredobservationsof theenvironment
embeddedrates.
protostars
reveala plethora
high excitation
studying
occurrence
rates, disk
properties,
and aroundstellar accretion
We findthat
two-armofspirals
are more

9

Spiralarm structures
seen inlines.
scatteredlightobservationsof areprotoplanetary
disks
can
serve as signposts
molecular
atomicemission
A intermediate
numberof diﬀerent
mechanisms
fordirectly
the originof theselinesplanet
havepotentiallybeen
proposed,commoninand
disks
surrounding
Herbigmass stars
than
imagedgiant
companions
to
http://arxiv.org/pdf/1806.08880
including
protostellar
jetsareandradiation
the embedded
protostarinteractingwithimmediateof planetarycompanions.
can
also
lend
uniqueinsights
disk
masses,whichsuggests
areitscriticalin setting the mass
mature A shocks
and B inducedstars. IfbyThey
two-arm
spirals
producedbyby
such
giantintoplanets,
thisdiscrepancy
that giant
surroundings.
planets
muchformation
fainter than but
predicted
by hot start
In addition,
the A
high
stellar accretion
rates
of Herbig
budgetfor areplanetare diﬃcult
to models.
determine
directly.
surprisinglyhighfraction
ofstars,
disks that have beenInthis paperover
we employextended
spectral-line
maps thatsuggest
spatially
resolveregionsare
where
diverseexcitation
processes
ifsustainedareasonablefractionof
theirlifetimes,
that
disk
massesmuchlargerthaninferredfromwell-studied inscattered light havespiral arms
somekind (8/29),
as do a high fraction(6/11) of well-studied Herbig
Herschel
spectral-line
mapping
of of
the
HH211
protostellar
systemappearto dominate.
Studying themorphology
andexcitationof themostimportantmolecular
and atomic
coolants,
their submillimeter
continuum
emission.Asa result,
gravitational
instability
is a possible
explanation
for multi-arm
intermediate
mass
stars
(i.e.,
Herbig
stars
>
1.5M
).
Here
we
exploretheoriginofspiralarms
in Herbig systems by
⊙
1
2
1
we
aim
to
constrainthephysicalconditions
aroundtheembedded
protostellar
system
HH
211-mm.
spirals. Future
observations
canRaylend insights
the issues
raised here.
Odysseas
Dionatos, Tom
and into
ManuelGüdelstudying
their occurrence
rates,
properties,
and emission
stellar accretion
We(CO,
findH2that
Spectro-imaging
observations
with disk
Herschel/PACS
providefrom major rates.
molecular
O andtwo-armOH) and spirals are more
Accepted by ApJ
1atomicincoolants(e.g.
[OI]).(IfA),
Emissionline maps
revealthe morphology
the observed
emissionsand allow
associations
Institutefor
Astronomy
Universityof Vienna,Türkenschanzstrasse
17, A-1180
Vienna;commondisks
surrounding
Herbigintermediate
mass
starsof thanare directly
imagedgiant
planet companions tohttps://arxiv.org/pdf/1806.05183
2
betweenthediﬀerent
species.
Comparisons
are
also
made
with
mid-infraredline-maps
fromSpitzerandsub-mmAstronomy& Astrophysics
Section,spirals
Dublinforby
Advanced
Studies,
31 thisFitzwilliam
Place,
Dublinthat
2, Ireland
matureA and
B stars. If two-arm
areInstituteproducedsuch giant
planets,
discrepancy
suggests
giant
interferometers. The excitation conditions of the detected molecular species along with the ortho-to-para ratio of
planetsaremuchodysseas.dionatos
fainterthan predictedby hot startmodels. In addition, the high stellar accretion rates of Herbig stars,
E-mailcontact:
at diagrams.
univie.ac.atwater
are assessed
through Boltzmann
Further investigations focus on constraining the CO/H2 ratio in
Radialvelocity
surveyofspatially
resolved
young,
low-massbinariesoverreasonable
ofastheir
lifetimes,suggestthat
diskmassesmuchlargerthan inferred from
11if sustained
shocks andthe amassflux of thefraction
atomic jet
tracedby [OI]. We
find thatmolecularlines areareexitedmainlyat the9Mid- and far-infrared observations of the environment around embedded protostars reveal a plethora of high excitation
molecularspectral-line
and atomic emission
lines. A numberof diﬀerent
mechanisms
for the originof these lines have been proposed,
Herschel
mappingof the
HH211
protostellar
systemincluding shocks inducedbyprotostellar
jets
andradiationbytheembedded
protostarinteracting with its immediate
Odysseas
Dionatos1 , Tom Ray2 and Manuel Güdel1
surroundings.
1
In thisforpaper
we employextended
spectral-line
mapsTürkenschanzstrassethat spatially resolve regions
whereVienna;
diverse excitation processes
Institute
Astronomy(IfA),
Universityof Vienna,
17, A-1180
2

Astronomy & Astrophysics Section, Dublin Institute for Advanced Studies, 31 Fitzwilliam Place, Dublin 2, IrelandE-mail contact: odysseas.dionatos at univie.ac.atMid- and far-infrared observations of the environment around embedded protostars reveal a plethora of high excitation
molecular and atomic emission lines. A number of diﬀerent mechanisms for the origin of these lines have been proposed,
including shocks induced by protostellar jets and radiation by the embedded protostar interacting with its immediatesurroundings.
In this paper we employ extended spectral-line maps that spatially resolve regions where diverse excitation processes
appear to dominate. Studying the morphology and excitation of the most important molecular and atomic coolants,
we aim to constrain the physical conditions around the embedded protostellar system HH 211-mm.
Spectro-imaging observations with Herschel/PACS provide emission from major molecular (CO, H2 O and OH) andatomic coolants (e.g. [OI]). Emission line maps reveal the morphology of the observed emissions and allow associations
between the diﬀerent species. Comparisons are also made with mid-infrared line-maps from Spitzer and sub-mm
interferometers. The excitation conditions of the detected molecular species along with the ortho-to-para ratio ofwater are assessed through Boltzmann diagrams. Further investigations focus on constraining the CO/H2 ratio inshocks and the mass flux of the atomic jet as traced by [OI]. We find that molecular lines are exited mainly at theterminal bowshocks of the outflow and around the position of the protostar. All lines show maxima at the SE bowshockwith the exception of water emission that peaks around the central source. Excitation analysis in all positions showsthat CO and H2 O are mainly thermally excited at Tex ∼ 350 K and 90 K respectively, with the CO showing a second
temperature component at 750 K towards the SE peak. Excitation analysis breaks down in the case of OH at theblue-shifted bowshock, indicating that the molecule is non-thermally excited. Comparisons between the CO and H2column densities suggest that the X[CO] value in shocks can be up to an order of magnitude lower than the canonicalvalue of 10−4 . The water ortho-to-para ratio around the protostar is only 0.65, indicating low-temperature water

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