星形成ゼミ
担当：SFN#330 (15-21)
2020/07/17
竹村英晃（総研大D1）

15. Uncovering distinct environments in an extended physical system around
the W33 complex
16. Investigating the physical conditions in extended system hosting mid-infrared
bubble N14
17. Feedback of molecular outﬂows from protostars in NGC 1333, revealed by
Herschel and Spitzer spectro-imaging observations
18. Strong Hα emission and signs of accretion in a circumbinary planetary
mass companion from MUSE
19. A Survey for New Stars and Brown Dwarfs in the Ophiuchus Star-forming
Complex
20. Seeds of Life in Space (SOLIS). IX. Chemical segregation of SO2 and SO toward
the low-mass protostellar shocked region of L1157
21. The chemical structure of young high-mass star-forming clumps: (I)
Deuteration

15

http://arxiv.org/pdf/2005.01902
https://arxiv.org/pdf/2005.13871.pdf

Uncovering distinct environments in an extended physical system around the W33 complex
L. K. Dewangan1 , T. Baug2 and D. K. Ojha3
1

Physical Research Laboratory, Navrangpura, Ahmedabad - 380 009, India.; 2 Kavli Institute for Astronomy andAstrophysics, Peking University, 5 Yiheyuan Road, Haidian District, Beijing 100871, P. R. China.; 3 Department of
Astronomy and Astrophysics, Tata Institute of Fundamental Research, Homi Bhabha Road, Mumbai 400 005, India.
E-mail contact: lokeshd at prl.res.in

We present a multi-wavelength investigation of a large-scale physical system containing the W33 complex. The
extended system (∼50 pc × 37 pc) is selected based on the distribution of molecular gas at [29.6, 60.2] km s−1 andof 88 ATLASGAL 870 µm dust clumps at d ∼2.6 kpc. The extended system/molecular cloud traced in the mapsof 13 CO and C18 O emission contains several H ii regions12excited by OB stars (age ∼0.3–1.0 Myr) and a thermallysupercritical filament (“fs1", length ∼17 pc). The filament, devoid of the ionized gas, shows dust temperature (Td ) of
∼19 K, while the H ii regions are depicted with Td of ∼21–29 K. It suggests the existence of two distinct environmentsin the cloud. The distribution of Class I young stellar objects (mean age ∼0.44 Myr) traces the early stage of starformation (SF) toward the cloud. At least three velocity components (around 35, 45, and 53 km s−1 ) are investigatedtoward the system. The analysis of 13 CO and C18 O reveals the spatial and velocity connections of cloud components
around 35 and 53 km s−1 . The observed positions of previously known sources, W33 Main, W33 A and O4-7I stars,
are found toward a complementary distribution of these two cloud components. The filament “fs1" and a previously
known object W33 B are seen toward the overlapping areas of the clouds, where ongoing SF activity is evident. A
scenario concerning the converging/colliding flows from two different velocity components appears to explain well theobserved signposts of SF activities in the system.
Accepted by MNRASkpc）のlarge-scale（~50 pc × 37 pc）でのclumpの分布やガス• W33（大質量性形成領域、d~2.6
https://arxiv.org/pdf/2005.13871.pdfの運動を870 μm、13CO (J=1-0)、C18O (J=1-0)を使って調べた。
Investigating the physical conditions
in extended system hosting mid-infrared bubble
collisionよりもむしろ）、異なる速度のガスからのconversing/• この領域の星形成は（cloud-cloud
N14

colliding
L. K. flowによって説明できる。
Dewangan1 , T. Baug2 , L. E. Pirogov3 and D. K. Ojha4
1

Physical Research Laboratory, Navrangpura, Ahmedabad - 380 009, India.; 2 Kavli Institute for Astronomy andAstrophysics, Peking University, 5 Yiheyuan Road, Haidian District, Beijing 100871, P. R. China.; 3 Institute ofApplied Physics of the Russian Academy of Sciences, 46 Ulyanov st., Nizhny Novgorod 603950, Russia.; 4 Departmentof Astronomy and Astrophysics, Tata Institute of Fundamental Research, Homi Bhabha Road, Mumbai 400 005, India.
E-mail contact: lokeshd at prl.res.inUncovering distinct environments in an extended physical system around the W33 complex

gan, T. Baug and D. K. Ojha

L. K. Dewangan1, T. Baug2 and D. K. Ojha3

0.26

(a)

6.17 12.09 18.00 23.92 29.83 35.75（88個 at 870 μm）

質量~51000 M◉

O4-7型星長さ~17 pc

W33A、 W33 Main、W33B

線質量~ 3000 M◉

Kohno et al. (2018)の観測領域

ダスト温度 ~19 K

Uncovering physical environments around W33

(b)

N11

(a)

N11
N10

G013.210−0.144

#7

N10

#8
W33B

W33 MainG013.210−0.144

fs1

W33A

IRDCs

#23

fs2

W33 complex

filamentary features

(c)

N11

(b)

N10

G013.210−0.144

N11
N10

W33 Main
W33A

W33B

G013.210−0.144

fs1

filamentary features

artifacts1283

critical line mass ~16-32 M◉ pc-1
(at T=10-20 K)
Mline, crit ∼ 16 M⊙ pc−1 (Tgas /10 K)

W33 complex

Herschel

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Downloaded from https://academic.oup.com/mnras/article-abstract/496/2/1278/5851285 by National Astronomical Observatory of Japan us

W33 complex

フィラメント fs1について

ATLASGAL ダストクランプ→ fs1はthermally subcritical→ radial方向に重力収縮 /fragmentation

artifacts

W33 complex

HerschelUncovering distinct environments in an extended physical system around the W33 complex
L. K. Dewangan1, T. Baug2 and D. K. Ojha3

angan, T. Baug and D. K. Ojha
(a)

0.26

6.17 12.09 18.00 23.92 29.83 35.75

Uncovering physical environments around W33

Downloaded from https://academic.oup.com/mnras/article-abstract/496/2/1278/5851285 by National Astronomical Observatory of Japan user on 09 July 2020

Class I YSOs（901個、

12

(a)

FUGINの観測領域

3.6-5.8 μmの点源、Spitzerのカタログ）

0.26

(b)

6.17 12.09 18.00 23.92 29.83 35.75(b)

コントア ：YSOの数密度

ダストクランプが3つの速度領域に分布している

大部分のYSOがフィラメン
トやHII領域に分布している→星形成の初期段階(c)

4.7

213.1 421.5 629.8 838.2 1046.6 1255.0(c)

Figure 4. (a) Spatial distribution of the ATLASGAL 870-µm dust continuum clumps (diamonds) towards the selected site (see also Fig. 1a). Filled starcyan) show the locations of O4–7-type stars, and filled circles (in red) highlight various subregions in the W33 complex (see Fig. 1b). (b) Distribution oradial velocity against the Galactic longitude (see text for more details). (c) The FUGIN 13 CO spectrum (magenta curve) and the FUGIN C18 O spectrum (curve). The profiles are produced by averaging the area highlighted by the solid box in Fig. 4(a). The FUGIN 13 CO spectrum has been divided by a factor

Uncovering distinct environments in an extended physical system around the W33 complex

288

L. K. Dewangan, T. Baug and D. K. Ojha
315

463

612

760

908

1057

1290
K. 3Dewangan, T. Baug and D. K. Ojha
L. K. Dewangan1, T. Baug2 andD. K.L.
Ojha

1205

49.5

PV図

(a)

(b)

intensity
enhancement(b)cavitycavity

463

612

760

908

1057

1205

Downloaded from https://academic.oup.com/mnras/article-abstract/496/2/1278/5851285 by National Astronomical Observatory of Japa

(d)

315

1291

gure 7. (a) Longitude–velocity map of 13 CO. The contour levels are 0.45 deg K × (700, 800, 900, 1000, 1100, 1200, 1300, 1400, 1500, 1600, 1700, 1800,(e) 2400, 2500, 2600 and 2680). The two dashed curves (in red) show the connections between different cloud components. (b)00, 2000, 2100, 2200, 2300,
ngitude–velocity map of C18 O. The contour levels are 0.45 deg K × (110, 150, 160, 170, 210, 240, 270, 300, 330, 360, 400, 440, 500, 600, 700, 800 and0). The arrows indicate three velocity components in the direction of the selected area around W33. In each panel, the molecular emission is integrated overlatitude range from −0.◦ 6 to 0.◦ 21.

Downloaded from https://academic.oup.com/mnras/article-abstract/496/2/1278/5851285 by National Astronomical Observatory of Japan user on 09

Uncovering physical environments around W33
intensity
enhancement(a)105.0 160.5 216.0 271.5 327.0 382.5• フィラメントfs1やW33 Bに相補的な構造（CCCの証拠）が見られない

ain (G012.81 − 0.19), and three O4–7I stars (see IDs 7, 8 and 23
Messineo et al. 2015) are seen towards the areas of the spatial fit
the cavity and the intensity-enhancement region. However, theament fs1 and W33 B are found towards the common zones of
two clouds.
Overall, the study of the molecular line data shows the spatial
d velocity connections of two cloud components in the direction
the selected physical system. We discuss these results in more
ail in Section 4.
Scutum Ncomponents (around 35, 45 and 53 km s−1 ) are identified in the
direction of our selected physical system (see Section 3.4). The
physical system is found to host embedded filaments (i.e. fs1 andfs2) and several H II regions. The filaments are not associated withany radio continuum emission, and exhibit a Td of ∼17–19 K. A
relatively warm dust emission (Td ∼ 21–29 K) is also found towards
the H II regions, excited by OB-type stars (see Table 2). These results
together show the existence of two distinct environments in our
selected physical system, which differ substantially in their dust
temperatures (see Section 3.2). The elongated filament (fs1: length∼17 pc, Td ∼19 K) is characterized as a thermally supercriticalfilament, and appears to be on the verge of collapse (see Section 3.2).
Based on the distribution of Class I YSOs (mean age ∼0.44 Myr;
Evans et al. 2009), the early phase of SF activity is investigatedtowards the filaments and the H II regions (age ∼0.35–1.0 Myr) in• 35 km/sと53 km/sのcloudの相互作用でこの領域の星形成が引き起こされている• この結果は、Kohno et al. (2018)（タイムDISCUSSION

Scutum F
Norma N

1 Physical environment around W33

PV図にクランプをプロット

noted earlier, previously published results focused mainly on theスケール~0.7-1.0 MyrのCCC）の拡張

(b)

(c)

filament fs1

W33 B

16

https://arxiv.org/pdf/2005.13871.pdf
https://arxiv.org/pdf/2005.08905.pdf

Investigating the physical conditions in extended system hosting mid-infrared bubble
N14
L. K. Dewangan1 , T. Baug2 , L. E. Pirogov3 and D. K. Ojha4
1

Physical Research Laboratory, Navrangpura, Ahmedabad - 380 009, India.; 2 Kavli Institute for Astronomy andAstrophysics, Peking University, 5 Yiheyuan Road, Haidian District, Beijing 100871, P. R. China.; 3 Institute ofApplied Physics of the Russian Academy of Sciences, 46 Ulyanov st., Nizhny Novgorod 603950, Russia.; 4 Departmentof Astronomy and Astrophysics, Tata Institute of Fundamental Research, Homi Bhabha Road, Mumbai 400 005, India.
E-mail contact: lokeshd at prl.res.in

To observationally explore physical processes, we present a multi-wavelength study of a wide-scale environment towardl = 13.7–14.9 degrees containing a mid-infrared bubble N14. The analysis of 12 CO, 13 CO, and C18 O gas at [31.6,
46] km s−1 reveals an extended physical system (extension ∼59 pc × 29 pc), which hosts at least five groups of
the ATLASGAL 870 µm dust clumps at d ∼3.1 kpc. These spatially-distinct groups/sub-regions contain unstablemolecular clumps, and are associated with several Class I young stellar objects (mean age ∼0.44 Myr). At least threegroups of ATLASGAL clumps associated with the expanding H ii regions (including the bubble N14) and embedded
infrared dark clouds, devoid of the ionized gas, are found in the system. The observed spectral indices derived using
the GMRT and THOR radio continuum data suggest the presence of non-thermal emission with the H ii regions. High
resolution GMRT radio continuum map at 1280 MHz traces several ionized clumps powered by massive B-type stars
toward N14, which are considerably young (age ∼103 –104 years). Locally, early stage of star formation is evident
toward all the groups of clumps. The position-velocity maps of 12 CO, 13 CO, and C18 O exhibit an oscillatory-likevelocity pattern toward the selected longitude range. Considering the presence of different groups/sub-regions in thesystem, the oscillatory pattern in velocity is indicative of the fragmentation process. All these observed findings favour
the applicability of the global collapse scenario in the extended physical system, which also seems to explain theobserved hierarchy.
Accepted by The Astrophysical Journal
https://arxiv.org/pdf/2005.08905.pdf

Feedback of molecular outflows from protostars in NGC 1333, revealed by Herschel andSpitzer spectro-imaging observations
Odysseas Dionatos1 , Lars. E. Kristensen2, Mario Tafalla3 , Manuel Güdel1 and Magnus Persson4
1

Department of Astrophysics, University of Vienna, Türkenschanzstrasse 17, A-1180 Vienna; 2 Centre for Star andPlanet Formation, Niels Bohr Institute and Natural History Museum of Denmark, University of Copenhagen, Øster
Voldgade 5-7, 1350 Copenhagen, Denmark; 3 Observatorio Astronómico Nacional (IGN), Alfonso XII 3, 28014 Madrid,
Spain; 4 Department of Space, Earth and Environment, Chalmers University of Technology, Onsala Space Observatory,

17

https://arxiv.org/pdf/2005.08905.pdf
http://arxiv.org/abs/2006.01087

Feedback of molecular outflows from protostars in NGC 1333, revealed by Herschel andSpitzer spectro-imaging observations
Odysseas Dionatos1 , Lars. E. Kristensen2, Mario Tafalla3 , Manuel Güdel1 and Magnus Persson4
1

Department of Astrophysics, University of Vienna, Türkenschanzstrasse 17, A-1180 Vienna; 2 Centre for Star andPlanet Formation, Niels Bohr Institute and Natural History Museum of Denmark, University of Copenhagen, Øster
Voldgade 5-7, 1350 Copenhagen, Denmark; 3 Observatorio Astronómico Nacional (IGN), Alfonso XII 3, 28014 Madrid,
Spain; 4 Department of Space, Earth and Environment, Chalmers University of Technology, Onsala Space Observatory,
439 92, Onsala, Sweden
E-mail contact: odysseas.dionatos at univie.ac.at

13
Context Far infrared cooling of excited gas around protostars has been predominantly studied in the context of pointed
observations. Large scale spectral maps of star forming regions enable the simultaneous, comparative study of the gas
excitation around an ensemble of sources at a common frame of reference, therefore providing direct insights in themultitude of physical processes involved.
Aims We employ extended spectral-line maps to decipher the excitation, the kinematical and dynamical processes in
NGC 1333 as revealed by a number of different molecular and atomic lines, aiming to set a reference for the applicability and limitations of difference tracers in constraining particular physical processes.
Methods We reconstruct line maps for H2 , CO, H2 O and [CI] using data obtained with the Spitzer/IRS spectrographand the Herschel HIFI and SPIRE instruments. We compare the morphological features revealed in the maps andderive the gas excitation conditions for regions of interest employing LTE and non-LTE methods. We also calculate thekinematical and dynamical properties for each outflow tracer in a consistent manner, for all observed outflows driven
by protostars in NGC 1333. We finally measure the water abundance in outflows with respect to carbon monoxideand molecular hydrogen.
Results CO and H2 are highly excited around B-stars and at lower levels trace protostellar outflows. H2 O emission isdominated by a moderately fast component associated with outflows. H2 O also displays a weak, narrow-line component in the vicinity of B-stars associated to their UV field. This narrow component it is also present in a handful ofoutflows, indicating UV radiation generated in shocks. Intermediate J CO lines appear brightest at the locations tracedby the narrow H2 O component, indicating that beyond the dominating collisional processes, a secondary, radiative
excitation component can also be active. The morphology, kinematics, excitation and abundance variations of water
are consistent with its excitation and partial dissociation in shocks. Water abundance ranges between 5 × 10−7 and ∼10−5 , with the lower values being more representative. Water is brightest and most abundant around IRAS 4A whichis consistent with the latter hosting a hot corino source. [CI] traces dense and warm gas in the envelopes surrounding
protostars. Outflow mass flux is highest for CO and decreases by one and two orders of magnitude for H2 and H2 O,
respectively.
Conclusions Large scale spectral line maps can provide unique insights into the excitation of gas in star-forming regions. Comparative analysis of line excitation and morphologies at different locations allows to decipher the dominant
excitation conditions in each region but also isolate exceptional cases.
Accepted by A&A18

http://arxiv.org/abs/2006.01087
http://arxiv.org/pdf/2005.11725

Strong Hα emission and signs of accretion in a circumbinary planetary mass companion
from MUSE
Simon C. Eriksson1 , Rubén Asensio Torres2 , Markus Janson1 , Yuhiko Aoyama3,4 , Gabriel-DominiqueMarleau5,6,2 et al.
1

Institutionen för astronomi, Stockholms universitet, AlbaNova universitetscentrum, 106 91, Stockholm, Sweden; 2
Max-Planck-Institut für Astronomie, Königstuhl 17, D-69117 Heidelberg, Germany; 3 Institute for Advanced Study,
Tsinghua University, Beijing 100084, People’s Republic of China; 4 Department of Astronomy, Tsinghua University,
Beijing 100084, People’s Republic of China; 5 Institut für Astronomie und Astrophysik, Tübingen, Auf der Morgenstelle
10, D-72076 Tübingen, Germany; 6 Physikalisches Institut, Universität Bern, Gesellschaftsstr. 6, CH-3012 Bern,
Switzerland
E-mail contact: simon.eriksson at astro.su.se
Context. Using intrinsic Hα emission to detect substellar companions can be advantageous for improving contrasts indirect imaging, and probing planetary formation theories through the characterisation of accreting exoplanets.
Aims. In this work we aim to characterise the young circumbinary planetary mass companion 2MASS J01033563−5515561(AB)b (Delorme 1 (AB)b) through medium resolution spectroscopy.
Methods. We have used the new Narrow-Field Mode (NFM) for the MUSE integral-field spectrograph, located on the
ESO Very Large Telescope, during SV time to obtain optical spectra of Delorme 1 (AB)b.
Results. We report the discovery of very strong Hα and Hβ emission, accompanied by He I emission, consistent withan active accretion scenario. We provide accretion rate estimates obtained from several independent methods and finda likely mass of 12–15 MJup for Delorme 1 (AB)b, also consistent with previous estimates.
Conclusions. Signs of active accretion in the Delorme 1 14
system could indicate a younger age than the ∼30–40 Myr
expected from a likely Tucana-Horologium (THA) membership. Previous works have also shown the central binary
to be overluminous, which gives further indication of a younger age. However, recent discoveries of active disks inrelatively old (∼40 Myr), very low-mass systems suggests that ongoing accretion in Delorme 1 (AB)b might not requirein and of itself that the system is younger than the age implied by its THA membership.

Accepted by A&A
companion、Delorme 1）。
• HeI放射を伴う、強いHαとHβの放射を発見した（circumbinary
http://arxiv.org/pdf/2005.11725• 活発な質量降着＋中心の連星系がover luminous →Tucana-Horologium (THA) membershipから推A Survey for New Stars
and Brown Dwarfs in the Ophiuchus Star-forming Complex
定される年齢（~30-40Myr）よりも若いはず。
T.L. Esplin1,2 and K.L. Luhman3,4Myr）の低質量の系でactive diskが最近発見されたので、Delorme 1（AB）b若• 比較的古い（~40
Steward Observatory, University of Arizona, Tucson, AZ, 85719, USA; Strittmatter Fellow; Department of1

2

3

Astronomy andい必要はない。Astrophysics, The Penn- sylvania State University, University Park, PA 16802; 4 Center for Exoplanets
and Habitable Worlds, The Pennsyl- vania State University, University Park, PA 16802

Strong Hα emission and signs of accretion in a circumbinary planetary mass companion from MUSE
Simon C. Eriksson1, Rubén Asensio Torres2, Markus Janson1, Yuhiko Aoyama3,4, Gabriel-Dominique Marleau5,6,2 et al.
S. C. Eriksson et al.: Strong H↵ emission and signs of accretion in a circumbinary planetary mass companion from MUSE

, L6 (2020)

S. C. Eriksson et al.: Strong H↵ emission and signs of accretion in a circumbinary planetary mass companion from MUSE

MUSEのnarrow-field modeで観測

Delorme 1 (AB)b

Delorme 1 A, B
（明るさを1/200として表示）
Fig. 2. Full averaged (over 11 cubes) MUSE spectrum of the companion Delorme 1 (AB)b (black line) showing very strong H↵ emission, andhighlighting other atomic lines (black text and red lines) and molecular absorption features (dashed red lines). The two narrow gaps in the spectrum
are caused by sections of unusable data at 5800 6051 Å and 7592 7681 Å.

連星間の距離：~0.25” (12 au) at 47.2 pc

Fig. 1. Composite-colour image of the Delorme 1 system, created from
Tableaveraged
1. Individual
line11characteristics(extinction-corrected
EW, and the
10% andline(black
profileline)
widths)of Delorme(AB)b for
Fig. 2. Full(overcubes) MUSE
spectrum of theflux,
companion
Delorme
1 50%(AB)bshowingvery1strongH↵detected
emission,
the MUSE NFM observations. The slightly brighter primary component
emissionlines,
obtainedfromtheaveraged
spectrum.
highlighting other atomic lines (black text and red lines) and molecular absorption features (dashed red lines). The two narrow gaps in the spect
A is located to the south-west in the image, with B to the north-east andare caused by sections of unusable data at 5800 6051 Å and 7592 7681 Å.
the significantly redder companion Delorme 1 (AB)b to the north. The
Line
Fline
EW
10% width FWHM
mA
mB
central binary is scaled down in flux by a factor of 200.
16
2
1
1
1
(10 (extinction-corrected
erg cm s ) (Å)flux, EW, and(kmthes 10%)(kms )line(mag)Table 1. Individual line characteristics
and50%
profile widths)(mag)of Delorme 1 (AB)b for detec◉◉
emission lines, obtainedHfrom the averaged
spectrum.
1.39 ± 0.10
...
<322
<177
3.21 ± 0.23 3.03 ± 0.24
H↵
12.80 ± 0.70
135 ± 5105 241
58 133 4.31 ± 0.16 3.89 ± 0.16
He i
0.18 ± 0.03
1.9 ± 0.2 <194
<108
...
...
This likely indicates that accretion onto this planetary-mass
Line He i 6678Fline0.15 ± 0.04
EW1.0 ± 0.1 10%
width . .FWHM
mA
mB
.
.
.
.
.
.
.
...
7065
object is ongoing. For key lines (Table 1) we provide line fluxes
16
2
1
1
1

連星のスペクトル型：M5.5連星の質量：0.19 M 、0.17 M

Delorme 1 (AB)bまでの距離：84 auandline profile 1
widthsbased on which we estimate theaccreDelorme(AB)bの質量：12-14
MJuption rate using three di↵erent models (Table 2). Supplementary
figures and tables can be found in Appendix B.

系の年齢：30 Myr

3.1. Detection of very strong line emission in Delorme 1
(AB)b

(10

erg cms )(Å)(km s )(km s )

(mag)

(mag)

1.0 ± 0.1

...

...

...

...

Notes. Negative EW indicates emission. For H there is no well-defined continuum, required for an EW estimate, and the measured FWHM is
1
± of
0.10
. . . ⇠ 177 km s <322
<177
0.23
± 0.24equivalent H
to the resolution1.39
width
MUSE (RH = 1694). For HeI7065 , theline profile 3.21
is not ±well
defined3.03
enoughfor an accurate
estimate ofH↵
the width. The 12.80
m values
compare the H↵ and
H ±lineof Delorme
with thoseof theprimary components± 0.70135
5 fluxes105
241 1 (AB)b
58 1334.31± 0.16
3.89 ± 0.16A and B at a
2.5 pixel aperture.
He i 6678 0.18 ± 0.03
1.9 ± 0.2 <194
<108
...
...

He i 7065

0.15 ± 0.04

indicate a lower-gravity atmosphere (e.g. McGovern et al. 2004), 1 (AB)b in the range of 12 15 MJup , spanning the deuteriumNotes. Negative EW indicates emission. For H there is no well-defined continuum, required for an EW estimate,
and the measured FWHM
which would be in line with the expectations of youth in this1 burning limit. This is consistent with Delorme et al. (2013). The
equivalent to the resolution width of MUSE (RH = 1694 ⇠ 177 km s ). For HeI7065 , the line profile is not well defined enough for an accu
use of cold- or warm-start models would imply a higher mass
The detected H↵ emission in the spectrum of Delorme 1 (AB)b estimateobject.
of the width. The m values compare the H↵ and H line fluxes of Delorme 1 (AB)b with those of the primary components A and B
It
is
clear
that
the
line
emissionisintrinsic
toDelorme1(e.g. Marleau & Cumming 2014), but we restrict ourselves here
(Fig. 2) clearly stands out, with an integrated flux of 1.28 ± 2.5 pixel aperture.
(AB)b. We therefore turn our attention to the question of the to hot starts, especially because recent modelling suggests that
0.70 ⇥ 10 15 erg cm 2 s 1 . H does not have a well-definedmechanism behind it.
these are more likely (Berardo et al. 2017; Marleau et al. 2019).
local continuum for comparison, and peaks at ⇠10% of H↵.
Thus, to calculate the mass accretion rate, we adopt a com-indicate a lower-gravity atmosphere (e.g. McGovern et al. 2004),

1 (AB)b in the range of 12 15 M

, spanning the deuteriu

Strong Hα emission and signs of accretion in a circumbinary planetary mass companion from MUSE
Simon C. Eriksson1, Rubén Asensio Torres2, Markus Janson1, Yuhiko Aoyama3,4, Gabriel-Dominique Marleau5,6,2 et al.

Delorme 1 (AB)bの質量と年齢：0.012M◉、10 Myr もしくは 0.015 M◉、50 Myr
A&A 638, L6 (2020)（DUSTY00 atmosphere isochronalmodels Cjabroer et al. (2000)）
Table 2. Accretion luminosities and mass accretion rates for Delorme 1 studies of accreting planets using MUSE, in more detail in(AB)b estimated from Table 1, and upper limits inferred from the non- Sect. 4. From this width, we tentatively estimate Ṁacc = 3 ⇥detections of the Ca IRT.
8+0.4
1
2
質量降着率
1.4

10
MJup yr using Eq. (1), which is a factor ⇠ 10 greater
than
what
we-10±0.4
obtainMfrom theline
luminosity
above.
-1
3.4
×
10
yr
（Hα
luminosity、Alcala
et al. (2012)）(a)(a),(b)
Jup
Line
Lline
Lacc
Ṁacc
A
similarestimatecanbeobtainedfromtheplanet-surface
log(Lline /L ) log(Lacc /L )log(MJup .yr 1 )
shock
model
Ikomaluminosity、Thanathibodee(2019), which combines the et al. (2019)）
0.8 ×
10-8ofMAoyama
Jup yr-1&（Hαline luminosity with the H↵ line profile widths to estimate Ṁacc ,H
8.01 ± 0.07
6.55 ± 0.37
9.79 ± 0.37
-8+0.4/-1.4 MJup yr-1 （Hαの線幅、Natta et al. (2012)）
× 10
as3wellas the planetary
mass MP (independently of evolutionaryH↵
7.05 ± 0.06
6.23 ± 0.41
9.47 ± 0.41
He i 6678
8.90 ± 0.09
6.43 ± 0.64
9.67 ± 0.64
models). Usinga radius
RP = 0.163 R , we tentatively estimate-8 MJup-1 （惑星表面のショックモデル、Aoyama
1
×
10
yr
& Ikoma (2019)）
He i 7065
8.98 ± 0.14
6.13 ± 0.56
9.37 ± 0.56
an accretion rate of Ṁacc = 1 ⇥ 10 8 MJup yr 1 , and a planetary(Ca ii 8498 ) < 8.38
< 5.70< 8.95
mass MP = 11 MJup . If the true line profile widths are closer
2桁の違いは観測の不定性（スペクトル、強度比）や（波長）(Ca ii 8542 ) < 8.36
< 5.67< 8.92to the lower limits of the width, this would indicate a similar(Ca ii 8662 ) < 8.54
< 5.65< 8.89Ṁacc but a substantially lower mass, down to MP ⇠ 6 MJup . We
分解能、放射の起源そのもに由来すると思われる
Notes. The non-detection of the Ca IRT is indicated by parentheses. note that this lower estimate is discrepant from the estimate pro(a)Obtained using the relations in Alcalá et al. (2017). (b) Derived from vided by the evolutionary models (Table 3). The accretion rates
Lacc using R = 0.163 R from the Chabrier et al. (2000) and Bara↵e derived from the methods of Natta et al. (2004) and Aoyama &et al. (2002) 0.012 M model at 10 Myr.
Ikoma (2019) are consistent with the Ṁacc = 0.8⇥10 8 MJup yr 1
obtained for Delorme 1 (AB)b using the H↵ line luminosity
Table 3. Absolute magnitudes of Delorme 1 (AB)b compared with the based model of Thanathibodee et al. (2019). It is important to
DUSTY00 isochrones (Chabrier et al. 2000; Bara↵e et al. 2002) that note that the applicability of this method to the case of Delorme 1
agree well with the photometry.
(AB)b depends on it having a comparable mass and radius to the
主星（Delorme 1 AとB）と伴星（Delorme 1 (AB)b）の質量比が~0.03-0.04と高いため、この系の形成シナ
PDS 70 planets (Thanathibodee et al. 2019). While both parameters are still highly uncertain for these planets, the mass estimates
FilterDelorme 1 (AB)b 0.012 M
0.015 M
Ref.
リオを構築するのは難しい。
for Delorme 1 (AB)b thus far are comparable to PDS 70 b, and
10 Myr50 Myrより高分解能の観測をすることで、詳細に質量降着の様子を調べることができる。
to the radius and mass assumed for the model by Thanathibodee
Mi
15.7 ± 0.3
15.77
15.71
1
et al. (2019) (MP = 6 MJup , RP = 1.3 RJup ).
Mz0
14.0
14.05 (a)14.39 (a)3
MJ
12.1 ± 0.3
11.86
11.88
2
MH
10.9 ± 0.2
10.95
11.01
2
4. Discussion
M KS
10.3 ± 0.2
10.25
10.34
2
We have presented photometry and spectroscopy from MUSE
M L0
9.3 ± 0.1
9.23
9.33
2
NFM observations of the Delorme 1 system. From the analysis(a)0Notes. SDSS z magnitudes from the AMES-Dusty isochrones at the of the detected emission lines (Fig. 2), we found several indica-

•
•
•
•

•
•

19

http://arxiv.org/pdf/2005.11725
http://arxiv.org/pdf/2005.10096

A Survey for New Stars and Brown Dwarfs in the Ophiuchus Star-forming Complex
T.L. Esplin1,2 and K.L. Luhman3,4
1

Steward Observatory, University of Arizona, Tucson, AZ, 85719, USA; 2 Strittmatter Fellow; 3 Department of
Astronomy and Astrophysics, The Penn- sylvania State University, University Park, PA 16802; 4 Center for Exoplanets
and Habitable Worlds, The Pennsyl- vania State University, University Park, PA 16802
E-mail contact: taranesplin at email.arizona.edu
We have performed a survey for new members of the Ophiuchus cloud complex using high-precision astrometry
from the second data release of Gaia, proper motions measured with multi-epoch images from the Spitzer Space
Telescope, and color-magnitude diagrams constructed with photometry from various sources. Through spectroscopyof candidates selected with those data, we have identified 155 new young stars. Based on available measurements ofkinematics, we classify 102, 47, and six of those stars as members of Ophiuchus, Upper Sco, and other populationsin Sco-Cen, respectively. We have also assessed the membership of all other stars in the vicinity of Ophiuchus thathave spectroscopic evidence of youth from previous studies, arriving at a catalog of 373 adopted members of thecloud complex. For those adopted members, we have compiled mid-IR photometry from Spitzer and the Wide-field
Infrared Survey Explorer and have used mid-IR colors to identify and classify circumstellar disks. We find that 210
of the members show evidence of disks, including 48 disks that are in advanced stages of evolution. Finally, we haveestimated the relative median ages of the populations near the Ophiuchus clouds and the surrounding Upper Sco
association using absolute K-band magnitudes (MK ) based on Gaia parallaxes. If we adopt an age 10 Myr for Upper
Sco, then the relative values of MK imply median ages of ∼2 Myr for L1689 and embedded stars in L1688, 3–4 Myr
for low-extinction stars near L1688, and ∼6 Myr for the group containing ρ Oph.
Accepted by AJ

http://arxiv.org/pdf/2005.10096

Seeds of Life in Space (SOLIS). IX. Chemical segregation of SO2 and SO toward thelow-mass protostellar shocked region of L1157
S. Feng1,2,3 , C. Codella4,5 , C. Ceccarelli5 , P. Caselli3 , A. Lopez-Sepulcre5,6 , R. Neri6 , F. Fontani3,4 , L.
Podio4 , B. Lefloch5 , H. B. Liu7 , R. Bachiller8 and S. Viti91National Astronomical Observatory of China, Datun Road 20, Chaoyang, Beijing, 100012, P. R. China; 2 CAS Key
Laboratory of FAST, NAOC, Chinese Academy of Sciences, P. R. China; 3 Max-Planck-Institut für Extraterrestrische
Physik, Gießenbachstraße 1, D-85748, Garching bei München, Germany; 4 INAF-Osservatorio Astrofisico di Arcetri,
Largo E. Fermi 5, I-50125, Florence, Italy; 5 Univ. Grenoble Alpes, CNRS, IPAG, F-38000 Grenoble, France; 6 Institut
de Radioastronomie Millimétrique, 300 rue de la Piscine, Domaine Universitaire de Grenoble, F-38406 Saint-Martind’Hères, France; 7 Academia Sinica Institute of Astronomy and Astrophysics, No.1, Sec. 4, Roosevelt Road, Taipei

20

http://arxiv.org/pdf/2005.10096
https://arxiv.org/pdf/2005.04629

Seeds of Life in Space (SOLIS). IX. Chemical segregation of SO2 and SO toward thelow-mass protostellar shocked region of L1157
S. Feng1,2,3 , C. Codella4,5 , C. Ceccarelli5 , P. Caselli3 , A. Lopez-Sepulcre5,6 , R. Neri6 , F. Fontani3,4 , L.
Podio4 , B. Lefloch5 , H. B. Liu7 , R. Bachiller8 and S. Viti91National Astronomical Observatory of China, Datun Road 20, Chaoyang, Beijing, 100012, P. R. China; 2 CAS Key
Laboratory of FAST, NAOC, Chinese Academy of Sciences, P. R. China; 3 Max-Planck-Institut für Extraterrestrische
Physik, Gießenbachstraße 1, D-85748, Garching bei München, Germany; 4 INAF-Osservatorio Astrofisico di Arcetri,
Largo E. Fermi 5, I-50125, Florence, Italy; 5 Univ. Grenoble Alpes, CNRS, IPAG, F-38000 Grenoble, France; 6 Institut
de Radioastronomie Millimétrique, 300 rue de la Piscine, Domaine Universitaire de Grenoble, F-38406 Saint-Martind’Hères, France; 7 Academia Sinica Institute of Astronomy and Astrophysics, No.1, Sec. 4, Roosevelt Road, Taipei
10617, Taiwan, Republic of China; 8 Observatorio Astronomico Nacional (OAN, IGN), Calle Alfonso XII, 3, E-28014
Madrid, Spain; 9 Department of Physics and Astronomy, University College London, Gower Street, London WC1E
6BT, UK
E-mail contact: siyi.s.feng at gmail.com
We present observations of SO and SO2 lines toward the shocked regions along the L1157 chemically rich outflow,
taken in the context of the Seeds Of Life In Space IRAM-NOrthern Extended Millimeter Array Large Program, andor the Radiation Driven Implosion (RDI) models and change their properties. We study the properties of two zones
located in the Photo Dissociation Region (PDR) of the Galactic HII region RCW120 and discussed them as a function
15of the physical conditions and young star contents found in both clumps. Using the APEX telescope, we mapped
two regions of size 1.! 5×1.! 5 toward the most massive clump of RCW120 hosting young massive sources and towarda clump showing a protrusion inside the HII region and hosting more evolved low-mass sources. The 12 CO(J=3–2),
13
CO(J=3–2) and C18 O(J=3–2) lines are used to derive the properties and dynamics of these clumps. We discuss theirrelation with the hosted star-formation. The increase of velocity dispersion and Tex are found toward the center of themaps, where star-formation is observed with Herschel. Furthermore, both regions show supersonic Mach number. No
strong evidences have been found concerning the impact of far ultraviolet (FUV) radiation on C18 O photodissociation.
The fragmentation time needed for the C&C to be at work is equivalent to the dynamical age of RCW120 andthe properties of region B are in agreement with bright-rimmed clouds. It strengthens the fact that, together withevidences of compression, C&C might be at work at the edges of RCW120. Additionally, the clump located at theeastern part of the PDR is a good candidate of pre-existing clump where star-formation may be induced by the RDI
mechanism.
Accepted by A&A
http://arxiv.org/pdf/2005.08810

Measuring turbulent motion in planet-forming disks with ALMA: A detection around21

https://arxiv.org/pdf/2005.04629
https://arxiv.org/pdf/1909.00209

The chemical structure of young high-mass star-forming clumps: (I) Deuteration
S. Feng1,2,3 , P. Caselli4, K. Wang5 , Y. Lin6 , H. Beuther7 and O. Sipilä41National Astronomical Observatory of China, Datun Road 20, Chaoyang, Beijing, 100012, P. R. China; 2 CAS
Key Laboratory of FAST, NAOC, Chinese Academy of Sciences, P. R. China; 3 National Astronomical Observatoryof Japan, 2 Chome-21-1 Osawa, Mitaka-shi, Tokyo-to 181-8588, Japan; 4 Max-Planck-Institut für Extraterrestrische
Physik, Gießenbachstraße 1, D-85748, Garching bei München, Germany; 5 Kavli Institute for Astronomy and Astrophysics, Peking University, 5 Yiheyuan Road, Haidian District, Beijing 100871, China; 6 Max Planck Institute forRadio Astronomy, Auf dem Hügel 69, D-53121 Bonn, Germany; 7 Max-Planck-Institut für Astronomie, Königstuhl
17, D-69117, Heidelberg, Germany
E-mail contact: siyi.s.feng at gmail.com
The chemical structure of high-mass star nurseries is important for a general understanding of star formation. Deuteration is a key chemical process in the earliest stages of star formation because its efficiency is sensitive to the environment.
Using the IRAM-30 m telescope at 1.3–4.3 mm wavelengths, we have imaged two parsec-scale high-mass protostellar
clumps (P1 and S) that show different evolutionary stages but are located in the same giant filamentary infrared darkcloud G28.34+0.06. Deep spectral images at subparsec resolution reveal the dust and gas physical structures of bothclumps. We find that (1) the low-J lines of N2 H+ , HCN, HNC, and HCO+ isotopologues are subthermally excited;and (2) the deuteration of N2 H+ is more efficient than that of HCO+ , HCN, and HNC by an order of magnitude.
The deuterations of these species are enriched toward the chemically younger clump S compared with P1, indicatingthat this process favors the colder and denser environment (Tkin ∼ 14K, N(NH3 ) ∼ 9 × 1015 cm−2 ). In contrast,
single deuteration of NH3 is insensitive to the environmental difference between P1 and S; and (3) single deuterationof CH3 OH (> 10%) is detected toward the location where CO shows a depletion of ∼ 10. This comparative chemical
study between P1 and S links the chemical variations to the environmental differences and shows chemical similarities
between the early phases of high- and low-mass star-forming regions.
Accepted by ApJkpc）を複数の分子輝線で重水素化に着目し• 進化段階の異なる若い大質量星形成クランプ（d~4.8
https://arxiv.org/pdf/1909.00209て観測した。

APEX
CO observations towards the photodissociation region of RCW120μmで暗いフィラメント（G28.34+0.06）内のクランプ• 70
M. Figueira , A. Zavagno , L. Bronfman , D. Russeil , R. Finger , and F. Schuller+の低いJ（J=1、2）の準位は非熱的に励起されている
H＋、HCN、HNC、HCO• N2National
Centre for Nuclear Research, ul. Pasteura 7, 02-093, Warszawa, Poland; Aix Marseille Univ, CNRS, CNES,
LAM,＋Marseille, France; Departamento de Astronomía,
Universidad de Chile, Casilla 36-D, Santiago, Chile; Max2H の重水素化は、HCN、HNC、HCO+に比べて数桁効率的• NPlanck-Institut
für Radioastronomie, Auf dem Hügel 69, 53121, Bonn, Germany; Leibniz-Institut für Astrophysik
Potsdam(AIP), An der Sternwarte 16,
14482 Potsdam, Germany
18O)~10の領域で、CH
3OHの一個のHが重水素化する割合が10%を超える• fD(CE-mail contact: Miguel.Figueira at ncbj.gov.pl
1

2

1

3

2

3

4,5

2

3

4

5

The chemical structure of young high-mass star-forming clumps: (I) Deuteration

trophysical Journal, 883:202 (23pp), 2019 October 1

5
6
S. Feng1,2,3, P. Caselli4, K. WangFeng, Y.et Lin, H. Beuther7 and O. Sipilä4al.

カラー：積分強度 [K km s-1]（IRAM-30-m）
コントア ：870 μmダスト連続波（APEX）
Clump S• 70 μmの吸収線のピーク• 0.8 pcスケールでは• 低いダスト温度（14-16 K、Wang et al. 2008）• 低い光度（10 L◉、Ragan et al. 2013）• COが多くdepletionしている• 0.08 pcスケールでは• SiO (2-1)と(5-4)でbipolarのredshiftとblueshiftしているlobeが観測されている→若いアウトフロー• 進化の進んだ大質量protostarからのアウトフロー
よりもエネルギーがファクター10程度小さい
Clump P1
• 赤外で明るい（~103 L◉、18-28 K、Wang et al.
2011）• Clump Sから1’.5（~1.8 pc @ 4.8 kpc）離れている• COのアウトフロー（10-5 M◉ yr-1、Wang et al. 2011;
Zhang et al. 2015）、H2Oメーザー、CH3OHメーザーが検出されている• Clump Sよりも進化が進んでいる

The chemical structure of young high-mass star-forming clumps: (I) Deuteration
The Astrophysical Journal, 883:202 (23pp), 2019 October 1

Feng et al.

S. Feng1,2,3, P. Caselli4, K. Wang5, Y. Lin6, H. Beuther7 and O. Sipilä4
Table 1
Transitions Detected toward G28.34 P1–S

Mol.

Freq.
(GHz)

Transition

Sμ2a
(D2)

Eu/kBa(K)

ncritb(×105 cm−3)

neffc(×105 cm−3)

Beam
(″)

H13CN
H13CN
HC15N
DCN

86.340172.67886.05572.415J=1–0dJ=2–1d1–0J=1–0d

26.7
53.4
8.9
26.8

4.1
12.4
4.1
3.5

9.3
89.0
9.8
5.5

2.2–3.5
8.6–19.0
–
–

30.0
15.0
30.1
35.8

HN13C
H15NC
DNC

87.09188.86676.306

1–0
1–0
1–0

7.3
7.3
9.3

4.2
4.3
3.7

1.9
2.0
1.7

–
–
–

29.8
29.2
34.0

H13CO+
H13CO+
HC18O+
DCO+

86.754173.50785.16272.039J=1–0eJ=2–1e
1–0J=1–0e

15.2
30.4
15.2
14.5

4.2
12.5
4.1
3.5

1.4
28.4
1.0
2.6

0.3–0.4
1.0–1.7
–
–

29.9
15.0
30.5
36.0

N2 H+
N2 D+
N2 D+

93.17377.109154.217J=1–0dJ=1–0dJ=2–1d

104.0
104.0
208.1

4.5
3.7
11.1

1.5
0.5
9.2

0.1
–
–

27.8
33.6
16.8

NH3f
NH2D

23.69485.926

11 0a–11 0s
11,1 0s–10,1 0a

6.6
28.6

23.8
20.7

0.1
39.0

0.01
–

30.2

CH3OH
CH3OH
CH3OH
CH3OH
CH3OH
CH3OH
CH3OH
CH3OH
CH3OH
CH3OH
CH3OH
CH3OH
CH3OH
CH2DOH
13
CH3OH
13
CH3OH

76.51084.52195.16995.91496.73996.74196.745157.246
157.271
157.272
157.276
170.061
218.440
89.40894.40594.40750,5–41,3 E
5−1,5–40,4 Eg
80,8–71,7 Ag
21,2–11,1 A
2−1, 2–1−1, 1 E
20,2–10,1 A
20,2–10,1 E
40,4–4−1, 4 E
10,1–1−1, 1 E
30,3–3−1, 3 E
20,2–2−1, 2 E
32,1–21,1 E
42,2–31,2 Eg
20,2–10,1 e02−1, 2–1−1, 1 E
20,2–10,1 A

1.9
3.1
7.2
1.2
1.2
1.6
1.6
4.2
1.5
3.3
2.4
3.1
3.5
1.2
1.2
1.6

47.9
40.4
83.5
21.4
12.5
7.0
20.1
36.3
15.4
27.1
20.1
36.2
45.5
6.4
12.4
6.9

0.4
3.0
1.6
0.5
82.5
0.5
3.4
60.0
1.8
32.5
1678.4
1963.1
1.6
0.2
82.5
0.4

–
–
–
–
–
–
–
–
–
–
–
–
–
–
–
–

33.9
30.7
27.3
27.0
26.8
26.8
26.8
16.5
16.5
16.5
16.5
15.3
11.9
29.0
27.5
27.5

H2CO
H2CO
H2CO
H2CO

72.838218.222218.476
218.760

10,1–00,030,3–20,232,2–22,1
32,1–22,0

5.4
16.3
9.1
9.1

3.5
21.0
68.1
68.1

1.6
28.8
12.1
25.9

0.3–0.5
2.9–7.7
–
–

35.6
11.9
11.9
11.9

The chemical structure of young high-mass star-forming clumps: (I) Deuteration
5
6
7
4
Feng ,et Y.
al. Lin , H. Beuther and O. Sipilä
S. Feng1,2,3, P. Caselli4, K. Wange Astrophysical Journal, 883:202 (23pp), 2019 October 1

c

a

e

老
d
f

若 b
ダスト温度、H2の柱密度はP1とSで大きくは変わらない

The Astrophysical Journal, 883:202 (23pp), 2019 October 1

Feng et al.

gure 3. Dust temperature and H2 column density maps for G28.34 P1–S. Maps are derived by iterative SED ﬁts to the data from Herschel PACS at 70 μm and from
O/SHARC-II at 350 μm, achieving an angular resolution of 10″ (Lin et al. 2017). The continuum images at 70, 160, 250, 350, 500, and 850 μm from Herschel,
O/SHARC-II, Planck, and JCMT-SCUBA2 are used to establish a reliable blackbody model pixel by pixel. Panel (I): dust temperature map. Panel (II): dust
mperature proﬁle extracted along the the ﬁlamentary elongation, plotted in black, with the ends labeled “a” and “b”; dust temperature proﬁle extracted along thependicular direction to the ﬁlamentary elongation is plotted in red (from point “c” over the 870 μm continuum peak P1 to point “d”) or blue (from point “e” over the
0 μm continuum peak S to point “f”). Panel (III): H2 column density map. Panel (IV): H2 column density proﬁle in the directions of a–b (in black), c–d (in red), and(in blue). The pixels with < 5σ continuum emission at 870 μm are blanked. The black contour of the 870 μm continuum emission starts from 10σ and increases in
ps of 10σ (σ = 0.042 Jy beam−1). The angular resolution achieved in SED ﬁts is shown in black in the bottom left corner of Panels (I) and (III).

nse15 (∼105 cm−3) and cold (∼19 K), with the H2 column
nsity (∼1.2 × 1023 cm−2) toward P1 higher than that toward
by a factor of 2.
We also note a decrease (∼4 K) of the dust temperature frome outskirts of the ﬁlament to the center. Because the dust
mperature derived from SED ﬁtting traces the weighted
erage temperature along the line of sight (e.g., Sokolov et al.
18), such a decrease can be explained considering that theating from the protostellar objects P1 and S to their gas
velopes is comparably less efﬁcient than the interstellar
diation impinging on the outskirts of this ﬁlament.

2. Gas Temperature and Density Maps Derived from p-NH3

The dust continuum map suffers from the contamination ofe foreground and background dust. In contrast to this, we cantegrate the line intensity of a gaseous species over its velocity
spersion around the system velocity of the target source, so

The average volume number density n of the gas can be estimated from theurce kinematic distance DGC, the angular resolution θ, and the H2 column
N (H )
nsity N(H2) as n  R D 2 .
GCthat the gas emission map toward the source can be wellcharacterized by excluding the foreground/background contamination (Section 3.1).
CO isotopologues are relatively more abundant than the otherspecies. Our observations imaged C18O (2–1) and C17O (2–1)
lines with high S/N. They show similar line proﬁles to the lines
we study in this work (see Feng et al. 2016b). Although 2–1
transitions of CO isotopologues are easily thermalized near theircritical densities (2 × 104 cm−3 at 10–20 K, derived using datafrom the Leiden Atomic and Molecular Database, LAMDA16),
CO is known to freeze out in an environment of T<20 K anddensity slightly higher than a few 104 cm−3 (e.g., Caselli et al.
1999; Fontani et al. 2006; Aikawa et al. 2008). Therefore,
showing high depletion (Feng et al. 2016b, see also Section 6),
it cannot be used as a high-density tracer.
Compared with CO, N-bearing species are more resilient todepletion (e.g., Caselli et al. 1999; Bergin et al. 2002; Caselli
et al. 2002a; Jørgensen et al. 2004). The (1, 1) and (2, 2)
inversion transition lines of NH3, with their critical density of(1–2)×103 cm−3 (Shirley 2015) in the temperature range ofNH3から求めたガスの（力学）温度、NH3の柱密度はP1とSで異なる16

http://home.strw.leidenuniv.nl/~moldata• P1：Tkin~20 K、NNH3~4 × 1015 cm-2
• S：Tkin~14 K、NNH3~9 × 1015 cm-2

The chemical structure of young high-mass star-forming clumps: (I) Deuteration
The Astrophysical Journal, 883:202 (23pp), 2019 October 1 S. Feng1,2,3, P. Caselli4, K. Wang5, Y. Lin6, H. Beuther7 and O. Sipilä4
Table 2
Excitation Temperature Derived from Hyperﬁne Transitions or from Line
Ratios
Line

T

P1
(K)

Soff
(K)

S
(K)

T(%F1, %F )T(%J , %K )20.0±10.1
18.0±2.6

10.4±13.2
13.5±2.9

10.2±1.0
14.0±3.9

o-NH2D(1, 0)

TΔF

3.0±2.4

5.7±2.9

3.0±2.4

N2H+(1-0)
N2D+(2–1)/(1–0)

TΔF
TΔJ

8.1±5.1
4.5±1.2

6.0±2.8
4.0±0.55.2±2.4
3.8±0.5

H13CN(1–0)
H13CN(2–1)
DCN(1-0)
H13CN(2–1)/(1–0)

TΔF
TΔF
TΔF
TΔJ

8.7±6.9
3.5±2.8
4.2±3.3
3.8±0.5

9.5±7.4
8.2±5.6
3.2±1.8
3.2±1.7

8.6±5.2La
3.5±1.5
3.0±0.3

H13CO+(2-1)/(1-0)

TΔJ

4.1±0.3

3.6±0.3

La

p-NH3(1, 1)
p-NH3(2, 2)/(1, 1)

Note.
S/N<4.

The
Astrophysical Journal, 883:202 (23pp), 2019 October 1aFeng et al.

emission due to S/N<4 in most pixels, the emission
maximum appears at ∼25″ offset NE of clump S.
We note that an offset of 20″ corresponds to 2/3 of the beamat 3 mm. Because these lines are observed simultaneously, thedifferent locations of their individual emission maxima is likely
the result of their different distributions, rather than any
uncertainty caused by the pointing error between the IRAM30 m (for molecular lines) and APEX (for the dust continuum)
telescopes.
Hereafter, we denote
thislocation (20″
NE of+S)
13CN、DCN、H
13CO
+、DCO
+、N
H
2H 、N2D+の低いJの準位のas “Soff.”•

励起温度は5-10K

4. Physical Structure

We have detected deuterated isotopologues of six species:
HCN, HNC, HCO+, N2H+, NH3, and CH3OH. They are
believed to have different gas-grain formation routes (e.g.,
Fontani et al. 2015). To understand how different environments
affect the deuterium fractionation process, it is essential tocharacterize the physical structure of the source, i.e., via
Feng et al.
reconstructing the gas and dust temperature
as well as density
proﬁles.

Table 3
Mean and Standard Deviation of Parameters from LVG and LTE RD FittingsSpeciﬁcally, when we compare the beam-averaged lineLVG
proﬁles5−3of these molecules
the hydrogenatedcm P1,)
Tkin(K)
Mol.
Positionbetween Sn(10andmolecularlines show
stronger0.5±0.1
emission at theircentroid
P1
51.6±6.2
p-H2CO
velocities
toward P1
S by a factor of 1.5–2,
which
p-H
S than toward0.5±0.1
26.4±2.0
2CO
p-H
CO
Soff
0.5±0.2
19.5±1.5
2
is consistent with the nature that P1 is chemically andphysicallymore evolved.
In contrast,
intensities
A-CH
P1
4.8±0.9the emission
28.1±1.3
3OH
E-CH
P1
40.6±2.8
at theof the 2.1±0.1
deuterated molecularlines do3OHcentroid velocities
A-CH
OH
S
5.1±0.8
22.4±0.8
not 3follow a unique enhancement trend from S to P1. The
E-CH3OHS
1.3±0.5
19.3±1.5
diversityofthemeasuredD-fractionenrichment
is discussed
A-CH3OH
Soff
2.9±0.4
24.2±1.2
later3OH
in Sections 3.2
E-CH
Soff and 5.5.
1.2±0.0
16.0±1.1

4.1. Dust TemperatureLTE
and Density Maps14−2

Ncol(10 cm )Trot(K)

Nrot(1014 cm−2)

Following the iterative SED ﬁtting procedure described in

0.3±0.0
Lin
et al. (2017), we19.3±6.5
establish a reliable0.8±0.7
blackbody model and
0.1±0.0
14.3±3.6
0.2±0.1
obtainthe dust opacity
index β map at anangular resolution of
0.1±0.0
13.0±2.9
0.2±0.1
2• H CO、CH3OH→Tkin>16 K•

22″ using the archival Herschel PACS 70, 160, Herschel
4.9±0.4a
SPIRE
250 maps, the350aμm map by2.9±2.1
combining
Herschel
23.4±7.8
2.8±0.1
NH3→Tkin>15-20 K
SPIRE
as well as the 850
μm map bya1.1±0.1and CSO/SHARC-II,a20.1 ± 5.8
0.8±0.5
combiningthe deconvolved
Planck 353
GHz and JCMT0.9±0.1a1.0±0.1 data (Section
SCUBA22.2). Then, assuming
19.2±0.5
0.7±0.5a the β map has
0.9±0.1
no local variation from 22″ to 10″ resolution, we apply theMonte Carlo method to ﬁt the continuum data from Herschel
Note.
PACS at 70 μm and from CSO/SHARC-II at 350 μm. At ana
Estimated without separating A-CH3OH and E-CH3OH.
3.2. Line Spatial Distribution Maps
angular resolution of 10″, we obtain the maps of H2 column＋+
density N(H2) and dust temperature T(dust) simultaneouslyの低いJ（J=1、2）の準位は非熱的に励起されている
2H 、HCN、HNC、HCO
To Ncompare
the spatial distribution of deuterated
and−3
toward
P1–S.
detailed
is also given inhydrogenatedmolecules, (∼19
the line
arealong
integrated
than
the dust temperature
K, intensities
Figure 3(II))
the over) might
be inThe
non-LTE,
weﬁtting
use theprocedurelarge velocity(>106 cm
A.
CH3OHについてLVG（large
gradient）近似より求めた柱密度と、LTE＋RD（rotational
diagram）
ﬁlament
elongation(seerange
also in(listed
Wang 2018),
with P1(20velocity± 3 K)
gradient Appendix(LVG) approximation
to ﬁt the p-H2CO, A-CH3OH,
the samevelocityin Table5),14
andthey are
As
shown
in
Figures3(I)and(III),
P1
andS
cannotbe
and E-CH3OH lines individually.
slightlyS (143 K). 2.OnTotheother hand,
shown warmer
as colorthan
maps
in ±
Figurecomparethe spatial
shows
the
columndensitymaximum
toward“Soff”
the statisticalequilibrium
radiative
transferresolutioncode
NH
as sphericalsources
at a linearof 0.2 pc;
3から求めた柱密度はconsitentcorrelation
between the dust and gas distribution, the Usingmodeled
16−2cm ),emission
higher than
towardasS white
and P1contours
by a factor(∼10
RADEXinstead,(van derthey
Takshow
et al. 2D2007)
and a related
solverGaussian
structuresin (Fujun
the plane of the sky.
continuumis thatoverlaid
onofeach of
18
)
as
well
as
the
MultiNest
algorithm(Feroz& and column
2 and 3, respectively (Figure 4(IV)), which is opposite to theDu’s myRadex
Therefore, instead of extracting the temperature
P1とSでの重水素化率の違いはリアル
the line maps.
Because P1 and S are dark at wavelengths•••

trend found with the dust column density (Figure 3(IV)).

Hobson 2008; Feroz et al. 2009, 2013), we derive theThe chemical structure of young high-mass star-forming clumps: (I) Deuteration

The Astrophysical Journal, 883:202 (23pp), 2019 October
1
1,2,3
S. Feng, P. Caselli4, K. Wang5, Y. Lin6, H. Beuther7 and O. Sipilä4

Feng et al

P1（老）
S（若）

•
•
•

Figure 5.
density ratio (relative abundance) maps＋
forthe deuterated isotopologues with respect to their hydrogenated isotopologues. The column densities of
NColumn、HCN、HNCよりも高い（先行研究とconsistent）
2H＋の重水素化率は数％で、HCO+
13
HCN, HNC, and HCO are converted from those of H CN, HN13C, and H13CO+ by assuming 12C/13C∼42.9. The black contour of 870 μm continuum emission
starts from
10σ and increases in steps of 10σ (σ = 0.042 Jy beam−1). The gray line along the ﬁlamentary elongation as well as the position marks on it are the same as
重水素化率はP1よりもS（温度が低く、密度が高い）の方が高い（先行研究とconsistent）
n Figure 3. The pixels are blanked where the lines used for calculation have <3σ integrated intensity. The angular resolution is shown as the black circle in the bottom
eft corner.
NH3の水素がひとつ重水素化した分子（気相とダスト表面の両方で形成される）の割合はP1とSで変わらないThe chemical structure of young high-mass star-forming clumps: (I) Deuteration

The Astrophysical Journal, 883:202 (23pp), 2019 October
1
1,2,3
S. Feng, P. Caselli4, K. Wang5, Y. Lin6, H. Beuther7 and O. Sipilä4

Feng et al.

P1（老）

S（若）

2019 October 1

Feng et al.

Figure 6. Maps for the C18O column density and depletion. Panel (I): C18O column density and depletion maps, derived by using the kinetic temperature of the gas
and H2 column density maps (Figures 3 and 4). The angular resolution of 11 8 is shown in black in the bottom left corner. C18O (2–1) shows >8σ emission
σ = 0.11 K) at the system velocity (79.5 km s−1) toward all pixels on the map. Panel (II): C18O depletion proﬁle along the directions of a–b (in black). The marked
positions are the same as those in Figure 3.

hin at pixels where S/N>4 for the following reasons: (1)of CH3OH agrees with the Tkin map derived from p-NH3+(Section 4.3), we estimate the CH2DOH column density by
The main hyperﬁne line of N2H (1–0) has a small opticaldepth toward P1 and S (τ=0.1–0.3). (2) The 1–0 lines ofassuming that its only detected line is optically thin, and that13
C isotopologues show a homogeneous intensity ratio with
the Trot map derived from the CH3OH lines can be applied15
respect to their less abundant isotopologue lines HC N (1–0),
to CH2DOH. The map of CH2DOH relative abundance ratio
H15NC (1–0), and HC18O+ (1–0) in the entire P1–S region (seewith respect to CH3OH, shown as χ(CH2DOH/CH3OH) in
15
18Oはdepletionしている（fD~10）
P1とSのいずれでも、Che •discussion
in Section 5.4). (3)Compared with the N or
Figure 5, indicates an enhancement peak at Soff.
18
13
O lines, the C lines show a higher S/N toward each pixel.
• 70 μmで暗い雲に対するパーセクスケールでのフォローアップ観測でも確認されている
The hyperﬁnesplittings of N2H+ (1–0), H13CN (1–0),
5.4. Error Budget(2–1),and DCN(1–0) are marginallyat our
H13CN%）resolvedが観測された（高いところでは~
40 %）3OHの高い重水素化率（>10• CH
velocity resolution, and blended into three Gaussian peaks
During our observations with the EMIR receiver, the
重水素化率のピークの位置とCOのdepletionのピークが一致• 1). For these, we derive the excitation temperature(Figureuncertainty in the absolute ﬂux calibration19,20 was <10%single line using the HFS method. Moreover, we(TΔF) for• each
(Carter et3OHがダスト表面で生成される）
al. 2012). Comparing different line-ﬁtting methods,
モデルの予測と一致（COがdepletionを起こすと直ちにCH+
detected two low-J transitions (2–1 and 1–0) of N2D and
we found that the uncertainty in the integrated intensity