The Star Formation Newsletter#301, 22-28
島和宏

#22 The evolution of young Hii regions
I. Continuum emission and internal dynamics

http://arxiv.org/pdf/1712.04735(< 0.01 pc)
ALMAで 9つの hyper- and ultra-compact HII regionsを観測-> 質量降着による大質量原始星進化の最終段階

を調べる(もしくは大質量星の pre-main-sequence 段階)
Red MSX Source (RMS) Survey が見つけた600個のHii regionのうち- ATCA & VLA でcompact (r<5”)- bolometric luminositiesが10^4 Lsun より大きいもの- 距離が3 ~ 5.5 kpc 以内に位置しているもの(expanding / rotating / infalling)
Hii regionでガス (ionised & molecular gas) の動きがどうなっているか？
-> high-resolution(~0.5”)で観測 (ALMA Band 6)- radio recombination line H29α
- molecular emission (CS, CH3CCH)- 256GHz continuum emission

G309.89+00.40

13:50:35.54

G330.28+00.49
G332.77 00.01
G336.98 00.18
G337.63 00.08
G337.84 00.37
G339.11+00.15

16:03:43.28
16:17:31.13
16:36:12.42
16:38:19.02
16:40:26.68
16:42:59.58

61:40:21.4
57.6
0.69
Targets near G335 (6 regions)
51:51:45.6
93.5
0.71
50:32:35.7
95.6
0.62
47:37:57.5
75.1
0.63
47:4:50.7
56.5
0.61
47:7:13.1
40.4
0.62
45:49:43.6
78.2
1.68

0.62

6.17

0.15

0.53
0.46
0.47
0.46
0.47
1.11

87.19
87.62
90.00
90.00
89.07
84.79

0.13
0.18
0.13
0.12
0.18
0.51

Table 2: Summary of radio properties of the Hii regions and their host molecular clumps. The luminosity in Column 7 is that of theHii region, and the final column gives the radio derived spectral index. For the targets which were not detected in all of the ATCA
and VLA wavebands in Urquhart et al. (2007, 2009), no spectral index (↵) was determined.
Source NameRA
(J2000)G302.02+00.25 12:43:31.49
G302.49 00.03 12:47:31.76
G309.89+00.40 13:50:35.54
G330.28+00.49 16:03:43.26
G332.77 00.01 16:17:31.13
G337.63 00.08 16:38:19.02
G337.84 00.37 16:40:26.68
G336.98 00.18 16:36:12.43
G339.11+00.15 16:42:59.58(a)Integrated Flux at 6 cm

Dec.
(J2000)62:36:13.7
62:53:59.6
61:40:21.4
51:51:45.9
50:32:35.7
47:04:51.0
47:07:13.1
47:37:58.0
45:49:43.6

Distance(kpc)
4.26±0.98
3.39±0.40
5.41±1.27
5.45±0.56
5.67±0.57
3.82±0.43
2.98±0.47
4.67±0.41
4.96±0.40

Log[Mclump ]
(M )
2.76
2.61
3.12
2.95
3.22
2.88
2.55
2.51
2.93

Table 3: Spectral Setup of the observed regions. The primarytargetted species of each spectral window are listed, with thenote that spectral windows 1 and 2 were combined to get thefull CH3 CN (J=12-11) k-ladder.
SPW
1

Freq
Species(GHz)
257.403 CH3 CN

N. Chan
3840

Vel. BW(km/s)
545.8

Vel. Res.
(km/s)
0.284

Log[LBol ]
(L )
4.16
3.75
4.40
4.13
4.16
4.01
4.59
4.43
4.24

Radio Size
(00 )
2.24
2.07
1.79
2.00
1.14
2.20
3.32
1.47
1.98

Flux(a) 6 cm
(mJy)
59.5
23.4
1.2
44.9
24.6
31
11.1
18
42.9

↵
0.03
0.03
···
0.08
···
0.01
0.63
0.52
0.04

and their implications are presented in follow-up papers. In thiswork, we focus on the continuum emission, ionised gas observed
within the Hii regions, and some of the small scale molecularemission (in CS and CH3 CCH) surrounding the Hii regions to
put the analysis of the ionised gas into context. Full analysis of
the molecular environments and the chemistry of these regions
is left to future work (e.g. Klaassen et al. in prep, van der Tak et
al. in prep).

H29αintegrated intensity(moment zero)

256GHz continuum
red: 5GHz
core: yellow

intensity weighted
velocity(moment one)“bulls-eye”-> infallingclumpiness
Jenas Length~2000 AU
(100K, 10^7/cc)< core separation

RRLs
H29α spectra
fit by Gaussian(no Lorentzian)

33Msun(@20K)

CS
no emission-> destroyed

VLSR = -37.1 km/s
Line Width = 11.4 km/s-> ne < 5x10^7 /cc(upper limit)
Fig. 1: Continuum, H29↵, and CS emission from G302.02. The top left panel shows the 256 GHz continuum in colour scale inwhich the 5 GHz emission is shown in red contours; the red contours in the other images represent this same 5 GHz emission forsimilar (to within 3 sigma of each other at 24.1 and 23.9 mJy/beam for the full and 12 m only data, respectively), however in the 12
m only dataset, we recover only 80% of the flux present in the full (i.e. including ACA) dataset.
Figure A.2 shows how the amplitude of the emission varies as a function of uv distance. Of note here is the overlapping uv
distances of the three configurations and generally consistent fluxes between configurations. The data are sampled well enough inthe overlap region to allow for proper combination of the datasets.
Appendix A.3: H29↵ emission

H29↵ was detected in most of our sources and on small enough scales to not require the use of ACA data. It was only detected in
the stand-alone ACA data for G302.02, which is the target with the brightest and most extended H29a emission. However, as shownin Figure A.3, the 12 m array data recover all the flux so it was not necessary to combine this data with the ACA data.
Table A.2: Clump positions, Areas, Derived Fluxes, Masses, and Column Densities
ID Number

1
2
3
ID Number
4
5
6
7
8
9
10
11
12
13
1
2
3
4
5
6
7
8
9
10

Peak RAPeak DEC
Area
Flux
Clump Mass (M )2(h:m:s)(d:m:s)(arcsec ) (mJy) (20 K) (50 K) (100 K)
A&A
no. EYH_Internal
3
G302.02 (1.00e+07
cm proofs:, 70.0manuscriptK)
12:43:31.50 -62:36:13.36
4.63
62.08
25.37
8.37
3.94
Table
A.2:
continued.
12:43:31.54 -62:36:17.68
13.45
81.48
33.29
10.99
5.17
12:43:30.71 -62:36:19.92
5.22
23.92
9.77
3.23
1.52
Peak RAPeak DEC
Area
Flux
Mass (M 0.29)
12:43:29.87-62:36:22.00
0.94
4.57
1.87Clump0.62(h:m:s)(d:m:s)(arcsec(20K) (50K) (100
12:43:32.33-62:36:16.80
0.75 2 ) (mJy)
3.01
1.23
0.41
0.19K)
12:43:30.92 -62:36:21.12
1.5
6.01
2.46
0.81
0.38
12:43:32.17 -62:36:18.32
1.39
5.57
2.28
0.75
0.35
12:43:30.41 -62:36:18.72
0.38
1.29
0.53
0.17
0.08
12:43:30.36 -62:36:21.28
0.3
0.83
0.34
0.11
0.05
12:43:31.23 -62:36:20.40
0.16
0.43
0.17
0.06
0.03
12:43:30.30 -62:36:22.08
0.09
0.23
0.09
0.03
0.01
12:43:32.52 -62:36:15.60
0.2
0.52
0.21
0.07
0.03
12:43:31.89 -62:36:14.40
0.11
0.27
0.11
0.04
0.02
3
G302.48 (1.00e+07 cm , 70.0 K)
12:47:31.80 -62:54:0.84
4.31
93.89
24.3
8.02
3.77
12:47:31.76 -62:54:3.32
6.84
73.15
18.93
6.25
2.94
12:47:31.97 -62:54:0.92
2.74
27.3
7.06
2.33
1.1
12:47:32.59 -62:53:57.72
1.5
8.32
2.15
0.71
0.33
12:47:31.31 -62:53:57.00
0.14
0.47
0.12
0.04
0.02
12:47:32.01 -62:53:59.32
0.2
0.62
0.16
0.05
0.02
12:47:32.44 -62:54:1.56
0.49
1.47
0.38
0.13
0.06
12:47:32.70 -62:53:59.96
0.13
0.4
0.1
0.03
0.02
12:47:31.35 -62:53:52.76
0.17
0.51
0.13
0.04
0.02
12:47:31.21 -62:53:54.28
0.17
0.46
0.12
0.04
0.02

Log(Column Density)(20 K) (50 K) (100 K)
24.41
23.93
23.6
23.79
23.31
22.98
23.77
23.29
22.96
Log(Column
23.62
23.14 Density)
22.81
(20
K) (50K) (100
K)
23.45
22.97
22.64
23.43
22.95
22.62
Articlenumber,page
19 of 25
23.41
22.92
22.6
23.32
22.84
22.51
23.18
22.7
22.37
23.12
22.64
22.31
23.09
22.61
22.28
23.07
22.59
22.26
23.04
22.56
22.23
24.69
24.21
24.14
23.68
23.28
23.21
23.18
23.15
23.14
23.11

24.21
23.73
23.65
23.2
22.79
22.72
22.7
22.67
22.66
22.63

23.88
23.4
23.33
22.87
22.47
22.4
22.37
22.34
22.33
22.3

#23 Stellar mass spectrum within massive collapsing clumps
I. Influence of the initial conditions
https://arxiv.org/pdf/1711.00316
B1++, 4 AU

IMF の傾きは何が決めるか-> density と turbulence を変化させてシミュレーションした (RAMSES + sink)
1000 Msun のコア
0.75 pc (~10^4 /cc)
0.084 pc (~10^7 /cc)
M=7
M = 22
A&A proofs: manuscript no. 31522corr
A1++, 9 AU

A1+, 19 AUC1+, 2 AU

Γ~0thermal support dominant
B1++, 4 AU

Γ ~ -3/4

turbulent dispersionD1,
dominant
2 AU
B1+, 8 AU#24 THE TOP-SCOPE SURVEY OF PLANCK GALACTIC COLD CLUMPS:SURVEY OVERVIEW AND RESULTS OF AN EXEMPLAR SOURCE, PGCC
G26.53+0.17
http://adsabs.harvard.edu/pdf/2017arXiv171104382L

TOP-SCOPE: Plank Galactic Cloud Clumps (PGCCs) の low temperature dust を観測-> 星形成の初期段階~2000 clumps with 12CO(1-0) & 13CO(1-0)~1000 clumps with 850μm continuum emissions

G26.53+0.17 (G26)
a filamentary infrared dark cloud
The TOP-SCOPE survey

11

(K)
HCO+ J=1-0
H2 CO 21,2

(K)

(K)

(km s

) (km s) (km s3.56 0.74 15.70 11.69 19.60

48.98

1.04

0.15

49.07

0.93

0.06

The TOP-SCOPE survey

11,1 2.21 0.79 15.44 12.03 19.54

enough energy themselves to drive the envelope
ansion.
he virial mass of the clump MM6 considering turbuRV2vir
support can be derived as M
=
210(
)(
)
1
M
pc km scLaren et al. 1988; Zhang et al. 2015), wheres the radius (1.15 pc) and V is the linewidth
2 km s 1 ) of C18 O (1-0). The virial mass is
00 M , which is much smaller than the clump mass
100 Msun ), indicating that the whole clump may bein collapse. Therefore, the expansion revealed by
O+ J=1-0 and H2 CO 21,2 11,1 lines should be very
lized.
gure 22 shows a cartoon to describe the PGCC
based on the results from the present data. Our
ngs of G26 are: (i) The G26 filament may be
med due to large-scale compression flows evidenced
the temperature and velocity gradients across its
l cloud; (ii) Sub-filaments in G26 have di↵erent
cities and may interact with each other; (iii) The
ral massive clump where massive stars are forming
still accrete gas along sub-filaments; (iv) The
sive clump in whole may be still in global collapse
e its inner part seems to be undergoing expansion)
25

Figure 22. This cartoon shows the environment of PG
G26.53+0.17. The main gas filament is shown in gre
The SCUBA-2 filament is shown in yellow. Other sm
sub-filaments
are shownin red,and blue. PG~6200 Msun,~12pc,(500green,
Msun/pc)
G26.53+0.17 is located in a parent cloud with veloc
and temperature gradients along the east-west directi
The central clump MM6 (dashed ellipse) may be stillcollapse while its inner part (color filled ellipse) is undergo
expansion due to outflow feedback from the protostars. T
zoomed-in picture of the central clump is shown in the upp

nMedian RangeDp-value p-sig.
#25
fingerprints
of hot Jupiter planet formation
8.0 Chemical
4.1/100.32 0.03
0.31
42.7
12.5/95
0.16 0.64
0.13
http://arxiv.org/pdf/1712.01035
2.4
0.1/110.28 0.09
0.03
1.07
0.83/1.41
0.09 0.99
0.20
Hot Jupiterがどうやって出来たか
5656
5025/6704
0.19 0.41
0.13
9 -7.49-73.53/29.03 0.25 0.15
0.12-> in situ
formation
v.s.0.37
migration
7.61
6.6/8.57
0.24
0.05); 45 (G); 31 (K)D); 7 (R)

#26 Shifting of the resonance location for planets embedded in circumstellar disks
http://arxiv.org/pdf/1712.04178

F. Marzari: Resonance shifting

Crit. Arg. (deg)ourmodels the planets are also in apsidal resonance and the frediscポテンシャルを含めて2つの惑星の軌道共鳴を計算
350
quency of the apsidal longitude of the outer planet matches thatof the inner one. As a consequence, the secular system responds
300
in a unitary way to the disk perturbations.
6
No disk
1 MMSN
5 MMSN

Fraction of cases

5

250
200
150
100

4

50
3
0
2
1
0

7.9

8

8.1
8.2
8.3
Semimajor axis (au)

8.4

8.5

Fig. 3. Distribution of the initial semimajor axes of the outerplanet of a massive pair (m1 = 1M J m2 = 1MS ) trapped ina 2:1 resonance for diﬀerent values of the disk gas density Σ.
For higher densities the resonant region is shifted inwards. The
volume of the phase space is also reduced and the size of theresonance region shrinks. This is revealed by the smaller area of
the Gaussian curve fitting the histogram.
There is also a shrinking of the volume in the phase space
where stable resonant systems (at east over 1 × 105 yr) can befound for increasing Σ. This reduction is 98% for Σ = Σ

0

0.4

0.8
Time (Myr)

1.2

#27 Planetary-like spirals caused by moving shadows in transition discs
http://arxiv.org/pdf/1712.09157

原始惑星系円盤のスパイラル構造はどうやって出来たか-> 惑星がなくてもできるのではないか
shadow を考慮したシミュレーションでもスパイラルができた
The Astrophysical Journal Letters, 798:L44 (4pp), 2015 January 10
The Astrophysical Journal Letters, 823:L8 (6pp), 2016 May 20

includes a blackbody radiative cooling. The code solves theNavier–Stokes, continuity, and energy equations on a staggeredmesh in polar coordinates (r, f). For detailed description of thecode see Masset (2000) and Baruteau & Masset (2008).
2.1. Code Units and Initial Setup
The simulations were run in code units, assuming the central
star mass, M0 = Må, and r0 = 1 au, as the units of mass andlength. The code unit of time, t0, corresponds to the orbital
period at r0 divided by 2π, that is t0 = (GM r03)-1 2 . The
gravitational constant is G = 1 in code units. The temperatureunit is GMåμmp/(kBr0), with μ being the mean molecularweight (μ = 2.35 in all our simulations), mp as the proton mass,
and kB as the Boltzmann constant. We adopt two values for the
disk-to-star mass ratio, q = 0.25 and 0.05.
Figure 1.TheSchematic
view with arbitraryof theparametricmodel
computational
domain orientationin physicalunits
extends
frompresented
inSection2.
The
centralstar
isplacedattheorigin.
The
outer
disk
lies
= 400
logarithmically spaced radial
r = 10–150 Marion
au over nr etal.inclination(2015)
in the x–y plane. The angle
α is the relative
between the midplane ofequallycells.
The
grid
samples2π
inazimuthwith
nf = 800
the outer disk and the plane of the inner disk. The dust mass density
distribution
is renderedallowedintofalse
outﬂowat theof the spaced
inner disksectors.
and outerGas
diskmaterial
sections arecolor. The
gapdisk
isedges.
shown devoid of material for simplicity. The inner disk is scaled up in size andTheinitialdensity proﬁle scales with r−1:
density forbettervisualization.

Marino, Perez, & Casassus

with Rs = 148 AU and where the azimuthal contrast in surface
et al. arateThe volume densityMontesinos
density isHeating
set to c = 10.0.
follows withstandard vertical Gaussian distribution:)
2 *Σg (r, φ)zρg (r, z, φ) = √
exp −
,
(5)
2H 2
2π H
with H (r) = 20.0(r/(130 AU))1.17 . The exact value of thisflaring exponent is not well constrained.
This parametric model also includes the effect of dust
trapping, following the procedure described in Birnstiel et al.
(2013) and Pinilla et al. (2012). However, the bulk of the opacity
in the H band is driven by particles well below the sizes required
for efficient aerodynamic coupling, and so the effects of dust
trapping in the outer disk are not relevant to this report. The
runs detailed in Section 3 confirm that the outer disk is opticallythick at the H band and that the scattered light does not trace thecrescent shape seen in the submillimeter.
2.1.1. Emergent intensities

Figure 1. Initial proﬁle for the stellar heating rate per unit area Qd+(r, f ) for a
3 shadows subtend 0.5 rad or 28°. 6. The plot is in log
modelwith radmc3d
Lå = 1 Le. The
We usefor radiative transfer computations (ver−1
scale with units erg s cm−2.

sion 0.38; Dullemond et al. 2014). Scattering and polarization
for the last scattering are treated with scatteringmatrices for our
5
Figure distribution
1 shows theinshadowsdustovera timescaleof 30
orbits.
different
species,each onewitha power-law

4Montesinos & CuelloFigure 2. Snapshots taken after 20 kyrs of disc evolution, of the pressure (top) and surface density field (bottom) for models withshadows rotating at diﬀerent periods: Ts = 1 (static), 5, 10 and 20 kyr.
Table 1. Set of simulations after 20 kyrs of disc evolution with shadows, for diﬀerent shadow’s rotating frequencies.

なぜスパイラルができるか

large pressure gradientsmall pressure gradientgasshadowgas
co-rotation point-> larger pitch angle-> small pitch angle

3

Guilloteau+1999#28 Morphology of the 13CO(3-2) millimeter emission across the gas discsurrounding the triple protostar GG Tau A using ALMA observatio

http://www.raa-journal.org/docs/papers_accepted/0225.pdf

ALMA でGG Tau Aを観測

GG Tau Ab1~ 0.38 Msun

-dust continuum-13CO(3-2)

GG Tau Aa~ 0.6 Msun

GG Tau Ab2~ 0.3 Msun

CO(3-2) emission across the disc surrounding protostar GG Tau A

n in multiple stellar system?

39the product of the disc thickness by the sine of the tilt angle.

0o

We estimate the thickness of the disc by comparing the value
dust disc tilt : 32°of the smearingof tilt
theinner edge of the disc map near the
gas
disc
:
35°
o
8 of the ellipse with its value nearN.T.
P.N. Diep90&o A. Dutrey et270al.,
major axis
the Phuong,minor axis.

180o
To 95% confidence level we obtain an
upper limit of 0.24 arcsec (34 au) for
the scale height H(r) at r=1 arcsec(140 au) where the Keplerian velocity
is ~3 kms−1; at 30 K, the soundvelocity is
0.5
kms−1
and
hydrostatic equilibrium implies
H(r) = 0.5/3 = 0.17 arcsec comparedwith the 0.24 arcsec obtained above.
6