The Star Formation Newsletter#314, 01-10

島 和宏#01: Revealing the dust grain size in the inner envelope of the Class I protostar Per-emb-50#04: Magnetic Field Structure of Dense Cores using Spectroscopic Methods#10: The Orion Region: Evidence of enhanced cosmic-ray density in a stellar wind forward shock
interaction with a high density shell

01

https://arxiv.org/abs/1901.05021

Dust is big in disks

μm ~ mm のダスト成長がいつ起きるか？

0.1μm

1m

1mm

10

102-4km(片岡さんのスライドから)

dust opacity5

amax=1 µm, κabs
Class II ではすでにmmサイズになっている
amax=1 µm, κsca
amax=100 µm, κabs
amax=100 µm, κsca

410κabs,sca [cm2/g]

1km

310102scattering> absorption

110100-110-210-31010

0

110(arXiv:1412.1162)
2310λ [µm]Akimasa Kataoka (NAOJ fellow)

10New! Class I では100μm以下だという観測結果

104

NOEMA109

Nov 6 2016
Nov 12 2016

New!

0333+321
0333+321

3c454.33c454.33c84

対象: Per-emb-50(a Class I protostar in NGC1333 at 293pc)
C. Agurto-Gangas et al.: Revealing the dust grain size in the inner envelope of the Class I protostar Per-emb-50

Fig. 4. Spectraline. The black
to grain proper

2.7mm
Fex=0.52
even if not v
therefore thi
related to theat these very
ranges at bo↵env bigger thcertainty in ↵shown in Appfor 2.7 mm d
We present ↵baseline in Fof the dust op
values found) Continuum map of the NGC1333 complex at 1.1 mm wavelength. (Right) Zoom-in to the direct enviroment of Per-emb-50. The map
om the Bolocam survey at the Caltech Submillimeter Observatory (CSO) by Enoch et al. (2006).

continuum map (1.1mm)

eration during the first track, and 6 antennas (6C) inor the second. Antennas were based on stations E10,, N20*, E18, N11*2 , N17 and E04. The projected
were from 7.8 k and 102 k .
0 was observed for hour angles from -5.8 to 1.5 h forom -5.3 to 1.4 h for 6C. In total we spent 9 hours
0333+321 was used as phase/amplitude calibrator.
s LkHa101 and MWC349 were used for the flux calhile the quasars 3C84 and 3C454.3 were used for thealibration. We consider an absolute flux uncertainty ofotal bandpass for the 110 GHz continuum measureGHz. Data reduction and image synthesis were carng the GILDAS software (Guilloteau & Lucas 2000)
ocedure of MAPPING> Selfcal. The continuum map
s produced using natural weighting and the resultings 2.00 1 ⇥ 1.00 6 at P.A. 34.84 . The clean map has a rms
of 2.1 mJy beam 1 .

Fig. 3. Continuum map of Per-emb-50 at 1.3 mm (SMA) and 2.7 mm

wavelengths. The synthesized beam FWHM is represented
観測: The Submillimeter Array (SMA) at 1.3mm (NOEMA)
as a white ellipse in the bottom-left corner of each map. For SMA andNOEMA data, the contours start at 76 mJy beam and 20 mJy beam ,respectively, (MOEMA)
and both increase in 25% intervals.
the IRAM NOrthern Extended Millimeter Arrayat 2.7mm

解析: working on the visibility domain

11

Using the fluxes between the u–v ranges 47–80 k at 1.3 and2.7 mm, we obtain therefore the average value ↵mm in theunresolved disk, which is ↵disk =1.71±0.3.
As shown in the Fig.2, an excess of emission is present at shortbaselines (<47 k ) at 2.7 mm and 1.3 mm, which correspondto physical scales of 1500–3000 AU. The excess values atthese baselines, after subtracting the disk visibilities, are:

モデル: extended envelope + unresolved disk (point source)
Article number, page 4 of 17+ dust opacity + radiative transfer

These prelim
previous studyounger souret al. 2014; K
tigate possibl
radiative tran
account possi
Jeans regime

4. Modeling

In order to mservations, w
ditions of theproperties of

C. Agurto-Gangas
et al.: Revealing the dust
grain size in the inner envelope of the Class I protostar Per-emb-50
thedust absorptionopacity

ダストの最大サイズごとのモデル

as et al.: Revealing the dust grain size in the inner envelope of the Class I protostar Per-emb-50-> best ﬁt を探す

よく合うFig. 7. Left panel shows the dust C.
absorption
opacity as aetfunctionof wavelength
for grain
distributions
characterized
a 3.0 andAgurto-Gangasal.: Revealing
the dust
grainsizesizein the innerenvelopebyof(a)the/ ClassI protostar Per-emb-50
increasing maximum grain size (amax ). Right panel shows the dust opacity spectral index ( ) calculated between 1.3 mm and 2.7 mm wavelengthsas a function of the maximum grain size. Black solid line is the env value from the parametric model and the black dashed lines are the uncertainties.
Green region shows an upper limit for amax in the envelope of Per-emb-50.

結果:

Table 7
Derived envelope masses

ModelM1envelope mass is 2.2 M . Additionally, since we have evidenceof an outflow in this source (Stephens et al. 2017), we included
an outflow cavity with an opening angle of 30 (M. Dunham,priv. comm.) and a lower density of 1.0 ⇥ 10 30 gr cm 3 for theregion inside the cavity and the background.

amax (µm) Menv (M )0.1,10
1.73
50
1.53
100
1.15
4.3.3. Backwarming effect
300
0.23
1000
0.34
The e↵ects of the envelope thermal emission on disk (i.e., backes as a function of theM2
deprojected
mm data while right panel shows 2.7 mm data.
0.1 baseline.
1.22Left panel shows 1.3warming) have been studied in di↵erent environment, as in the10,50 We show
1.38 a variety of models
ertainties due the flux calibration.
maximumgrain
sizeL1551
in thecasewithof theaheavily
embeddedsourceIRSenvelope
5 (Butner ofet al.
1000.85m. At the bottom of each panel are the residuals between the data
and the best model.
1994).
300
0.16
In the case of an envelope around a disk, the millimeter emis1000
0.29
sion of the disk increases. This is because the envelope acts as
Table 9a thermal cavity, not letting the temperature within the cavity
Notes. Envelope mass
within
8 800 AU radius
Fullcalculated
radiativetransfer
best fit models to fall below the temperature of the envelope wall. Therefore, asubstantial backwarming e↵ect on the disk can be present depending on the optical depth and geometry of the cavity.
profile is defined by:
Description
Best-Model
1 Best-Model
2 Miotello et al.
In theprevious envelopemodeling following
01Fig. 8. Real 2part of the visibilities as a function of the deprojected baseline. Left panel shows 1.3 mm data while right panel shows 2

Discussion

The eﬀects of Backwarming

envelope が熱浴になる

Fig. D.1. Temperature structure in cylindrical coordinates of two cases: (top left panel) 25 AU disk withadisk
cm and (top right panel) a 25 AU
disk
max =1 はそこまで冷えない
env
disk with a 1.3 M Ulrich envelope structure and grain sizes with amax =100 µm. (Bottom right panel) is the case of a 1.3 M Tafalla et al. envelope
profile with aenv
max =100 µm heating the 25 AU disk. 2D temperature contours are presented in black lines.

Article number, page 17 of 17

04

https://arxiv.org/abs/1901.09537

The Astrophysical Journal, 868:51 (19pp), 2018 November 20

Myers, Basu, & Auddy

分子雲コアの磁場構造の観測
Zeeman detection
dust polarization
Faraday rotation(Myers et al. 2018)

Figure 8. ALMA 1.3 mm ﬂux and polarization image of VLA 1623 protostars
A and B, the extended disk around VLA 1623A, and SFF model magnetic ﬁeld
lines threading a tilted model spheroid. Black segments are e-vectors, blue
segments are b-vectors. The black ellipse shows the outline of the modelspheroid. From Sadavoy et al. (2018).

Figure 10. Closed curves: magnetic ﬁeld strength, which exceeds thebackground ﬁeld strength by factors 1.5, 3, 6, 12, and 24. Open curves: ﬂux
tube lines as in Figure 1. The peak density exceeds the background density
n0 by a factor of 300. The scale bar is based on temperature 10 K andbackground density nu=300 cm−3. With these parameters, the scale length isr0=0.011 pc.

磁場の強さはどうやって観測するか？

(popular)

Davis-Chandrasekhar-Fermi (DCF) methodNew!

S (from SW to SE), and W (from SE to NE). The polarization
directions agree well with the ﬂux contours in the N and S
portions of the map, where the polarization directions havecore ﬁeld structure (CFS)
model
approximateline symmetry about an axis through the protostar
VLA 1623A, and less well in the W region, where the polarization
directions are highly ordered but depart from line symmetry.

FieldStructure of Dense Cores
NH3 (J,K) = (1, 1) and (2,2)データを使用

3gas kinematics

pcs = kT /µmHpvN T / 2 ln 2
NT =<latexit sha1_base64="DI0W/WLOwJL5tXkxQ85Q5yVdvyU=">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</latexit><latexit sha1_base64="CaxSGVwRBXEbCJCX9tJOriH4aAs=">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</latexit>

Field Structure of Dense Cores

対象:Figure
1. Integrated intensity map of the NH3 (1, 1) linefor the L1688 region taken from Friesen et al. (2017). The
B18in Taurusbeamsize andscale bar are shown in the bottom left andrightcorners1333
respectively.
The cores studied in this paper
NGCin Perseus
are indicated by name.
L1688 in Ophiuchus
Orion A NorthNH (1, 1) line for the L1688 region in Ophiuchus, along
3with the marked cores that are studied in this paper.
観測:
Themap includes four prominent isolated starless cores(including H-MM1 and H-MM2) lying on the outskirts
the Green Bank Telescope K-bandof the cloud, plus more than a dozen local line width
minima in the main cloud (mainly in the south-easternpart in regions called Oph-C, E, and F). Many of thesecore

3Figure 2. Velocity dispersion profiles of the H-MM1 corecalculated using the NH3 (1, 1) and NH3 (2, 2) spectral line
cubes from the GAS survey of the L1688 region of Ophiuchus(Friesen et al. 2017). Here cs and NT are calculated fromannularly averaged spectra, by first aligning the spectra invelocity with the help of the vLSR map. The transonic radius(where cs = NT ) of H-MM1 can be identified as r0 ' 8600
(0.05 pc at the 120 pc distance of Ophiuchus).

for the Greenbank K-band Focal Plane Array Receiver(Masters et al. 2011; Friesen et al. 2017)1 .
The stacked NH3 (1, 1) and (2, 2) spectra were analyzed using the standard method described by Ho &Townes (1983) and, recently, by Friesen et al. (2017).
transonic
radiusFigureVelocity
profilesof thecore
In this 2.
method,thedispersion
velocity,line width,
theH-MM1
total opticalculated
NH3 (2, 2) ofspectral
3 (1, 1) andcal depth,using
and thethe NH
excitation
temperature
the (1,line1)

he transonic radius, within whichsourcesthe nonthermalline width, for examself-gravity
isofdominant.
presumed
to be dominant.
sumed
to be
model
the nonthermal
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weTheassumeAlfvénic fluctuations
rmal motions
we assume
Alfvénicresolved
infallmotions.
Alfvénic
New!
ations.
means possiblethat we addiignore possible addians
thatThis
we ignore
sources of theline width, for examnonthermalline nonthermal
width,forexamCFSNT
model
B fluctuations
nresolved
infallmotions.
TheAlfvénicotions. The Alfvénic fluctuations=,(5).6, with the distribution having a mean and standard
eviation of 0.57 and 0.16, respectively. Overall, the asDCF method
umptions of . 1 at the transonic radius and µ & 1vAB
B
B the core
withinconsistent.
Furthermore,=, are mutually(5)p=,(5)v
Bis defined by v ⌘ B/( 4⇡⇢).
speedvthe AlfvénB
p A
in directionofp by v ⌘value
heaverageinteriorof⌘✓=0.12
KandoritheAlfvénspeed
isdefined
B/(4⇡⇢).
directlyleads
d is definedby v to⌘ B/( 4⇡⇢).
directly leads tothe polarization vectors
t al. (2017) forthep starless core Fest 1-457 lies within
pp4⇡⇢
.
(6)
B = B = 4⇡⇢.
(6)
NT= range
4⇡⇢ . of estimated(6)
hevalues of inside the transonicso use Equation (5) to get(5) useto getEquationso(5)to predict
getcore-average ﬁeld strengthscaleofadius
ofa ﬁner
H-MM1(seeFigure7).
pNTA<latexit sha1_base64="m1hPVAD5dRpQ6UrJVhiOYwZjQag=">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</latexit>

{NTA

A

A

NT

NT

( NT )cpB(r)=4⇡⇢(rc )( NT)cal. cﬁeld structure
uddyet=4⇡⇢(rc )( NT(7))c p

B(rc ) =500

B (µG)

exge
renareerd
er.
%tynonhe2),4⇡⇢(rc )H-MM1(7)1 = 1/2
2 = 1/2
1 = 2/3400

2 = 2/3

300
200
100
00.00

0.01

0.02

0.03

Radius (pc)

しか計算できない(7)

0.04

0.05

10

https://arxiv.org/abs/1901.01764

arX

hundred OB stars, and two giant molecul
A and Orion B (Pillitteri et al. 2016).
observations by AGILE and Fermi-LAT In recent years, an important survey
XMM-Newton
in the Orion region has
Bremsstrahlung and proton-proton
emissionof InterStellar
several Young
Stellar Objects
inverse-Compton scattering on theRadiation
Field (YSO)
overlappingtheMCOrion
Abutprobabl
CMB photons などなど
Orion This shell is shaped as
teriM.Cardillo:et al. 2016).
around -Ori, a blue super giant B0.5 I
240-280 pc from us, with an estimated ag
tions in the near- and far-IR, especially inwith the analysis of new XMM-Newton dwinds
this shell is closer than the Orion A MC,
ble with that of -Ori. Consequently, the(B0.5)
within it could havebeen triggered by thethat has swept up the shell, a hypothesis cOrion A 分子雲

γ-ray excess

CO mapFig. 1. Left: Ring of -ray excess detected by AGILE. Right: CO map(Dame et al. 2001), which reveals the star formation shell discussed byPillitterial. (2016); thecontour levels from -ray data are shown in
γ-rayet excessの起源は？
black. The figure is from M18.

New! stellar wind forward shock interaction with a high density shell

Fig. 2. AGILE -ray spectrum obtained withhood analysis centred on (l, b) = (214.4, -18.

pression ratio r sh = 4. However, a cut-o↵ at such a low energy,
together with loss-limited energization, implies a certain degreeof covariance in the spectral index values. In fact, models deκ-Ori が約1Myr前にシェルを形成 -> 6 pcまで膨張
veloped with a spectral index in the range 3.5 < ↵ < 5 turnout tobe equally
physicallywith only small varia現在:
slow
Forward
Shockconsistent,(~10 km/s)
tions of the other parameters involved. In Fig. 3 we show theSpectral Energy Distribution (SED) resulting from our best-fit
best-ﬁtre-acceleration
model.re-acceleration model SED

plain the -ray excess sparameters. However, w
ther contribution from f
Keeping the physica
model, we calculated an⇠CR such that the total and acceleration, is com
value we found, ⇠CR ⇠freshly accelerated CRsmarginal compared toshown in Fig. 4.

Secondary electrons からの放射が寄与

Fig. 3. AGILE (red) -ray points plotted with -ray emission from pion
decay (blue line), from primary Bremsstrahlung (cyan dashed line),

02

https://arxiv.org/abs/1901.05029

03https://arxiv.org/abs/1812.04040

05

https://arxiv.org/abs/1901.03713

06

https://arxiv.org/abs/1901.02959

07https://arxiv.org/abs/1812.04043

08https://arxiv.org/abs/1901.02371

09https://arxiv.org/abs/1901.06475