THE STAR FORMATIONNEWSLETTER
No. 250 10 Oct. 2013
塚越崇 (茨城大)
25 Oct. 2013

The B1 shock in the L1157 outﬂow as seen at high spatial
resolution
Milena Benedettini et al.

• L1157 outﬂowのB1領域の高分解能観測 (shock region)• PdBI• CS, HC3N, p-H2CO, CH3OH at 2mm• 750AU resolution• 高速度成分 - いくつかのcompact component(HV bullet)• 低速度成分 - ジェット起因のcavity構造• CS強度比を使ってLVGで密度導出• 全体: (1E5)<n<1E6, HV bullet: 5E3<n<5E5 [cm-3]• 柱密度導出(LTE)とモデル計算(UCL̲CHEM)との比較• C-type shockで再現• HC3Nが高アバンダンス -> 4000K必要(~40km/s & nH2>1E4 cm-3相当)

B1

6Benedettini et al.

The B1 shock in the L1157 outflow as seen at high spatial resolution

3

B0e
B1a
B1c

L1157 outflow as seen at high spatial resolution

py
is
cy
e
e
nne
e
n
cal
d

Figure 2. Interferometric images of L1157–B1. The first contour and steps correspond to a 3σ level and are: 0.75 Jy beam−1 km s−1 forCS (3–2), 3 Jy beam−1 km s−1 for CH3 OH (3K –2K ), 0.54 Jy beam−1 km s−1 for p-H2 CO (202 –101 ) and 0.15 Jy beam−1 km s−1 forHC3 N (16–15). The filled ellipse in the bottom left corner represent the HPBW, the arrow indicates the direction toward the central
driving source L1157–mm.

CS(3-2)/CS(2-1)

spectrum of each transition produced summing the emission
measured at PdB in a circle of diameter equal to the HPBWof the IRAM–30m telescope, with the spectrum measured at
the single dish IRAM-30m (Gómez-Riuz et al. in prep). In
Fig. 1 we show the two spectra of the CS (3–2) line. We
found that the percentage of the missing flux depends onthe velocity: for the high velocity gas (v < - 6 km s−1 ) PdB
recovers 100% of the flux while for the low velocity gas (v >- 6 km s−1 ) the flux measured at PdB is ∼ 62% of the IRAM
flux. Similar percentage of missing flux is also found for theother observed lines HC3 N (16–15) and p-H2 CO (202 –101 )while for methanol is not possible to evaluate the missing
flux because the lines are blended. We performed the same
analysis for the CS (2–1) line previously observed with PdB(Benedettini et al. 2007) with the same CD configuration
but a slightly higher value of the shortest baseline (19 m),
resulting in a similar value of the largest sensible structure(14"" ) and spatial resolution (3.11"" × 2.79"" ) of the 2 mm observations. Unlike the case of the CS (3–2) transition, for

the CS (2–1) line the flux filtering affects all the velocities(see Fig. 1). In particular, for the high velocity gas (v < - 6
km s−1 ) about half (∼ 50%) of the IRAM flux in the (2–1)
line is missed in the PdB spectrum while for v > -6 km s−1
a similar percentage (∼ 57%) of filtering is measured in the
two lines. However, the largest sensitive structure for the CS(2–1) line is similar to the value of the CS (3–2), therefore
the difference in the missing flux indicates that a consistent part of the emission of the CS (2–1) line comes fromextended (>14"" ) structures also for high velocity gas andtherefore is filtered in the PdB spectrum while the emissionof this high velocity structure in the CS (3–2) is negligible(see Sect. 5.1 for further discussion).

4

RESULTSLine maps of the four observed transitions are shown in
Fig. 2. The morphology is well in agreement with that of7

B1b

Fragmentation, infall, and outﬂow around the showcase
massive protostar NGC7538 IRS1 at 500 AU resolution
H.Beuther, H. Linz, and Th. Henning• High-mass star NGC7538IRS1 (d=2.7kpc)• O6 star, 30M⦿, 8E4L⦿

• PdBI• 843µm cont., HCO+, HCN, CH3OH : 500 AU resolution• 連続波で3つのsub-structure• 全体で11M⦿。sub-structureは~1M⦿程度(free-free放射補正後)• HCN(v=1)を検出• ~3000AUの広がり。吸収あり。
• infall rate 1.8E-3 M⦿/yr• 回転はnon-keplerian• 複雑なHCO+の分布 -> ほぼline-of-sightのoutﬂow

H. Beuther et al.: Fragmentation, infall and outflow in NGC7538 IRS1

H. Beuther et al.: Fragmentation, infall and outflow in NGC7538 IRS1

mid-infrared continuum imaging (De Buizer & Minier, 2005)
that detect a disk-like structure in the northeast-southwestern
direction perpendicular to the molecular outflow (Keto, 1991;
Davis et al., 1998). Figure 1 shows the various outflow/disk axes
discussed in the literature so far. Setting high-spatial-resolution
near-infrared speckle images of the region into context withthe existing data, Kraus et al. (2006) propose precession of theunderlying disk-jet structure as the main reason for observing
different axis orientations. Furthermore, Hoffman et al. (2003)
report high-spatial-resolution observations of the rare H2 COmaser emission that is also consistent with a very young disk
candidate (cf. Araya et al. 2007). In addition to the proposed
CH3 OH maser disk, Minier et al. (2000) identified a few additional CH3 OH maser positions, several of them approximately
in thepresent
east-west thedirection
one also (bottom,
in the southintegratedof theFig. 2. The color scales in the left panels
0th but
momentintensity) and 1st moment (top, intensity
core (Fig. 1). All these additional maser components are blueweighted velocity) maps of the HCN(4–3)v= respect
1 emission.
In themiddleand isrightshifted 2withto the vlsr andthe southern
position
said panels, the color-scale shows the 0th and 1sttobeassociatedwiththeionizednorth-southjet(Minieretal.,moment maps (bottom and top, respectively) of CH3 OH(151,14 − 150,15 ). Black contours
in all panels outline the dust continuum2001). Qiu et al. (2011) observed red-shifted absorption towardemission (Fig. 1) starting at the 3σ levelNGC7538IRS,
and continuingin 2σ
steps.
andred contours in the right panel show the blue- andwhich theyinterpret
as Theinfall blue
motionsof the+dense gas.

sub-structure

843µm

The Gemini NICI Planet-Finding Campaign: The Frequency ofPlanets around Young Moving Group Stars
Beth A. Biller et al.

• 100pc以内にあるmoving groupの惑星探査観測• 年齢: 10-200 Myr• ~80天体• 4つの天体で伴星• brown dwarf: PZ Tel B(36Mj, 16AU), CD -35 2722B(31Mjup, 67AU)• sub-stellar: HD12894B(0.5M⦿, 16AU), BD+07 1919C(0.2M⦿, 13AU)• 1-20Mjup伴星の頻度• 10-150AU: <18%
• 10-50AU: <7%

Infrared Spectroscopic Survey of the Quiescent Medium of
Nearby Clouds: I. Ice Formation and Grain Growth in Lupus
A.C.A. Boogert et al.

• LupusI~IVの星間ダストの性質調査• 背景星のスペクトル観測を使用• 赤外測光と1-25µm分光• H2OアバンダンスはTaurusと同程度• 近傍にhot starがないのでiceの蒸発が起きない• envelopeよりもファクターで小さい• Lupusはearly chemical stage

Interplay between chemistry and dynamics in embedded
protostellar disks
Christian Brinch and Jes K. Jorgensen• Class I天体IRS63とIRS43の星周構造観測• SMA, 1.1mm cont., HCO+(3-2)• radiative transferを解いて放射+SEDを再現• 原始星+envelope+disk• ダスト連続波でring構造(IRS63)• ケプラー回転(IRS43)• IRS63ではfreeze-out chemistryを入れるとHCO+を良く再現• 低Lbol、円盤質量が大きいことからもfreeze-outが予想される(diskで)

HCO+(3-2)
contour: mom.0
C. Brinch and J. K. Jørgensen:
Interplay
1.1mm
cont.between chemistry and dynamics in embedded protostellar disks
color: mom.1

We did not include the disk inclination as a free parameter,
rather adopted a value for IRS 63 of 30 from Lommen et(2008) who based that number on the brightness of the 3-5
fluxes. Note also that in order to see the ring structure invisibility amplitudes as described in Sect. 3, the disk needs
be relatively face-on. We did however test SEDs calculated
both higher andHCO+のPV図
lower inclinations and found that while any filargely indistinguishable at inclinations lower than 30 , the
data
model
becomerapidly worse at inclinations
higher than 50 . We
not have a previous estimate for the inclination for IRS 43,
we adopted a high inclination of 70 based on the flattened
pearance of the HCO+ moment map (Fig. 1) and the fact that
do not see any sign of a ring pattern in the continuum visibi
amplitudes.
For the envelope we use a simple spherical power-law mod⇢env (r) = ⇢0 (r/r0 ) p ,Fig. 1. Moment 0 (contour) and 1 (color) maps of the HCO+ J=3-2
line (left) and 1.1 mm continuum image (right) of IRS 63 and IRS 43.
The beam is shown by the black ellipses. The dashed grey line marks
the direction of the velocity gradient.

with four free parameters, the density ⇢0 at R0 , the powerslope p and the inner and outer radius of the envelope. The todensity is given by the sum of ⇢disk and ⇢env .
With these profiles we have eight free parameters in to
The temperature is calculated self-consistently using the radtion transfer code RADMC-3D3 and opacities of coagulated dwith thin ice mantles from Ossenkopf & Henning (1994). We
the LIME radiation transfer code (Brinch & Hogerheijde 20

Identifying Young Stars in Massive Star-Forming Regions
for the MYStIX Project
Patrick S. Broos et al.

• Massive Young star-forming Complex Study in Infrared and
X-rays(MYStIX) project• 20の近傍大質量星形成領域(0.4-3.6kpc)• Chandra(X-ray), UKIRT(NIR), 2MASS(NIR), SST(MIR)• X-rayの“Naive Bayes Classiﬁer”• Chandraで受かってないやつはSEDを使用• カタログリスト論文• ~32000天体• 今後のプロジェクトに使用

The Mopra Southern Galactic Plane CO Survey
Michael Burton et al.
journals.cambridge.org/pasa

19• Mopraを使った銀河面サーベイの初期成果• CO, 13CO, C18O(1-0)• 35” and 0.1 km/s resolution• 1ºx1ºの結果を示す• 柱密度、質量、輝線強度比、光学的厚み、など

Figure 1: Spitzer/MIPSGAL 24µm image of the Galactic plane (Carey et al. 2009), shown as a series of11◦ × 2◦ panels (with 1◦ overlap between each), overlaid with red contours of 12 CO emission from theDame, Hartmann & Thaddeus (2001) survey. The region planned for our Mopra survey, from l = 305◦ to345◦ , b = ± 0.5◦ , is indicated with the blue dotted lines. The data included in this paper, from the G323

Massive stars in massive clusters IV: Disruption of clouds
by momentum-driven winds
J.E. Dale et al.

• momentum-drivenの星風(OB star)のSPHシミュレーション• 分子雲を破壊する効率はHII領域の輻射より低い• 星風があると星形成効率が減少する• 降着を止める• 星形成をトリガーできないNitrogen isotopic ratios in Barnard 1: a consistent study of
the N2H+, NH3, CN, HCN and HNC isotopologues
F. Daniel et al.: N H , NH , CN, HCN and
2+

3

F. Daniel et al.

• Class0天体B1bの多輝線観測• 14N/15Nアバンダンス比の導出• 太陽系内天体では大きい違いがある• IRAM30m(80-280GHz)

350µm
SHARC/CSO

Fig. 1. Continuum map at 350 µm obtained at the CSO with the Fig. 2• N2H+,NH3,CN,HCN,HNCの同位体(15N,13C,D)をカバー
SHARC instrument. The contours have a step of 0.5 Jy/beam the IRfrom 0.5 to 4 Jy/beam and 1 Jy/beam for larger fluxes, as drawn
on the right. The white stars indicate the position of B1–bS
and B1–bN and the black star corresponds to the Spitzer source[EDJ2009] 295. The black dot gives the position of our molecular survey.

• ダスト連続波から構造を推定->輝線モデリングに使用• 温度の動径方向変化あり• infall(0.1km/s) + turbulence(0.4km/s)

from the wobbler–switched spectra, while higher order polynomials were necessary for the frequency switched data.

• 柱密度と分子アバンダンスを導出

3. Continuum and molecular line modelling
The distance of the source is taken to be 235 pc (Hirota et al.,2008). At this distance, an angular size of 1000 corresponds to aphysical size of 0.0114 pc.

• 中心ではどの分子もアバンダンス低下 -> 主にdepletion• 14N/15N比はどの分子でも一定(~300)でISMとコンパラ
3.1. Continuum

In order to derive the gas temperature and H2 density profiles,
we used continuum observations at = 350 µm and = 1.2 mm,
respectively obtained at the CSO and IRAM telescopes. The corresponding continuum maps are reported in Fig. 1 and 2. In thesefigures, we indicate the positions of the B1–bS and B1–bN cores

have
mJy/b
right.

in thi
one s

3.1.1

In ord
serva
As an
gives
rame
vatio
spect
the C
A
that t= 12K
to the(1990

F. Daniel et al.: N2 H , NH3 , CN, HCN and HNC isotopologues in B1

F. Daniel et al.: N2 H+ , NH3 , CN, HCN and HNC isotopologues in B1

(a)

(b)

Fig. 4. Temperatureダスト連続波から導出し(blue curve, right axis) and H2 density(black curve, left axis) derived from the SED fitting.

たコアのモデル

計算した分子アバンダン
cm 3 , ↵1 = 2, ↵2 = 1.2 and = 1.9. The dust temperature
F. Daniel et al.:
N
H
,
NH
,
CN,
HCN
and
HNC
isotopologues
inB1
Fig. 3. Comparison of the observed andmodel fluxes as a func- and H2 density are represented in Fig. 4. With the density proスと輝線再現性の例
(c)
2

+

3

tion of radius at 350 µm (bottom panel) and 1.2 mm (upper file defined this way, the peak value of the H2 column density
panel). The blue curve corresponds to a model obtained assum- is N(H2 ) = 2.1 1023 cm 2 . The average column density, within
ing that the source is isothermal at Td =12K. The red curve corre- a 3000 FWHM beam, is N(H2 ) = 7.6 1022 cm 2 , in good agree. 5. Abundance profiles of the N2 H+ isotopologues
derivedthewheremodeling(red lines). aTheshaded areas
give a confidence
ment with the estimate of Johnstone et al. (2010), i.e.+ N(H2 ) =spondsto afrommodel
we introduced
temperature
gradient.
ne for the abundance as delimited by the lower and upper boundaries in each region (see Sect. 3.2 for details).
F. Daniel
et al.: NThe
NH3 , CN, HCN and
2 H , FHWM
各分子の14N/15N比
8.2 1022 cm 2 , obtained
assuming thesame beam.
00of the column density distribution is ⇠16 . Finally, the current
5. Condensity profile corresponds to enclosed masses of 0.5, 1.8, 4.500
with expressed in µm and 1300 being the absorption coeffi- and 13.1 M for delimiting radii of 10, 30, 60 and 120 , respecWe rep
cient at 1.3 mm. Values for the dust absorption coefficient were tively (⇠ 0.01, 0.03, 0.07 and 0.14 pc, assuming a distance to B1
lar linemolecudetermined by Ossenkopf & Henning (1994), for the case of dust of 235 pc).
continu
grains surrounded by ice mantles. The values were found to be inture anthe range 0.5 < 1300 < 1.1 cm2 /g, where 1300 is given in func- 3.1.2. Comparison with previous studies
tempertion of the dust mass. Hence, we fixed the gas–to–dust mass ratio
non–loto 100 and furthermore fixed the absorption coefficient to 1300 = B1b has been the subject of many studies with both ground–molecu0.005 cm2 /g, where 1300 is this time refereed to the mass of gas. and space–based telescopes. In particular, interferometric oblogues
The results of the models depend only on the product 1300 ⇥ n0 . servations by Hirano et al. (1999) lead to the identification ofi.e. N200
The grid is then computed considering as an additional free two cores, separated by ⇠20 and designated as B1–bS andi.e. HC
00
00
parameter.
B1–bN. These objects are respectively o↵set by (+6 ,-7 ) and(a)(b)
profile00
00
From the results of the grid, it appears that the best models (+5 ,+10 ) with respect to the central position of our observaabunda
66
300
are found for parametersin the range : 3 10 < n0 < 6(c)10 cm , tions (see Sect. 2) and are thus both at a projected distance ⇠10 .
(a)(b)
for the
2.0 < ↵1 < 2.4, 1.2 < ↵2 < 1.5 and 1.7 < < 2.4. However, we By modelling
14 the15 SED from 350 µm to 3.5 mm, these authors

Imaging diagnostics for transitional discs
M. de Juan Ovelar et al.

• Transition diskにおいてNIRとサブミリ波で異なる穴の様子• 惑星に夜pressure bump生成とlarge dustの集積• 動径方向のダストサイズ分布の違いで再現• 計算• ダスト進化を入れた流体計算(radial drift, fragmentation, coagulation)• radiative transferを解く• 観測をシミュレート• SPHERE ZIMPOL/VLT (R-band)• HiCIAO/Subaru (H-band)• Band7/ALMA• 波長によるギャップサイズの違いを再現• bumpでせき止めるダストサイズは惑星質量に依存
A&A proofs: manuscript no. TransitionDiscs_14axiv

ZIMPOL (R-band PI)

HiCIAO (H-band PI)

1 Mjup

ALMA (Band 7 I)

1 MjupM. de Juan Ovelar et al.: Imaging diagnostics for transitional discs

1 Mjup0.2

Full resolution

10 11

Simulated observations
R-band (0.65 µm)
H-band (1.6 µm)
sub-mm (850 µm)
R-band IP
H-band IP

1 Mjup

m 2]

0.0
10 13

0.2
[W

DEC [arcsec]

0.4

30 AU

10 15

F

0.4

1 Mjup9 Mjup9 Mjup
10 17

m 2]

0.2

9 Mjup9 Mjup15 Mjup

15 Mjup

10 13

[W

0.0
0.2
0.4

10 15

30 AU

0.4

1.2

1.2

15 Mjup

15 Mjup

15 Mjup

10 13

[W

m 2]

0.2

10 17

0.0

10 15

0.2
0.4

F

DEC [arcsec]

9 MjupF

DEC [arcsec]

0.4

30 AU

0.4

1.2
0.2

0.0

0.2

RA [arcsec]

0.0
F

1.5
⌫ [W

3.0
m 2]

1.2

0.4

0.4

4.5

0.0

10 14

0.2

0.0

0.2

RA [arcsec]

F

0.5
⌫ [W

1.0
m 2]

10 17

0.4

0.4

1.5

0.0

10 14

0.2

0.0

0.2

RA [arcsec]

F

0.4
⌫ [W

0.8
m 2]

0.4

0

10

20

30

40

50

60

70

R [AU ]

0

10

20

30

40

50

60

70

80

R [AU ]

1.2Fig. 3: Radial profiles of the theoretical images (left panel) and simulated observations (right panel) of a 3 Myr disc with a planet

10 14 of mass Mp = [1, 9, 15] MJup from upper to lower panels, in the R (0.65 µm), H (1.6 µm) and 850 µm bands. Solid lines correspondto intensity (I) profiles while dashed lines correspond to polarised intensity (PI). The vertical dotted black line indicates the radial
position of the planet at 20 AU.

2: Simulated images of the disc-planet models used in this study for the case of an embedded planet orbiting at 20 AU (white
Left to right columns correspond to polarised intensity (PI) ZIMPOL images in the R-band (0.65 µm),
images depending on their size with respect
fact PI
thatHiCIAO
dust particles,

by the star in the far side, while we are seeing the cold dust