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 spatialresolution
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.

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

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 3-5fluxes. 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 , thedatamodel
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=3-2line (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 andX-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• 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

19

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 and2

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)• N2H+,NH3,CN,HCN,HNCの同位体(15N,13C,D)をカバー• 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)• 柱密度と分子アバンダンスを導出• 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F. Daniel et al.: N2 H , NH3 , CN, HCN and HNC isotopologues in B1

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
[WDEC [arcsec]

0.4

30 AU

10 15

F

0.4

1 Mjup9 Mjup9 Mjup10 17m 2]

0.2

9 Mjup9 Mjup15 Mjup

15 Mjup

10 13[W0.00.2
0.4

10 1530 AU

0.4

1.2

1.2

15 Mjup

15 Mjup15 Mjup

10 13[Wm 2]

0.2

10 170.0

10 150.20.4F

DEC [arcsec]

9 Mjup

FDEC [arcsec]

0.4

30 AU

0.4

1.2
0.2

0.00.2RA [arcsec]

0.0F

1.5
⌫ [W3.0m 2]

1.2

0.4

0.4

4.5

0.0

10 14

0.2

0.00.2RA [arcsec]

F0.5⌫ [W1.0m 2]

10 17

0.4

0.4

1.5

0.0

10 14

0.2

0.00.2RA [arcsec]

F0.4⌫ [W0.8m 2]

0.4010203040506070

R [AU ]

01020304050607080

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