THE STAR FORMATIONNEWSLETTER
No. 278 (#18-22)
塚越崇(茨城大)11 Mar. 2016

1. On the universality of interstellar filaments: theory meets
simulations and observations
2. The SPHERE view of the planet-forming disk around HD100546
3. On the 2015 outburst of the EXor variable star V1118 Ori
4. A new insight into the V1184 Tau variability
5. Hot ammonia around young O-type stars.
III. High-mass star formation and hot core activity in W51 Main

On the universality of interstellar filaments: theory meets simulations and observations
Christoph Federrath
Universality of interstellar filaments

柱密度• hydrodynamical simulationで分子雲フィラメント形成を計算• 観測の~0.1pcを説明できるか?
• gravity, turbulence, magnetic field, jet/outflow feedbackのoff/on• 全計算でフィラメントを生成• DisPerSEでフィラメント同定• 観測でも使用されている• 面密度はΣ∝r-1でよく再現

L=2pc, M=388M⦿

379

• 重力のみでは細め。乱流を入れると0.1pcに。
• 重力はdense partの形成のみに影響• sonic scale λによる幅の説明=> 今回の計算ではλ=0.050.15pcとなりconsistent• フィラメント内で亜音速、外では超音速となる

The SPHERE view of the planet-forming disk around HD100546
A. Garufi et al.A&A proofs: manuscript no. aa(d)(b) Qφ FastPol

Uφ SlowPol• HD100546• B9V, d=97pc• 2 companion candidates
0.5″• SPHERE/VLT(c)0.5″(e)Qφ SlowPolbNorthernarm• ZIMPOL•

highest resolution atopt. (0.02”)

AO artifact
SpiralDark wedge• IRDIS

0.5″

Brightwedge

FARcNEAR

Qφ SlowPol (unsharp masking)0.1″

Garufi et al. 2016: The SPHERE view on HD100546

IRDIS image

Surface brightness (arbitrary units)

A&A proofs: manuscript no. aalarge scale (H)

たくさんのarm100

Northernspirals
0.100.150.20

Wing
structure

0.25

Radius ('')

Westernspirals?
Southernspirals

Medium1″

Composite

Large1″• ZIMPOL• 北西-南東方向にinner cavity

1″1″

Enhancedbrightnessarm(K band only)• 赤外(NACOデータ)と位置のずれがある• maskを強めるとspiral armが見える• IRDIS

Knot(mainly H band)arm

small scale (composite H&K)
RDIS imagery of HD100546. Images in the top row are in the H2H3 band, in the bottom row in the K1K2 band. The first three• 大小のスケールでarmが見える• 色々なデータと比較•

散乱光では内側のrimまで拾えている • ZIMPOLのarmはb-sourceに向かって伸びている•

Garufi et al. 2016: The SPHERE
viewon HD100546
広がった放射は波長によらず見える
scalearmsの位置は2010-2015で変化なし• large(a)(b)

(c)

(d)

0.2″0.2″0.2″

H band: polarized light vs intensity

R′ polarized light vs M′ intensity

R′ polarized light vs K vs M′ intensity

0.2″
K band intensity: 2015 vs 2010

Fig. 4. Multi-wavelength and -epoch images of HD100546. (a): NACO polarized light H band (colors) and IRDIS H band (contours). (b): ZIMPOL
polarized light R0 band (colors) and NACO M0 band (contours). (c): ZIMPOL polarized light R0 band after unsharp masking (colors), IRDIS Kband (yellow contours), and NACO M0 band (cyan contours). The inset image is the NACO polarized light KS band image from 2006 after unsharp
masking. (d): IRDIS K band from May 2015 (colors) and NICI K band from March 2010 (contours).

•observed in the visible (colors) are also evident from the IR 4.1), on the global disk morphology (Sect. 4.2), on the disk fea円盤構造等を過去の観測と比較して議論
NACO data (contours). Particularly good is the match between tures (Sect. 4.3), and on the environment around planet b (Sect.
the bright/dark edge to East. Also worth mentioning is the tenta- 4.4).
tive detectionof the spiral at 0.200 (Fig. 1e) from the M0 dataset.
惑星候補天体(b-source)位置でK-bandでのみ広がった放射がある
In Fig. 4c, we show the spatial connection between the northern arm spotted from the ZIMPOL image after unsharp masking 4.1. Cavity and inner rim
H,theK bandが散乱するτ(高さ)でちょうど円盤構造が変わっている(colors)di↵use emission from the M0 band (cyan con- Our results on the disk cavity (from Sect. 3.1.1) support the pre• andtours) surrounding planet b (Quanz et al. 2015). The same emis- vious findings in DPI (Quanz et al. 2011; Avenhaus et al. 2014a),sion from heating
the IRDISsourceが円盤に埋もれていて視線方向に減光されている
K band is shown (yellow contours). The that are that the disk around HD100546 is truncated at roughly•
arm seems to head to the location of b and a blurred counterpart 15 AU and that this cavity is consistent with being intrinsically•0On the 2015 outburst of the EXor variable star V1118 Ori
T. Giannini et al.

• V1181Ori• EXor型増光天体• 過去に4回増光(いずれも数年ほど持続)–1• データ: EXORCISM project• JHK photometry; 1.1m AZT-24望遠鏡Fig. 1.— V1118 Ori JHK lightcurve (blue, green and red, respectively).
10−6• 増光前後の比較• 質量降着率の増大

dMacc/dt (M ∀/yr)• optical spectra; 8.4m LBT, 3.6m TNG
1010−7−8• 質量損失率の増大([OI],[SII]など)
HeI447HγHδ

HeI403CaIIK

H8H9H10H11H12H13H14−9H15• 過去のバーストよりも弱い

10• もしくは増光/減光途中かもFig. 3.— Mass accretion rate determination coA new insight into the V1184 Tau variability
T. Giannini et al.

T. Giannini et al.: A new insight into the variability of V1184 Tau• V1184Tau (d=1.5kpc)• G5 star, 7-39L⦿
• UXor型の変光と言われはじめた• データ: EXORCISM project• + published photometry data

• EXorよりUXor的な増光の証拠• 強度変化が緩やか• 強い赤外超過• 現在増光のピーク• 距離は1.5kpcでなく200pc• SED fittingより

C. Goddi et al.: Hot NH3 around Young O
Hot ammonia around young O-type stars. III. High-mass star formation and hotcore activity in
W51 Mainand (and (Ciriaco Goddi et al.

W51 MainNW• W51: 大質量星形成領域

WE• 2x107L⦿, 7000M⦿
• Main(UC,HC HII region) (, IRS1, IRS2)• JVLA• NH3(J,K=6~13), CH3OH,CH3CN• ~<0.3”• W51e2(substructure), W51e8の構造に着目

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contour: NH3(6,6) (blue:emm., red:abs.) sionline-wout, w(disp• 吸収はHC HIIコア+ionized flow

• 高励起に行くほど速度勾配は東西になる• 低い励起ではionized flowのコンタミがある• 東西方向がリアルなコアの速度勾配 (回転)• W51e8についても同様の解析=>EW方向、NS方向にわずかに速度勾配• スペクトルフィットによりτ, Trot, Ncolを導出• W51e2 complexについて• W51e2-E

hot molecular gasが付随、molecular outflowを駆動、ジェットによるH2O maserが付随、低速のOH
expanding shell=> high mass protostar• W51e2-W
Fig. 14. Overlay of the CO J=3-2 0 moment image from the SMA
W51e2のactive star forming regionだと思われていたが実はEのほうがactiveだった。低th(blue and red contours; Shi et al. 2010b) onto the total intensity (0thmoment) map of the (6,6) inversion transition of NH3 (gray scale andwhite+black contours). The NH3 emission is displayed with white contours, representing 30% to 90% with steps of 20% of the line peakfor the (6,6) line, 107 mJy beam 1 km s 1 ). The NH3 absorption isdisplayed with black contours, representing
factors 1, 5, 9,.... of –⦿
50 mJy beam 1 , for all transitions. The CO 3-2 line contours are from
10% to 90% with steps of 10% of the line peak (67 Jy beam 1 km s 1 forthe red contours and 82 Jy beam 1 km s 1 for the blue contours). Blueand red contours correspond to blue- and redshifted gas, with integrated
velocity ranging from –124 to –12 km s 1 and from +10 to +116 kms 1 , respectively. The cyan contour locates the peak of the total intensity map of the most highly-excited NH3 transitions (13,13): we assume
that this peak pinpoints the high-mass YSO driving the CO outflow.

速のOH expanding shellがあり、UC HII regionによるものと思われる。回転は見えるがケプラーかどうかは不明。中心YSO質量20M⦿に対しNH3ガス質量5M=> 降着フェーズが終わったO型星• W51e2-NW

ホットガスが付随、コンパクトアウトフローが付随=> (high mass) YSO forming region0.00 06, 320 AU). This material could be potentially accreting onto
the central YSO, either in the form of an accretion disk or an infalling envelope, provided that it has not been stopped by theintense radiation pressure from the central O-type star and thethermal pressure from the ionized gas in the HII region. Indeed,
the observed velocity gradient provides evidence for rotation in
the molecular core surrounding the HC HII (§ 3.1.1).

• W51e8 => massive hot core (70M⦿、T~200K)