星形成ゼミ 2014年6月13日
論文速報 SFN #257 (46–50本目)
東京大学 博士2年 小屋松 進"ESO-Ha 574 and Par-Lup3-4 jets: Exploring the spectral, kinematical and physicalproperties” E.T. Whelan et al.
"Multi-epoch Sub-arcsecond [Fe II] Spectroimaging of the DG Tau Outflows with NIFS. I.
First data epoch” Marc C White et al.
"Multi-epoch Sub-arcsecond [Fe II] Spectroimaging of the DG Tau Outflows with NIFS. II.
On the Nature of the Bipolar Outflow Asymmetry” Marc C White et al.
"A Parametric Modeling Approach to Measuring the Gas Masses of Circumstellar Disks”
Jonathan P. Williams and William M. J. Best"A spider-like outflow in Barnard 5 - IRS 1: The transition from a collimated jet to a wideangle outflow?” Luis A. Zapata et al.

ESO-Hα 574 and Par-Lup3-4 jets: Exploring the spectral,
kinematical and physical properties
E. T. Whelan, R. Bonito, S. Antoniucci, J. M. Alcalá, T. Giannini, B. Nisini, F. Bacciotti6, L. Podio, B.
Stelzer, and F. Comerón

ジェットを伴う2つの系のVLTのX-ShooterおよびUVESによる観測
2011年のレター(Bacciotti et al. 2011)の詳細【背景】
ジェットの形成シナリオ
Magneto-centrifugal jet launching model が有力だが観測的な証拠がほしい
多波長分光観測により正確な質量の放出率と降着率の比を求めてモデルを検証【天体】
・ESO-Hα 574: K8, 古典的おうし座T型星(CTTS)
・Par-Lup 3-4: 超低質量(0.13 Msun)(VLMS), M5
X-Shooter Spectra of the Par-Lup3-4 Jet
ともにedge-onに近い降着円盤をもつ天体

Shooter observations of the ESO-H↵ 574 and Par-Lup 3-4 Jets

A&A 5

-

R

-

B

Fig. 7. Position velocity diagram of the Par-Lup 3-4 jet in [S II] 67
with the velocity centroid measured at various positions along theTable A.1. continued.
Identification
Ion

Knot
Flux (⇥10 17 erg/s/cm2 )obs (Å)A
10 286.6 20 ± 1
2
10 320.5[S II]
P3/2 –2 D5/2
24 571.5
10 320.4 64 ± 1
A 57410and
320.4
203-4
± 1Jets
E. T. Whelan et al.: X-Shooter observations of the ESO-H↵
Par-Lup2
2
10 336.4[S II]
P1/2 – D3/2
24 524.8
10 336.3 50 ± 1
A
10 336.3 14 ± 1
Appendix A: Tables of identified lines and line fluxes
2
10 370.5[S II]
P1/2 –2 D5/2
24 524.8
10 370.4 22 ± 1
Table A.1. ESO-H↵ 574 emission line fluxes.
A
10 370.4 7 ± 1
2
10 397.7a[N I]
P3/2 –2 D5/2
28 839.3
10 398.0 4 ±1
2
2
10 398.2a[N I]
28 838.9
Identification 2 P1/2 –2 D5/2
10 407.2a[N I]
P3/2 – D3/2
28 839.3
10 407.2 3 ± 1
Eu (cm 1 ) Knot obs (Å) Flux (⇥10 17 erg/s/cm2 )air (Å) a Ion
2Type 210 407.6[N I]
P1/2 – D3/2
28 838.9
a3721.9
H
I
109
119.2
± 0.5
314–23
10 830.3
He I
P–S
169 087.0
103721.8
830.1 3.5
132.7
± 0.8
1 1 3 13721.6a[S III]S0 – P1
27 161.00 A
10
830.3
56.2
± 0.3
2
4
3726.0
[O
II]
D
–
S
26
830.6
3726.0
76.8
±
3/2
3/2
10 938.0HI
0–3
106 632.2
10 937.8 14.5 ± 0.5
0.8
11 618.9[Ti II]
a2 G7/2 –a4 F9/2
8997.7 A
113726.0
618.9 71.7
6 ± 1± 0.5
46B3726.018.3±
0.5
12 485.4[Fe II]a D5/2 –a D7/2
8391.912 484.9 2.3 ± 0.4
612 566.8[Fe II]a2 4 D7/2 –aD9/2
7955.3 E
123726.6
566.6 9.2
82.7±±0.50.73728.8[O II]
D5/2 –4 S3/2
26 810.6 A
123728.8
566.4 38.0
16.7 ±± 0.5
0.2
12 610.9[Cr I]
a5 D2 –a7 S3
7927.5 A
123728.8
611.0 46.7
3 ± 1± 0.5
B3728.822.5±
0.5
12 787.8[Fe II]a4 D3/2 –a6 D3/2
8680.45
12 787.5 11 ± 2
12 818.1
HI
5–3
105 291.7 E
123729.0
817.7 13.3
13 ± ±1 0.5
3734.4
H
I
13–2
109
029.8
4
6
12 942.7[Fe II]a D5/2 –a D5/2
8391.9123734.3
942.5 1.3
13.8±±0.50.83750.2H[FeI II]
108680.4
8917.1
4
6
12
977.7
a12–2
123750.3
977.8 1.4
3.7 ±
± 0.5
0.8
a
3D3/2 –a
3 D1/23769.9
[Co
II]
a
27
469.1
1.7
±
0.5
4 H5 –a F
63
13 205.5[Fe II]a3 D7/2 –a7955.30
13 205.3 26.9 ± 0.8
a
3 D7/23770.2I II]
F4 –a–aG63D
418391.9
624.2
13277.8 Ti[Feas4 D
13 277.8 9.5 ± 0.9
5/2
3/2
3770.6
H
I
11–2
108
772.3
4
4
15 334.7[Fe II]a D5/2 –a F9/2
8391.9153771.3
334.4 1.713.9±±0.5
0.63797.9HI
10–2
108 582.0
3797.8 2.3 ± 0.5
15 994.7[Fe II]a4 D3/2 –a4 F7/2
8680.515 994.7 14.4 ± 0.5
中略3835.3HI
9–2
108 324.7
3835.3 4.9 ± 0.5
16 435.5[Fe II]a1 4 D7/23 –a4 F9/2
7955.316 435.3 72.5 ± 0.7
3869.1[Ne III]D – P2 4
25 838.7
3968.9 11.5 ± 0.5
16 637.7[Fe II]a4 D2 1/2 –aF5/2
8846.816 637.4 7.2 ± 0.6
3889.0HI
8–2
107 965.1
3888.9 1.2 ± 0.5
16 768.8[Fe II]a2 4 D5/22–a4 F7/2
8391.916 768.1 16.7 ± 0.6
3933.7
Ca II
P3/2 – S1/2
25 414.4
3933.7 16.6 ± 0.3
17 475.0H
1-0S(7)
1.74746 9.3 ± 0.9
133967.8[Ne2 III]D
25 838.7
3967.4 4.7 ± 0.3
4 2 – P1 4
17 971.0
[Fe
II]
a
D
–a
F
8680.517970.7 4 ± 1
3/2
3/2
a
4
3968.2[Fe
G5/2–a–a46FD3/2
267955.3
055.4
18
093.9
[FeII]II]aa42D
183968.5
093.5 12.5
16 ± ±2 0.3
7/2
a
4 7/2
3968.2
[Ti
II]
c
D
–a
F
25
192.8
5/2
3/2
19 570.2
H2
1-0S(3)19 570.8 69.7 ± 0.2a22
3968.4
P1/2 – S1/2
25 191.5
21212.5 CaH2II
1-0S(1)21 212.5 39.2 ± 0.2
3970.1
7–2
107 440.5
0.3
22226.8 HHI 2
1-0S(0)223970.1
227.0 10.0
8.4 ±±0.3
A0.3
22 471.0
H2
2-1S(1)223970.1
470.0 3.35
4.8 ±±0.3244068.6[S II]
P3/2 – S3/2
24 571.5
4068.6 149.0 ± 0.4
A4068.5 41.7 ± 0.4
24076.3[S II]
P1/2 –4 S3/2
24 524.8
4076.3 50.1 ± 0.4
A4076.3 15.9 ± 0.4
4101.7HI
6–2
106 632.2
4101.8 13.4 ± 0.4
A4101.8 8.8 ± 0.4
4114.5[Fe II]b2 H11/2 –a4 F9/2
26 170.2
4114.5 2.7 ± 0.4
244211.1[Fe II]b H11/2 –a F7/2
26 170.2
4211.1 1.2 ± 0.4
4244.0[Fe II]
a4 G11/2 –a4 F9/2
25 428.84244.0 6.0 ± 0.5444276.8[Fe II]a G9/2 –a F7/2
25 805.3
4276.9 2.5 ± 0.5664287.4[Fe II]a S5/2 –a D9/2
23 317.6
4287.4 6.6 ± 0.4444319.6[Fe II]a G7/2 –a F5/2
25 981.6
4319.6 1.9 ± 0.3
4340.5HI
5–2
105 291.7
4340.4 25.0 ± 0.4
A4340.5 18 ± 0.4
4346.9[Fe II]
a4 G11/2 –a4 F7/2
25 428.84346.6 0.7 ± 0.3
4347.4[Fe II]b4 D5/2 –a4 D5/2
31 387.94347.6 1.0 ± 0.3
4352.8[Fe II]
a4 G9/2 –a4 F5/2
25 805.3
4352.8 1.0 ± 0.3
664359.3[Fe II]a S5/2 –a D7/2
23 317.6
4359.3 4.8 ± 0.3
334362.7CI
D3 – D3
87 002.3
4362.5 0.8 ± 0.3
114363.2[O III]S0 – D2
43 185.7
4363.4 3.0 ± 0.3
664413.8[Fe II]a S5/2 –a D5/2
23 317.6
4413.8 3.1 ± 0.3
464416.3[Fe II]b F9/2 –a D9/2
22 637.2
4416.3 4.4 ± 0.3
464432.4[Fe II]b F5/2 –a D7/2
22 939.4
4432.7 1.6 ± 0.3
444438.9[Fe II]b D1/2 –a D1/2
31 368.5
4439.2 1.0 ± 0.4664452.1[Fe II]a S5/2 –a D3/2
23 317.6
4452.2 2.8 ± 0.4464457.9[Fe II]b F7/2 –a D7/2
22 810.4
4457.9 2.3 ± 0.3
34471.7He I
D1 –3 P0
191 444.6
4471.5 4.0 ± 0.4
24571.1aKI
D3/2 –2 P3/2
34 913.3
4571.5 3.2 ± 0.4
a
3
Mg I]
P1 –1 S0
21 870.5
A80, page 20 of 4571.1
224580.8[Cr II]a4 P3/2 –a6 S5/2
21 824.1
4580.8 1.4 ± 0.3
34607.0[Fe III]F3 –5 D4
21 699.9
4606.8 1.0 ± 0.3
34658.1[Fe III]F4 –5 D4
21 462.2
4658.1 9.2 ± 0.3
air (Å)【結果】
輝線を同定してフラックステーブルを作成

Eu (cm 1 )Type

Table A.1. ̶ ESO Hα 574で検出された輝線とそのフラックス

ESO-Hα 574
・jet lineは多いがaccretion lineは少なく弱い・H, O, Fe, S, N, He, Ca, H2など数十の輝線・弱いながらもたくさんのBalmer線, Paschen
ラインはγ, βのみ, Brackett線はなし
・Ca IIの三重線はCTTSよりも弱い
CTTSの典型ではないがedge-onに近い円盤をもったCTTSの特徴(TWA30と似ている)
Par-Lup 3-4
・通常の降着トレーサー
・jetではいくらかの弱い輝線([OI]λ6300, [SII]λ6731など)
典型的なVLMSのスペクトル

Notes. Fluxes refer to knot A1, are in units of erg/s/cm2 ⇥ 10 17 and are not extinction corrected. Where the identified lines are also found inknots A, B or E the observed wavelengths and fluxes are also given. The regions over which the spectra for A1, A, B and E are extracted are shown(a)減光量の評価 (質量降着率の見積もりに必要)
同じスペクトル型の減光なしClass IIIテンプレートとスペクトルを比較(i) 750 nmのフラックスでテンプレートを規格化(ii) Av=0–4.0 magの人工的な赤化を加えて観測の傾きを再現
Relative extinctionはESO-Hα 574 で1.5 mag、Par-Lup 3-4ではなし
・光度は上の減光補正を加えても同質量の典型的なものより小さい・円盤による掩蔽のためのgrey extinction(波長に依らない減光?)の影響
・ESO-Hα 574では150倍、Par-Lup 3-4では25倍暗い
質量降着率の見積もりにより質量降着率を計算

以前に比べて・フラックスキャリブレーションが改善
・天体に近い成分のみでLline→Laccを計算
・新たな減光量を適用
・LlineからLaccを求める際に新たな関係を適用
掩蔽の補正後の降着率はにより掩蔽の影響を補正

ESO-Hα 574
Par-Lup 3-4

A&A 565, A80 (2014)
Par−Lup3−4

ESO−Ha 574 A1

100.001012 cm−3, 1000 K
1012 cm−3, 10000 K
108 cm−3, 1000 K
108 cm−3, 10000 K
104 cm−3, 1000 K
104 cm−3, 10000 K

2500K
3000K
5000K

Fn / Fβ

10.00

20000K

1.00

100.0

2000K
2500K
3000K

10.0

Fn / Fβガスの物理性質と質量放出率
Balmer decrementsを計算
輝線比を上準位の量子数の関数としてプロット
・Case B (赤・黒)・光学的に薄いLTE (青)と比較 (光学的に厚い場合も試したが合わなかった)

2000K

5000K
20000K

1.0

LTE
opt.thin

0.10

LTE

0.1
0.01
0

2

4

6

8

10

12

14

opt.thin

0

nup

2

ESO−Ha 574 A

Fig. 10. Balmer decremen
ESO-Hα 574 (A1, A)
the source spectrum. The
100.0010 cm , 1000 K
nation (black and red line
10 cm , 10000 K
The best fit is o↵ered by・Case B (104 cm-3, ~10000 K) がよく合う (A1はTe=20000
10 cm , 1000 K
10 000 K. This is consiste
10 cm , 10000 K
10.00
KのLTEでもよい)
10 cm , 1000 K
10 cm , 10000 K
The optically thick cas
4-3
not provide a good fit t
1.00
・密度10 cm , 温度10000–20000 Kはjet起源と矛盾しない
For regions A1 andB model for n = 10
・A1はESO-Hα 574自身を含んでいるが放射の大半はdecrements, as well as,
0.10
T = 20 000 K. A dens
outflowからきているof 10 000–20 000 K isagrees with results pu
0.01
2011, 2008). This ana
0
2
4
6
8
10
12
14
Par-Lup 3-4
emission from A1 comnup
the appearance of the
A&A 565, A80 (2014)
・Case B (108–10 cm-3, ~10000 K)
Fig. 9. Balmer decrements for ESO-H↵ 574, regions A1 (top) and A astrometric analysis of
The gas from Par(bottom), fittedwith Case B recombination (black and red lines) and
ESO−Ha 574 A1
Par−Lup3−4
LTE optically thin models (blue line). For the Case B scenario, the best B models, a high den
・Magnetospheric accretion flow起源
fit is 100.0o↵ered by n = 10 cm , T = 10 000 K. The LTE optically thin ture of ⇠10 000 K. Su
100.00
2000K

12

2500K
3000K

Fn / Fβ

5000K

20000K

−3

12

−3

8

−3

8

−3

4

−3

4

−3

e

LTE

4

opt.thine1012 cm−3, 1000 K
1012 cm−3, 10000 K
108 cm−3, 1000 K
108 cm−3, 10000 K
104 cm−3, 1000 K
104 cm−3, 10000 K

2500K
3000K
5000K

Fn / Fβ

10.00

20000K

1.00
LTE
opt.thin

0.10

0.01
0

2

4

6

8

10

12

14

nup
ESO−Ha 574 A

100.00

2000K
2500K
3000K

1012 cm−3, 1000 K
1012 cm−3, 10000 K

2000K
e

4

3

e

case with T e = 20000 K provides an equally good10
fit. Theagree
cm results, 1000 K
2500K
with the fact thatfor region A1, emission from thezone
cm , 10000
K is
10 accretion
3000K
dominated by the outflow emission.
10 cm , 1000 K
5000K
10 cm , 10000 K
10.0

Fn / Fβ

2000K

20000K

12

−3

12

−3

10

−3

10

−3

8

−3

10 cm , 1000 K

K A
10 cm , 10000
both sources and the Balmer decrements for ESO-H↵
574 A1,and Par-Lup 3-4 were computed (with respect to H ). The line
1.0
ratios are plotted as a function of their upper quantum number(nup ) and results are presented in Figs. 9 and 10. While the specLTE
tral range of X-Shooter
covers all of the Balmer lines, any lines
with nup0.1> 13opt.thin
were found to be too noisy for inclusion in theanalysis. Additionally, at the intermediate spectral resolution of
X-Shooter the H7 and H8 lines are blended with other lines andare therefore
It6 is noted
only the12brightest
0 also 2not included.
4
8 that 10
14
Balmer lines were detected in knot A. To constrain the physn
upical conditions in the emitting gas the decrements were firstly
compared
to standard
Case
predictions(red andcurves)Fig. 10. Balmer
decrements
forBPar-Lup
3-4. Fluxes
are blackextracted
fromcalculated
for a range
temperatureand density.
Case Bthe source spectrum.
Theofdecrements
are fittedwith CaseThe
B recombicurves
were andderivedusingand
theLTE
calculationsof Hummer& Storeynation (black
red lines)
optically thinmodels (bluelines).
3
The bestand
fit istheo↵eredtheprovided
Case B scenarioand &ne Hummer= 1010 cm(1995).
, Te =(1987)
data byfiles
by Storey
8−3

an origin in magnetos
For example, Muzero
spheric accretion in T
magneto-spherically ac
for 10 6 M yr 1 Ṁatemperatures correspon
rates. The origin of thgas is in agreement wi
H↵ line (Bacciotti et al
The temperature e
the results of Bary et aof the gas emitting theof TTSs, was best fittethat while this value ismagnetospheric accretallow for the absorptio
the hot corona and/or aof heating and ionisat
can still be consistentgas, as the ionising ph

電離輝線の診断
Post-shocked ガス内で物理状態の勾配？
観測の輝線比と5準位モデル原子の数値計算から予測される値を比較
ESO-Hα 574
・1.4x104 K, 水素電離率 > 0.65, BとEでより高励起・電子密度は内から外に向かって4500 cm-3から160 cm-3へと減少
Par-Lup 3-4・電離度は低い xe=2–6×10-3, 温度と電子密度は高い(2.5–3×104 K, 4000 cm-3)
ESO-Hα 574のほうが高電離の輝線が豊富なのはこのため・励起度は高いが電子密度が低いためにBとEでは高励起輝線は検出されなかった・BとEはshock速度がA1とAおよびPar-Lup 3-4よりも速い
E. T. Whelan et al.: X-Shooter observations of the ESO-H↵ 574 and Par-Lup 3-4 Jets
ESO-Hα 574••

Par-Lup 3-4

JetにおけるOutflow rateのよりよい診断
5段階モデル原子を用いる

E

A1

A

B

R

B

Fig. 11. Various line ratios tracing the excitation, ne , T e and xe of the gas in ESO-H↵ 574 A1, A, B and E and the Par-Lup 3-4 blue and red jets areplotted. As some lines were not detected in B and E and in the Par-Lup 3-4 jets upper limits of 3 were assumed.

o 60 km s 1 are indicated, while speeds reachの見積もり
表の電子密度と電子温度から質量放出率を見積もる

質量放出率と円盤による掩蔽を考慮した質量降着率から・Par-Lup 3-4はjet launching modelと一致
・ESO-Hα 574は大きい誤差があるがこのモデルを棄却はできない

1684

M. C. White et al.

adjacent to the spectral region of interest around the H2 1–0 S(1)line, averaging them and subtracting this averaged continuum image
from each wavelength plane of the data cube.

3.3 Circumstellar environment[Fe II] 1.644 µmのチャネルマップ
Fig. 2 shows channel maps of the circumstellar environment of DG
Tau, as seen in [Fe II] 1.644 µm line emission, with the stellar and
3つの成分
unresolved line emission components removed. The top-left and(i) よくコリメートした高速度Blueshiftジェット
bottom-right frames show the velocity ranges used for continuum
scaling. Here, and in all subsequent figures, the outflow axis is(ii) Blueshiftした中速度のあまりコリメートしていない縁の明るいV字構造
labelled as x, and the axis across the outflow as y. The data have been(iii) Redshiftした分子流Figure 2. Channel maps of the DG Tau outflow. Panels show images of the extended [Fe II] 1.644 µm line emission around DG Tau, binned into 40 km s−1 -wide

Downloaded from http://mnras.oxfordjournals.org/ at National Astronomical Observatory of Japan on May 26, 2014(ii) An intermediate-velocity, less-collimated, edge-brightened,‘V’-shaped structure in the blueshifted outflow. Within approximately 1 arcsec of the central star, the outer edges of this structure are linear, and are aligned radially with respect to the central
star. The opening half-angle of this feature is 15◦ ± 1◦ . AgraAmboage et al. (2011) obtained an opening half-angle of 14◦ forthe same structure from SINFONI data of DG Tau obtained on 2005
Oct 15. This structure is ‘pinched’ ∼1 arcsec from the star, and thenre-expands with increasing distance from DG Tau (Fig. 2, panel[−180 : −140] km s−1 ).
(iii) A redshifted outflow, which becomes visible approximately
0.7 arcsec from the central star. The inner region of this structure is近づく(Blueshift)成分 (下図右)・高速ジェットは歪んだ軌道
・3つのノット(A, B, C)
遠ざかる(Redshift)成分 (下図左)・Blueshift成分とちがって速い成分や尾根がない・泡状の構造. The difficulty in accurately fittings in a larger uncertainty in the knot

hologyce of the DG Tau redshifted outflow,from that of the blueshifted outflow
ly discernible fast outflow, nor ridge-

1687

obscured by the circumstellar disc around DG Tau. We estimate theradial extent of the obscuration, and hence of the DG Tau circumstellar disc, to be ∼160 au, after correction for the inclination of thejet–disc system to the line of sight (38◦ ; Eislöffel & Mundt 1998).
This is in agreement with the measurement by Agra-Amboage et al.
(2011), who used this obscuration to place limits on the disc modelsof Isella, Carpenter & Sargent (2010). The redshifted outflow takes
the form of a bubble-like structure. The material with the greatest
receding line-of-sight velocity is concentrated on the outflow axis,
and at the apex of the bubble. The material along the edges of thestructure emits at progressively lower line-of-sight velocities withdecreasing distance from the central star.
3.3.1 Approaching jet trajectory

The high-velocity blueshifted jet does not travel a linear path, but
bends along its length (Fig. 2, rightmost-top panel). We define theridgeline of the jet as the location of the jet brightness centre at eachposition along the outflow axis. Single-component Gaussian fitswere performed across the jet, at every recorded position along theoutflow axis, on an image of integrated [Fe II] 1.644 µm emissionline flux formed over the velocity range −300 to −180 km s−1 . Thisvelocity range was chosen so that the ridgeline was computed forthe highest-velocity gas, corresponding to the high-velocity jet (seebelow, also, Pyo et al. 2003b). The ridgeline computed from thesefits is shown in Fig. 3(b). The uncertainties in the lateral position of
the fitted ridgeline are of the order of ±0.01 arcsec.
The jet ridgeline was fitted in spatial coordinates with a simple sinusoidal
functionorderµm
to characterize
the nature of the jet trajecFigure 4. DG Tau receding outflow.
(a) Integrated[FeinII] 1.644
line fluxof the receding outflow from DG
Tau.TheTheamplitude
line flux is computed
oversinusoid
the
tory.
of the fitted
is 0.027 ± 0.001 arcsec ≈velocity range 0–300 km s−1 . (b)3.8
Contourplot theof thewavelength
same integrated
II]au, andis [Fe1.035± 0.006 arcsec. Deprojecting
line flux. Contours are labelled in units of 10−15 erg cm−2 s−1 arcsec−2 . The
thisdistancetoaccountforthejet
inclination to the line of sight
position of the central star and the position and size of the occulting disca bothphysical
235 au. If the sinusoidal jet traused during the observations areyields
shown inpanels wavelength
by a yellow starofand
jectory is due to jet precession, the amplitude corresponds to acircle, respectively.

Figure 3. The DG Tau approaching outflow. (a) Integrated [Fe II] 1.644 µmline flux of the approaching outflow from DG Tau. The line flux is computed
over the velocity range −300 to 0 km s−1 . Knots A, B and C are labelled.
(b) Contour plot of the same integrated [Fe II] line flux. Contours are labelled in units of 10−15 erg cm−2 s−1 arcsec−2 . The unlabelled contour corresponds to 170 × 10−15 erg cm−2 s−1 arcsec−2 . Knots A, B and C are

Downloaded from http://mnras.oxfordjournals.org/ at National Astrono

a Gaussian profile, which is extended
h an axial ratio of ∼2.3. This knoty Agra-Amboage et al. (2011), who± 0.03 arcsec along the outflow axis
5 Oct 15. Our positions agree to 1σ .
than knots A and B, at ∼15 per cent2 and 3). As with knot B, knot C istion, but with an axial ratio of ∼1.7.
y Agra-Amboage et al. (2011), with a
05 arcsec along the outflow axis from
5. This agrees with our measurement
position is within their uncertainties.
e recent knot ejection history of DG

M. C. White et al.

Downloaded from http://mnras.oxfordjournals.org/ at National Astronomical Ob

n of knot A have been observed preÅ (Solf & Böhm 1993), [O I] 6300
lley et al. 1997) and He I 10 830 Årmore, Lavalley et al. (1997) reportobserve at ∼0.15 arcsec ≈ 34 au deentral star2 exhibits very little proper
not represents a steady region in the
nced. A feature similar to knot A apof Agra-Amboage et al. (2011, fig. 3
ors did not mention it. We interpretin the jet, resulting from the recoland further on this interpretation in

1686

DG Tau outflows – I. First epoch静止ノットA
X-ray, FUVの観測も考慮するとJet recollimation shockの特徴
X-ray観測からpre-shock flowの速度は400–700 km/s
MHD円盤風を仮定
最も内側のJetの流線は中心星から半径0.01–0.15 AUの位置から出ている
Post-recollimation-shock jetは215 km/s以下まで減速されて[Fe II]のHVCとして観測
Jetは速度と直径を変化させながらまっすぐでない軌道
DG Tau outflows – I. First epoch
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回転しているかはわからない(←強いrecollimation shockを通過したときの効果)
2つのジェットノットB, C
ノット放出の間隔は周期的でないジェットの速度は215 km/sから315 km/sへと増加
速度の変化が動くノットの形成要因かもしれない[Fe II] 1.644 µmの第二の分子流成分を複数成分ガウシアンフィットにより分離
中速度成分は大きく開いた流れ
1688 M. C. White et al.
中心のジェットと広角の分子風の間のshocking,turbulent entrainment layerだろうMulti-epoch Sub-arcsecond [Fe II] Spectroimaging of the
DG Tau Outflows with NIFS. II. On the Nature of the Bipolar
Outflow Asymmetry
M. C. White, G. V. Bicknell, P. J. McGregor and R. Salmeron

前の論文の続き遠ざかる成分のバブル状の構造に焦点を当てている
34

M. C. White et al.

A Parametric Modeling Approach to Measuring the Gas
Masses of Circumstellar Disks
Jonathan P. Williams and William M. J. Best

星周円盤のガス成分の観測からモデルを介して質量を求めようという試み
以前、麻生さんが紹介したため省略いたしますA spider-like outflow in Barnard 5 - IRS 1: The transition
from a collimated jet to a wide-angle outflow?
Luis A. Zapata, Héctor G. Arce, Erin Brassfield, Aina Palau, Nimesh Patel and Jaime E. Pineda

Barnard 5 - IRS1のSMAによる電波輝線・連続波観測
12CO (2–1)

北東–南西方向の高速双極分子流を分解
赤青それぞれ3つの速度領域で異なる構造(i) 低速では大きく開いたコーン状のローブ(ii) 中速の原始星近くの双極シェル(iii) 高速のバレット
結果として蜘蛛のような形態に星風により分子ガスが巻き込まれた結果だろう3698

L. A. Zapata et al.

velocities that are attributed to the presence of molecular outflows.
This is confirmed by our integrated intensity maps showing a clear
bipolar structure, see Figs 1 and 3.
In Fig. 1(a), we show the velocity-integrated intensity, or zeromoment map, of 12 CO(2–1) for both the blue and red outflow lobes.
The velocity range of integration for the blueshifted lobe is from−50.9 to +6.2 km s−1 , while for the redshifted lobe is from +14.7
to +70.8 km s−1 . With our SMA observations, we detect a substantially larger spread of velocities because the SMA data havesignificantly better sensitivity than previous studies (see Velusamy& Langer 1998). The left-hand panel in Fig. 1 shows the wide-angle
bipolar outflow that has been reported in previous high-angular resolution studies of this source (Langer et al. 1996; Velusamy &Downloaded from http://mnras.oxfordjournals.org/ at National Astronomical Observatory of Japan on Ju

Figure 1. (a) SMA integrated intensity (moment 0) colour scale and contour map of the 12 CO(2–1) emission (grey contours), and the continuum emission at
1300 µm (white contours) from B5-IRS1. The blue colour scale represents blueshifted gas, while the red colour scale represents redshifted gas. The integrated
velocity range for the blueshifted side is from −50.9 to +6.2 km s−1 , while for the redshifted side is from +14.7 to +70.8 km s−1 . The white contours range
from 35 to 85 per cent of the peak emission, in steps of 10 per cent. The peak of the continuum emission is 0.032 Jy beam−1 . The grey contours range from 10
to 87 per cent of the peak emission, in steps of 7 per cent. The peak of the 12 CO(2–1) line emission is 150 Jy beam−1 km s−1 . The emission peak here is thearithmetic sum of the total integrated CO emission. The synthesized beam of the continuum image is shown in the lower-left corner. (b) Integrated intensity mapof the B5-IRS1 12 CO(2–1) outflow at different velocity ranges. The different blue and red colour tones of the contours represent different range of velocities
with the lighter (darker) hues representing lower (higher) outflow velocities. The low-velocity blue and red ranges are [−4.3 to +6.2 km s−1 ] and [+14.7 to+24.2 km s−1 ]. The intermediate-velocity ranges are [−39.0 to −15.9 km s−1 ] and [+35.1 to +59.7 km s−1 ], while the high-velocity ranges are [−50.9 to−40.3 km s−1 ] and [+60.2 to +70.8 km s−1 ]. The high-velocity bullets show a larger spread of velocities (see Fig. 4), however, for clarity, we choose theseslightly narrower high-velocity windows. The contours for the different blue and red contours range from about 30 to 90 per cent of the peak emission, in stepsof 5 per cent. In the high-velocity emission, the contours start from 50 per cent the peak of the line emission. The two pink hexagons mark the positions of thestrongest H2 and Hα knots reported by Yu et al. (1999).