Star formation news letter# 275 61-65本目	
• 大橋聡史	

2Spitzer	  SAGE	  surveyでYSO	  candidates	  が同定されてきた(LMC)。が分解能が悪くおそらくcluster	  VLT/SINFONI	  K-­‐band(cont),	  H2,	  HeIの高分解能観測を3つのYSOに行った	  6つ同定できた	  	J.L. Ward, J. M. Oliveira, J.Th. van Loon, M. Sewilo

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J.L. Ward, J. M. Oliveira, J.Th. van Loon, M. Sewilo

Table 1. Properties of Spitzer YSOs analysed in this paper. YSO02 has been included for completeness using the values fromSewi!lo et al. (2010). The value for envelope mass is not included in Sewi!lo et al. (2010). The S09 group refers to the YSO classifications
by Seale et al. (2009; S09) where P type sources show prominent PAH emission, PE sources show strong PAH and fine-structure emission.
All three of the targets observed in this work have been classed as definite YSOs by Gruendl & Chu (2009) and by Carlson et al.
(2012). The bolometric luminosities and masses for N113-YSO01, N113-YSO03 and N113-YSO04 are from new SED fits using existing
photometry (see text for full details).

TargetN113-YSO02

Spitzer Source

S09 group

log(Lbol /L⊙ )Central Mass (M⊙ )+0.29
4.51−0.30

13±2Envelope Mass (M⊙ )AssociatedMaser emissio+0.18+0.3+6.3
N113-YSO01
Y051317.69−692225.0PE
5.18−0.08
32.3−0.7
1.8−0.2×102
H2 O+0.28+2.3
N113-YSO03
Y051325.09−692245.1
P
5.27−0.27
35.3+12.8
1.6−1.1×102
H2 O, OH
−0.9+0.31+13.9
Y051321.43−692241.5 1PE
5.24−0.51
34.3−15.8
1.2+33.3×102
H2 O−0.6 squares)
FigureN113-YSO04
1. Top left panel:wide field Hα image of N113
with positions
of YSOs fromSewi!lo et al. (2010)(cyanand the region
shown in the main image marked (green rectangle). Main image: three colour Hα (red), IRSF Ks-band (green) and IRSF H -band (blue)(Kato et al. 2007) composite showing positions of the observed N113 SINFONI FOVs (green squares) and YSO candidates identified
4 J.L. Ward, J. M. Oliveira, J.Th. van Loon, M. Sewilo
in this work (red circles). Also included are the spectroscopically confirmed Spitzer YSOs (red squares), the Herschel YSO candidates(green circles; Seale et al. 2014), the water maser positions (white circles) and the position of the OH maser (yellow circle). TheSINFONI
Table 1. Properties of Spitzer YSOs analysed in this paper. YSO02 has been included for completeness using the values
from red circles represent the region from which a spectrum was extracted for each continuum source whilst all other symbol sizes
are representative of the spatial accuracy of the data.
Sewi!lo et al. (2010). The value for envelope mass is not included in Sewi!lo et al. (2010). The S09 group refers to the YSO classifications

VLT	by Seale et al. (2009; S09) where P type sources show prominent PAH emission, PE sources show strong PAH and fine-structure emission.
All three of the targets observed in this work have been classed as definite YSOs by Gruendl & Chu (2009) and by Carlson et al.
Theeﬀect of this poor spatial resolution in Spitzer imagery(2012). The bolometric luminosities and masses for N113-YSO01, N113-YSO03 and N113-YSO04 are from new SED fits usingexistingphotometry (see text for full details).
is that many Spitzer sources classified as YSOs will in fact

TargetSpitzer Source

S09 groupN113-YSO02
N113-YSO01
N113-YSO03
N113-YSO04

Y051317.69−692225.0
Y051325.09−692245.1
Y051321.43−692241.5

PEPPElog(Lbol /L⊙ )Central Mass (M⊙ )+0.29
4.51−0.30

13±2+0.18
5.18−0.08+0.28
5.27−0.27+0.31
5.24−0.51+0.3
32.3−0.7
35.3+12.8
−0.9
+13.9
34.3−15.8

Envelope Mass (M⊙ )+6.3
1.8−0.2
×102+2.3
1.6−1.1×102
2
1.2+33.3−0.6 ×10

1 and YSO-2 from Sewi"lo et al. (2010) but add the prefix
N113- (N113-YSO01 and N113-YSO02) and add two additional YSOs in N113 (N113-YSO03 and N113-YSO04).
be multiple objects which may exhibit a wide range of charIn order to compare the massive YSO population ofacteristics. The physical properties of the sources based on
AssociatedMaser
theemission
Spitzer data may apply to groups of objects rather thanN113 with that of the Milky Way we require a suitable
Galactic data set. The Red MSX2 Source Survey (RMSindividual sources.
Survey; Lumsden et al. 2013) provides the most comprehenH2 O
LHA 120-N113 (hereafter N113, Henize 1956) is an acsive catalogue of Galactic massive YSOs and Ultra-compact
H2 O, OHtive
H ii regions to date. H - and K -band infrared spectroscopy
H2 Ostar forming region within the LMC which contains
a number of Spitzer and Herschel YSO candidate sources
has been carried out for a large number of these objects byFigure
SINFONI-bandContinuumemission
N113-YSO03,
N113-YSO04,
N113-YSO01.
regionsshow(see Fig.
1). 2.We
presentK K-band
observationsof maps.
three Leftof to right:
Cooperet al. (2013,
henceforth
C13). ThisMarked
Galacticsample

UCHII	  03A,	  04B	  (2.13u	  He	  I)	  OuQlow	  	  03C	  H2	  emission	  Massive	  YSO	  	  03B	  	  a	  point	  source	  Br	  γ,	  weak	  He	  I	  	  イントロ	  OuQlowはX	  windとdisc	  window	  modelがあり、T-­‐tauriの晴れ上がった段階ではopWcalからNIRでcolimateしたmicro	  jetが観測されている	  またintermediate	  velocityのforbidden-­‐lineが検出、steady	  stateなouQlow	  modelでは説明できずshock	  excitaWon	  mechanismが必要	  Entrainmentがsupersonic	  jetとまわりのガスでturbulent	  mixing	  layerをつくりshockを生成	  Turbulent	  mixing	  layerはKelvin-­‐Helmholtz	  instabilityで生成されるので、jetがまわりの層を破壊したりKHIがﬂowの増加でMach	  numberの変化で減少する問題が	  ただトロイダル磁場によってshock面でKHIを起こすかも	  つまりentrainmentがおこればintermediate	  ouQlowを起こせる	Model	  	IonizaWon	  fracWonからFeの観測値を予測	  DG	  Tauと一致	L	  1688	  cloud	  (intermediate	  –	  low	  mass	  acWve	  star	  formaWn	  region)を近赤で12年間観測し、propoer	  moWonを測定	  YSOsのradial	  velocity	  dispersionを計測	  	  ExWncWonがひどいので各center	  posiWon
からのrelaWve	  proper	  moWon	

R.A,	  Dec方向とも	  1km/sの速度分散を持つ.	  13COの速度分散とconsistentでgasのvirialとも合う	  Dense	  coreでは0.25	  km/s	  (N2H+)と求められている	  	  磁場かglobal	  collapseか星をencountさせて速度分散をかせぐ	  磁場の場合、重力ポテンシャルと同等だとすると100-­‐300uG	  	  External	  forceやはやりのﬁlament	  accreWonもありうるかも	SOFIAを使ってNH3	  32+-­‐22-­‐	  1.8	  THzの観測	  Infallによる吸収線からinfall	  rateやaccreWon	  rateを見積もった	モデルﬁtした,合わないのはouQlow成分と自己吸収	  Infall	  rateは~10-­‐3	  Msun/yr	  (0.03-­‐0.3	  vﬀ),	  infall	  velocityとvirial	  parameterに相関	  Infall	  は重力が主な担い手	  D-­‐wind	  modelによるouQlowでH2Oのproﬁleを再現	  Ion-­‐neutral	  fricWonでheaWng,	  C-­‐type	  shock	  	  Keplar	  disk上でMHDによるouQlow	  Launchする半径によって	  
温度も速度も依存	すべてのclass	  0天体がkeplar	  diskをもち	  H2Oは3-­‐25AUから出ている	  	  Class	  1ではH2Oの線幅が狭くなっているので	  H2Oのabundance減少か、回転が遅い