Star	  Forma)on	
  Newsle0er	
  #268	
  16-­‐20本目	
麻生 有佑	

Chemical	
  evolu)on	
  in	
  the	
  early	
  phases	
  of	
  massive	  star	  forma)on	
  II:	
  Deutera)on	
  T.	
  Gerner	
  et	
  al.	  2015	Ø 大質量星に対しては進化段階を区別する分子種(chemical	
  clocks)はわかっていない。	
  Ø InfraRed	
  Dark	  CloudàHigh-­‐Mass	
  Protostellar	
  ObjectàHot	
  Molecular	
  CoreàUCHII	  Ø 小質量星D/Hがその指標になると言われ、大質量星でも若いほど高いという先行研究あり。	
  Ø SMT	
  (~0.3	
  km/s,	
  ~30”)で19	
  IRDC,	
  20	
  HMPO,	
  11	
  HMC,	
  9	
  UCHIIを観測(どこもd~4	
  kpc)。	
  Ø 分子種はDCN,	
  DNC,	
  DCO+,	
  N2D+とnon-­‐deuteratedの1.3	
  mm帯。	
  Gerner et al.: Early phases of massive star formation II: Deuteration

結果:	  1) N2D+	
  (3-­‐2)はIRDCとHMPOでのみ検出。T>30	
  Kで消失。	
  2) 24um,	
  70um点源なしIRDCのD
化物はDCO+のみ。	
  3) DCN,	
  DNC,	
  DCO+の検出率は同程度でHMCで最大。	
  Fig. 3. Detection fraction of the 4 observed deuterated species in the di↵erent evolutionary stages. Here the infrared dark cloud (IRDC) stage
is divided into the two subsamples without and with an embedded point source at 24 or 70 µm, indicated in the caption as IRDC(wops) andIRDC(wps), respectively. The detection fractions are shown from left to right with infrared dark clouds without embedded point sources in red(IRDC(wops)), infrared dark clouds with embedded point sources (IRDC(wps)) in grey, high-mass protostellar objects (HMPO) in blue, hotmolecular cores (HMC) in yellow and ultracompact Hii regions (UCHii) in black.

	
  
IRAM	
  30	
  mの1-­‐0も使った。	
  
領域ごとの1-­‐0のTexはモデルがあって、1-­‐0の柱密度を説明するようにRADEXからTex	
  (3-­‐2)を決めた。	
  

T (r) = T in ,r < rin ,COa , HNCa , HCN, HCO+a , HNCO, H2 CO, N2 H+ , CSa , SO
Chemical	
  evolu)on	  in	
  t3he	  arly	
  +p,hases	
  of	
  massive	  tar	
  forma)on	  II:	
  Deutera)on	  OCS,
C2 H, SiO,
CH3 CN, CH
OH,eDCODCN, DNC,
N2 D+ srespectively.
The temperatureand density profiles do no(a)T.	
  Gerner	
  et	
  Minoral.	
  2015	  (続き)	
 observed
isotopologue
with time. The fitted physical quantities are the inner ra
the temperature and density at the inner radius, T in andthe power law index of the density p. The inner radius iØ deutera)on	
  (柱密度の比)とFWHM、H
characteristicsof the twoparts of “MUSCLE-D”, the physical
2柱密度、luminosityの相関をPearson相関係数でbetween 5 ⇥ 10 5 5 ⇥ 10 2 pc. While we assume thmodel in測った。	
  Section 6.3.1 and the chemical model “ALCHEMIC” is an isothermal sphere, the temperature structure of t
in Section 6.3.2.
evolved stages is modeled by a inner flat plateau withàFWHMとの相関係数は<0.5だが、早期に乱流が小さくD比が高いという描像もある。	
  A&A proofs: manuscript no. paper_0315_astropha power-law with slope q = 0.4 as a standard value foGerner et al.: Early phases of massive star formation II: Deuteration
A&A proofs: manuscript no. paper_0315_astrophØ また、早期ほどFWHMが小さい。luminosityとは少し相関、Hは相関なし。	
  (see van der Tak2et
al. 2000). The radial density profil
6.3.1. Physical model
rin is flat with ⇢in and decreases for r > rin as a power
The physical model treats the star-forming region as spherically slope p. The value of p is limited to values between
symmetric 1D-clouds with a fixed outer radius of rout = 0.5 pc, 2.0 in order to save computing time. That range is supp
based on the largest beam size of our observations of 3000 and several observations, e.g. Guertler et al. (1991); Beuth
the typical size of high-mass star forming regions. High an- (2002b); Mueller et al. (2002); Hatchell & van der Tak
gular resolution studies revealed in some of the sources com- The temperature and density profiles are simultaneousplex structures that deviate from the spherically symmetric case The model does not take into account radiative transpo(e.g., Beuther et al. 2002a). However, in single-dish maps these model, the whole cloud is embedded in a larger di↵usources appear to be symmetric (e.g., Beuther et al. 2002b). density medium that shields the high-mass star formin
Since we are analyzing single-dish data, a 1D-model physi- from the interstellar FUV radiation.
cal model appears to be sufficient. More sophisticated models,that takeinto
account complicated substructures, would increaseØ
物理化学モデルで18種をフィット。1D,	
  
rout
pc,	
  inq=0.4,
物理量は進化なし、化学量6.3.2.
Chemical
model
Fig.=0.5	
  6. Spreadfractionsamong
the 4 evolutionary stages for DCN/DNC an
the number of fitting parameters and might lead+ to an
overmore
detections
withinonestage,
theblue box shows the 25%-75% range and+は進化、D化物+高温反応+H
H2 ,	
  temperatureHin3bothのortho/paraも含む。	
  utionarystagesforofDCN/DNC
for detections
molecules
only.
In
case
of
6
or
interpretation
the data.and
TheHCN/HNC
radial density
2,	
  and
The
chemical
model
is
an
versionof theless than 6 data points, only the individualupdated
data points
are shown.
Thetime-de
red solid
oxstructure
shows
the
25%-75%
range
and
the
crossesmark
theremaining
50%
of
the
data
points.
In
cases
of
is
modeledwithgas-grain chemical model “ALCHEMIC” described in SØ パラメーターは物理の4つで、観測された柱密度をstage毎にχ2フィット。	
  ta points are shown. The red solid line shows the median of the ratio of detections
in(2010)
both molecules.
et al.
andwithalreadyused and described in GernØ 前のstageのベストフィットが次のstageの初期値à後ほどフィットは悪い。	
Table 4. Listof species
fittedthe model.
(2014). In addition, the deuterium network from Alberts
p
⇢(r)
=
⇢
(r/r
)
,
r
r
;
in
in
in
and extended with high-temperatu.
Molecules(5) (2013) was addedT⇢(r) = ⇢in ,r < rintions (Harada et al. 2010, 2012; Albertsson et al. 201
Ta ortho/paraa+a H2 , H+ and H+ and+theira isotopolog
statesofq
CO , HNC , HCN, HCO , HNCO,
2 H2 CO,3 N2 H , CS , SO
T (r) = T in (r/rin ) , r rin ;+the chemical network(6)
andbertssonetal.
2014a).
In
total,
co
OCS,
C
H,
SiO,
CH
CN,
CH
OH,
DCO
, DCN, DNC, N2 D+ res
23
3
T (r) = T in ,r < rin ,(a)aMinor isotopologue observed
wit
HHCO2 CO,H+ ,of CS, SO
and N HNvs.2FWHM
non-deuterated
species from HCN (or H CN in case HCN is not
Article number, pag
+

2

+

13

+ from the+
ctively. The dots mark detections, the triangles upper limits. The typical size of an error bar++

This value is limited by the largest 29 IRAM beam size used in our observations.

Table A.5. Parameters of the best-fit HMPO model.

Chemical	
  evolu)on	
  in	
  the	
  early	
  phases	
  of	
  massive	  star	
  forma)on	
  II:	
  Deutera)on	
  Parameter
Symbol Model
Inner radiusr
103 AUT.	
  Gerner	
  et	
  al.	  2015	
  (続き)	
Outer radiusr
0.5 pcDensity at the inner radius
Average density with a beam of 21 700 AU
Average density with a beam of 57 300 AU
Density profile
Temperature at the inner radius
Average temperature
Temperature profile
Lifetime

0
1

⇢0
⇢¯
⇢¯
p
T0
T̄
q

a

1.5 ⇥ 109 cm 3
1.6 ⇥ 106 cm 3
3.7 ⇥ 105 cm 3
1.8
75.8 K
21.5 K
0.4
32 000 yearsØ IRDCは18種とも1桁以内でフィットできた。HMPOは16/18、HMCは14/18、UCHIIは13/18ができた。	  
Ø できなかったものの理由はshock,	
  ouilow,	
  UVは考慮されていなかったり、SOはよくわ
Notes.
かっていなかったり。	
  Gerner et al.: Early phases of massive star formation
II: Deuteration
This value
is limited by the largest 29 IRAM beam size used in our observations.
(a)Table A.4. Parameters of the best-fit IRDC model.
Parameter
Inner radius
Outer radius
Density at the inner radius
Average density with a beam of 26 000 AU
Average density with a beam of 54 000 AU
Density profile
Temperature at the inner radius
Average temperature
Temperature profile
Lifetime

Symbol
r0
r1
⇢0
⇢¯
⇢¯
p
T0
T̄
q

00

Table A.6. Parameters of the best-fit HMC model.
Model
12 700 AU
0.5 pca
1.4 ⇥ 105 cm 3
8.9 ⇥ 104 cm 3
5.2 ⇥ 104 cm 3
1.5
11.3 K
11.3 K0
16 500 years

Parameter
Inner radius
Outer radius
Density at the inner radius
Average density with a beam of 45 400 AU
Average density with a beam of 63 100 AU
Density profile
Temperature at the inner radius
Average temperature
Temperature profile
Lifetime

Symbol
r0
r1
⇢0
⇢¯
⇢¯
p
T0
T̄
q

Notes.

Notes.

Table A.5. Parameters of the best-fit HMPO model.

Table A.7. Parameters of the best-fit UCHii model.

(a) This value is limited by the largest 2900 IRAM beam size used in our observations.

Parameter
Inner radius
Outer radius
Density at the inner radius
Average density with a beam of 21 700 AU
Average density with a beam of 57 300 AU
Density profile
Temperature at the inner radius
Average temperature
Temperature profile
Lifetime

Notes.

Symbol
r0
r1
⇢0
⇢¯
⇢¯
p
T0
T̄
q

Model
103 AU
0.5 pca
1.5 ⇥ 109 cm 3
1.6 ⇥ 106 cm 3
3.7 ⇥ 105 cm 3
1.8
75.8 K
21.5 K
0.4
32 000 years(a) This value is limited by the largest 2900 IRAM beam size used in our observations.

Model
1 140 AU0.5 pca
1.3 ⇥ 108 cm 3
1.7 ⇥ 106 cm 3
9.6 ⇥ 105 cm 3
2.0
162.9 K50 55 K
0.4
35 000 years(a) This value is limited by the largest 2900 IRAM beam size used in our observations.

Parameter
Inner radius
Outer radius
Density at the inner radius
Average density with a beam of 57 800 AU
Average density with a beam of 85 400 AU
Density profile
Temperature at the inner radius
Average temperature
Temperature profile
Lifetime

Notes.

Symbol
r0
r1
⇢0
⇢¯
⇢¯
p
T0
T̄
q

Model
103 AU
0.5 pca
1.0 ⇥ 1010 cm 3
1.3 ⇥ 106 cm 3
7.1 ⇥ 105 cm 3
2.0
244.3 K31 34 K
0.4
3 000 years(a) This value is limited by the largest 2900 IRAM beam size used in our observations.

particles; the estimated oscillator strength pe
nX fX /nH ≃ 9.3×10−6 for the 2175 Å bump (DVaria)on	
  of	
  the	
  ultraviolet	  ex)nc)on	
  law	
  across	
  the	
  Taurus-­‐Auriga	
  star	  forming	
  complex.	
  For completeness, we also note that,

AGALEX	
  based	  study.	
  
Ana	
  I.	
  Gomez	
  de	
  Castro	
  et	
  al.	  2015	ANU V − AK = E(B − V )(0.19 + c1 + 4.49c2 −+ 1.38c3 + 0.85R)
Ø Taurus-­‐Auriga分子雲(TMC)はSPEAR/FIMSを使って、0.2-­‐0.4	
  pcのスケールでハロー(Av<1.5等)に散乱FUVが観測されている。à重力が弱くなる分子雲境界の物理。	
  and thus, (ANU V − AK )/E(B − V ) can be parterms of the strength of the bump and, as aboØ PAHによるNUVの2175	
  A	
  bumpは小さなダスト粒子の存在に最も敏感である。	
  scaling can be made in terms of the extinction la
LoS,	
  (GALEX)とA 	
  (2MASS,	
  UCAC4)からbumpの大きさを決める。	
  Ø ANUVKØ 0.6°のFOVで~200	
  deg2をカバー。	
  Wolf	
  method・・・ある視等級を持つ星の数の累積分
布を減光なしの近くのstellar	  ﬁeldと比べる。大きなサンプ
ルと空間分解能の調整が必要で良くない。	
  Star	
  counts・・・ある減光なし
領域から”期待される”星の数と実際の星の数を比べる。	
  	
  Abump = (2.4 ± 0.5)

ANU V − AK
− (0.9 ± 1.5)
E(B − V )Dust properties in Taurus-Auriga 5
Dust properties in Taurus-Auriga 5though the fit is significantly less accurate (see3

THE GALEX SURVEY OF THE TM

The baseline of the GALEX All Sky Survey wa
in 2007. GALEX AIS covers 26,000 deg2 (∼Sky) and provides broadband imaging in two

Figure 3. Fields observed by GALEX (AIS GR5) towards the
Taurus Molecular Complex (open circles) are overlaid on themap of hydrogen column density (NH ) produced by LLA10 from
2MASS star counts.

limits are well above the magnitude of M-type stars at the
distance of the Taurus-Auriga molecular complex. J mag-Figure 4. Density of NUV GALEX sources in the TMC. The
densities are colour coded in stars per 3 arcmin2 (see lateral bar).
The 2MASS extinction map (LLA10) is overlaid for reference. The
location of the main molecular cores and the main UV sources in
the field (asterisks) are marked.

Lombardi et al (2010) from the 2MASS survey of the TMC.

Varia)on	
  of	
  the	
  ultraviolet	  ex)nc)on	
  law	
  across	
  the	
  Taurus-­‐Auriga	
  star	  forming	
  complex.	
  AGALEX	
  based	  study.	
   8 A.I. Gómez de Castro et al.
Ana	
  I.	
  Gomez	
  de	
  Castro	
  et	
  al.	  2015	
  (続き)	
ANU V /AK across the region. ANU V /AK ≃ 33 in the diffuse ISM, around the TMC in agreement with FM07. However, westwards, at the tail of the cloud, where the main
filaments reside, and the column density of molecular gas
increases, ANU V /AK decreases pointing out the weakeningof the UV bump and, in general, a larger average size of the
NUV
K compared with the diﬀuse ISM. This trend
dust
grains whenis confirmed at both intermediate resolutions.
Some of the areas mapped by GALEX have very low
and thus, uncertain, AK values (LLA10 estimates dAK =±0.04 mag). This results in abnormally high ANU V /AKrates, especially at high galactic latitudes (see Fig. 8).
Experimentally, the UV bump is known to be producedby mixtures of suﬃciently large, neutral PAHs (Steglich etal. 2011). Moreover, the UV-visible measurements provide
a reliable fingerprint of the presence of specific PAHs since
the electronic transitions of these species are detected inthis range while the near infrared vibrational bands are notmolecule specific.
A recent UV-visible (3050-3850 Å ) study based on
the observations towards five lines of sight with moderate reddenings measured PAHs abundances two orders ofmagnitude smaller than those in the diﬀuse ISM (Gredel
et al. 2011); the measurements were made over column
densities of NH = 5.7 − 9.2 × 1021 cm−2 , slightly above
the dominant column density of our study in the TMC,
NH ! 4 × 1021 atoms cm−2 . This study was sensitive tomolecules such as anthracene, pyrene or benzofluorene. Laboratory experiments suggest that the UV bump is producedby larger PAHs with sizes above 50-60 carbon molecules(Steglich et al., 2010) thus, our results suggests that large
PAHs are neither abundant in traslucent clouds.
ANUV /AK is small close to the filamentary networks(compare Fig 3 with Fig 8) where also mid infrared data
have detected the formation of large dust grains (Flagey etal. 2010), as high density of molecular gas makes collisional
processes more eﬃcient assisting grain growth. In addition,
the large density of dust in the filaments eﬀectively shields
the growing mantles against the environmental UV radiation. A detailed comparison between Figure 4 and 8, showsthat the bump is less prominent towards the tail of the fil-

結果:	
  	
  
西のmain	  ﬁlamentsでA /A が減少し、大きいダスト粒子を示唆する。	
  UV	
  bumpは50-­‐60個の炭素のPAHが作るので、そのくらいのPAHが少ないことを示唆する。	
  (smaller	
  PAHが少ないことはわかっていた。)	
  ANUV/AKはﬁlament	
  networksの近くで小さい。	
  これは高密度ガスが衝突を励起してダストの成長を促して、大きい粒子がUV輻射を防ぐためと考えられる。	

Figure 8. ANU V /AK on the TMC computed for bins of
24 arcmin2 and 12 arcmin2 , top and bottom panels respectively. The gray scale runs from ANU V /AK = 0 (black) to
ANU V /AV " 33 (white). ANU V /AK " 33 corresponds to thepredictions of the standard ISM extinction law (see Table 1).

The	
  Impact	
  of	
  Dust	  Evolu)on	
  and	
  Photoevapora)on	
  on	
  Disk	  Dispersal	
  U.	
  Gor)	
  et	
  al.	  2015	
(AbstractとConclusionsだけ。。。)	
  Ø 粘性、EUV+FUV+X線の光蒸発、ダスト粒子のradial	
  drio、ダストのサイズ進化、ガス円盤の進化を含む1+1Dモデル。	
  Ø ダスト進化はBirns)el,	  Ormel	  &	
  Dullemond	
  (2011)のcollision-­‐fragmenta)on平衡	
  
	
  
結論	
  
1. ダストの断面積はFUVによるmass	
  loss	  rateで決まり、断面積が大きいと円盤は早く散逸する。しかし、その依存性はとても小さい。	
  2. coagula)on/fragmenta)onを含むと、円盤の表面積が減るほど小さい粒子が増え、ダストの乱流速度とsha0eringを上げる。円盤の寿命は2倍小さくなる。	
  3. ダスト進化が円盤の寿命に与える影響は小さいが、表面積の進化に与える影響は大きい。	  4. 寿命と粘性の関係はα^(–1.2)。粘性が低いダストだとradial	
  drioが大きく、g/dが増える。	
  5. 光蒸発によって惑星形成のための不安定が起きやすいg/d~50-­‐10が達成できる。
g/d~50で2-­‐15	
  MJ、g/d~10で1-­‐2	
  MJのガスが残る。10になってから0.5-­‐1	
  Myrで完全に散逸する。	
  
6. 残ったガスやダストがコアに降着するとC,	
  N,	
  Oなどがenhanceされる。	
  7. ダスト質量は55%が粘性とドリフトで中心に落ち、15%が光蒸発でなくなり、30%が残る。	

Isola)ng	
  signatures	
  of	
  major	
  cloud-­‐cloud	  collisions	
  using	
  posi)on-­‐velocity	
  diagrams	
  
T.	
  J.	
  Haworth	
  et	
  al.	  2015	Ø 大質量星(やsuper	
  star	  clusters)は形成途中で輻射が質量降着を止めるという問題があるが、分子雲衝突なら解決できる。	
  Ø しかし、i)	
  a	
  few	  Myrのスケール,	
  ii)	
  GMC同士の衝突は10	
  Myrに1回,	
  iii)	
  フィードバックで衝突の証拠が消される,	
  iv)	
  銀河の腕などISMが複雑で星形成に足る衝突なのか区別できない、ので観測が困難。à観測され得るサインをモデル擬似観測で調べる。	
  Ø グリッド、流体、ENZO、違う2つの雲、乱流、理想雲、正面衝突、3	
  km/sと10	
  km/s。	
  Ø 2つの雲は半径7.2	
  pcと3.5	
  pc、乱流1.71	
  km/sと1.25	
  km/s、平均密度25.3	
  cm–3と47.4	
  cm–3。	  
Ø 0.3×104	
  cm–3でコア、空間分解能は0.06	
  pc	
  Ø 大質量星からの輻射を扱うDale	
  et	
  al.	  (2012,	
  2013)のJ,	
  UP,	
  UQという3つのSPHモデルとも比較(衝突していない)。	
  Signatures of cloud–cloud
5 1-­‐0のPVØ TORUSでnon-­‐LTE輻射輸送を解いて擬似観測。分解能0.04	
  km/s,	
  0collisions.2	
  pc。12CO	
  図。	
   Table 1. Summary of the numerical models post processed in this paper.
Model
ID

ScenarioA
B
C
D

Turbulent clouds coincident along the line of sight
Turbulent clouds collided at 10 km/s
Turbulent clouds collided at 3 km/s
A cloud that has evolved in a galactic discJ

A gravitationally bound cloud withinternal radiative feedback
A partially gravitationally unbound cloud withinternal radiative feedback
A partially gravitationally unbound cloud withinternal radiative feedback

UP
UQ

OriginSurface densiity
snapshotp–v diagram

Takahira et al (2014)
Takahira et al (2014)
Takahira et al (2014)
Benincasa et al. (2013)(Shima et al. in prep.)
Dale et al (2012, 2013)

Fig 1, top panel
Fig 1, middle panel
Fig 1, bottom panel
Fig 2

Fig 5, top panel
Fig 5, middle panel
Fig 5, botom panel
Fig 8

Fig 3, top panel

Fig 6, top panel

Dale et al (2012, 2013)

Fig 3, middle panel

Fig 6, middle panel

Dale et al (2012, 2013)

Fig 3, bottom panel

Fig 6, bottom panel

Isola)ng	
  signatures	
  of	
  major	
  cloud-­‐cloud	  collisions	
  using	
  posi)on-­‐velocity	
  diagrams	
  
T.	
  J.	
  Haworth	
  et	
  al.	  2015	
  (続き)	

J. Haworth et al.
6 T. J. Haworth et al.

←衝突軸と視線は同じ。	
  
<衝突>	
  10	
  km/sでbroad	
  bridge。3km/sでは中心低速のスパイクのみ。	
  <輻射>	
  球状HII領域は実は95%光子が漏れるため、期待される楕円構造は見えない。	
  ∴broad	  bridgeが衝突でのみ見られる。	
  	  Ø Mopra、12CO	
  1-­‐0観測と比較→	
  (rms~0.2	
  K,	
  0.9	
  km/s)	
  Ø M20	  (d=1.7	
  kpc)、O7星含む。	
  Ø 同じスケールのbroad	
  bridgeが見える。	
  Ø 今回の速度条件でviewing	
  angleを変えると4π中20-­‐30%でbridgeが見える。	
  8

T. J. Haworth et al.

12 CO J=1-0 position–velocity diagrams of the enzo

Figure 6. 12 CO J=1-0 position–velocity diagrams for the feedloud–cloud
collisions.
The
upper
panel is for a simofFigure
Dale et 6.
al. 12From
top to bottom
the panelsdiagrams
areFigure5. 12 CO
J=1-0
position–velocity
diagrams backof thesimulations
enzo
CO J=1-0
position–velocity
for the feedpshot justprior
the collision(the clouds
justpanel ismodels
UP and backUQ. simulations of Dale et al. From top to bottom the panels aremodelsof tocloud–cloud
collisions.
The areupper
for a J,
simthe 10ulation
km/s collision
with toboth
along
snapshotmodel,
just priortheclouds
collision(the clouds are justmodels J, UP and UQ.
ght. The
middle andlowerpanelscollision
are frommodel,
the 10withand both clouds along
touching)
in the10 km/sion models
respectively
at thepointandof maximum
coreare from the 10 andthe lineof sight. The
middlelower panels
n each model
2.1.1).
5 km/s (c.f.
collisionmodels respectively at the point of maximum coreformation in each model (c.f. 2.1.1).

(左)	
  上から衝突前、10	
  km/
s,	
  3	
  km/s	  (右)	
  上からJ,	
  UP,	  UQ	c 2012 RAS, MNRAS 000, 1–12
c 2012 RAS, MNRAS 000, 1–12

Figure 10. MOPRA 12 CO J=1-0 position–velocity diagram oservations of candidate broad bridge features towards M20,
young site of massive star formation.

→観測。上が右の白四角、下が左。	

To check our simple estimate we produce p–v diagram
over a range of di↵erent viewing angles. To summarise th
results of this process we calculate the mean profile over th
middle of the p–v diagram where the bridge feature is foun
For the 10 km/s collision model this is shown for a selectioof example ✓ in the top panel of Figure 11. At some viewin
angles two peaks in the p-v diagram are discernible and w
conclude that the broad bridge can be identified, whereas
others there is a single (albeit broad) peak and the broa
bridge is not identified. We create a grid of viewing angl
spanning ✓ = 0 to 90 in 10 degree intervals and = 0THE	
  GOULD	  BELT	
  ‘MISFITS’	  SURVERY:	
  THE	  REAL	
  SOLAR	  NEIGHBORHOOD	
  PROTOSTARS	  Amanda	  Heiderman	
  &	
  Neal	  J.	
  Evans	
  II	
  2015	12Ø 2-­‐25	
  umのスペクトル指数αによるClassと、物理構造から定義されるStageがある。	
  Ø Stage	
  0:	
  Menv>M*+Md,	
  Stage	
  I:	
  Menv<M*+Md,	
  Stage	
  II:	
  Menv~0	
  Ø αやTbolはinclina)onが大きいと進化の指標としてmisleading。	
  Ø Menv>0.2	
  MoとHCO+	
  4-­‐3	
  TMB	
  ΔV>0.4	
  K	
  km/sはStage	
  0+Iによく対応。	
  Heiderman & Evans

Ø MIsiden)ﬁed	
  YSOs	
  from	  SED	
  FITS	  Survey、ClassとStage	
  0+Iの関係を統計調査。	
  Ø APEX,	
  CSOでHCO+	
  4-­‐3と3-­‐2を観測。	
  Ø 4-­‐3を過去観測と比較して、3-­‐2ではTMB	
  ΔV>0.68	
  K	
  km/sがStage	
  0+Iとする。	
  Ø sub-­‐mm連続波が円盤より広がっているかチェックà概ね一致。	
  Ø Class	
  IIの)mescaleを2	
  Myrと仮定するとStage	
  0+Iは0.51-­‐0.62	
  Myr。(Class	
  IIは~4Myrかも)	
  Ø HCO+	
  3-­‐2の積分強度とα,	
  Tbol,	  Lbolには正、負、正の相関。検出比でも同様。	
  

THE	
  GOULD	  BELT	
  ‘MISFITS’	  SURVERY:	
  THE	  REAL	
  SOLAR	  NEIGHBORHOOD	
  PROTOSTARS	  Amanda	  Heiderman	
  &	
  Neal	  J.	
  Evans	
  II	
  2015	
  (続き)	

THE	
  8GOULD	  BELT	
  ‘MISFITS’	  SURVERY:	
  THE	  REAL	
  &SOLAR	  Heiderman
Evans NEIGHBORHOOD	
  PROTOSTARS	  Amanda	  Heiderman	
  &	
  Neal	  J.	
  Evans	
  II	
  2015	
  (続き)	
Table 4
HCO+ J = 3 → 2 Detection Statistics for Cloudsa
Cloud
(1)

D
(pc)
(2)

Size
(pc)
(3)

0+I
Y
(4)

0+I
N
(5)

Flat
Y
(6)

Flat
N
(7)

II
Y
(8)

II
N
(9)

V
(km s−1 )(10)∆V(km s−1 )(11)

Number
Stg 0+1b(12)

AquilaAuriga/CMC
Auriga North
Cepheus 1

260
450
450
300

7.56
5.98
1.31
1.75

66
28
1
5

15
5
0
0

39
5
0
2

21
3
0
1

13
6
0
0

26
1
0
1

288
325
200
150
178
130
950

1.75
1.08
1.07
1.30
1.78
0.98
4.42

4
0
0
3
1
5
8

2
0
0
1
1
1
5

0
0
3
1
0
2
0

1
1
0
4
0
2
2

0
0
0
2
1
0
0

1
0
0
5
0
1
3

IC5146 NW
Lupus I
Lupus III
Lupus IV
Lupus VI
Musca
Ophiuchus

950
150
200
150
150
160
125

5.28
1.68
2.22
0.90
1.46
1.47
3.08

13
0
1
0
0
0
24

0
1
1
1
1
1
3

3
0
0
0
0
0
26

1
2
5
0
0
0
14

0
0
0
0
0
0
1

0
0
1
0
0
0
2

Perseus

250
250
130
429

4.83

66

7

18

16

1

0

...
3.92

0
15

1
2

0
13

1
2

0
4

0
1

3.0
1.8
1.9
1.3
1.0
1.3
...
1.4
1.7
0.8
2.9
1.2
1.3
2.0
0.8
...
...
...
...
1.8
1.3
2.0
2.7
...
2.1
1.6

97
30
1
5

Cepheus 3
Cepheus 4
Cepheus 5
Chamaeleon I
Chamaeleon II
Corona Australis (CrA)
IC5146 E

7.4
0.9
-6.9
-4.4
-2.9
2.6
...
-8.0
4.8
2.9
5.2
6.5
8.1
4.2
4.9
...
...
...
...
3.1
4.6
5.3
7.8
...
7.6
9.6

240
0.83

48
0.17

112
0.60

76
0.40

28
0.40

42
0.60

Scorpius/OphN
Serpens
TotalcFractiond

Notes
(13)

stronger
weaker

4
0
3
2
1
7
7
stronger
11
0
1
0
0
0
45

stronger77
stronger
028

stronger319
0.58

Note. — Columns are : (1) Cloud Name; (2) Cloud Distance in parsec; (3) Average Cloud Size in parsec; (4) Number of detected
Class 0+I sources; (5) Number of undetected Class 0+I sources; (6) Number of detected Flat SED sources; (7) Number of undetected
Flat SED sources; (8) Number of detected Class II sources; (9) Number of undetected Class II sources; (10) Cloud velocity (seeSection 5); (11) Cloud line width (see Section 5); (12) Number of cloud sources classified as Stage 0+1; (13) Comparative notes on
average cloud HCO+ spectra.
a Only clouds with at least 1 observed source are included in the table.
b Counts only detections above the threshold value of integrated intensity.
c Total number of sources separated by class that are detected or undetected or are classified as Stage 0+1.
d Fraction of sources in each column compared to total number surveyed.