A multiwavelength study of embedded clusters in W5-east,
NGC 7538, S235, S252 and S254-S258
L. Chavarr ́ıa,1,2,3,4‹ L. Allen,5 C. Brunt,6 J. L. Hora,2 A. Muench2 and G. Fazio2(背景) high mass star forming regionとlow massで違いはあるのか？
(手法)
Spitzer, NIR(→星の同定), ミリ波(CO line)で大質量星形成領域を調べた。
(結果)
3021個のYSOを同定( Class Iが539個、Class IIが1186個)
Class Iの方がIIよりhierarchicallyで分子雲の濃いところに集中していた41のクラスターを同定 (そのうち15個は本論文で初めて同定)(解釈)
MEC (massive star embedded cluster)とLEC (low-mass star embeddedcluster) を比較。→際立った違いは見つからなかった。
↓フィラメントで星が生まれ、その後乱流によってdynamicalにYSOが中心付近に集まる、というシナリオを支持

26 L. Chavarrı́a et al.
mean: 相関なし、peak:MEC is higher

Study of embedded clusters

25

YSOの数26

L. Chavarrı́a et al.
26

L. Chavarrı́a et al.

values.

Figure 26. Corrected number of cluster members and molecular mass above
Figure 23. Embedded clusters K-band extinction. Left: the upper charts
AK = 0.8 mag (M0.8 ). The dotted line shows the best fit to the data usingshows the mean AK for LEC selectedand MEC.clusters.
The lower chart show the meanorthogonal regression. The error-bars are derived from the N∗ YSO values
AK versus the number of cluster members. Right: the same for the peak AKobtainedmass
with "abovenumbervalues. Figure 26. Corrected
HM in the range −1.21 ± 0.5 (see Appendix C).
Clustername of cluster members
Q
Qand molecular

AK = 0.8 mag (M0.8 ). The dotted line shows the best fit to the data using SFEもほぼ一定値
orthogonal regression.
The error-bars areAFGL4029
0.79derived
0.74 from the N∗ YSO values
obtained with " HMin the range −1.21 ±0.5 (seeAppendix C).
S235AB
0.670.74
S252A
0.750.79
S255-2 and S255N 0.76
0.94
NGC 7538
0.680.76
III

何とも相関がない
乱流によって支配されている
Figure分布に違いはない
24. Distribution of clusters CO linewidth (FWHM). The thermal
broadening for a 30 K cloud is ∼0.3 km s .
13−1

Figure 24. Distribution of clusters 13 CO linewidth (FWHM). The thermal
broadening for a 30 K cloud is ∼0.3 km s−1 .

Figure 27. Star formation efficiency (SFE) in embedded clusters. The chartshows the SFE for the corrected number of cluster members (N *YSO ).

Figure 24. Distribution of clusters 13 CO linewidth (FWHM). The thermal
broadening for a 30 K cloud is ∼0.3 km s−1 .

Ginsburg et al. (2011). This source is also identified as the outflow counterpart
by Deharveng
et al. (2012),clusters.
corresponding
to theirFigure 27. Star formation
efficiency(SFE) in embedded
The chart
Herschelpoint source
BRC14-c1.
shows the SFE for thecorrected
numberof cluster members (N *YSO ).

Downloaded from http://mnras.oxfordjournals.org/ at National Astronomical Observatory of Japan on April 10, 2014Figure 21. Structural Q parameter (QYSO) for26.
clustermembers.
BlackFigure
Corrected
numberof cluster members and molecular mass above
Figure 23. Embedded clusters K-band extinction. Left: the upper chartssquares correspond to MEC while empty squares correspond to LEC.
AK = 0.8 mag (M0.8 ). The dotted line shows the best fit to the data usingshows the mean AK for LEC and MEC. The lower chart show the mean
Figure 19. Clusters mean (left) and peak (right) YSOs surface density.
orthogonalregression. The error-bars are derived from the N∗ YSO values
A versus the number of cluster members. Right: the same for Table
the peakK
6. AStructural
Q parameThe histograms (upper charts) show K
the ! YSO distribution for all clusters
obtainedvalues.
ter for different YSOs
classeswith
in " HM in the range −1.21 ± 0.5 (see Appendix C).

(grey), MEC (continuous line) and LEC (segmented line). The YSOs surface
densities versus the number of cluster members are shown in the lowercharts. The crosses show the values obtained by Gutermuth et al. (2009)
Figure23. Embedded clusters K-band extinction. Left: the upper charts
in LEC. Dotted lines in the lower-right chart enclose most clusters (exceptshowsthemean7538)
AK forMEC.
The lowercluster NGCand LEC
show anda weakcorrelation
withchart
indexshow
0.8 ±the0.2meanandAKcorrelation
versus theindex
numberofcluster
members.
Right:
thesameforthepeak
AKr = 0.75.

Downloaded from http://mnras.oxfordjournals.org/ at National Astronomical Observatory of Japan on April 10, 201

Downloaded from http://mnras.oxfordjournals.org/ at National Astronomical Observatory of JapanDownloaded from http://mnras.oxfordjournals.org/ at National Astronomical Observatory of Japan on April 10, 2014

濃い分子雲の重さ

The Phases of Water Ice in the Solar Nebula
F. J. Ciesla, Accepted by ApJL, http://arxiv.org/pdf/1402.5333(背景)
amorphous iceはガス粒子を貯めこんで太陽系内を運べる。
原始太陽系星雲でどうやってamorphous iceを作るか？
気相からの水分子のfluxが小さい→最小エネルギーの状態が実現→crystalline
気相からの水分子のfluxが大きい→amorphous (不定形)
Kouchi et al. 1994 : T<20K でamorphousになる→円盤では不可能(この論文)
Kouchi et al. ではhexagonally crystalline water iceを考えていたが、この著者はpolycrystalline iceを考えてみた。データはKouchi et al.からもってきた。
その結果、amorphous ice は依然考えられていたより作られやすい。T<70Kでできる。
円盤表面でamorphous iceは形成可能である。
→gas 粒子や揮発性元素を円盤外側で氷にもっておける。

polycrystalline ice
いままでのcriticalﬂux
The AstrophysicalJournal Letters,
784:L1 (4pp), 2014 March 20
amorphous

crystalline

表面赤道面

Figure 1. Black lines show the critical flux (Fc ) for amorphous ice formation
vs. temperature for a substrate of hexagonal ice (Ih , solid) and polycrystalline
ice (Ip , dashed) from Kouchi et al. (1994). The flux of condensing water atthe disk midplane for a minimum mass solar nebula (MMSN, red) and for anirradiated disk with surface density Σ = 2000(r/1 AU)−1 g cm−2 (irr, blue) arealso shown.
(A color version of this figure is available in the online journal.)(D = 1.74 × 105 exp(−4590/T) cm2 s−1 ; Kouchi et al. 1994).

leaving negligible w
temperatures wher
However, a rese
detected in the pro
Herschel Space O
water vapor is infe
most of the obser
from the central sta
desorption would b
to result from thegrains at the disk s
photons liberates aet al. 2009). Wate
would not remain
at the low temperat
not photodissociate
To explore howout again in this mvapor in a column
a surface density(values close to thvalues would be excolumn to be isoth
higher temperaturestar, the temperatu

THE ROLE OF TURBULENCE IN STAR FORMATION LAWS
AND THRESHOLDS
Katarina Kraljic, Florent Renaud, and Fr ́ed ́eric Bournaud(背景)
Kennicutt-Schmidt relation (Σgas SFR)
(手法)RAMSESを使ったシミュレーション。darkmatterの運動を解く(結論)
transitionは
1. 亜音速乱流から超音速乱流への遷移
2. self-shieldingとは関係ない

マッハ数低い→ずれる

5

Fig. 8.— The local surface density of the star formation rate asa function of surface density of gas for the MWPC model. The
color indicates the Mach number (panel a), temperature (panel b)
and velocity dispersion (panel c) in each beam. The dotted line
indicates a power-law of index 3/2. Note that regions at high Σgas
and high ΣSFR that have high temperatures represent unresolved
dense gas situated on the Jeans polytrope (see Section 2.2).

considered solely. Some recent studies (e.g. Eales et al.

Chemical abundances of the high-latitude Herbig Ae Star PDS2
C. R. Cowley,1‹ S. Hubrig2 and N. Przybilla3ABSTRACTThe Herbig Ae star PDS2 (CD −53◦ 251) is unusual in several ways. It has a high Galactic latitude, unrelated to any known starforming region. It is at the cool end of the Herbig Ae sequence, where favourable circumstances facilitate the determination of stellar
parameters and chemical abundances. We find Teff = 6500K and log(g) = 3.5. The relatively low v sin (i) = 12 ± 2 km s−1 made it
possible to use mostly weak lines for the abundances. PDS2 appears to belong to the class of Herbig Ae stars with normal volatile anddepleted involatile elements, thus resembling the λ Boo stars. The intermediate volatile zinc consistently violates this pattern.

2462

C. R. Cowley, S. Hubrig and N. Przybilla

Figure 8. Logarithmic abundance differences between PDS2 and the solar
photosphere versus condensation temperatures Tc from Lodders (2003).
Data points are the lower-left corner of the chemical symbols. An average
error bar is shown at the lower-left corner. Individual values are in Table 2.

Tauri and post-asymptotic giant branch stars, objects with vastly

Molecules, dust, and protostars in NGC 3503
N. U. Duronea1,3, J. Vasquez1,2, G. A. Romero2,5, C. E. Cappa1,2, R. Barba 4
́ , and L. Bronfman3

NGC3503という星形成領域のfollow-up観測
電離面の拡大 HII領域と分子雲・星形成の関わり
CO(2-1), 13CO(2-1), C18O(2-1), HCN(3-2)@APEX, ATLASGAL 870μmcont.
電離ガスは母天体分子雲に向かって広がっている
N. U. Duronea et al.: Molecules, dust, and protostars in NGC 3503

46 00
47 00

NGC 3503

DECLINATION (J2000)

UKST
48 00
49 00
−59 50 00

PIS 17SFO 62

51 00
52 00
53 00
02 00

30

11 01 00

00 30

RIGHT ASCENSION (J2000)
Fig. 1. UKST red plate image of the nebula NGC 3503 in the area covered by the APEX data. The positions of NGC 3503, the bright rimmed cloudSFO 62 , and the open cluster Pis 17 are indicated.

nent of 7.6 × 103 M" in mass having a mean radial velocity1of −24.7 km s−1 (in agreement with the velocity of the ionizedgas of NGC 3503; Georgelin et al. 2000), which is associatedwith the nebula and its surroundings. We reported an overdensity

Experiment (APEX) 12 m telescope2 . To account for the properties of the dust in the nebula and its surroundings, we use unpublished images at 870 µm from the APEX Telescope Large
Area Survey of the Galaxy (ATLASGAL). The aim of this work

N. U. Duronea et al.: Molecules, dust, and protostars in NGC 3503

30
1500
30
1500
RIGHT ASCENSION(J2000)

00 4500 45

3030

11 02 00
1102 00

46−59-5946

4747

4848

4848

4949

DECLINATION (J2000)

4747

C25050C35151
5252

49 00

15353

C411 02 00
1102 00

59 50 00
251 0052 0053 0050505151

01 4501455353

C530150000 4530 and protostars in11NGC
N. U. Duronea
et00al.: Molecules,
30153011 0202000035
00 45 dust,
RIGHT ASCENSION(J2000)

RIGHT ASCENSION (J2000)
46−59-5946−25.4 to −24.9 km s −1

46−59-5946

13Fig. 3. Left panels: Integrated
CO emission in the velocity range47from ∼ −27.8 km s47(see continuation). The velocity
intervalof each image is indicated48in the upper-left coC648rms). The contour spacing49 temperature is 1.5 K km s−1 to 9.7 K km49s−1 , and then 4 K k
corner of each image. Rightpanels: Overlay of the IRAC GLIMPSE
50 4 (8 µm) emission
50
the velocity intervals shownin the C7left panels (contour lines).
5151
47

34949

5252

47

DECLINATION (J2000)

48 00

8.0μm
4.5μm
cont.@4800MHz
CO01 4501
45−26.0 to −25.5 km s −1

DECLINATION (J2000)
DECLINATION(J2000)

47 00

46−59-5946

DECLINATION(J2000)
DECLINATION (J2000)

46 00

11 02 00
1102 00

484950484950515152525252

N. U. Duronea et al.: Molecules, dust, and protostars in NGC 3503

5353

5353

−1
on
overa velocity
interval
0.5.15In 00this00way,
11 02 00based
01 4530 th02 00
01 45km30sclumps
30 the final
45Table 2. Geometrical andline emission
parameters
obtained11offor
themolecular−1
rms30noise for each interval
results∆T18rms≈ 120.15 HCN
K km 13s −59. 46To of13each clu
30
02 00
11 01 0000
13−1
46 (13 CO)
Vel. int. ( CO)Clump
RADec.(J2000) −59
AclumpT peak T peak
vcentr
−24.8 to T
−24.3
speakpeak kmTin T betw
analyze
therelationbetween
themoleculargas
andthewarm
h m s◦ " ""−8−1
13CO
channelmapから、molecular
RIGHT ASCENSION (J2000)()()(10ster)
(K)
(K)
(K)
(K)
(km s ) 47
(km s−1 ) mb47
dust
nebula,panels- of 13.6
Fig. 3 -we show
theC1
11 : 00in: 52the−59: 47 : 57 in 48the
7.8 right 3.2−26.3 48−27.1 larger
to −25.6 thanosite image of NGC 3503 and its environs. Red and green show emission at 8.0 and 4.5 µm (IRAC-GLIMPSE),
respectively.
White13C2
11CO: 00 : emission40 −59 : 46 in: 40 the 49velocity
7.3
3.4
17.9
−25.3 49(in−27.3 atto −24.3
least alointervals
mentioned
beforeで動いている
ours show the radio continuum 4800 MHz and integrated CO line emissions. Circles in light blue indicateC3the positionof: thethree
11 : 01
05gasは-28~-23km/s−59 : 51 : 30
10.7
13.7 ∼ 2.1 33.2
−26.0
−27.1 to −24,9definecontours)
projected
the IRAC(8 µm)
emis50 8.6
50 −27.8 We
compact Hii region identified using the MSX Catalog (see Table 3 in Paper I). The CO temperature contours
km: 12s−1 (∼10C4 are 0.5
11K: 01−59 : 51 : 25 onto
19.7 GLIMPSE-4∼ 2.3 50.3 ∼ 2.3−25.7
to −24.5−1−1
11 : 00: 40rms)−59: 51 : 30(grayscale).
13.3- small-scale−26.1 51 −26.6 encloses
to −24.6, 10.5, 15.5, 20.5, 25.5, and 30.5 K km s . The radio continuum 4800 MHz contours levels go from 2.4C5
mJy beam(∼3to 3503
51 5.5thsionofNGC
In3.8order- to study
theC6
11 : 01 : 06その他、clumpを幾つか同定−59 : 48 : 40
4.1
4.3
13.4
−25.7−26.1 to −25.0
m−1 in steps of 2 mJy beam−1 , and from 10.4 mJy beam−1 in steps of 4 mJy beam−1 .
52
52
intstructure
thewe have
C7
11 : 01 : 10 of−59: 50molecular: 28
8.9cloud 10.7
∼ 0.9 identified
34.2- a number−25.5 of−27.1 velocity
to −24.7
53
53
C8
11 : 00 : molecular
53 −59 : 51 :clumps.
00
8.6
10.5 ∼were
1.5 26.2−25.6 indicatedto −24.1
C8 - by −25.2
insmall
The clumps
selectedeye and01 4530
1500
RIGHT ASCENSION (J2000)

00 4530

11 02 00

-59 46-59 46

47

47

DECLINATION (J2000)

DECLINATION (J2000)
DECLINATION(J2000)

11 02 00

4849
50

01 45

48

49
50

51

51

52

52

C9
11 : 01 : 37C3,C4,C7はおそらくPIS17からのUV−59 : 50 : 00
9.1
1.8
6.7
−16.1
−17.1 to −15.3
emissionsstronglyis the measured flux density, d is the adopted dis- molecular and 4800 MHz radio continuum
C10
11 : 01 : 11 −59 : 48 : 57
3.9
4.7
9.9
20.1
17.2 to 22.5
compressed
an ionsource, κ is the dust opacity per unit mass at 870 suggests that the molecular gas is being C11
11 : 01by: 05−59 : 47 : 40
6.0
3.3
7.3
20.9
15.3 to 22.8
other(TCOガスは電離面から圧縮されている) is the Planck function for a temperature ization front and is interacting with the nebula. On the で照らされている。
53

11 02 00

11 02 00870

dopted a dust opacity κ870 = 1.0 cm2 g−1 estimatedns with thin ice mantles in cold clumps (Ossenkopf1994).

46−59-5946

01 45

30
1500
30
1500
RIGHT ASCENSION(J2000)

00 4500 4530

11 02 00
1102 00

30

01 45
01
4530
30
RIGHT AS46−59-5946−24.2 to −23.7 km s −1

4747

4747

hand, the ionized gas seems toTable
be expanding
freelytowards
the derived for the molecular clumps.
3. Physical anddynamicalproperties
48
48
opposite direction (i.e. the intercloud medium). The location of
49
49
peak
MLTE
∆v13
12 8.0the PDR is traced by the emission of
PAHs molecules
Clump
T exc
τ13 in τthe
∆v13
∆v12
N(H2 )LTEN(H2 )level
MLTEMvir
LTEMvir
∆v13
th50
50
µm image (shown in red). Since these complex(K)molecules are de(km s−1 ) (km s−1 )(1021 cm−2 ) (1021 cm−2 )
(M% )
(M% )
5151
stroyed inside the ionized gas of anC1Hii region
18.7 (see0.26Deharveng
7.1
0.91
1.92
5.4
1.2 ± 0.2
0.8 ± 0.2
11 ± 536 ± 12∼ 0.352
et al. 2010 and references therein), theyC2 delineate23.1 the0.21boundaries
9.0
1.82
2.41
9.6
3.3 ± 0.7
2.2 ± 0.4
29 ± 15 52 170 ± 55
∼ 0.2
C339.1 the0.51position
19.6 of1.48
2.20
5.9
13.8 ± 2.7
9.8 ± 1.9191 ± 95 53 147 ± 50
∼ 1.3of NGC 3503. The molecular gas clearly
depicts
53C4
57.2
0.48
17.6
1.39
2.13
4.5
27.1
±5.4
18.2
±3.6
282±140120±41∼ 2.4
the ionization front. As predicted in Paper I, no molecular emis11 02 00 01 45
3000 01 45
303000 45
C518.3 0.33 12.7
1.03
1.53 11 02 6.1
1.6 ±0.3 15 1.200± 0.2
12 ± 651 ± 17∼0.2
sion is detected in this velocity range
towards
thelowelectron
RIGHT ASCENSION (J2000)
RIGHT ASCEN
C618.5 0.38 13.1
0.77
1.25
4.5
1.3 ± 0.3
0.9 ± 0.2
7±322 ± 8
∼ 0.3
density region, which is compatibleC7
with a champagne-flow
39.7 0.37 14.2 sce2.26
6.1
10.0 ± 2.1
6.5 ± 1.3
169 ± 84
144 ± 49
∼ 1.2
Fig.1.53
3. continuation
C8 IR arc-like
31.6 filament
0.50 19.0
2.42
8.1
8.5 ± 1.7
5.8 ± 1.2
92 ± 46
165 ± 56
∼ 0.6
nario. However, we speculate that the(from1.61
C9
11.5
0.29
10.3
1.15
1.81
8.3
1.4
±0.3
0.4
±0.1
6±379
±28
∼ 0.1
here onwards called the IR arc) seen in the northeastern border of(†)
h ±m 83s(†)◦∼ 0.7$
C100.62
3.62
12.4
8.0
±
1.6
5.6
±
1.1
303
±90408h m 15.2s◦ $ 18.5$$ the 1.92
the nebula at RA, Dec. (J2000) ∼ (11 01 30 , −59 50 10 ) andvelocity interval at which they reach the maximum emission (†)≈ (11 00 50 ,(†)−59 47 57
C1112.2
0.58
24.2
3.11
4.23
22.2
7.1
±1.4
4.9
±
1.0
408
±821340±270∼
0.3RA, Dec. (J2000) ∼ (11h 01m 25 s , −59◦ 49$ 00$$ ), might be still peakas- temperature. These molecular clumps are also identified in velocity range from −27.1
COshowing more extended emission.
In the velocity range fsociated with small amounts ofmoleculargas adopting
at velocities
beNotes:(†) Values obtained
a kinematicaldistance of 8 kpc. Uncertainties were calculated taking into account only innacuracies in the boundary selection.

8.0μmはPAHでPDRをトレース→COガスとCont.が同じ分布:
分子ガス
andanalysis of the observations
distribution of the molecular gas
は電離面によって圧縮されている
e molecular gas associated with NGC 3503 we havesed on Component 1 of Paper I (which is undoubtPAHは電離領域では壊される
ated with the nebula). We will also make a brief
he molecular gas associated with Component 2 and3. →8.0μmは境界を表す

2 we show an overlay of the mean CO emission asth APEX, in the velocity interval from −29 km s−101 45

DECLINATION (J2000)

dust

DECLINATION (J2000)
DECLINATION(J2000)

870

5330
RIGHT AS484950484950

5151525253

53

11 02 00

01 4530
1500
RIGHT ASCENSION (J2000)

00 4530

11 02 00

01 4530
RIGHT AS