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

Study of embedded clusters

25

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。

The Astrophysical Journal Letters, 784:L1 (4pp), 2014 March 20

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

Chemical abundances of the high-latitude Herbig Ae Star PDS2
C. R. Cowley,1‹ S. Hubrig2 and N. Przybilla3ABSTRACT
The 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 17

SFO 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