Star Formation Newsletter#291 31-35
麻生 有佑 （ASIAA）

Estimating Extinction using Unsupervised Machine Learning
Stefan Meingast1, Marco Lombardi2, and João Alves1

Ø 赤外線の強度や色à減光、柱密度。
Ø mm, FIR熱放射、分子輝線：変換ファクター不明、NIR減光：背景星の数。減光則は既知。
Ø Near-Infrared Color Excess Revisited：減光なし観測から固有色のガウシアン分布を外挿。
Ø 2MASSは良かったが、deep surveyでは銀河など複数成分が入り、どれが固有か不明。
形状で分けるGNICER：
銀河、星の分布は普通は未知。
ガウシアンではなく離散化し、MCMCで評価。：計算が膨大。
PNICER：複数ガウシアン、観測量(パラメーター)を増やして縮退を解く。
Python open source.

銀河の分布

星の分布

Estimating Extinction using Unsupervised Machine Learning
3次元の例。

←減光ベクトルに沿った分布の期待値と分散で評価。
A&A proofs: manuscript no. aanda

銀河星
NICERは単一ガウシアンなので銀河の分布星の分布共に無理がある。

Fig. 4. Kernel densities for the derived line-of-sight extinction values for both Pnicer (blue) and Nicer (red) when applying the algorithms tothe VISION control field itself. In this case and since the entire control field is extinction-free, the calculated values for should be close to zero.
From left to right the number of features is incrementally increased, while from top to bottom we apply magnitude cuts to the “science” field. The
magnitude cuts simulate the e↵ects of having an extincted science field, resulting in di↵erent populations when compared to the extinction-freecontrol field (e.g. galaxies will be shifted beyond the survey sensitivity limit). In the first row we use all data, while the second and third row
simulate the e↵ect of 1 and 2 mag extinction in the KS band (i.e. KS < 18 mag and < 17 mag, respectively for our completeness of KS = 19 mag).
Clearly, Pnicer performs better for increasingly di↵erent populations and number of available features.

減光なし観測で検証(Av=0が答え)。
縦軸は適用時の強度カットオフ。

For only two features (J and H; leftmost column) we obtain very similar results for both methods across all magnitude
cuts. However, for increasingly strict magnitude cuts (more extinction) we can see that the peak in the distribution is shifted

negative AK ), Pnicer starts to perform systematically better. Fora simulated extinction of AK = 1 and 2 mag (i.e. KS < 18 and17 mag) the increased dimensionality helps to break degeneracies in the intrinsic feature space and the extinction distribution

Impact of photometric variability on age and mass determination inyoung stellar objects: the case of the Orion Nebula Cluster
Sergio Messina,1‹ Padmakar Parihar2‹ and Elisa Distefano1‹

Ø ONCはほぼ全て変光Tタウリ。à年齢と質量推定への影響。
Ø 346個、V, R, Iで5年連続。Himalayan Chandra Telescope 2 m, Vainu Bappu Telescope 2.3 m。
正弦波、R=振幅/残差。
isochronemass track

R>2.5、cleanな変光。

cleanとdirty
で棒の傾きに差。

Impact of photometric variability on age and mass determination inal.
young stellar objects:14the Messina
case ofSergio,the etOrion
Nebula Cluster

最大と最小で推定年齢に差。

フィットからの強度の残差=age spread
観測された変光の幅。

Ø 大部分の非周期的変光の原因を調べる。
Ø カラーをTeffにして、2次多項式でフィット。
(質量の違いを引く)

Ø Vの変光はage spreadなしで説明可能。
Ø Iの変光は50%しか説明不可。
Ø 本当にage spreadがあるか、またはA genuine radius dispersion among coeval
members as a consequence of nonuniform accretion at early stages.

Polarized Disk Emission from Herbig Ae/Be Stars Observed Using Gemini
Planet Imager: HD 144432, HD 150193, HD 163296, and HD 169142
John D. Monnier1, Tim J. Harries2, Alicia Aarnio1, Fred C. Adams1, Sean Andrews3, Nuria Calvet1, Catherine
Espaillat4, Lee Hartmann1, Sasha Hinkley2, Stefan Kraus2, Melissa McClure5, Rebecca Oppenheimer6, MarshallPerrin7, and David Wilner3

Ø 最近観測される円盤のギャップは惑星か、snow lineか、ダスト進化か？
Ø Gemini Planet Imager、4つのHerbig Ae/Be、初のJバンド偏光。
145 pc150 pc119 pc145 pcØ 下の2つにouter ring。
Ø 上の2つは伴星によるtruncateだろう。
Ø HD169142をモデルフィット。

Polarized Disk Emission from Herbig Ae/Be Stars Observed Using Gemini
Planet Imager: HD 144432, HD 150193, HD 163296, and HD 169142

過去のSEDに合うようにギャップを配置。

Ø Outer ringで赤い(Hが強い)ことはギャップでは説明できない。
Ø Inner ringの上層を通った光がouterringで散乱か。

Ø HD163296でoff center ringの全貌を初めて見た。
Ø 目でフィット。半径77 AU、18 AU上空。
Ø ガスのスケールハイト6-9 AUより高い。
Ø ALMA 1.3 mmのリングのまさに真上。
Ø CO snow line 90 AUの内側だけでダスト放射がエンハンスされれば、大小の粒子の寄与が見えるはずだ。
Ø COの観測を待つ。

PCbk[]00

FilamentProlate
Modelsstudied to a lesser degree thanStar-forming
cylindrical models.
spheroidal models of varying
A formulation which meets the three constraints of Section 2.2.2 has the aspect ratio a inPhilip C. Myers

ellipticity,presented
here, dowith
notz,appear
have beenstudiedpreviously.
equation(10) increasing
so thatto
columndensitycontours
progress from nearly round near€where ξ ≡ x / r0 and where a constant background column density Nbk is assumed. Here NPC
Ø フィラメントの性質と星形成の関係。Plummer-like分布：指数pが物理に対応。
the center where z = 0, to elongated near the extreme values ± z . This result can be achieved
and filamentary ridges. This condition is met when the axial profilemaxn(0, z) depends on z with aØ しかし、無限の長さ、質量、中心密度一定(pole)。2Dでより現実的に。
declines from its maximum NPC = Nbk + πn0r0 at x = 0 to its minimum NPC = Nbk at x = ∞.
formif similar
to thelinearly
TPC dependenceof n(r,ζ 0)
a increases
from amin when
= 0ontor.amax when |ζ| = ζmax, i.e.

2.3.1. Truncated Prolate Spheroid2Dモデルの条件:(TPS)€The TPC
hascylinder
the samemodel.
densityThethe PC in equation(2), models are met in a
2.2.3.
TPPC
aboveasconstraints
on 2D cylinderpolestructure
free、n(r=0,z)がzによる。

The spheroidal models used here are Plummer-like, in order to approximate the radial

観測に近いp=2 Plummerを基準に。
a(ζ ) ≡ aobservationsamin ) ζA16).
/ ζ maxTheir volume(18)profiles derived from Herscheldensity n depends on
min + (amax −(A11,等柱密度線がellipsoidal、n(0,z)とn(r,0)が同じ形。
"TPPC" cylinder model

space coordinates as[2 −1]][(4) , η=y/r , ζ=x/r
nTPC = n0 1 + ( r r0)
ξ=x/r
000n0
€
nTPPC =(7)With this variable aspect ratio, the 2expression
for the2 STPS density becomes
21 + ξ + η 1 + ( ζ a)[]€n0but its –––––––––>
maximum radiusthan infinite. Then equation(4) defines
the bounding(13)
nTPS rather=Spheroid,aspectratio一定。
z R is finite

1 + ξ 2 + η 2 + ( ζ a)2

surface in terms of €the minimum density nmin by n0nSTPS =21 + ξ 2 + η 2 + [ζ a( ζ ) ]Spheroid,,(19)aspect ratio外で大。

Star-forming Filament Models
Ø Star Formation Zone: IMF平均(1.0 Moコアà0.36 Mo星)、
半径0.05 pc、nmin=1.3x104 cm–3。
Ø SFZの集中度: 1<qz=Mz/Vz/ρmin<qs=Ms/Vs/ρmin=2.46
観測の1<qz<2.05に合う。
背景柱密度、最大柱密度、長さ、太さ、HWHMを観測に合わせた(天球面に平行を仮定)。
最初の3個ができそう。

影がSFZ星形成中8個を加えそう。

星形成終了期。

Wide-ﬁeld 12 CO (J = 2–1) and 13 CO (J = 2–1) Observations toward the Aquila Rift andSerpens Molecular Cloud Complexes. I. Molecular Clouds and Their Physical Properties
2o0o

6o(b) Fumitaka
Background Nakamura

-0.5
6.5

1,2,3, Kazuhito Dobashi4, Tomomi Shimoikura4, Tomohiro Tanaka5, and Toshikazu Onishi5

Ø 分子雲形成ßバブル、超音速乱流フロー。
Ø Aquila Rift: a few 105 Mo、分子雲の力学相互作用、superbubbleが収束。
Ø 距離はSerpens Mainで260 pcか415 pc。
Ø 大スケールのfirst step観測、野辺山、12CO 2-1、13CO 2-1、2.7’、0.08 km/s。
4o3.02o

166o

Galactic Latitude

K km/s-0.550(a) 4.5 - 6 km/s(c) AV

155°

Serpens cluster A

cluster B
Serpens SouthSh2 62/MWC2974o

20

Galactic Latitude

0o

4°

103°
52°

W40

2o0o
34 o

32°

-1032 o30 o
28 o
Galactic Longitude

26 o

24 omag5°4°Dobashi (2011) andexcess map of E(J H) of the Aquila Rift and Serpens molecular cloud complex generated byThe fits data were downloaded from their website (http://darkclouds.u-gakugei.ac.jp/2MASS/download.html). (b)map is masked for small-scale structures to determine the background. (c) Extinction map of AV derived from thed E(J H) map. The names of the regions discussed in the text are designated in the panel. 3°

30°

28°

Galactic Longitude

26°0Wide-ﬁeld 12 CO (J = 2–1) and 13 CO (J = 2–1) Observations toward the Aquila Rift andSerpens Molecular Cloud Complexes. I. Molecular Clouds and Their Physical Properties
2127(a) 260 pc(b) 415 pc

Fig. 18.— Mass-Radius Relations assuming a distance of (a) 216 pc and (b) 415 pc. The dashed and dashed-dotted lines indicate
Kau↵mann et al. (2010)’s relation and Krumholz & McKee (2008)’s criteria for massive star formation, respectively.