THE STAR FORMATIONNEWSLETTER
No. 265 (#16-20)
塚越崇(茨城大)13 Feb. 2015

Herschel Far-infrared Spectral-mapping of Orion BN/KL Outflows:
Spatial Distribution of Excited CO, H2O, OH, O, and C+ in Shocked Gas
J.R.Goicoechea et al.
Spatial distribution of excited CO, H2 O, OH, O and C+ in Orion BN/KL outflows• Herschelによる複数輝線イメー
ジング観測• Orion BN/KL周辺• hot core
• low- velocity outflow• high- velocity outflow• 二つのH2 Peak
Peak1 and Peak2• Herschel HEXOS GT Key
Programによる観測• 高分解能によってPeakを分解• 多くの輝線を検出• Peak1とPeak2で強度が異なる

38Goicoechea et al.

dances with accuracy (e.g., Chen et al. 2014).
Table 2
Peak1のgascoolingに寄与しているのは？
23200
king N (H2 )⇡10 cm
in a 30 beam for theObserved luminosities and cooling budget (assuming d=414 pc)
plateau component (Blake et al. 1987; MelSpecies
Lobs (L )%aLobs (L )%b4et al. 2010),
weobtain(CO)⇡2⇥10,plat• 半分はH2、続いてCOin Peak 1c in Peak 1c
in mapc
in mapc
55(H2 O)⇡0.7⇥10and plat (OH)⇡0.2⇥10abunFIR 12 CO
18.7⇠(22±5)%84⇠31%es.
Hence, in the less excited swept-up gas,
FIR H2 O
7.0⇠(8±2)%32⇠12%
r vapor is •notFIRだけで見るとCOが突出
the dominant O-bearing species.
FIR OH
3.5⇠(4±1)%13⇠5%ver, if we only consider the hot shock-excited
FIR [O i]
3.5⇠(4±1)%
18⇠7%
onent, the derived H2 O/CO abundance ratio
FIR [C ii]
0.3⇠(0±0)%7⇠3%13FIR CO0.3⇠(0±0)%
2⇠1%
uch higher (⇠1.3).
Rosenthal et al.
(2000)
12 CO v=1-0dd⇠6.1⇠7%⇠14⇠5%
red that the column density of hot H2 withdd202shock
H2 O v2 =1-0
⇠1.3
⇠2%
⇠3
⇠1%
>1200 K toward
Peakproperties
1 is N (H2 ).10 cm . TakeeMIR H2
⇠43
⇠51%
⇠102
⇠37%
he columns from this component alone, we de4Total⇠84100%274
100%
C-shockだとH2Oが重要な
ne hot (H2•O)&2⇥10, hot (CO)&1.5⇥10 4 and
35FIR dust
⇠4⇥10⇠10OH)&0.8⇥10 5 .

••coolantになるので観測と合わない

5. Model uncertainties and Peak 1/2 di↵erencesa In a ⇠3000 ⇥3000 aperture (⇠12500 AU ⇥ 12500 AU).
b In the entire ⇠20 ⇥20 map (⇠0.25 pc ⇥ 0.25 pc).
c Absolute calibration accuracy up to ±30%.

• H2Oを減らすメカニズム
r multi-component
model satisfactorily reproduces
d Scaled from ISO/SWS observations (González-Alfonso et al.
fluxes of most observed lines. Despite this model2002).
e Scaled from ISO/SWS observations (Rosenthal et al. 2000).
ion is certently •not初期のOを減らすかUV
unique, the agreement withobdissociationか -> J-type shock?
tions suggests that the model captures the averagecal conditions of the shocked-exited gas.
C- andJ-typeshocks?
e best fit to•themized
CO J=41
to 48
absoluteline fluxes
the cooling budget in shocked gas. This tabulation also
63gives Tk '2300-3000 K and n(H2 )'(3-4)⇥10 cm
includes an extrapolation of the mid-IR H2 line fluxes
shock?
16• UV irradiatedN (CO)=(5.0-2.5)⇥10cm 2 C-typefor Orion
Peak 1.
and of the CO and H2 O ro-vibrational emission detected
e values suggest that the postshock4gas -3
where theISO/SWS(Rosenthalet al. 2000; González-Alfonso et4by6 cm-3 & G <100
二つの解:n=10cm&G=5x10or
n=10•00excitation CO, H2 O and OH lines arise might beal. 2002). Their measured luminosities have been multio ⇠5 times less dense than our assumed value
plied by73(H2 )'2⇥10 • cmPeak1はextremeな環境である(but see Sempere et al. 2000;(3000 ⇥3000 )/(1400 ⇥2000 )'3 to approximately take into acález-Alfonso et al. 2002). In such a case, the H2 O
count the di↵erent aperture sizes. Roughly half of
mn densities in the hot component will be a factor
the total line luminosity is provided by H2 rotational
gher and the H2 O/CO abundance ratio will increase
and vibrational line cooling. CO is the next most im⇠1.3 to ⇠1.6. Finally, the presence of a moderate

A GALEX based search for the sparse young stellar populationin the Taurus-Aurigae star forming region
Ana I Comez de Castro et al.
– 33 –• UVによるTTS同定も有効なツールの一つである•

観測例がほとんど無い•

UVデータを使った新しいcriteriaを提案– 29 –• GALEX all sky surveyのUVデータ– 30 –を使ってTaurus領域で確認••

50cm NUV&FUVの宇宙望遠鏡

Fig. 6.— Density of NUV GALEX sources in the TMC. The densities are color coded instars per 3 arcmin2 (see lateral bar). The molecular gas distribution, as unveiled by the2MASS extinction map (Lombardi et al. 2010) is overlaid for reference.

可視や赤外データも使用• 63天体の新検出に成功

G0G1 G5K2
K1K5K4M0•

既知の天体もしっかり検出• 今後のプロシージャとなる

M2
M4e
M1
M2

A new approach to determine optically thick H2 cooling and its
effect on primordial star formation
Tilman Hartwig et al.

• 光学的に厚い部分のH2 cooling rateを見積もる新しい手法•TeeCol algorithmがベース•Sobolev approximationと比較• 収縮するコアにおいて10%程度のエラーでcooling rateを見積もれる•

原始星+円盤が出来ると対称性が崩れてエラーが大きくなる• 温度が低く出るのでframentationが起きやすい• 質量降着率も小さくなりPop III星の質量が小さいものが出来るPre-main sequence accretion in the low metallicity Galactic starforming region Sh2-284
V.M.Kalari and J.S.Vink
a Identification no. in Delgado et al. (2010).

考えられている観測でも低Zでは早い散逸時間が指摘されている•

質量降着率はどうか？

• 低Z領域Sh2-284でPMSの質量降着率を観測的に調べる• Halpha emissionを観測•dures. Wavelength calibration was performed using Ne
arc spectra using the IRAF identify task. Spectra werecorrected for sensitivity using the Sutherland extinction
curve. The variable pupil design of the SALT telescope
makes absolute flux calibration impossible. The final ex10m Southern African Large Telescope(SALT)による観測
tracted 1-dimensional spectra are shown in Fig 2. The
average signal to noise is ⇠ 20 - 40.

••

Fig. 1.— Sh 2-284 in H↵ taken from Parker et al. (2005). Northis up and east is to the left. Stars observed with SALT are marked
by circles, and stars with VIMOS spectra are marked by crosses.
The central cluster Dolidze 25 is also marked. At d = 4000 pc, 0.15
corresponds to ⇠ 10 pc.

IRデータを元に6天体を選定

VIMOS/VLTの観測データも使用 [Cusano+2011]•

サンプルは全部で24天体にF
cantopsta
the2.1. Basic analysis of the SALT data

Equivalent widths (EW) of emission and absorption
lines were measured using the IRAF task splot. Spectral types were derived from the EW of the (i) Mg II
5711 Å(ii) Mn II 6015 Å(iii) Ca I 5711 Å lines following
the method devised by Hernández et al. (2004). E↵ective temperatures (Te↵ ) were estimated using the spectraltype-Te↵ calibration of Kenyon & Hartmann (1995). H↵
line profiles are displayed in Fig. 3. Five stars show H↵
in emission. Combined with the fact that these stars allshow near to mid-infrared excess resembling PMS stars,

Normalized Intensity•

Normalized Intensity• metallicity(Z)↓で質量降着率↑の関係がNormalized Relative flux

b Identification no. in Puga et al. (2009).

• 物理量の導出•

質量と年齢; HR diagram•

降着ルミノシティ; log Lacc ∝ log LHa•

質量降着率; Macc∝Lacc•

円盤のIR class; SED• 質量降着率とZの関係•Maccの中間値で比較•

ほとんど違いは見られない

The HIFI spectral survey of AFGL2591(CHESS). III.
Chemical structure of the protostellar envelope
Maja Kazmierczak-Barthel et al.

M. Kaźmierczak-Barthel et al.: Chemical• アバンダンス分布をモデル化して、観測で得られているスペクトルを再
cal radiative transfer model (ratran) for the envelope of AFGL

Table 1. Abundances (relative to H2 ) estimated with the spheri2591, based on HIFI and JCMT data.

現する• well known isolated massive protostar AFGL2591• disk-like structure, outflow, envelope…

• 物理モデルを与えて輝線モデリング• RATRAN• chi-squareで合わせる• アバンダンス分布• constant• jump-like distribution•100K (water関連; van der Tak+2006)•230K (N-beargin species Rodgers & Charnley 2001)• アバンダンスは５つに分類された

MoleculeCOCNCSHCO+
H2 CON2 H+
CCHNO∗OCS∗
OH∗

Inner abundance Outer abundance
2 × 10−4
1 × 10−9
4 × 10−8
3 × 10−11
3 × 10−8
1 × 10−11
1 × 10−8
8 × 10−13
8 × 10−10
8 × 10−12
8 × 10−8
5 × 10−8
4 × 10−82Jump at
const
const
const
100 K
100 K
100 K
100 K
const
const

• 時間発展化学計算••

化学モデル: 13元素からなる1268分子種、38812個の反応•cosmic-ray ionization rate of 5E-17 1/s•photoreaction by interstellar UV•

grains are uniform amorphous olivine particles 3 g/cm^3 and 0.1µm•

gas-grain interaction•

surface recombination

初期アバンダンス導出の為0D分子雲の化学計算を実行•

三種類の初期値を使用 - low metallicityモデルがベストフィット(C/O=0.44)• 20個の計算を走らせ観測(RATRAN)と比較•

基本的には良く合うが合わせにくいケースもある•

HCN/HNC, complex organics, S-bearing species• 初期アバンダンスモデルを変えても合う。複雑な分子は再現するが、シンプルな分子の再現がうまくいかない•

初期温度が高くなる為

1e−02

radiative transfer model
chemical model

1e−03
1e−04
1e−05

[CO]

1e−06

1e−06
1e−07
1e−08
1e−09
1e−10
1e−111e−12
1e−13
1e−14

radiative transfer model
chemial model

[CN]
1e+13

1e+13

1e+14

1e+14

1e+15

1e+15

1e−04
1e−05
1e−06
1e−07
1e−08
1e−09
1e−10
1e−11
1e−12
1e−13

radiative transfer model
chemical model

[CS]
1e+13

Radius [m]

1e+14

1e+15

Fig. 2. The radial distribution of abundances with error-bars of CO, CN, and CS at the time of 104 years. The ratran-derived values(dashed lines) are compared with the results of the best-fit 1D chemical model (solid lines); see Table 4 for the specifications.

1e−05
1e−061e−07
1e−08
1e−09
1e−10
1e−11
1e−12
1e−13

radiative transfer model
chemical model

radiative transfer model
chemical model

1e−06
1e−08
1e−10

[HCO+]
1e+13

1e−04

1e+14

1e+15

1e−12

[H2CO]

1e−14

1e−06
1e−07
1e−08
1e−09
1e−10
1e−11
1e−12
1e−13
1e−14
1e−15

radiative transfer model
chemical model[N2H+]
1e+13

1e+13

1e+14

1e+15

1e+14

1e+15

Radius [m]radiative transfer model
chemical model

1e−06
1e−08
1e−10
1e−12

[CCH]

1e−14
1e+13

1e+14

1e+15

Radius [m]Fig. 3. The same as Fig. 2. Radiative transfer models are with a jump at 100 K (lower inner abundance) .
4.1. Photostable species located in the outflow cavity+

Where the modeled abundance profiles for CCH, C, C , CH,CS, SO2 , and HCl coincide with the respective ratran profiles
at some radii, the HCN and CH3 OH abundances in the best-fit
model are lower than the ratran-derived values. The first reason for this disagreement is a fundamental restriction of the utilized 1D approach with which one cannot properly capture thephysical and chemical processes that occur on the walls of UVirradiated outflow cavity. The presence of the outflow cavity andeven a disk-like rotating structure in the AFGL 2591 is well established (see, e.g., Tamura & Yamashita (1992), Bruderer et al.
(2010b), and Wang et al. (2012)). Clearly, in this case such acomplex environment is better characterized by a 2D or even
3D model.
As shown by Bruderer et al. (2010b), a multidimensional approach is required to explain the observed abundances of light
hydrides and hydride ions, such as OH+ . As we do not include
a central UV source in our model (since its radiation in the 1D
approach is quickly absorbed by the massive envelope inner regions), our model tends to under-predict the abundances of simple photostable radicals and PDR-like species. This may explain
why the abundances of species like C, C+ , CH, CN, CCH, and
14
HCl at small radii (<∼ 10 m) are lower in the model than theratran-derived observed values. For HCl, which has a very limited chemistry network in our model of only 58 channels, thelack of major high-temperature production channels may also
play a role.