初期宇宙における大質量星形成領域のプローブとしての遠赤外電離酸素
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Transcript 初期宇宙における大質量星形成領域のプローブとしての遠赤外電離酸素
初期宇宙における
大質量星形成領域のプローブとしての
遠赤外線電離酸素輝線
Hiroshi Matsuo (NAOJ)
Akio Inoue (Osaka Sangyo Univ.)
Atmospheric Windows from Atacama(alt. 4800m)
1mm
500um
300um
200um
2
Matsushita, Matsuo et al. PASJ (1999)
THz Cosmic Window
3
High-z universe beyond
redshift 8
To probe the period of Re-Ionization.
Interstellar space should be already
contaminated by heavy elements from Pop III.
High UV field prevent formation of dust,
hence low extinction.
Massive stars are formed in clusters, nearby
counter parts are R136 in 30Dor, LMC.
SFG and GRB can trace massive star clusters.
FIR SED of
Starburst galaxies
OI, OIII
NII, NIII
CII
Fischer et al. (1999)
FIR atomic fine structure lines
OI
– 63.185mm
– 145.54mm
4.745THz
2.060THz
5.0×105 cm-3
1.5×105 cm-3
5.786THz
3.393THz
3.4×103 cm-3
5.0×102 cm-3
2.461THz
1.460THz
2.8×102 cm-3
4.5×101 cm-3
5.229THz
3×103 cm-3
1.901THz
2.7×103 cm-3
OIII 35.1eV
– 51.815mm
– 88.356mm
NII 14.5eV
– 121.80mm
– 205.30mm
NIII 29.6eV
– 57.330mm
CII 11.3eV
– 157.68mm
Carina Nebula by ISO LWS
[CII]
Mizutani, Onaka, Shibai. (2002)
The Carina Nebula
[CII] 158 mm
A very massive star-forming
region at 2.3 kpc
[NII] 122 mm
[OIII] 88 mm
from N. Smith
24’x12’ Hubble Image
Matsuo et al. (2009)
30Dor region and
R136
300 Mo stars
[OIII] 88mm is
observed widely
distributed around
R136
Contour: MIPS 24mm
Kawada et al. (2011)
Observation with ALMA
Primordial Massive Star-Forming Region
[OIII] 52um, 88um (ion potential 35 eV)
– Probe of electron density and UV radiation
Z > 8 observation of SFGs and GRBs
Site of Cosmic Re-ionization
Example of [OIII] observations
in submillimeter-wave
~ 10 -18 W/m2
Ferkinhoff (2010)
High-z Star-Forming Galaxies
M82
Line Intensity W/m2
10-17
[NeII]
[SiIII]
z=0.1
[OI] [OIII] [CII]
[OIII]
ALMA Bands
10 9
8
7
6
Herschel
z=0.2
10-18
z=0.5
10-19
SPICA
z=1
10-20
z=2
z=3
10-21
z=5
z=8
z=10
10 um
100 um
Wavelength
1 mm
[OIII] 88 mm line intensities
Single massive cluster
– 1 ×10-5 W/m2/sr
from Carina
– 10 arcmin in diameter @ 50 kpc from 30 Dor
7 × 10-11 W/m2 at z=10-5
2 × 10-22 W/m2 at z=8
1.7 mJy for 10 km/s @ 350 GHz
angular diameter 10 milli-arcsec
» Band 7: 339-364 GHz → [OIII]88 @ z=8.3—9.0!
» 感度は十分か?
˃ [OIII]88/Hα相関
(Kawada+11)
˃ Cloudy計算
で予想フラックスを推定
linear
2013/1/26
Kawada et al. 2011
14
ALMA時代の宇宙の構造形成理論研究会
» Kawada et al. 2011
˃ I_[OIII]88 / I_Hα ~ 2/3
˃ Hα / Hβ ~ 3 (Case B近似)
» Cloudy (Ferland et al. 1998)
˃ Z = 0.2 Zsun, log10(U) = -1.0, log10(n_H) = 0.0
𝐿[OIII]88
≈2
𝐿Hβ
» NOTE: nebula parameter dependence
2013/1/26
˃ Especially, metallicity
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ALMA時代の宇宙の構造形成理論研究会
» z>8 candidates are detected only in rest-UV.
» [OIII] – UV relation is required.
» Let us relate Hβ with UV:
˃ SFR conversion laws (~100Myr constant SF):
𝐿Hβ = 1.6 × 1041 erg s−1
𝑆𝐹𝑅
𝑀sun yr −1
𝜈UV 𝐿𝜈
= 1.4 × 1043 erg s−1
UV
2013/1/26
𝐿Hβ
≈ 0.01
𝜈UV 𝐿ν UV
𝑆𝐹𝑅
𝑀sun
yr −1
For Z=1/5Zsun (Inoue 2011)
For Z=Zsun (Kennicutt 1998)
Lower Z: larger UV—SFR factor
Dust obscuration: smaller UV—SFR factor
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ALMA時代の宇宙の構造形成理論研究会
» Kawada+11 obs.
» Cloudy calculations
» Hβ, UV – SFR relation
𝐿[OIII]88
𝐿Hβ
𝐿Hβ
𝜈UV 𝐿ν UV
≈2
≈ 0.01
» Finally, we obtain
2013/1/26
𝐹[OIII]88
≈ 0.02
𝜈obs 𝐹ν obs
𝜈obs = 𝜈UV /(1 + 𝑧)
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ALMA時代の宇宙の構造形成理論研究会
2013/1/26
27.5—28.0 ABで
~1 mJy (100 km/s)
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ALMA時代の宇宙の構造形成理論研究会
Expected Brightness
Gravitational lensed sources
– 25-26 mag at H160
– 10 mJy Dv=100km/s
– Limited redshift information
HUDF sources (Dec. -28deg)
– 27-28 mag at H160
– 2 mJy Dv=100km/s
– Many candidates at z~8
Redshift probability
distributions
Z=8.11 for [OIII] 88um
Z=8.74
» UDF12によりUV slopeの測定精度が向上
˃ β~-2
˃ Z~Zsun, no dust
OR
Z~0.1—0.2 Zsun with Av~1mag
(Dunlop et al. 2013)
Robertson et al. 2013
2013/1/26
» 十分に酸素はあるはず
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ALMA時代の宇宙の構造形成理論研究会
» 赤方偏移z>8.3を狙うため、Y105-J125 > 1.6
を課し、Cycle1で観測条件の良い天体
» UDF092y-07580550 H160=27.1mag
˃ Y105-J125 > 2.4
» CANDY-2350049216 H160=27.0mag
˃ Y105-J125 > 2.3
» 残念ながら不採択
2013/1/26
˃ Too risky!
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ALMA時代の宇宙の構造形成理論研究会
Schenker et al. 2013
2013/1/26
» BoRGやCANDELSにも<28AB天体が20個ほ
どある
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ALMA時代の宇宙の構造形成理論研究会
2013/1/26
Ellis et al. 2013
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ALMA時代の宇宙の構造形成理論研究会
High-z universe beyond
redshift 8
To probe the period of Re-Ionization.
Interstellar space should be already
contaminated by heavy elements from Pop III.
High UV field prevent formation of dust,
hence low extinction.
Massive stars are formed in clusters, nearby
counter parts are R136 in 30Dor, LMC.
SFG and GRB can trace massive star clusters.
宇宙背景放射観測の現状
宇宙赤外線背景放射(CIB) = 観測値 ー 前景放射
前景放射: 太陽系(黄道光)、銀河系(星、星間ダスト放射)
近赤外域には銀河の重ねあわせでは説明できない超過成分
黄道光(前景放射)
背景放射
CMB
系外銀河 第一世代の星
の重ねあわせ
Ly-?
From
S. Matsuura
(SUBARU, HST, Spitzer, BLAST)
28
Carinae Nebula at 2.3 kpc