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.)

200um300um500um1mmAtmospheric Windows from Atacama （ alt. 4800m ）

Matsushita, Matsuo et al. PASJ (1999)2

10-2210-2010-1810-1610-1410-1210-1010-810-6

109 1010 1011 1012 1013 1014 1015

Blackbody Radiation

Frequency[Hz]

REDSHIFT

2.73K

10K

30K

100K

300K

1000K

4000K

0 10 100 1000

H2O CO

CI CIINII OI NeIISiII

HI

LiH HD H2 H2

HaBra

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, OIIINII, NIIICII

Fischer et al. (1999)

FIR atomic fine structure lines OI

– 63.185mm 4.745THz 5.0×105 cm-3

– 145.54mm 2.060THz 1.5×105 cm-3

OIII 35.1eV– 51.815mm 5.786THz 3.4×103 cm-3

– 88.356mm 3.393THz 5.0×102 cm-3

NII 14.5eV– 121.80mm 2.461THz 2.8×102 cm-3

– 205.30mm 1.460THz 4.5×101 cm-3

NIII 29.6eV– 57.330mm 5.229THz 3×103 cm-3

CII 11.3eV– 157.68mm 1.901THz 2.7×103 cm-3

Carina Nebula by ISO LWS

Mizutani, Onaka, Shibai. (2002)

[CII]

The Carina NebulaA very massive star-formingregion at 2.3 kpc

from N. Smith 24’x12’ Hubble Image

[CII] 158 mm

[NII] 122 mm

[OIII] 88 mm

Matsuo et al. (2009)

30Dor region andR136

[OIII] 88mm is observed widely distributed around R136Contour: MIPS 24mmKawada et al. (2011)

300 Mo stars

Observation with ALMA

Primordial Massive Star-Forming Region[OIII] 52um, 88um (ion potential 35 eV)

– Probe of electron density and UV radiationZ > 8 observation of SFGs and GRBsSite of Cosmic Re-ionization

Example of [OIII] observationsin submillimeter-wave

Ferkinhoff (2010)~ 10 -18 W/m2

Herschel

10 um 100 um 1 mm

[NeII] [SiIII] [OIII][OI] [OIII]

10-17

10-18

10-19

z=0.1

z=0.2

z=2

z=3

z=5

z=0.5

z=1

[CII]

z=8

Wavelength

Line

Inte

nsity

W/m

2

M82

SPICA

High-z Star-Forming Galaxies

ALMA Bands10 9 8 7 6

10-20

z=10

10-21

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=81.7 mJy for 10 km/s @ 350 GHz

angular diameter 10 milli-arcsec

[OIII] 88 mm line intensities

ALMA で[OIII]88 ？

» 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

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Kawada et al. 2011

linear

[OIII]88フラックス予想

» 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

» NOTE: nebula parameter dependence˃ Especially, metallicity

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𝐿[ OIII]88

𝐿Hβ≈2

[OIII]88 フラックス予想

» 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):

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𝐿Hβ

𝜈UV 𝐿νUV≈0.01

𝐿Hβ=1.6×1041erg   s−1( 𝑆𝐹𝑅𝑀 sun y r−1 )

𝜈UV 𝐿𝜈UV=1.4×1043 erg  s−1( 𝑆𝐹𝑅

𝑀 sun y r−1 )For Z=1/5Zsun (Inoue 2011)

For Z=Zsun (Kennicutt 1998)

Lower Z: larger UV—SFR factorDust obscuration: smaller UV—SFR factor

[OIII]88フラックス予想

» Kawada+11 obs.» Cloudy calculations

» Hβ, UV – SFR relation

» Finally, we obtain

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𝐹 [OIII ]88

𝜈obs𝐹 νobs≈0.02

𝐿Hβ

𝜈UV 𝐿νUV≈0.01

𝐿[ OIII]88

𝐿Hβ≈2

𝜈obs=𝜈UV /(1+𝑧)

[OIII]88フラックス予想2013

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27.5—28.0 AB で～ 1 mJy (100 km/s)

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

金属量は十分か？

» 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)

» 十分に酸素はあるはず

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Robertson et al. 2013

Cycle1 ターゲット

» 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˃ Too risky!

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ターゲット候補

» BoRG や CANDELS にも <28AB 天体が２０個ほどある

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Schenker et al. 2013

ターゲット候補2013

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Ellis et al. 2013

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）

系外銀河　の重ねあわせ（ SUBARU, HST, Spitzer, BLAST ）

背景放射CMB

第一世代の星 　　　　　　Ly-?

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FromS. Matsuura

Carinae Nebula at 2.3 kpc