NAOJ

Akio K. Inoue (Osaka Sangyo U.)

ALMA/45m/ASTE UM@NAOJ

December 19 2016 An review of 2016 ALMA results about galaxies atz>6: Epoch of Cosmic Reionization
 Especially, emission lines of [CII]158 and [OIII]88.

Spinoglio+12
ALMA/45m/ASTE UM@NAOJ

December 19 20162 First billion years in the cosmic history
 Redshift z~6—20
 Epoch of the first objects and galaxies
 The first metal and dust

NAOJ
ALMA/45m/ASTE UM@NAOJ

December 19 20163 The [CII] line is one of the strongest emission

lines in the local Universe.
 L_[CII]/L_TIR~1%

 However,…

Ouchi+13

very weak in the EoR?
z=6.6

ALMA/45m/ASTE UM@NAOJ

December 19 20164 The [CII] line is one of the strongest emission

lines in the local Universe.
 L_[CII]/L_TIR~1%

 However,…

very weak in LAEs
in the EoR!
 Lya and [CII] anti-correlation?

(Harikane+ ASJ16b)
LBG: Lyman break galaxy(UV continuum selection)
LAE: Lya emitter(Lya emission line selection)
ALMA/45m/ASTE UM@NAOJ

Pentericci+16

Local relation

z~5-6
LAE, LBG(Capak+15)

z~6 LBG(Willott+15)
z~6-7 LBG
(Pentericci+16)z~6-7 LAE
December 19 20165 The [CII] line is one of the strongest emission

lines in the local Universe.
 L_[CII]/L_TIR~1%

 However,… [CII] emitter candidates w/o counterpart?
 Blind [CII] searches and detections.
Hayatsu+17
Aravena+16

Magenta = [CII]

ALMA/45m/ASTE UM@NAOJ

December 19 20166 The [CII] line is one of the strongest emission

lines in the local Universe.
 L_[CII]/L_TIR~1%

 However,…some LBGs?
Hayatsu+17

are over-luminous in [CII]??
60% arespurious!
Photo-zs are notvery consistent
with [CII] lines.

ALMA/45m/ASTE UM@NAOJ

Aravena+16

December 19 20167 Spatially offset [CII] line?
 Redshift z=7.1 LAE
Pentericci+16
Color: Y-band
Contour: [CII]

Simulation

Maiolino+15
ALMA/45m/ASTE UM@NAOJ

Color: Ionized gas (LyA)
Contour: Neutral gas ([CII])
Black points: Young stars (Y-band)
December 19 20168 The [CII] line luminosity functions.
[CII] search around massive
halos such as QSOs and SMGs
by Miller+16

Blind [CII] searches

Hayatsu+17
ALMA/45m/ASTE UM@NAOJ

December 19 2016

9ObjectRedshift

EW(LyA) [A]1A1689-zD1

7.6031 ? - 3σ

2ID27

7.575 ?

3z8-GND-5296

7.508

4ID31

7.494 ?

5IDX347.491 ?

6

L[CII]/SFR [1e7Lo/Mo yr-1]

Reference

0.14 ? (SFR=13)

Knudsen+16b4.7σ 2.8 (SFR=10.5)0.9″off
8<0.03 (SFR=330)
4.5σ- 0.7″off
2.7 (SFR=12.4)

Aravena+16-

Aravena+16

SXDF-NB1006-2 7.2120- 5.3σBlind33<0.02 (SFR=350)

Inoue+167COSMOS13679

7.1416

158BDF-3299

9BDF-512

10 IOK-1
ALMA/45m/ASTE UM@NAOJ-Schaerer+15
Aravena+16

Pentericci+16

7.109

0.30 (SFR=24)
4.5σ
50 0.4”off <0.37 (SFR=6)

7.008

64

<1.00 (SFR=6)

Maiolino+15

6.96

24

<0.14 (SFR=24)

Ota+15Maiolino+15

December 19 201610 First detection of [OIII] 88 mm in EoR (5.3σ).
 z([OIII])=7.2120  The most distant oxygen ever found!
Contour: [OIII]88
Color: Lyα (NB1006)

ΔLyα=+110±30 km/s

ALMA/45m/ASTE UM@NAOJ

Inoue+16, Science

December 19 201611

>3s signal in all three days data

Pixel S/N distribution
Red: Positive
Blue: Negative

ALMA/45m/ASTE UM@NAOJ

Inoue+16, ScienceDecember 19 2016

12

NAOJ

ALMA/45m/ASTE UM@NAOJ

December 19 2016 Neither [CII] line nor dust continuum at theposition of [OIII].

Black: [CII]White: [OIII]
Inoue+16, Science
ALMA/45m/ASTE UM@NAOJ

December 19 201614

[O/H]−1.0+1.0−0.3log(SFR[Msun/yr])

2.54+0.17−0.71log(age[yr])6.00+1.00log(Mstar[Msun])

8.54+0.79−0.22

E(B-V) [mag]0.00+0.04

fesc0.54+0.17−0.54

PEGASE2, Sapleter IMF, constant
SFR, Calzetti dust law, nebular lines
and continuum

βUV<-2.6log(fescξion[Hz/erg]) 25.44+0.46−0.84
Inoue+16, Science
ALMA/45m/ASTE UM@NAOJ

December 19 2016

15

[OIII]/[CII] [OIII]/IR [OIII]/UV SED fit  [O/H]~-1
 [OIII] line flux constrains [O/H]well.
 [OIII]/UV ~ Nearby dwarfs

 Large [OIII]/IR Less dust
 Large [OIII]/[CII] Weak [CII] Less HI gas (PDR)
Metallicity
ALMA/45m/ASTE UM@NAOJ

Inoue+16, Science
December 19 201616

 [CII] 158 line seems to be weak in LAEs at z>6.
 Anti-correlation between [CII] and LyA lines?
 Blind [CII] searches may have found z~6 [CII]

emitters without any counterpart.
 [CII] over-luminous galaxies?
 Spatial offset of [CII]?

 [OIII] 88 line was detected from an LAE at z=7.2.
 High [OIII]-to-[CII] line ratio  Lack of HI gas Opened a new window for probing the ISM in the EoR.

ALMA/45m/ASTE UM@NAOJ

December 19 201617High-z Far-Infrared Nebular Emission STudy SXDF-NB1006-2 [OIII]88 line kinematics
 Cycle3 DDT program SXDF-NB1006-2 [NII]122 line observations
 Cycle4 Rank B

 [OIII]/[CII] ratio measurements
 Cycle4 Rank B: 4 objects at z=6--8
 Higher-z [OIII]88 line observations
 Cycle3 Rank A: MACS1149JD at z(photo)=9.6
 Cycle4 Rank A: MACS0416 #491 at z(photo)=8.5
 (PI: Y.Tamura)

ALMA/45m/ASTE UM@NAOJ

December 19 201618