Credit: NAOJ

How submillimeter facilities such as
ALMA reveals early metal enrichment
in the epoch of reionization

田村 陽一 (名古屋大学)
SKA ワークショップ「銀河進化と遠方宇宙」
神奈川大学, 11-13 March 20191

Outline

ALMA

SKA

• Exploring the `dirty' universe• Well into the EoR• Poor spatial dynamic range• Poor instantaneous redshift coverage

www.almaobservatory.org

www.skatelescope.org

2Outline•Introduction•Submillimeter observations reveal "dirty" (!?) universe in the EoR•Case study with ALMA (Tamura+)•Metal/dust enrichment in the EoR: [OIII] and dust in LBG at z = 8.3•Future galaxy survey in the submillimeter•Simulation: Cross-correlation between 21cm vs. galaxies (Moriwaki+)•Technical challenge in submillimeter facilities•Large Submillimeter Telescope (LST) and synergy with SKA
3Introduction

4

Far-IR Emission as Important Coolant
The effect of FIR lines on th
Rest-frame wavelength (μm)

Credit: SPICA

CO rotational

dust
continuum

FIR FSLC+, O++

submm

mm
Smail et al., 2011

Observing wavelength (μm)

spectrumofJ2135−0102,
a lenseda typical
SMGhigh-redshift
at z = 2.5
Figure 2. Model
The rest-frame
SED of SMM
SMG at z = 2.3259, showing the bright, narrow molecular and atomic emission lines seen in the FIR and submillimetre. The continuum component of

Figure 3. The contuum emission in the
bands, from the em[C II] 158 µm line ca5z ∼ 0.6, 1.2, 2.2 andProperties ofPhotodissociation
FIR Fine Structureregion
Lines

O++
(35.1 eV)C+(11.3 eV)O0(13.6 eV)
Tielens & Hollenbach 2005, Phys. Rev.
96

[C II] 158 μm: Star-formation indicatorlog SFR (Msun/yr)[CII] on IRAS Far-IR

log L_[CII] (erg/s)
175 um continuum
ISO/LWS [CII] image of M31(Rodriguez--Fernandez+2006)

SFR — L_[CII] correlation (De Looze+2011)7

[C II] 158 μm: Important coolant

t_on-source ~ 25 mint_on-source ~ 20 hr
BR1202-0725 @ z = 4.7 (Iono+2006)

BR1202-0725 @ z = 4.7 (Wagg+2012)

LBGs @ z ~ 5-6 (Capak+2015)
ULAS J1120 @ z = 7.1(Venemans+2017)

SDSS QSOs @ z ~ 6(Wang+2013)8

Suppressed C+ and dust in young galaxies?

• Many ALMA non-detections of z > 6 LAEs/LBGs in[CII]158um and submm continuum have been reported.

• Walter+2012, Kaneker+2012, Ouchi+2013, Ota+2014, Maiolino+2015,
Inoue+2016• Something different from post EoR seems to happen…!
log L([CII]) (erg/s)

Himiko(z = 6.6)

HimikoIOK-1

ALMAz > 6 LAEs
Ota+2014

log SFR (Mo/yr)

Ouchi+2013
9

Strong [OIII] 88 um in a local HII region•ISO LWS observations of eta Car (Mizutani, Onaka & Shibai

Brightness

2002)

[CII]
[CII]
|

Wavelength (μm)

10Herschel Dwarf Galaxy Survey(Madden+2013, Cormier+2015)•Local dwarfs as low-z analogs of typical SF galaxies at high-z.
•[OIII]88 is the brightest[OIII] is more
important[CII] is more important

Normal SF galaxies(Brauer+08)[OIII]88 / [CII]158 luminosity ratio• L_[OIII]88 / L_[CII]158 > 1 (up to ~10).

Metallicity
Madden+2013

Cormier+2015

11

High-z [OIII] 88um detections thus far•Two ZEUS/CSO [OIII]88 detections (Ferkinhoff+2010)•detections in a z = 3.9 QSO and a z = 2.8 SMG•Only limited to lensed dusty sources

Ferkinhoff+201012Is [OIII] 88um detection feasible?

• Simulation where [OIII]88 luminosities are scaled by SFR.
• ALMA will detect [OIII]88 at z > 7!
[OIII] Emissivity

ALMA sensitivity[OIII] 88um“[OIII] Emissivity”

L[OIII] 88µm = C[OIII] 88µm (Z, U, nH ) Ṁ

A. K. Inoue, I. Shimizu, YT+2014

13

First detection of [O III] in the reionization era
SXDF-NB1006-2 at z = 7.215

Inoue A. K, YT, et al. (2016) Science, 352, 1559

Contours: [OIII] 88um
Background: Subaru/Lyα•Young star-forming metal-poor galaxy•Age < 30 Myr, SFR ~ 300 Mo/yr, Z = 0.05–1 Zo•No dust and [C II] emission were found.
14

Furthest detection of [O III] at z = 9.1096
MACS1149-JD1

Hashimoto, incl. YT et al. (2018) Nature, 557, 392

Contours: [OIII] 88um
Background: HST/H160•Low-mass star-forming galaxy•Age = 290 Myr, SFR ~ 4 (μ /10) Mo/yr, Z = 0.05–1 Zo•No dust emission
g

−1

15

Early dust production•Diversity in dust contents in EoR•Small dust mass in LAEs (e.g. Ouchi+13, Ota+14, Inoue+16, )•Large dust mass of ~10^7 M⦿ in LBGs (Watson+15, Laporte+17)•Dust budget crisis: How galaxies got dust so quickly?
•Type II SNe is the major contributors to dust mass at z > 8•Grain growth in dense ISM plays an important role?
z ~ 7.5 (A1689-zD1)

Watson+2015, Naturez = 8.38 (A2744-YD4)

Laporte+2017

z = 7.541 (ULAS J1342+0928)

Venemans+201716

Redshift Record#

Redshift

ObjectReferences

Telescope/Line

Dust?

1

9.110

MACS J1149-JD

Hashimoto+ (2018)

ALMA/[OIII]

N

2

8.683

EGSY-2008532660

Zitrin+ (2015)

Keck/Lyα

n/a

3

8.38

A2744_YD4

Laporte+ (2017)

ALMA/[OIII]

Y (4σ)

4

8.312

MACS0416_Y1

Tamura+ (2019)

ALMA/[OIII]

Y

5

7.664

z7_GSD_3811

Song+ (2016)

Keck/Lyα

n/a

6

7.640

MACS1423-z7p64

Hoag+ (2017)

HST/Lyα & ALMA/[CII]

N

7

7.541

ULAS J1342+0928

Banados+(2017)

Magellan/Lyα &ALMA/[CII]

Y

8

7.508

z8-GND-5296

Finkelstein+ (2013)

Keck/Lyα

n/a

9

7.477

EGS-zs8-2

Stark+(2018)

Keck/Lyα, CIII]1909

n/a

10

7.452

GS2_1406

Larson+ (2018)

HST/Lyαn/a

SXDF-NB1006-2

Shibuya+(2012)
Inoue, YT+ (2016)

Subaru+Keck/Lya

11

7.212

ALMA/[OIII]

N
17

Case Study with ALMA18

Motivations••

Key questions:
Can submillimeter telescopes serve as “zmachine” at z > 8?
How and when metal enrichment happened?
Why dust exists in the earliest universe?

•••

Purpose:
ALMA observations of a galaxy at EoR
SED modeling with [OIII] + dust
Dust mass evolution modeling•19

Target: Frontier Field candidate LBG “MACS0416_Y1”•The best among > 100 LBGs at z > 8•Bright (H = 26.0 AB, μ = 1.4)
•Well-constrained redshift (z_ph ~ 8.3–8.7)•Accessible from ALMA (Cycle 4)160

g

MACS J0416-24
Critical line
for z = 9
(Kawamata+16)

Laporte et al. (2015)20

ALMA + [OIII] reveals a spectroscopic redshift[OIII] on F160W
6.3 sigma
Photo-z’s

0’’.5•Spectroscopic redshift z = 8.3118 ± 0.0003(YT+2019)

21

Dust detection at S/N = 7.6•Second detection of dust at z > 8•S_850um = 137 ± 26 μJy

Contours: 850 um continuum
Background: HST/F160W•Spatially resolved•Size: 0”.36 × 0”.10 = 1.7 × 0.5 kpc•Tracing UV emission•Peak at/between E-C clumps•Large dust mass•assuming T_dust = 50 K, β = 1.5…
•L_TIR = (1.7 ± 0.3) × 10^11 L⦿
•M_dust = (0.4 ± 0.1) × 10^7 M⦿

0’’.2~1 kpcE C W
YT+18, submitted
22

[O III]-to-IR Luminosity Ratio
SXDF-NB1006-2
Local dwarfs

MACS1149-JD1
MACS0416_Y1
B14-65666

A2744_YD4

SMGs
QSOs

Local starbursts/spirals
Filled: z ≳ 7
Open: Low-z•MACS0416_Y1 is a scale-up version of local dwarfs.

23

How does "dust" coexist12with UV SED?

•PANHIT (Mawatari+2019, in prep.)

Tamur

Table 5. The best-fitting parame
far-infrared spectral energy distrib•Stellar population synthesis analysis

with Rest-frame UV-optical and FIR [OIII] + dust continuum

Items

χ2
Fitting parameters•SED components•Stellar: Bruzual & Charlot 2003 (BC03)•Nebular: SFR -> N_ion -> Hβ -> Nebular (Inoue+11)
SFR + Z -> [OIII]88 (Inoue+14)•

Dust (FIR): Local LIRGs (Rieke+09)•Three extinction curves are used

Degree Of Freedom
Dust attenuation AV (mag)Age τage (Myr)♯−1
SFH τSFH(Gyr−1 )Metallicity Z (Z⊙ )LyC escape fraction fesc†
Stellar mass Mstar (108 M⊙ )†SFR (M⊙ yr−1 )†11
LIR (10 L⊙ )

0

0
0

5
1

Note—The error bars represent the 68% confidence interval.
estimated for the parameters, such as AV , τSFH , Z an
Calzetti, Milky Way (MW), Small Magellanic† The value is Cloud
corrected(SMC)
for lensing magnification with µ = 1•
include the uncertainty in µ .
2175
A
bump
(carbon)isevidentinthe MW law•♯τ= 0, τ
> 0 and τ< 0 represent for constant, expo
g

g

−1
SFH

−1
SFH

−1
SFH

in Equation 1.
24

SED Fits: Results•UV-bright stellar component can co-exist with luminous
dust component if the dust mass pre-exists.

•Favors a young, but moderately metal-enriched solution
12•Age ~ 4 Myr, metallicity = 0.2 Z_Sun

0.3

Extinctio

300
100
30
500

1000 2000

Observed Wavelength [µm]
0.1

0.05
0.03

(a) Calzetti
13
5
Observed Wavelength [µm]Flux [10−18 erg s−1 cm−2]

Flux density [µJy]0.5

Table 5. The best-fitting parameters of the rest-fr
far-infrared spectral energy distribution of MACS041

DustCon
Used plot
Ori plot
2σ upperBest−fit

Flux density [µJy]1

Tamura et al.

[OIII]88 line
10
5
3

1
500 1000 2000
Observed Wavelength [µm]Items

CalzettiMWχ2
Degree Of Freedom
Dust attenuation AV (mag)Age τage (Myr)♯−1
SFH τSFH(Gyr−1 )Metallicity Z (Z⊙ )LyC escape fraction fesc†
Stellar mass Mstar (108 M⊙ )−1 †SFR (M⊙ yr )†LIR (1011 L⊙ )7.0
3
0.50+0.02
−0.04
+3.5
3.5−0.7
100+0−200
0.20+0.08−0.17
0.00+0.15−0.00
2.5+2.9−0.6
59.8+2166.2−29.8
1.56+0.60
−0.51

6.8
3
0.50+
−
+
4.2−
−10+
−
+
0.20−
0.00+
−
2.5+
−
62.4+2
−3
1.68+
−
25

!
"
!
"

SED Fits: Results•UV-bright stellar component can co-exist with luminous
dust component if the dust mass pre-exists.

•Favors a young, but moderately metal-enriched solution
12

Tamura etTamuraal.
et al.

12

Z_Sun•Age ~ 4 Myr, metallicity = 0.2 Table
5. Thebest-fitting
the rest-frame
ultraviol
Table
5. Theparameters
best-fittingofparametersof therest-fr

far-infrared spectralenergydistribution
MACS0416ofY1.
far-infrared
spectralenergy of
distribution
MACS041

Extinction law
Extinctio
Calzetti

Calzetti
MW

MW
SMC

χ2
χ2
7.0
Degree Of Freedom
Degree Of Freedom
3+0.02
DustAattenuation
A0.50
Dust attenuation
V (mag)V (mag)−0.04+3.5
Age τage (Myr)Age τage (Myr)
3.5−0.7♯−1 +0−1−1 ♯ −1
SFH)−200
SFH τSFH(Gyr)τSFH (Gyr100
+0.08
Z (Z
Metallicity Z Metallicity
(Z⊙ )
0.20
⊙ )−0.17
LyC escape
LyC escape fraction
fesc fraction
0.00f+0.15
esc
−0.00
†
†
8
Stellarmass
M)
Stellar mass M
M⊙M) star (102.58+2.9⊙
star (10−0.6††−1 +2166.2
SFR) −29.8
SFR (M⊙ yr−1
) (M⊙ yr59.8††) +0.60
LIR (1011 L⊙ )LIR (1011 L⊙1.56
−0.51

7.0
6.8
3
0.50+0.02
−0.04
−0.06
+3.5
+5.2
3.5
4.2−0.7
−1.1
+110
100+0
−10
−200
−90
+0.08
+0.10
0.20−0.17
−0.15
+0.15
+0.12
0.00−0.00
2.5+2.9−0.6−0.8+2235.3
59.8
62.4+2166.2
−29.8
−34.7
+0.53
1.56
1.68+0.60
−0.51
−0.88

6.8
8.4
33
+
0.50+0
0.20
−
−0
+
+1
4.2−0
2.0
−
+
+0
−10
100
−
−2
+
0.20+0
0.20
−
−0
+
+0
0.00−0
0.40
−
+
2.5+2
2.3
−
−0
+2
62.4
104+20−3−73+
1.68+0
1.27
−
−0
26

Items

Items

!
"
!
"

SED Fits: Results•UV-bright stellar component can co-exist with luminous
dust component if the dust mass pre-exists.

•Favors a young, but moderately metal-enriched solution
12

Tamura et al.

12

Tamura et al.

= 0.2 Z_Sun•Age ~ 4 Myr, metallicity
Table 5. The best-fitting
parameters
the rest-frame
ultraviolet
to rest-fr
Table
5. Theofbest-fitting
parametersof thefar-infrared spectral energy
distributionof MACS0416
Y1.
far-infrared
spectralenergy distributionof MACS041
Extinction law
Calzetti
SMC

MW

7.0
χ2
7.0 χ2
6.8
8.4
Degree3 Of Freedom3
Degree Of Freedom
3
+0.02
+0.02
+0.05
Dust attenuation
A
(mag)
0.50
Dust attenuation AV (mag)0.50+0.02
0.50
0.20
V
−0.04
−0.04
−0.06
−0.01
+3.5
+3.5
+5.2
+1.0
Age
τage (Myr)4.2−1.1
3.5−0.6
Age τage (Myr)
3.5−0.7
2.0
−0.7
♯
♯
−1
−1 +110
−1
+0
SFH
) −90
SFH τSFH(Gyr−1 )100τSFH100+0−200 (Gyr −10
−200
+0.08
+0.10
+0.21
Metallicity
Z
(Z
)
0.20
Metallicity Z (Z⊙ )0.20+0.08
0.20
⊙
−0.17
−0.17
−0.15
−0.15
+0.15
+0.15
+0.12
+0.20
escapefraction
0.00−0.23
LyC escape fraction fesc LyC 0.00
0.00f−0.00
0.40
esc
−0.00
−0.00
†
†
+2.9
8 +2.9Stellarmass
Mstar (10M
2.5+2.8
Stellar mass Mstar (108 M⊙)
2.5+2.9
2.5
2.3
⊙)
−0.6
−0.8
−0.6
+2166.2 −1 † +2235.3
+2091
−1 †
SFR
(M⊙ yr 62.4
) −34.7
59.8
SFR (M⊙ yr )59.8−29.8
104+2166.2
−29.8
−73
†
†
+0.60
11
+0.60
+0.53
11
LIR −0.51(10 L⊙ )1.68−0.88
1.56+0.90
LIR (10 L⊙ )
1.56
1.27
−0.51
−0.38

6.8
3
0.50+
−
+
4.2−
−10+
−
+
0.20−
0.00+
−
2.5+
−
62.4+2
−3
1.68+
−
27

Items

Items
Calzetti

Extinctio

MW

!
"
!
"

Dust mass evolution model (Asano & Takeuchi+13)•Dust budget crisis: How did a galaxy get dust so quickly?
•Can our current understanding of dust evolution explain the observed
M_dust?

•Setup•SF timescale tau_SF = 0.3 Gyr•Roughly scaled so thatpredicted M_star and SFR
match the observed ones

Few AGB stars
at z ~ 8
Credit: Tsutomu T. Takeuchi
28

Dust and metallicity cannot be reproduced...!

MW Calzetti

SMC

Tdust =
40 K
50 K
SMC
MW
Calzetti

Figure 6. The time evolution of (a) stellar mass, (b) SFR, (c) metallicity, and (d) dust mass predicted in a dust formation model(Asano et al. 2013a,b, 2014; Nozawa et al. 2015) as a function of galaxy age with an initial gas mass of Mgas = 1 × 1010 M⊙ and astar-formation time-scale of τSFH = 0.3 Gyr. The open square, filled circle and triangle represent the best-fitting parameters of
the physical properties of MACS0416 Y1 estimated by the Calzetti, MW, and SMC extinction laws, respectively (see Table 5).
In panel (d) two delensed dust mass estimates for Tdust = 50 K (lower symbols) and 40 K (upper symbols) are plotted.

•More massive (~1e9 M_Sun), mature (~0.1 Gyr) stellar

6componentisrequiredto
reproduce
M
≈
4
×
10
follows, we show that there is at least a soluduration of 0.1
Gyr and attains M
a stellar
mass ofdust⊙
tion which reasonably explains the physical properties required to reproduce the observed dust
mass without any substantial change in the SED

Mstar = 3 × 109 M⊙ .
This massive, old stellar component does not
29
conflict with the best-fitting SED (§ 5.2), if theUnderlying massive, mature stellar component

SFR (M⦿/yr)

60 M⦿/yr

Young component(Best-fit solution)

mature component
30 M⦿/yr

0

300

400

Time (Myr)600(z = 8.3)

density [µJy]
FluxFluxdensity
(μJy)

10

1

Best−fit Total
Best−fit
Used photOldcomponent
2σ upperUsed phot
2σ upper

0.1

0.01

0.001

3
1
Observed Wavelength [µm]5

Observed wavelength (μm)•

A mature component (3×109 M⦿, age = 0.1 Gyr) as theorigin of dust can coexist with the young component.
30

What we learned from submm + NIR observations
Mature (~300 Myr) stars

Supernovae
as origins of dust

Young (~4 Myr) stars

Dust
Depleted PDR (?)•Futre prospects

Highly-ionized gas
Artist's impression (Credit: NAOJ)•Sub-kpc ALMA imaging of multi-phase ISM in dust (MCs), [CII] (PDRs) and [OIII] (HII)•JWST/WFIRST search for "past star-formation" components

34

Future Galaxy Survey in the Submillimeter35

Far-Infrared Fine-Structure Lines•Reach z = 20. Competitive with JWST/NIRSpec C III]1909A
MACSJ0416_Y1(z = 8.3)
z=2[O III][C II][O I]

z = 10z = 20

ALMA 3 hr integration
1σ sensitivity @100 km/s resolution36

Line Emission from HII region

Kana Moriwaki-san (UTokyo)

50h-1 cMpc
gas
star

subgrid model- Each star particle forms a HII region.
- Density in HII region is constant andscales with surrounding gas density.
nH = Knglobal
2/3
3↵B ⇣ 3QnH ⌘1/3
hU i =
4c
4⇡<latexit sha1_base64="J4WVansFPVhgBHa5i7gtyF6T1Ek=">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</latexit>

caseB
Lline = Cline (Z, n, U ) ⇥ LH
Moriwaki+ (incl. YT) 2018
CLOUDY output

star particle
M* ~ 106 M⦿

HII region
nHII = K × ncell
fiducial K = 5<latexit sha1_base64="0/Ft4BLJYjb8hvQZOhwHVD/505U=">AAACVXicbVBNSwMxEE3Xr1q/qh69BIugILIrgl4EqZcePCjYKnZryaZTDU2ySzIrlGX/kr9GEA/6M7wJpnUPtjoQePNmHm/yokQKi77/VvJmZufmF8qLlaXlldW16vpGy8ap4dDksYzNbcQsSKGhiQIl3CYGmIok3ESD89H85gmMFbG+xmECHcUetOgLztBR3WrjopuFRtGRPqen9Px3u0vv9qnep809GqJQYGmx3QgjQJbfjxvu7Ot5t1rzD/xx0b8gKECNFHXZrX6GvZinCjRyyaxtB36CnYwZFFxCXglTCwnjA/YAbQc1c/6dbPzjnO44pkf7sXFPIx2zvxUZU9YOVeQ2FcNHOz0bkf/N2in2TzqZ0EmKoPmPUT+VFGM6io/2hAGOcugA40a4Wyl/ZIZxdCFPuEQqn+wNGwDmFRdUMB3LX9A6PAgcvjqqndWLyMpki2yTXRKQY3JGGuSSNAknz+SFvJOP0mvpy5v15n9WvVKh2SQT5a19A4RCtB0=</latexit>

37

Kana Moriwaki-san (UTokyo)

Properties of high-z [OIII] emitters• well-established star forming• LOIII88 is higher than expected from thelocal relation: high ionization

log metallicity (Z⦿)

Simulation[OIII] 88μm (L⦿)

galaxies are selectively observed

Observationz=9

SFR (M⦿/yr)
Moriwaki+ 2018

parameter & moderate metallicity

log [OIII]88/Hβ

z=7

z>7
U↑

z=0
Z↓

log Z/Z⦿
38

Kana Moriwaki-san (UTokyo)

Cross-correlation: 21cm vs galaxies

Reionization
6

7

8

9

10

11

12

redshift

13

14

16

18
20
Park+ 2018

- 21-cm observation:
WFA, LOFAR, PAPER, HERA, SKA
Only statistical information: power spectrum
Foreground (synchrotron) should be excluded.
- galaxy survey/intensity mapping:
LAE (HSC), [CII] (CONCERT, TIME), CO (COMAP), [OIII] (SPHEREx?)- Foreground contamination is excluded in cross-correlation signal
39

Kana Moriwaki-san (UTokyo)

Cross-correlation
Coeﬃcient

Cross-Power Spectrum |Δ|2

Result: Ideal 3D Cross-Power Spectrum

z = 7.5, <xHI> = 0.46

When even very dark
galaxies can be detected

r21,OIII (k) = p<latexit sha1_base64="rzULWXHiRKsyBWhNyftblJoMo5k=">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</latexit>

P21,OIII (k)P21 (k)POIII (k)k (h Mpc-1)

100h−1 cMpc
40

Kana Moriwaki-san (UTokyo)

Cross-correlation
Coeﬃcient

Cross-Power Spectrum |Δ|2

Result: Ideal 3D Cross-Power Spectrum

z = 7.5, <xHI> = 0.46

When only some brightgalaxies can be detected

r21,OIII (k) = p<latexit sha1_base64="rzULWXHiRKsyBWhNyftblJoMo5k=">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</latexit>k (h Mpc-1)

P21,OIII (k)P21 (k)POIII (k)ALMA FoV

L_[OIII]88 > 3e7 L⦿

No turnover can be seen: observed galaxies reside in large HII bubble.
→ It is better to focus on large-scale power spectrum (at least for a while).
41

New discovery space?

Spectralcoverage
Cosmologicalvolume & time
Wide field

Depth
Spectralresolution
Angularresolution
Polarization

Yoichi Tamura / AtLAST Science Workshop 201842

HerMES Lockman Hole
© HerMES / ESA

4 deg

Yoichi Tamura / AtLAST Science Workshop 201843

Large Submm Telescope• Large aperture (D = 50 m)• Wide field of view (> 0.5 deg)
• Long-submm/mm frequency band
• Survey-oriented(Endo et al. 2011)

Yoichi Tamura / AtLAST Science Workshop 201844

CO/[CII]/[OIII] Tomography

Fig. 3.— Blue contours show the 250GHz continuum emission from the z = 4.0 SMG GN20. Green
contours show the CO 2-1 emissio. The greyscale shows the HST i-band image (from Carilli et al.
2010).
Cloverleaf QSO at z=2.6(Bradford et al. 2009, ApJ, 705, 112.)

CO in SMGs w/ NRO45m(Iono et al. 2012, PASJ)

Arp 220 model(Carilli et al. 2011, Astron. Nachrichten.)

LST Beam

Fig. 4.— Radio through submm spectrum of a star forming galaxy with a star formation rate 100
CO/[CII]: representative emission
lines in mm-FIR.
M⊙ year redshifted to z = 5. Also shown are the line and continuum sensitivity for the EVLA in
Benefit from negative k-correction
ofand
COtheladderand FIR
12 hours,
line sensitivity
forlines.
ALMA and the existing (sub)mm interferometers.
Overcome the confusion problems.

Yoichi Tamura / AtLAST Science Workshop 201845

Sensitivity-Limited Survey with LST• The depth achieved in the 2 deg2 survey is comparable to that obtainedin a 10-hr ALMA observation, but the survey area is ~13000 times larger
than the ALMA FoV at 3 mm.

• The survey can detect the MW-like galaxies at z ~ 2.
1.0
0.5
1 Jy km/s →

0.0
−0.5

0.1 Jy km/s →

−1.0
−1.5

0.01 Jy km/s →[OIII]88(Muv ~ −)M(H2) ~ 1e9 Mo
ALMA
10 hr

z = 15

12

−2.0
−2.5
−3.0

M(H2) ~ 1e9 Mo: S3-SAX model limitation

Yoichi Tamura / AtLAST Science Workshop 2018

10

9

8

LST 2 deg2 survey(R = 1000, i.e., Δv = 300 km/s)

46

Light cone from the LST 2-deg2 Survey
Observer (z=0)↓

Comoving Y (h-1 Mpc)

z=1

z=2

z=3

z=5

z=4

Comoving distance (h-1 Mpc)
z=6

z=7

10^5 galaxies across the cosmic time10^3 galaxies
in
the
epoch
of
reionization
Yoichi Tamura / AtLAST Science Workshop 201847

RSD Redshift Space Distortion

CO/[CII]/[OIII]
Tomography

.

.

,

EoR Epoch of Reionization/

Evolution of//

Galaxies
./
.

,

,,

/

LSS Cosmic Large-Scale Structure
/

,

.

/
/

,
/

.

,

CSFH Cosmic Star-formation History
/

/

,,

/

.

.
.

.

,

.

.

... and serendipitous discoveries,

Yoichi Tamura / AtLAST Science Workshop 2018,48

Summary•サブミリ波によって、宇宙再電離期の銀河の ISM 物理状態・
進化や星形成活動の変遷がわかってきた49