SIXER

SCUBA-2 Imaging Exploration
of the Epoch of Reionization
(SIXER)
Yoichi Tamura (IoA, UTokyo)
on behalf of the proposal tiger team:
K. Kohno, S. Ishii, T. Izumi, Y. Yamaguchi, R. Makiya (UTokyo)
M. Ouchi, S. Fujimoto, Y. Ono (ICRR, UTokyo)
T. Nagao (RCSCE, Ehime U.)
B. Hatsukade, Y. Matsuda (NAOJ-Chile),
T. T. Takeuchi (Nagoya), K. Morokuma (NRO)
6 November 2014
1
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HSC SSP のようなかたちの、semi-public survey を想定しています
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この場にいる皆さんには、ぜひプロポーザルにご参加ください！（いや、それはマズいとい
う人だけ、ご連絡ください。。。）
2
Cosmic star formation history:
Roles of dusty galaxy population
Burgarella+
...?
...?
Bouwens+
Burgarella et al. 2013
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Cosmic SFR density (SFRD) peaks at z = 1-3.
What is the role of dusty galaxies at z > 4?
Madau & Dickinson 2014
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Cosmic evolution of extinction.
What is the role of dust in z > 4 galaxies?
cosmic “obscured” star-formation through
the cosmic time is still unknown.
3
AzTEC selects many “red” SMGs
(so-called “500-um peakers”)
40% of AzTEC 1.1-mm sources are actually 500-um peakers! (40% of SMGs are
at z > 3?)
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Characterizing “red” SMGs are important in studying z > 4 SF history.
500 um peakers
(h
igh
-z Red
/lo
w
-T
)→
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4
SCUBA-2
SCUBA-2 (Holland+13)
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Submm Common User Bolometer Array 2 (Holland+13)
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Large-format bolometer array camera using TES +
SQUID technologies
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Simultaneous 450 and 850 um observations with
5120 pix each + dichroic filter (yield ~ 70%)
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FoV: 45 arcmin2 each
θHPBW: 8” (450um) and 13” (850um)
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Ω850um = 1/6 of SPT, 1/4 of AzTEC/ASTE
Mapping speed ~ 10–15 arcmin2/hr/mJy2 (fastest!)
SMURF (Chappin+13)
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Well-constructed, user-friendly reduction software
suite and pipelines
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High fidelity reproduction of astronomical emission
using the maximum likelihood approach
450 and 850 um windows
(PWV = 1mm)
450 um filter
Iterative modeling...
Extended emission
recovered
850 um filter
5
SCUBA2 Imaging Exploration of the EoR
(SIXER): The Survey Concept
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SCUBA-2 Intensive Exploration of the Epoch of Reionization (SIXER)
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Proposal will be submitted in 2014 Nov, survey will start in 2015 Feb.
Systematic survey of S > 20 mJy SMGs at z > 4 (especially, z > 6).
Submm properties of z > 4 QSOs (including ~10 z > 6 QSOs).
Submm properties of z > 4 LBGs/LAEs
Exploring ~100 mJy submm transients such as blazars (too small area?)
Method / strategy
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“From discoveries to complete follow-up observations”
Science from SIXER (+ HerMES and HSC surveys)
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10x wider, 3x more luminous layer than S2CLS
200–600 “S850 > 20mJy” SMGs over ~50 deg2 by spending ~1000 hr
HerMES Level 5 data (~35 deg2, σ500um ~ 4 mJy)
Deep optical images and huge QSO/LBG/LAE samples from HSC-Deep/Wide
Easy pre-selection with SPIRE, easy follow-up with ALMA (ASTE, LMT, ...)
toward ~200 spectroscopic sample.
Merits
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Follow-up is easy! Will feed flux-limited sample of SMGs for ALMA/ASTE
Less confusion effect, lensing magnification, ...
6
Why S850 > 20 mJy?
Easy pre-selection and follow-up
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Easy SPIRE pre-selection
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unveil a new population that has not been revealed by Herschel.
SPIRE 500um (HerMES/L5) will detect all SIXER sources at 0 < z < 5.
“SPIRE-dropouts” (or “850-um peakers”) will isolate z > 6 candidate SMGs.
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Easy identification with ALMA snapshots in 850 um continuum
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10 s integration will result in a >50σ detection.
Observing ~600 SIXER sources will take just 2 hr.
Easy redshift determination with ALMA spectral scan in 3 mm
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e.g. λpeak ~ 500, 600, 700 um at z = 5, 6 and 7, respectively (for a graybody with Tdust = 40K and β=1.5).
will double (triple?) the number of SMGs with spec-z.
A 5-min spectral scan over the whole Band 3 will yield a >5σ detection.
17 hr integration will yield ~200 spectroscopic redshifts of SMGs.
Feeding a set of bright SMGs to be followed up by DESHIMA/ASTE.
7
5σ limiting FIR luminosity
500-um peakers
850-um peakers
8
Limiting LFIR vs survey area at z=2
+ SASSy
SPT
AzTEC ◆+ S2CLS
SPIRE confusion limit (1σ)
r
pe r
ee e
D Wid
&
Oliver+2012
9
Limiting LFIR vs survey area at z=6
SPIRE confusion limit (1σ)
SPT
+ SIXER
(Legacy-type survey)
AzTEC ◆ + S2CLS
r
pe r
ee e
D Wid
&
Oliver+2012
10
SMG science
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サーベイから得られるもの
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200個を超える明るい (S850 > 20 mJy) SMG のサンプル
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すべてのCO輝線を検出するには ALMA で合計 17hr (on-source)。限られた個数
(<10) に対しても、CARMA でもフォローアップが可能になる。
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赤方偏移、分子ガス質量、ダスト質量、dust-to-gas ratio が得られる。
サイエンスケース
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Bright SMGの赤方偏移分布 (z > 4 も高精度で)。星形成率密度の進化。
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z > 4, 5 でのダスト生成メカニズムへの制限
11
Dust in z > 5 objects
Nozawa et al. 2014, arXiv:1410.7861
Graphite carbon
Amorphous carbon
z = 6.3 QSO
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遠方 QSO で大量のダスト (~10^8 Msun) が見つかった
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Type SNe II で説明しようとすると、巨大な dust yield (~0.1-1 Msun/SN) が必要
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星間空間中のダスト成長 (shuttering+coagulation) (Asano+13, Nozawa+14)
減光曲線のかたちがちがう？
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分子雲内部で効率的に amorphous carbon を主成分としたダスト成長が生じている
(Nozawa+14)
z > 5 QSO のダスト質量 + (分子)ガス質量の測定によって検証することが重要→ ALMA, SCUBA-2
12
LBG Science
藤本さん、大内さん、小野さん
[A/I: HSC samples plan] Seiji Fujimoto, Masami Ouchi, Yoshiaki Ono (ver. 2) 2014/10/27
1. JCMTサーベイでHSC/LBGサンプルをStackingしたときdust emissionの見積もり。
z 6 LBGsサンプル個数の間違いを修正(コラムずれでした..)
•
from Tamura-san slide
サーベイスピードは右図青線が妥当ということでサーベイ
•
1.
27deg^2 1σ 3.0mJy
3.
80deg^2 1σ 5.7mJy
2.
の広さと深さをそれに対応させた上で、右図の3ケースで再
導出。
50deg^2 1σ 4.0mJy
β-IRXの関係を見るために各redshiftソース全部stacking
•
するのではなく光度毎でstackingを行った。
HSC/deep samples
HSC/wide samples
z=4
0.6
0.6
0.4
0.4
0.4
0.4
0.2
-2.1
-2
3.6σ
-1.9
-1.8 -1.7
beta
0
-1.5
-1.4
-1.3
-2.2
-2.1
-2
-1.9
-1.8 -1.7
beta
-1.6
-1.5
-2.2
-1.3
-1.4
-2
-1.9
-1.8 -1.7
beta
-1.6
-1.5
-1.4
-1.3
-2.2
0.4
0.4
0.4
0.4
4.7σ
-0.2
-2.2
0.2
0
0
0
-2.1
-2
-1.9
-1.8 -1.7
beta
4.5σ
-0.2
-1.6
-1.5
-2.2
-1.3
-1.4
log(Ffir/F1600)
0.6
log(Ffir/F1600)
0.6
-2.1
-2
-1.9
-1.8 -1.7
beta
-1.5
-2.2
-1.3
-1.4
-2
-1.9
-1.8 -1.7
beta
-1.6
-1.5
-1.4
-1.3
-2.2
0.4
0.4
0.4
0
3.2σ
-0.2
-2.2
-2.1
-2
-1.9
-1.8 -1.7
beta
3.1σ
-0.2
-1.6
-1.5
-1.4
-2.2
-1.3
-2.1
-2
-1.9
-1.8 -1.7
beta
-1.6
-1.5
-1.4
log(Ffir/F1600)
0.4
log(Ffir/F1600)
0.6
log(Ffir/F1600)
0.6
0
0.2
0
-0.2
-0.2
-2.2
-1.3
-1.6
-1.5
3.7σ
-2.1
-2
-1.9
-1.8 -1.7
beta
-1.6
-1.5
-1.4
-2.1
-2
-1.9
-1.8 -1.7
beta
-1.3
-2.2
-1.6
-1.5
-1.4
-1.3
広さあまり関係ない.
•
さが効く->狭い方が
50deg^2
1σ 4.0mJy
-1.4
2.6σ
有利.
-1.3
-2.1
-2
-1.9
-1.8 -1.7
beta
-1.6
-1.5
80deg^2
1σ 5.8mJy
-1.4
-1.3
βが小さい(uv暗い)
ものはサーベイの深
•
0.2
0
β
-1.8 -1.7
beta
-0.2
-2.1
0.6
0.2
-1.9
0.2
0.6
0.2
-2
0
-0.2
-1.6
-2.1
βが大きい(uv明る
い)側ではサーベイの
27deg^2
1σ 3.0mJy
-0.2
-2.1
0.6
0.2
4.8σ
0.2
0.6
0.2
•
0
-0.2
-0.2
-1.6
log(Ffir/F1600)
log(Ffir/F1600)
log(Ffir/F1600)
0.2
0
-0.2
-2.2
0.2
log(Ffir/F1600)
0.6
log(Ffir/F1600)
0.6
0
log(Ffir/F1600)
z=7
z=6
z=5
log(Ffir/F1600)
log(Ffir/F1600)
結果:
z 7ソースも非検出
であってもupper
limitはつく.
13
QSO Science
2014年10月8日＠IoA
SCUBA-2/JCMT survey
QSO science検討
QSO science検討班
（泉拓磨、長尾透）
SMBHは母銀河より先に成長したのか？
低光度quasarの大量観測 + stacking解析を利用して、微分形マゴリ
アン関係の赤方偏移進化を（極力観測バイアスを低減して）捉える。
14
Low-z Disk Galaxies
諸隈さん、竹内さん
15
Activities and Timeline
- Start of SIXER (winter?)
- Initial results (σ = 5 mJy, A ~ 10 deg2)
- (ALMA Cycle 3)
2016
- Continuation of SIXER
- Interim results (σ = 5 mJy, A ~ 30 deg2)
- (ALMA Cycle 4?)
2017
- Completion of SIXER (winter?)
- Final results (σ = 5 mJy, A ~ 50 deg2)
- (ALMA Cycle 5?)
Follow-up observations
2015
Kickoff (8E)
JCMT Science WS (9B)
1st proposal team meeting (9M)
SCUBA-2/SMURF seminar (10B)
2nd proposal team meeting (10B)
Announcement (11M)
JCMT proposal (informal letter?) (12B)
Input from the HSC survey
2014
Quick completion in short period (~2yr)
-
16
Feasibility study / field selection
17
Lensed
SMGs
SIXER
S2CLS
SIXER
- Total exposure time is fixed to 1000 hr.
- The model counts are scaled using a factor of
S1.1mm/S850um = 0.51.
- 200–300 > 5σ sources or
~1000 > 3.5σ sources may be detected in 1000 hr.
S2CLS
SIXER
S2CLS
Number counts (updated)
18
4. Pipeline
• 
–  1 hour
– 
–  Jack-knife map
Jack-knife map
temporary file
FAINT_POINT_SOURCES_JACKKNIFE
– 
A 1835 map
A 1835 S/N map
Viewgraph prepared by Yamaguchi-san
19
Level
Name
Area (deg2)
Budget (hr)
L1
ECDFS
[CDFS-SWIRE]
0.35, 0.58,
11.4, 10.9
20, 8.8,
41, 50
1.1, 3.3
03h32
–27d50
COSMOS
2.8, 4.4
50, 25
2.0, 4.9
10h00
+02d10
GOODS-North
0.55
14
bad data?
Groth-Strip
[EGS-HerMES]
0.60, 2.7
4, 23
3.2, 5.1
14h20
+52d50
(maybe yes)
Lockman-North
[Lockman-SWIRE]
0.65, 7.6
4, 41
3.2, 4.9
10h47
+58d00
SWIRE
Lockman-E-ROSAT
[Lockman-SWIRE]
0.57, 1.4, 7.6
3, 5, 41
3.2, 4.9
10h47
+58d00
SWIRE
UDS
2, 19
11, 46
3.4, 6.2
02h18
–05d05
HSC-U/D/W
SWIRE
SpUDS
VVDS
2, 19
10, 46
3.4, 6.2
02h26
–04d30
HSC-D/W
SWIRE
CDFS-SWIRE
11.4, 10.9
42, 50
3.3
03h32
–28d10
Lockman-SWIRE
17.4, 7.6
14, 41
11, 4.9
10h47
+58d00
SWIRE
EGS-HerMES
2.7
23
5.1
14h20
+52d50
(maybe yes)
Bootes-HerMES
3.3, 10.6
20, 28
3.2, 6.1
14h33
+34d10
SDWFS
ELAIS-N1-HerMES
3.3
21
3.9
16h10
+54d20
σ500 (mJy)
RA
Dec
HSC
HSC-U/D/W
VLA
IRAC
VLASS-D
GOODS
SWIRE
SIMPLE
VLASS-D
S-COSMOS
L2
L3
GOODS
L4
L5
YT’s first
impression
Accessible from
ALMA
VLASS-D
HSC-D
VLASS-D
GOODS
SWIRE
SWIRE
20
EGS
Level 5
v
Le
Lev 3
3
Lev 3
ELAIS-N1
Lev 5
Level 5
Bootes
FLS
Lockman-SWIRE
Level 6
Level 5
Level 6
XMM-LSS
30 deg2
Level 6
ECDFS
1 deg2
Level 4
Level 4
Lev 1
Level 5
COSMOS
Level 2
21
XMM-LSS
HerMES
SIXER
ES
rM
e
H
VLASS
(Wide)
/L3
SERVS/IRAC
SWIRE
VLA
S2CLS
HSC-D
SW
IRE
/IR
AC
H
/
ES
M
er
L3
SERVS
Average SMG
(z = 1, 2, 3, 4, 5, 6, 7, 8)
HerMES/L6
HSC-D
SIXER? (10 deg2)
22
COSMOS
HerMES
SIXER
S-COSMOS/IRAC
VLASS
(Deep)
S2CLS
HSC-D
LA
V
S
S
Her
MES
/
S-COSMOS
L2
Average SMG
(z = 1, 2, 3, 4, 5, 6, 7, 8)
HSC-D
CLS? (4.0 deg2)
23
ev
el
6
da
ta
あ
り
ELAIS-N1
er
M
ES
/L
VLASS
【
田
村
注
】
H
HerMES
SIXER
H
E
M
r
e
L
S/
5
SWIRE
VLASS
(Deep)
HSC-D
SE
S
RV
S/
W
IR
A
IR
C
E/
IR
A
SERVS
C
Average SMG
(z = 1, 2, 3, 4, 5, 6, 7, 8)
HSC-D
SIXER? (3.2 deg2)
SIXER? (9.4 deg2)
24
ECDF-S
HerMES
VLASS
SIXER
SWIRE
VLASS
(Deep)
SERVS/IRAC
RAC
SWIRE/I
E
HerM
S/L5
SERVS
Average SMG
(z = 1, 2, 3, 4, 5, 6, 7, 8)
SIXER? (8.5 deg2)
25
Lockman Hole
HerMES
SIXER
IR
A
/L
3
SWIRE
RV
S/
rM
ES
SE
He
C
HerMES/L3
H
er
M
ES
/L
S
W
IR
IR
/
E
A
C
SERVS
Average SMG
(z = 1, 2, 3, 4, 5, 6, 7, 8)
5
SIXER? (11 deg2)
26
Bootes
HerMES
SIXER
SDWFS
S
D
W
FS
R
/I
A
5
Average SMG
(z = 1, 2, 3, 4, 5, 6, 7, 8)
C
HerME
S/L
E
M
r
He
S/L6
HSC-D
SIXER? (8 deg2)
27
Deep 2/3
PI Obs (partially available)
SIXER
HSC-D
Average SMG
(z = 1, 2, 3, 4, 5, 6, 7, 8)
HSC-D
SIXER? (7 deg2)
28
Visibility plot
29