HSC SSP で銀河を究めよう
嶋作一大 (東大)

HSC とは？
SSP とは？
HSC SSP とは？
HSC SSP の銀河サイエンス
HSC SSP に参加するには2Hyper Suprime-Cam
Hyper Subaru Prime-focus Camera

104 CCDs3

1視野に対応する共動長と共動体積

HSC

Coma
Cluster

SupCam共動体積

z = 1, 2, 7

HST
8Mpc 電離泡 BAO

共動長4

HSC とは？
SSP とは？
HSC SSP とは？
HSC SSP の銀河サイエンス
HSC SSP に参加するには

5

すばるプロポーザルの3カテゴリー

ノーマル
インテンシブ戦略枠 (SSP)

5夜
40夜
300夜

6

Subaru Strategic Program
すばる望遠鏡「戦略枠」とは、他の追随を許さないユニークな観測装置（またはその組み合わせ）を用い、個人または個別グループの研究課題を超えて、長期にわたるまとまった観測を行うもので、これによってすばる望遠鏡の成果を世界により強く発信するとともに、当該分野でサイエンスのリーダーシップを確立することを目的とするものである。(すばるウェブより)

All Japan で歴史的観測[過去のSSP]SEEDS (系外惑星探査、田村元秀ほか、120夜)
FastSound (宇宙論、戸谷友則ほか、40夜)

7

HSC とは？
SSP とは？
HSC SSP とは？
HSC SSP の銀河サイエンス
HSC SSP に参加するには

8

HSCを300夜使う広域サーベイ
Wide-field imaging with Hyper Suprime-Cam:
Cosmology and Galaxy Evolution
A Strategic Survey Proposal for the Subaru Telescope
PI: Satoshi Miyazaki (NAOJ)
Co-PI: Ikuru Iwata (NAOJ)
The HSC collaboration team1 : S. Abe(1) , H. Aihara⋆(2),(3) , M. Akiyama(4) , K. Aoki(5) , N. Arimoto⋆(5) , N. A. Bahcall(6) ,S. J. Bickerton(3) , J. Bosch(6) , K. Bundy†(3) , C. W. Chen(7) , M. Chiba†(4) , T. Chiba(8) , N. E. Chisari(6) , J. Coupon(7) , M.
Doi(2) , M. Enoki(9) S. Foucaud(10) , M. Fukugita(3) , H. Furusawa†(5) , T. Futamase(4) , R. Goto(2) , T. Goto(11) , J. E. Greene(6) ,J. E. Gunn†(6) , T. Hamana†(5) , T. Hashimoto(2) , M. Hayashi(5) , Y. Higuchi(2),(5) , C. Hikage(12) , J. C. Hill(6) , P. T. P. Ho⋆(7) ,B. C. Hsieh(7) , K. Y. Huang†(7) , H. Ikeda(13) , M. Imanishi(5) , N. Inada(14) , A. K. Inoue(15) , W.-H. Ip(1) , T. Ito(5) , K.
Iwasawa(16) , M. Iye(5) , H. Y. Jian(17) , Y. Kakazu(18) , H. Karoji(3) , N. Kashikawa(5) , N. Katayama(3) , T. Kawaguchi(19) , S.
Kawanomoto(5) , I. Kayo(20) , T. Kitayama(20) , G. R. Knapp(6) , T. Kodama(5) , K. Kohno(2) , M. Koike(5) , E. Kokubo(5) , M.
Kokubo(2) , Y. Komiyama(5) , A. Konno(2) , Y. Koyama(5) , C. N. Lackner(3) , D. Lang(6) , A. Leauthaud†(3) , M. J. Lehner(7) , K.Y. Lin(7) , L. Lin(7) , Y.-T. Lin†(7) , C. P. Loomis(6) , R. H. Lupton†(6) , P. S. Lykawka(21) , K. Maeda(3) , R. Mandelbaum†(22) , Y.
Matsuda(5) , K. Matsuoka(13),(23) , Y. Matsuoka(12) , S. Mineo(2) , T. Minezaki(2) , H. Miyatake(6) , R. Momose(2) , A. More(3) , S.
More(3) , T. J. Moriya(3) , T. Morokuma†(2) , H. Murayama⋆(3) , K. Nagamine(24) , T. Nagao†(23) , S. Nagataki(23) , Y. Naito(2) , K.
Nakajima(2) , F. Nakata(5) , H. Nakaya(5) , T. Namikawa(2) , C.-C. Ngeow(1) , T. Nishimichi(3) , H. Nishioka(7) , A. J. Nishizawa†(3) ,K. Nomoto(3) , M. Oguri†(3) , A. Oka(2) , N. Okabe(7) , S. Okamoto(25) , S. Okamura(26) , J. Okumura(23) , S. Okumura(27) , Y.
Okura(5) , Y. Ono(2) M. Onodera(28) , K. Ota(23) , M. Ouchi†(2) , S. Oyabu(12) , P. A. Price(6) , R. Quimby(3) , C. E. Rusu(2),(5) , S.
Saito(29) , T. Saito(3) , Y. Saitou(30) , M. Sato(12) , T. Shibuya(5) , K. Shimasaku†(2) , A. Shimono(3) , S. Shinogi(2) , M. Shirasaki(2) ,J. D. Silverman(3) , D. N. Spergel⋆(6),(3) , M. A. Strauss†(6) , H. Sugai(3) , N. Sugiyama(12),(3) , D. Suto(2) , Y. Suto⋆(2) , K. Tadaki(2) ,M. Takada†(3) , R. Takahashi(31) , S. Takahashi(5) , T. Takata(5) , T. T. Takeuchi(12) , N. Tamura(3) , M. Tanaka(5) , M. Tanaka†(3) ,M. Tanaka(4) , Y. Taniguchi(13) , A. Taruya(2) , T. Terai(5) , Y. Terashima(13) , N. Tominaga(32) , J. Toshikawa(30) , T. Totani(23) ,M. Tsai(1) , E. L. Turner⋆(6) , Y. Ueda(23) , K. Umetsu(7) , Y. Urata†(1) , Y. Utsumi(5) , B. Vulcani(3) , K. Wada(33) , S.-Y. Wang(7) ,W.-H. Wang(7) , T. Yamada(4) , Y. Yamada(5) , K. Yamamoto(34) , H. Yamanoi(5) , C.-H. Yan(7) , N. Yasuda†(3) , A. Yonehara(35) ,F. Yoshida†(5) , N. Yoshida(2) , M. Yoshikawa(36) , S. Yuma(2) (1) NCU, Taiwan (2) Tokyo (3) Kavli IPMU (4) Tohoku (5) NAOJ
(6) Princeton (7) ASIAA (8) Nihon (9) Tokyo Keizai (10) NTNU, Taiwan (11) DARK, Copenhagen (12) Nagoya (13) Ehime(14) NNCT (15) Osaka Sangyo (16) Barcelona (17) NTU, Taiwan (18) Chicago (19) Tsukuba (20) Toho (21) Kinki (22) CMU(23) Kyoto (24) Las Vegas (25) KIAA, China (26) Hosei (27) JSGA (28) ETH (29) Berkeley (30) GUAS (31) Hirosaki (32)
Konan (33) Kagoshima (34) Hiroshima (35) Kyoto Sangyo (36) JAXA

2012 Oct 申請2013 Apr 採択
2014 Feb 観測開始
2016 Apr 80夜終了

Executive Summary

9

of the standard model of cosmology, and test for exotic variations such as deviations from the predictions ofGeneral Relativity on cosmological scales. Studies of the highest-redshift galaxies and quasars discoveredin this survey will lead to a deeper understanding of reionization, a key event in the thermal history of theUniverse.

サーベイデザイン

Table 1: Summary of HSC-Wide, Deep and Ultradeep layers
Layer
WideDeep
UltradeepArea[deg2 ]
140027
3.5# ofFilters & Depth
Comoving volume
HSC fields[h−3 Gpc3 ]916
grizy (r ≃ 26)∼ 4.4 (z < 2)15
grizy+3NBs (r ≃ 27) ∼ 0.5 (1 < z < 5)
Wide-fieldimaging with Hyper Suprime-Cam
2grizy+3NBs (r ≃ 28) ∼ 0.07 (2 < z < 7)

Key Science
WL cosmology, z ∼ 1 gals, clusters< 2 gals, reionization, WL calib.
z∼> 2 gals, reionization, SNeIaz∼

HSC-UDThe experience of the Sloan Digital
Sky Survey (SDSS; York et al. 2000), and the tremendous success ofthe current prime-focus camera on Subaru, Suprime-Cam (Miyazaki et al. 2002a), have demonstrated theHSC-D
power of wide-field imaging to make science breakthroughs in a broad range of topics. The SDSS imaged
in five broad-bands (u, g, r, i, and z), to a depth of r ≈ 22.5 (5σ point source). It has produced more
HSC-Wide facility, including the Keck Telescopes
highly cited papers in recent years than any other observational
and the Hubble Space Telescope (Madrid & Macchetto 2009). The SDSS characterized the nature anddistribution of galaxies in the local present-day Universe. Observations with Suprime-Cam have led theworld in studies of the distant Universe, and have shown that an imager on the Subaru telescope has thepotential to extend SDSS low-redshift discoveries in the field of cosmology and galaxy formation/evolution
to the intermediate- and high-redshift Universe. The HSC survey we propose will cover SDSS-like volumes
at high redshift, making it the first truly large-scale survey of the distant Universe.

10Figure 1: Left: The limiting magnitudes (in r) and solid angles of the HSC-Wide, Deep and Ultradeep (Ucompared with other existing, on-going, and planned surveys. The three layers are complementary to each

サーベイ天域

秋

春

他の撮像プロジェクトとのシナジー
・CLAUDS (D 4): CFHT U・Arizona (D 2): UKIRT/WFCAM J,H,K・SPLASH (UD 2): Spitzer/IRAC ch1,ch2
11

3

狭帯域フィルター

grizy

名称z(Lyα)

NB387

2.2

NB816

5.7

NB921

6.6

NB101

7.2

大気夜光

d solid angles of the HSC-Wide, Deep and Ultradeep (UD) layers,
ed surveys. The three layers are complementary to each other, ander area than do other on-going surveys of comparable depth. The12

画像とカタログ
Pipeline team が提供
・整約済みの画像・マルチバンドカタログ
各サイエンスワーキンググループが提供
・photometric redshifts
・特定の天体種族のカタログ (eg, clusters, LAEs)→ 古澤さんの講演

13

過去の栄光(1) Sloan Digital Sky Survey
口径2.5m専用望遠鏡による米日独他の撮像分光サーベイよく整備された「サーベイポリシー」
4,700 refereed papers (“SDSS”)
210,000 citations (“SDSS”)(2) Suprime-Cam
HSC の前身
Subaru Deep Field, Subaru/XMM-Newton Deep Field
220 refereed papers (“Suprime-Cam”)
6,600 citations (“Suprime-Cam”)

14

HSC とは？
SSP とは？
HSC SSP とは？
HSC SSP の銀河サイエンス
HSC SSP に参加するには15

どの時代を調べるか？

再電離quenching
形態
銀河団

銀河形成
Madau & Dickinson 1416

検出される銀河の数

2 < z < 7.3
z<2
LBGs

QSOs

LAEs
10000
(z~4-7)Wide

2.2e+7

1.9e+7Deep

7.7e+52.2e+62.1e+42000(9割z<1)

UDeep?

1.4e+6

1.8e+4?

17

銀河サイエンス■プロポーザルに書かれているサイエンス
Galaxy evolution at z<2 (成熟期)
・Relationship between galaxies and dark haloes
・Physics of growth, quenching, and mass assembly・Galaxy evolution in clusters of galaxies
Galaxy evolution at z>2 (形成期)・Relationship between galaxies and dark haloes
・Nature of LAEs and LABs
・Quasars and AGNs (SMBHs, dark haloes, environments, host gals)
Cosmic reionization
・Epoch and topology
・Sources■参加者が自由にサイエンスを発案、実行してよい■他の装置や望遠鏡での追観測 (PFS, Keck, ALMA, TMT, ...)
18星質量/ダークハロー質量銀河とダークハローの関係

独立に、幅広い範囲で Mh・weak lensing (z<2)
・clustering (all z)

z<2

Mstar 以外の物理量
・SFR, 形態…

z>2

特定の銀河種族
・LAEs, LABs, …
Behroozi+13

ダークハロー質量 [Msun]

19

Wide-field imaging with Hyper Suprime-Cam

宇宙再電離
21

再電離時期の推定
・LAEs LF, clustering
・それ以外の方法
電離源
・明るい銀河の性質
・AGN

igure 10: Left: Expected measurements of the Lyα LFs at z = 5.7 (blue), 6.6 (green), and 7.3 (red) with theltradeep and Deep layer data. The existing Suprime-Cam measurements at z = 7.3 go very deep, although oververy small area. The open circles are the current best measurements given by Suprime-Cam observations. Theecrease in the LF with increasing redshift is interpreted as due to the onset of reionization. Right: ExpectedCF ω(θ) of z = 6.6 LAEs from the Deep layer in the case of full ionization, assuming that they are hosted byMhalo = 3 × 1010 M⊙ halos (red dots). The solid curves indicate the ACFs of LAEs with Mhalo = 3 × 1010 M⊙
r xHI = 0, 0.3, 0.5, 0.8 taken from McQuinn et al. (2007) simulations of inhomogeneous reionization. The blackquares are the best estimates of the z = 6.6 LAE ACF available to date (Ouchi et al. 2010). Our accurate ACF
easurements over a range of a factor of 30 in θ will allow us to detect the diﬀerence in the ACF shape between thell and partial ionization cases and to constrain xHI with an uncertainty of ∼ 0.2.

20

HSC とは？
SSP とは？
HSC SSP とは？
HSC SSP の銀河サイエンス
HSC SSP に参加するには21

“Collaboration Policy”
10ページの文書 (誰でも読める)
参加権・Japanese astronomers・Faculty and long-term staff members at Princeton or ASIAA
・Executive Board に特別に認められた個人
・External collaborators
データアクセス権論文の著者になる権利
サイエンスの宣言から論文投稿まで・始める前にプロジェクトとして宣言
・誰でも宣言できる・既存プロジェクトへの参加も可能
・PhD thesis プロジェクトの保護 (競合の禁止)
・現在184プロジェクト
22

HSC SSP に参加するには日本の研究者なら誰でも参加可能
現在200名hscsurvey

2016/05/17 12:13

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2324限界等級25

銀河の数の詳細
Wide-field imaging with Hyper Suprime-Cam

14z<2z
0.1
0.3
0.5
0.7
0.9
1.2
1.5
1.8′′

0.65 (kpc)
1.2
2.9
4.0
4.6
5.1
5.4
5.5
5.5

HSC-Wide
Vol (Gpc ) log M∗lim
0.1
8.2
0.5
8.9
1.0
9.4
1.6
9.8
2.6
10.0
3.9
11.5
4.5
11.6
4.8
11.8
3

Ngal
0.4M
2.2M
4.4M
6.0M
8.8M
0.1M
23k1kHSC-Deep
Vol (Gpc ) log M∗lim
0.001
8.70.008
9.3
0.019
9.8
0.029
10.1
0.049
10.2
0.073
10.4
0.083
10.6
0.090
10.8
3Ngal
7.2k
38.3k
71.8k
94.4k
137.3k166.2k145.7k
108.9kTable 4: Galaxy sample characteristics in a series of redshift slices for both Wide and Deep. The first column provides
the mean redshift of each slice. The second column gives the physical scale subtended by 0.65′′ , the median i-band
seeing in both layers. The remaining columns indicate the volumes, stellar mass completeness limits, and numberof galaxies expected above these limits for both layers. For Wide at z < 1, log M∗lim is defined by the faintest red
galaxy that is detectable with a y-band flux 1 mag shallower than our 5σ depth limit. At z > 1, we switch to a
UKIDSS/LAS K-band 5σ depth limit of K = 20.2 AB. For Deep, mass limits correspond to 1 mag shallower than a
5σ limit of K = 22.8 AB. We assume a standard cosmology with H0 = 70 km s−1 Mpc−1 .

The median expected seeing of 0.65′′ corresponds to a PSF whose area is 50% the size of a typical galaxy
at z ∼ 1 (see Table 4). This allows for size, concentration, and inclination measurements. In addition,
10–15% of HSC data will have a seeing FWHM of 0.35′′ or better, vastly increasing the volume and sample
size of studies tracking detailed morphological evolution (e.g., bulge growth, bars, spiral arms).

z>2

4.2

The physics of growth, star formation quenching, and mass assembly at z < 2Numerous studies have now confirmed that the SFR density in the Universe peaks roughly at z ∼ 1–2 andthen falls by a factor of ∼30 to the present day (e.g., Hopkins et al. 2006a). The average amount of starformation depends on the stellar mass, M∗ ; low-mass galaxies typically form stars at a greater relative
rate, and their star formation is quenched later, than in high-mass galaxies. The processes responsible for26