Yoshiki Matsuoka (NAOJ)

すばるHSC + WFIRSTによる遠方クエーサー探査の可能性
松岡 良樹（国立天文台）

GOPIRA symposium (NAOJ, Mitaka; Sep 26-28, 2016)

Yoshiki Matsuoka (NAOJ)

GOPIRA symposium (NAOJ, Mitaka; Sep 26-28, 2016)

Yoshiki Matsuoka (NAOJ)

クエーサー／１型AGNは。。
・多波長測光データから情報を得にくい

Selsing+16- 静止系紫外 - 可視光は基本的にpower-law continuumに支配される- 静止系近赤外線から、トーラスの塵放射の寄与が見えてくる・銀河に比べて面密度が小さい
・銀河に比べて明るい➔ 分光に対する撮像観測のメリットが限定的
・時間軸を足すと、話は別

GOPIRA symposium (NAOJ, Mitaka; Sep 26-28, 2016)

Yoshiki Matsuoka (NAOJ)

GOPIRA symposium (NAOJ, Mitaka; Sep 26-28, 2016)

Yoshiki Matsuoka (NAOJ)

今日の内容✶ 遠方クエーサー探査の目的✶ すばるHSCによる探査の進展✶ 赤方偏移の壁を超えて：
HSC + WFIRST による新探査の可能性

GOPIRA symposium (NAOJ, Mitaka; Sep 26-28, 2016)

Yoshiki Matsuoka (NAOJ)

High-z quasars - Unique probe of the early Universe
Fundamental questions we aim to answer:
Why do supermassive black holes (SMBHs) exist?
✶ When were they born?
✶ What were their seeds?
✶ How did they grow in the early and late epochs of the cosmic history?
[Observational signatures]- What are the luminosity/mass functions of quasars/SMBHs?
- Are 109 Msun-class SMBHs common or exceptional at z > 6?
- How do the luminosity/mass functions evolve towards lower redshift?

How did the host galaxies form and (co-)evolve?
✶ When and how did the first stellar-mass assembly happen?
✶ Did SMBHs impact the host galaxy evolution? If so, how?
✶ Do they mark the highest density peaks of the underlying matter distribution?
[Observational signatures]- What are the current and past star formation activities, inferred from the amount andkinematics of the gas, current SFR, and chemical enrichment?
- Do we find special (e.g., over-dense) environments around the quasars/host galaxies?

When and how was the Universe re-ionized?
✶ When did re-ionization start and complete?
✶ How did it proceed, as a function of space and time?
✶ What provided the ionizing photons?
[Observational signatures]- How does the IGM neutral fraction change along redshift and transverse direction?
- Do low-luminosity quasars emit enough UV photons to re-ionize the Universe?

and many more!
GOPIRA symposium (NAOJ, Mitaka; Sep 26-28, 2016)

Yoshiki Matsuoka (NAOJ)

Past/ongoing surveys and their immense legacy value

SDSS 2.5m

CFHT 3.6m

UKIDSS/VIKING 4m>100 quasars known at z > 5.7:
only several (one) at z > 6.5 (z > 7)
or M1450 > −24 mag

Pan-STARRS1 1.8m

Luminosity function

DES 4mComparison with theoretical models

Mortlock+11
Kashikawa+15

A wide variety of follow-up observations with
✶ ALMA for FIR-based SFR, gas and dust masses, gas kinematics, dynamical galaxy mass, ...
✶ Subaru and other large optical/near-IR telescopes (→ELTs) for SMBH mass, metallicity distribution, IGM properties, ...
✶ HST (→JWST) for the morphology, UV-based SFR, etc. in the host galaxies, surrounding ionized gas, ...
✶ Chandra and XMM-Newton (→ATHENA) for intrinsic mass accretion rate, Eddington ratio, absorbers, ...

GOPIRA symposium (NAOJ, Mitaka; Sep 26-28, 2016)

Yoshiki Matsuoka (NAOJ)

Subaru Hyper Suprime-Cam SSP survey
Hyper Suprime-Cam (HSC)✶ 116 2K x 4K Hamamatsu FD CCDs(104 CCDs are used for science exposures)✶ Circular FoV of 1°.5 diameter✶ Installed on the Subaru 8.2-m telescope✶ Miyazaki et al. (2016, in prep.)
The HSC SSP (Subaru Strategic Program) survey✶ 300 Subaru nights over 5 years, started in early 2014.
- Wide: rAB < 26.1 mag over 1400 deg2
- Deep: rAB < 27.1 mag over 27 deg2
- UDeep: rAB < 27.7 mag over 3.5 deg2
✶ Filters: (g, r, i, z, y) in Wide, + NBs in Deep & UDeep

GOPIRA symposium (NAOJ, Mitaka; Sep 26-28, 2016)

Yoshiki Matsuoka (NAOJ)

The first outcomeDiscovered in September 2015, by the first GTC/OSIRIS observations
HSC grizy

OSIRIS 2d spectrum
Blue (~7300 A)

Red (~10200 A)

OSIRIS 1d spectrum
Blue: SDSS low-z composite(shifted to z = 6.09)

GOPIRA symposium (NAOJ, Mitaka; Sep 26-28, 2016)

Yoshiki Matsuoka (NAOJ)

Discovery continues

Quasars

GOPIRA symposium (NAOJ, Mitaka; Sep 26-28, 2016)

Yoshiki Matsuoka (NAOJ)

Surprisingly...

GOPIRA symposium (NAOJ, Mitaka; Sep 26-28, 2016)

Yoshiki Matsuoka (NAOJ)

Our score sheet✶ Spectroscopic identification as of 2016 Sep 2Candidates(zAB < 24.5, yAB < 24.0)

80Known z ≥ 6 quasars

5Spectroscopy done

55

Quasars at z ≥ 631Galaxies at z ~ 68

[O III] emitters at z ~ 0.8

2Brown dwarfs

8

Moving/transient

6

GOPIRA symposium (NAOJ, Mitaka; Sep 26-28, 2016)

Yoshiki Matsuoka (NAOJ)

赤方偏移の壁を越えて：HSC + WFIRSTによる新探査の可能性
137億年
(現在)

初代天体の時代
10億年(z ~ 6)

7.5億年(z ~ 7)

すばる望遠鏡 (HSC探査)

5億年(z ~ 10)

暗黒時代

宇宙誕生

2億年
(z ~ 20)

東京大学アタカマ天文台 (TAO)
6.5m望遠鏡

ATHENAWFIRST& more future space missions

地上可視光探査（2014 〜 2020年）

地上近赤外線探査（2018 〜 2025年）
GOPIRA symposium (NAOJ, Mitaka; Sep 26-28, 2016)

スペース近赤外線・X線探査（2024年〜）

Yoshiki Matsuoka (NAOJ)WFIRST-AFTA SDT 2015 Report
Table 2-1
(High-Latitude Survey; HLS)LSST Science Book v.2

GOPIRA symposium (NAOJ, Mitaka; Sep 26-28, 2016)

Yoshiki Matsuoka (NAOJ)

Prospect for HSC + WFIRSTFor example...
✶ HSC z- and y-band imaging over 50 deg2 of the WFIRST-HLS fields.
✶ HSC (zAB, yAB) < (26.5, 26.0) mag combined with WFIRST-HLS YAB < 26.5 mag (5σ).
✶ cf. LSST coadd 5σ depth (zAB, yAB) ~ (26.2, 24.9) mag.
✶ >10 quasars at z ~ 7 with yHSC < 25.0 mag, zHSC − yHSC > 1.5.
✶ Several quasars at z ~ 8 with YWFIRST < 25.0 mag, yHSC − YWFIRST > 1.0.
✶ Quasars at z > 8 can be searched for with the WFIRST colors alone as YWFIRST dropouts.
✶ The above HSC survey will require 50 nights each in the z and y band, including overheads
and weather factor (scaled from the HSC-SSP survey).

GOPIRA symposium (NAOJ, Mitaka; Sep 26-28, 2016)

Yoshiki Matsuoka (NAOJ)

GOPIRA symposium (NAOJ, Mitaka; Sep 26-28, 2016)