松岡 良樹 (愛媛大学)

遠方クエーサー探査と宇宙再電離
愛媛大学/宇宙進化研究センター

松岡 良樹「銀河進化と遠方宇宙」2019 (Yokohama, Japan; Mar 11-13, 2019)

松岡 良樹 (愛媛大学)

遠くへ✶ z = 0.158 (1963年)✶ z = 7.54 (2017年)

Banados+17「銀河進化と遠方宇宙」2019 (Yokohama, Japan; Mar 11-13, 2019)Ⓒ Xiaohui Fan

松岡 良樹 (愛媛大学)

遠いクエーサーは、何を教えてくれるのか？

Formation of SMBHs✶ What were the seeds?
✶ When were they born?
✶ How did they grow?
Maximum MBH
M(t) = M0 e[λ(1-ε)/ε](t/0.45 Gyr)

Number density

Shen11

L/MBH/REdd functions

Richards+06「銀河進化と遠方宇宙」2019 (Yokohama, Japan; Mar 11-13, 2019)

Venemans+13

松岡 良樹 (愛媛大学)

遠いクエーサーは、何を教えてくれるのか？

Host galaxy evolution✶ Star formation history✶ Quasar feedback?
✶ Chemical enrichment
Stars and gas in the hosts

Venemans+16

Scaling relations

Wang+10「銀河進化と遠方宇宙」2019 (Yokohama, Japan; Mar 11-13, 2019)

Chemical evolution

De Rosa+14

松岡 良樹 (愛媛大学)

遠いクエーサーは、何を教えてくれるのか？

Cosmic Reionization✶ When and where?
✶ How did it proceed?
✶ Ionizing sources?

Fan+06「銀河進化と遠方宇宙」2019 (Yokohama, Japan; Mar 11-13, 2019)

松岡 良樹 (愛媛大学)✶ IGMにおけるLy α吸収

中性水素雲 (zabs)

光の経路 rνobs < ναν > ναν = να✓ 観測周波数νobs の光に対するIGM Ly α吸収の光学的深さは
水素 n = 2 → 1の崩壊率

原子のLy α吸収断面積

密度揺らぎ→ わずかな中性水素 (xHI ~ 10-4) によって、IGMはLy αに対して極めて不透明になる「銀河進化と遠方宇宙」2019 (Yokohama, Japan; Mar 11-13, 2019)

松岡 良樹 (愛媛大学)✶ “Lyman-α forest”

Songaila & Cowie (2010)→ 背景光源スペクトルに刻まれる
Lyman-α forestから、視線上のIGMの分布を調べられる「銀河進化と遠方宇宙」2019 (Yokohama, Japan; Mar 11-13, 2019)

松岡 良樹 (愛媛大学)✶ “Gunn-Peterson trough”「銀河進化と遠方宇宙」2019 (Yokohama, Japan; Mar 11-13, 2019)

Fan et al. (2006)

松岡 良樹 (愛媛大学)

IGMの中性度

Ly αに対する光学的深さ✶ “Gunn-Peterson trough”

Eilers et al. (2018)

赤方偏移
赤方偏移
「銀河進化と遠方宇宙」2019 (Yokohama, Japan; Mar 11-13, 2019)

Fan et al. (2006)

松岡 良樹 (愛媛大学)

遠いクエーサーは、何を教えてくれるのか？

IGM neutral fraction

galaxies?

quasars?

Planck2015
instantaneous(Robertson+15)「銀河進化と遠方宇宙」2019 (Yokohama, Japan; Mar 11-13, 2019)(Madau+15)

松岡 良樹 (愛媛大学)

Past/ongoing high-z quasar surveys

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 magPan-STARRS1 1.8m

DES 4mLuminosity function

Comparison 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, ...

「銀河進化と遠方宇宙」2019 (Yokohama, Japan; Mar 11-13, 2019)

松岡 良樹 (愛媛大学)

z > 6クエーサーの積算発見数

Pan-STARRS1,DES, HSC, …

HSC

Without
HSC「銀河進化と遠方宇宙」2019 (Yokohama, Japan; Mar 11-13, 2019)SHELLQs

Subaru High-z Exploration of Low-Luminosity Quasars

Members
Y. Matsuoka1 (PI)
M. Akiyama2, N. Asami3, S. Foucaud, T. Goto4, Y. Harikane5, H. Ikeda1, M. Imanishi1, K. Iwasawa6, T.
Izumi5, N. Kashikawa1 T. Kawaguchi7, S. Kikuta1, K. Kohno5, C.-H. Lee1, R. H. Lupton9, T. Minezaki5, T.
Morokuma5, T. Nagao8, M. Niida8, M. Oguri5, Y. Ono5, M. Onoue1, M. Ouchi5, P. Price9, H. Sameshima10,A. Schulze5, T. Shibuya5, H. Shirakata11, J. D. Silverman5, M. A. Strauss9, M. Tanaka1, J. Tang12, Y. Toba8
1NAOJ, 2Tohoku, 3JPSE, 4Tsinghua, 5Tokyo, 6Barcelona, 7Sapporo Medical, 8Ehime, 9Princeton, 10Kyoto Sangyo, 11Hokkaido,12ASIAA

松岡 良樹 (愛媛大学)

gri

HSC SSP survey「銀河進化と遠方宇宙」2019 (Yokohama, Japan; Mar 11-13, 2019)zy松岡 良樹 (愛媛大学)

Subaru Hyper Suprime-Cam SSP survey
Hyper Suprime-Cam (HSC)✶ 116 2K x 4K Hamamatsu FD CCDs
(104 CCDs for science exposures)✶ Circular FoV of 1°.5 diameter✶ Miyazaki et al. (2018)
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「銀河進化と遠方宇宙」2019 (Yokohama, Japan; Mar 11-13, 2019)

松岡 良樹 (愛媛大学)“Needle in a haystack”「銀河進化と遠方宇宙」2019 (Yokohama, Japan; Mar 11-13, 2019)

松岡 良樹 (愛媛大学)

Survey strategy
1. Look for red point sources in the HSC catalog(+ UKIDSS/VIKING catalog)griz(2. Follow-up photometry)y

3. Follow-up spectroscopy

4. Discovery「銀河進化と遠方宇宙」2019 (Yokohama, Japan; Mar 11-13, 2019)

松岡 良樹 (愛媛大学)

Bayesian probabilistic selection
Prioritization of the candidates with the probabilistic approach:
PQ = the Bayesian probability of being a high-z quasar rather than a Galactic brown dwarf= WQ/(WQ+WD) where WQ/D is the weighted evidence of being a quasar/dwarf.

observed magnitudes
the fact of detection(model) magnitude and redshift

WQ (m, det) = ∫ ∫ ρQ(mint, z) Pr(det | mint, z) Pr(m | mint, z) dmint dz(1) Quasar LF and its
evolution (Willott+10)
0 if mint > mlimit
1 if mint < mlimit(2) Mean quasar colors from ~340 SDSS quasars
at z~3 with the Songaila (2004) IGM opacity(3) multi-D Gaussian error function with σ = merr

WD (m, det) = ∫ ∫ ρD(mint, tsp) Pr(det | mint, tsp) Pr(m | mint, tsp) dmint dtsp
(4) Galactic brown-dwarf
distribution model (Caballero+08)(5) SpeX and CGS4
spectral library「銀河進化と遠方宇宙」2019 (Yokohama, Japan; Mar 11-13, 2019)

松岡 良樹 (愛媛大学)

Bayesian probabilistic selection
Quasar probability: PQ = WQ/(WQ+WD)
WQ (m, det) = ∫ ∫ ρQ (mint, z) Pr (det | mint, z) Pr (m | mint, z) dmint dz
WD (m, det) = ∫ ∫ ρD (mint, tsp) Pr (det | mint, tsp) Pr (m | mint, tsp) dmint dtsp
observed magnitudes
in HSC + NIR bands
grsource detectionizy→ Spectroscopic follow-up of all the photometric candidates with PQ > 0.1「銀河進化と遠方宇宙」2019 (Yokohama, Japan; Mar 11-13, 2019)

松岡 良樹 (愛媛大学)

Brief summary of the SHELLQs progress✶ HSC-SSP survey: the latest, S18A data release contains ~1 billion objects over~900 deg2 (>1 exposures in i, z, and y) in the Wide fields.
✶ Candidate selection: ~300 candidates with (zAB < 24.5 or yAB < 24.0) & PQ > 0.1.
✶ Spectroscopic follow-up is underway, with Subaru, Gemini, and GTC. In particular,
we were allocated 60 Subaru nights in total, including two “intensive program”s.

✶ We have identified 163 candidates so far, which include 83 high-z quasars, 25 high-z
galaxies, 6 [O III] emitters at z~0.8, and 53 brown dwarfs.
✶ A series of publications:- Paper I (Matsuoka+16): initial discovery of 9 quasars- Paper II (Matsuoka+18a): more discovery of 24 quasars- Paper III (Izumi+18): ALMA follow-up- Paper IV (Matsuoka+18b): more discovery of 31 quasars- Paper V (Matsuoka+18c): quasar luminosity function at z = 6- Paper VI (Onoue+, in prep.): black-hole mass measurements- Paper VII (Matsuoka+19): discovery of a z = 7.07 quasar「銀河進化と遠方宇宙」2019 (Yokohama, Japan; Mar 11-13, 2019)

松岡 良樹 (愛媛大学)

発見された遠方クエーサー群

新発見83

再発見17

「銀河進化と遠方宇宙」2019 (Yokohama, Japan; Mar 11-13, 2019)

松岡 良樹 (愛媛大学)

発見天体の例J1429-0104 (z = 6.8)

J1205-0000 (z = 6.75)

J0921+0007 (z = 6.56)

J1545+4232 (z = 6.50)

J1004+0239 (z = 6.41)「銀河進化と遠方宇宙」2019 (Yokohama, Japan; Mar 11-13, 2019)

松岡 良樹 (愛媛大学)

Highlight (1/5):
Sample statistics「銀河進化と遠方宇宙」2019 (Yokohama, Japan; Mar 11-13, 2019)

松岡 良樹 (愛媛大学)

SHELLQs in a Nutshell

これまでの発見天体

最遠記録

z=7

次点の記録

z=6

ブラックホール
質量の近似値（比 太陽）

10億倍

1億倍

今回の発見天体

1000万倍「銀河進化と遠方宇宙」2019 (Yokohama, Japan; Mar 11-13, 2019)

松岡 良樹 (愛媛大学)

Highlight (2/5) : the first low-L quasar at z > 7✶ HSC images (g, r, i, z, y)✶ Subaru/FOCAS spectroscopy on April 24, 2018

✶ Gemini/GNIRS spectroscopy on June 25 - July 29, 2018

「銀河進化と遠方宇宙」2019 (Yokohama, Japan; Mar 11-13, 2019)

松岡 良樹 (愛媛大学)

Highlight (2/5) : the first low-L quasar at z > 7

日本天文学会2019年春季年会 (Koganei, Japan; Mar 14-17, 2019)

松岡 良樹 (愛媛大学)

Highlight (3/5): Luminosity function at z = 6✶ Bright-end slope
β = −2.73 ± 0.27
✓ Consistent with thepast (SDSS, CFHQS)
measurements.

✶ Faint-end slope
α = −1.23 ± 0.39
✓ Determined for thefirst time.
✓ Rather flat.
✶ Break magnitude
M1450* = −24.9 ± 0.9✓ The existence confirmedfor the first time.
✶ Characteristic densityΦ* = 9.1+10.8-6.2 (Gpc-3 mag-1)「銀河進化と遠方宇宙」2019 (Yokohama, Japan; Mar 11-13, 2019)

松岡 良樹 (愛媛大学)

Highlight (3/5): Luminosity function at z = 6✶ Comparison with other measurements✶ LF evolution over 4 ≤ z ≤ 6→ Similar overall shape→ Strong decline in the number densities→ Galaxies outnumber at M1450 > −23 mag→ contradicts with the previous claim of“numerous faint AGNs dominating cosmicreionization”「銀河進化と遠方宇宙」2019 (Yokohama, Japan; Mar 11-13, 2019)

松岡 良樹 (愛媛大学)

Highlight (4/5): Contribution to reionization

Critical rate to keepthe IGM fully ionized→ Integrating the luminosity function over-18 < M1450 < -30 mag gives the ionizing
photon density:.

nion = 1048.9±0.2 (s-1 Mpc-3)→ <10 % of the density necessary tokeep the IGM fully ionized→ Quasars alone cannot reionize theUniverse. They contribute <10 % of thephotons necessary to keep the IGM fullyionized.

「銀河進化と遠方宇宙」2019 (Yokohama, Japan; Mar 11-13, 2019)

松岡 良樹 (愛媛大学)

Highlight (5/5): diﬀerent classes of objects

7500

8500

9500(Angstrom)← composite spectrumof 12 similar objects✶ We classify these objects
as “possible quasars”,given their bright Lyα
and NV mini-BAL (?) inthe composite spectrum.
「銀河進化と遠方宇宙」2019 (Yokohama, Japan; Mar 11-13, 2019)

松岡 良樹 (愛媛大学)

Highlight (5/5): diﬀerent classes of objects

7500

8500

9500

(Angstrom)← composite spectrumof 14 high-z galaxies「銀河進化と遠方宇宙」2019 (Yokohama, Japan; Mar 11-13, 2019)

松岡 良樹 (愛媛大学)

Highlight (5/5): diﬀerent classes of objects

7500

7500

8500

8500
「銀河進化と遠方宇宙」2019 (Yokohama, Japan; Mar 11-13, 2019)

9500

9500

(Angstrom)(Angstrom)松岡 良樹 (愛媛大学)

Multi-wavelength follow-up (1/2): near-IR✶ Luminosity function = BH mass function x Eddington ratio function

Bongiorno+16→ BH mass measurements with Mg II λ2800 line in near-IR (Onoue+, in prep)… 9 objects observed so far with Subaru/MOIRCS, VLT/X-Shooter, Gemini/GNIRS「銀河進化と遠方宇宙」2019 (Yokohama, Japan; Mar 11-13, 2019)

松岡 良樹 (愛媛大学)

Multi-wavelength follow-up (2/2): ALMA
✶ 7 quasars observed in Cycles 4 & 5 (Band 6)

Izumi+18; Izumi+ in prep
「銀河進化と遠方宇宙」2019 (Yokohama, Japan; Mar 11-13, 2019)

松岡 良樹 (愛媛大学)

To the farthest reaches of the Universe (future prospects)?
30 nights with Subaru/FOCAS
through 2021A「銀河進化と遠方宇宙」2019 (Yokohama, Japan; Mar 11-13, 2019)

松岡 良樹 (愛媛大学)

To the farthest reaches of the Universe (future prospects)✶ TAOⒸ Xiaohui Fan✶ WFIRST「銀河進化と遠方宇宙」2019 (Yokohama, Japan; Mar 11-13, 2019)

松岡 良樹 (愛媛大学)✶ Lyman-α 遷移によるIGM観測の限界(1) わずかな中性水素があるだけで、IGMは非常に不透明になる→ 再電離の完了に近い時期より昔を見ることができない(2) 宇宙初期には極めて稀な、明るい紫外線背景光源が必要(3) 再電離前のIGMは低温であり、熱衝突によってLyman-α励起を起こせないことから、（たとえ(1)の問題がなくても）再電離期前の観測には使えない
水素21cm輝線とSKA(c) SPDO/TDP/DRAO/Swinburne Astronomy Productions「銀河進化と遠方宇宙」2019 (Yokohama, Japan; Mar 11-13, 2019)