HSC-SSPを用いたz>6低光度クェーサー探査
尾上匡房 (総研大D3)
With the great helps of HSC-SSP collaboratorsfrom project #47 (SHELLQs) , #18, and #222

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✦

ContentsIntroduction- High redshift (z>6) quasar, z>6 quasar survey✦ S-Cam search of z~6 quasars(MO+ in prep., Kashikawa+15)- z~6 QLF and photon budget✦ HSC-Wide search of z>6 quasars(SHELLQs)- Initial Success (Matsuoka, MO+17, 16)✦ Status of NIR follow-up- MBH estimate of one z~6 quasar✦ SHELLQs view on JWST
2017/06/07 銀河進化研究会@大阪大学

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• Introduction

2017/06/07 銀河進化研究会@大阪大学

Why we care high-z (z>6) quasar ?

タイトルテキスト~ 6 - 20

✦ SMBH evolution/formation scenario~1000Big Bang

Recombination

z=0 (now)✦ IGM opacity during cosmic reionization

Redshift✦✦
IGM
opacity duringreionization
Co-evolution
withcosmic
host galaxy✦✦
SMBH
evolution/formation
scenario
Chemicalenrichment of broadline region✦ Co-evolution with host galaxy → Izumi-san’s talk✦ Chemical enrichment of broad line region

Unique probe of the early Universe !!
2016/10/25
初代星・初代銀河研究会2016@金沢
2017/06/07
銀河進化研究会@大阪大学

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Why we care high-z (z>6) quasar ?
z=7.1[CII] 158μm

Mortlock+11

Venemans+12✦ IGM opacity during cosmic reionization✦ SMBH evolution/formation scenario✦ Co-evolution with host galaxy → Izumi-san’s talk✦ Chemical enrichment of broad line region

Unique probe of the early Universe !!
2017/06/07 銀河進化研究会@大阪大学

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IGM OpacityGRBsLAEs∝(1+z)>10.9

τLyα,effτQuasars

Konno+17∝(1+z)4.3z

5.5Becker+14✦ Redshift evolution of IGM neutral fraction during EoR✦ Spatially patchy reionization process suggested

2017/06/07 銀河進化研究会@大阪大学

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Why we care high-z (z>6) quasar ?
[CII] 158μm

Mortlock+11

Venemans+12✦ IGM opacity during cosmic reionization✦ SMBH evolution/formation scenario✦ Co-evolution with host galaxy → Izumi-san’s talk✦ Chemical enrichment of broad line region

Unique probe of the early Universe !!
2017/06/07 銀河進化研究会@大阪大学

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MBH vs Lbol of Luminous z>6 Quasars
color plots: z>6 QSOs with MBH measurements

color plots: z>6 QSOs with MBH measurements(CFHQS:green, SDSS: blue and red, UKIDSS: purple)(CFHQS: green, SDSS: blue and red, UKIDSS: purple)

contour: low-z SDSS QSOs

contour: low-z SDSS QSOs

Willott+10a
Willott+10a
GeminiGemini(+VLT
VLT&&Gemini
GeminiFT)(+FT)
KeckKeck

Wu+15

Currently known z>6 quasars are powered by
the most massive and active BHs
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• S-Cam search of z~6 low-luminosity quasar(MO in prep., Kashikawa+15)

2017/06/07 銀河進化研究会@大阪大学

S-Cam Observation and Follow-up✦UKIDSS-DXS field (6.56 deg2), zR,3σ=24.15- 17 candidates (zR=23.6-24.1) from i-zB and zB-zR color selection
Subaru/FOCAS spectroscopy(11 candidates)

HSC-SSP photometry (Deep and Wide)
Brown Dwarfs

z=6.156, M1450=-23.10

Filled symbols:
remaining candidates
Quasarz=6.041, M1450=-22.58[OII] emitter

Possibly LAE (427 km s-1)

Kashikawa+15

Two (or one) quasars found. No additional quasars from Kashikawa+15.
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z~6 Quasar Luminosity Function
Nion [s-1Mpc-3]

0.5%

2QSOs
1QSO
2σ

1%

1σ

5%

10%

Faint-end slope

1-12% contribution to ionizing photons (95.4% confidence)-> Quasars are minor contributors of reionization
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Hyper Suprime-Cam Subaru Strategic
Program (HSC-SSP) Survey• HSC-Wide search of z~6 quasar(Matsuoka, MO, Kashikawa+16, 17)
2016/06/08 Sokendai Colloquium

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HSC survey
HSC-SSPSurvey
2016/06/08 Sokendai Colloquium

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2016/06/08 Sokendai Colloquium

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VIKING-N

2~500 deg
VIKING
500 overlapped
deg2 overlappedwith
with VIKING!

Subaru/HSC (5years, 300nights)

HSC-UD
HSC-UDDeep✦ Optical multi-band survey with

✦Optical multi-band survey with Subaru/HSC-Wide: 14002 deg2, rlim,5σ~26- Wide: 1400 deg , rlim,5σ~26- Deep: 272 deg2, rlim,5σ~27- Deep: 27 deg , r~27lim,5σ2, r2UD:
3.5deglim,5- U-Deep: 2 deg , r~28σ~28lim,5σ✦ Mostpowerful✦Most
powerful
opticalopticalsurveysurvey
before LSST

before LSST

2016/06/08
2017/06/07
Sokendai銀河進化研究会@大阪大学
Colloquium

HSC-deep
HSC-deep

LSST(wide)
LSST(wide)

HSC-wide
HSC-wide
CFHTLSCFHTLS

DES(wide)
DES(wide)
KiDS
KiDS
PS1(3π)PS1(3π)SDSSSDSS

Candidate Selectiongrizy✦Efficient selection is necessary(300@z~6, 50@z~7)-Based on quasar probability
using an Bayesian framework-Evidence of being quasar/browndwarfs is calculated from theobserved HSC colors withsurface density ρQ/D(m, z) as aprior✦Optical spectroscopy
Subaru/FOCAS

2017/06/07 銀河進化研究会@大阪大学

GTC/OSIRISInitial Discovery
HSC high-z quasar survey

Matsuoka+16, 17
30 new quasars at 5.9<z<6.9 from ~150 deg229 luminous(-23.5<Mfound<-22.0)
LBGs
at
5.7<z<6.1
33 quasars
at5.9<z<6.8
in~400deg
1350~3 indistinguishable objects similar to those found in our Scam study
2017/06/07
Matsuoka+
16 銀河進化研究会@大阪大学

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2017/06/07 銀河進化研究会@大阪大学

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Composite of 12 possible quasars

FWHMLyα ~300 km s-1

Type-II quasars? Galaxy & type-I composite?
2017/06/07 銀河進化研究会@大阪大学

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z vs M1450 distribution

Previoussearches

SubaruWe are exploring beyond the tip of iceberg!
2017/06/07 銀河進化研究会@大阪大学

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Follow-up Observation of SHELLQs

2017/06/07 銀河進化研究会@大阪大学

~60hrs in Gemini/GNIRS& VLT/X-Shooter (7 targets)-

BH mass, BLR metallicity,
IGM absorption, etc.

-

Data has been delivered
J2239+0207(zLyα=6.26, M1450=-24.69)✦-➡

zMgII=6.24, Δv=1513 km s-1
L3000=5.2e+41 erg s-1

2.0

Preliminary

Gemini/GNIRS(Texp=3.7hr, R~1700 @ K)

-zMgII=6.24, Δv=1513 km s-1-

Lbol=8.1×1045 erg s-1

2.1

MBH=6.5×107 Msun, Lbol/LEdd=0.94
2017/06/07 銀河進化研究会@大阪大学

2.2

2.3

λobs [μm]Preliminar y!

J2239+0207
Lbol [erg s-1]

✦Fλ [x 10-18 erg s-1 cm-2 A-1]

SHELLQs NIR follow-up

Again, J2239 accretes
with the Eddington-limit
MBH [Msun]

2.4

• SHELLQs view on JWST

2017/06/07 銀河進化研究会@大阪大学

Synergy with JWSTJWST/NIRSpec, R=1000

2016/06/08 Sokendai Colloquium

13/21

Current limit
for NIR follow-up

Our NIR follow-up is limited to bright sample
JWST enables MBH measurements of
the whole HSC sample down to ~107 Msun at z~6
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Summary✦ High redshift quasar is an important tracer of cosmicreionization✦ From our S-Cam project, we found quasars have onlymoderate (1-12%) contribution on the UV photon
during the reionization✦ SHELLQs project has been quite successful in the 1styear, discovering >30 QSOs in ~400deg2✦ From the first NIR follow-up, the target quasar isfound to be a ~108 Msun BH with Eddington
accretion✦ JWST will probe further down the BHMF at z>6
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• Additional Slides

2017/06/07 銀河進化研究会@大阪大学

Publishedz>6qsos
(Oct.
2016)
Published100z>6qsos(Oct.
2016)
J0100+2802(z=6.3, Wu+15)

SDSS

PS1
J1120+0168(z=7.1, Mortlock+11)

UKIDSS
CFHQS

VIKING

DES
optical NIR(z-band)

HSC

without
Now, we should go
deeperHSC& higher-z (z>7)

2016/10/25
初代星・初代銀河研究会2016@金沢
2017/06/07
銀河進化研究会@大阪大学

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Our New Quasars & Galaxy
LBG LFQLF

Lyα emitter with type-I
AGN contribution?
or type-II quasar?
2017/06/07 銀河進化研究会@大阪大学

Publishedz>6qsos(Oct.
2016)
Published
100z>6qsos(Oct.
2016)
J0100+2802(z=6.3, Wu+15)J1120+0168(z=7.1, Mortlock+11)

optical NIR(z-band)without HSC

without HSC

2016/10/25
初代星・初代銀河研究会2016@金沢
2017/06/07
銀河進化研究会@大阪大学

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Publishedz>6qsos(Oct.
2016)
Published
100z>6qsos(Oct.
2016)
J0100+2802(z=6.3, Wu+15)

SDSS
J1120+0168(z=7.1, Mortlock+11)

UKIDSS
CFHQS

optical NIR(z-band)without HSC

without HSC

2016/10/25
初代星・初代銀河研究会2016@金沢
2017/06/07
銀河進化研究会@大阪大学

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Publishedz>6qsos(Oct.
2016)
Published
100z>6qsos(Oct.
2016)
J0100+2802(z=6.3, Wu+15)

SDSS

PS1
J1120+0168(z=7.1, Mortlock+11)

UKIDSS
CFHQS

VIKING

DES
optical NIR(z-band)

HSC

withoutNow, we should go
deeperHSC& higher-z (z>7)

2016/10/25
初代星・初代銀河研究会2016@金沢
2017/06/07
銀河進化研究会@大阪大学

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Fainter QSO Search with HSC-Deep (Elias-N1)(Elais-N1)
Fainter QSO Search with HSC-Deep (Elias-N1)~1 mag deeper than HSC-Wide (ylim,5σ=25.3)✦ ~1 mag deeper than HSC-Wide (ylim,5σ=25.3=25.3)✦ HSC NBs & UKIRT NIR photometry are available!
✦ HSC NBs & UKIRT NIR photometry are available!
✦QuasarBrown
dwarfs

NBs
NBs

zphoto=5.93
zphoto=5.93
z=24.0,y=24.0, J=24.2 ABmag
z=24.0, y=24.0, J=24.2 ABmag

2016/10/25
初代星・初代銀河研究会2016@金沢
2017/06/07
銀河進化研究会@大阪大学
2016/10/25
初代星・初代銀河研究会2016@金沢

UKIRT
UKIRT

ainter QSO Search with HSC-Deep (Elias-N
Fainter QSO Search with HSC-Deep (Elais-N1)✦~1✦magdeeperthanHSC-Wide(ylim,5σ=25.3)~1 mag deeper than HSC-Wide (ylim,5σ=25.3✦

HSC& UKIRT
photometry
available!
✦ NBs
Faintest
z~6 quasar
ever?
HSC NBs& UKIRTNIR
NIR
photometry
areareavailable!
zphoto=5.93
zz=24.0,y=24.0, J=24.2 ABmag
photo=5.93

NBs

NBs

z=24.0, y=24.0, J=24.2 ABmag
UKIRT

UKIRT

HSC-Deep probes down the quasar LF to MUV~-21
First
follow-up
innextMar.
&Apr.
2017/02/01 Sokendai colloquium

Data Flow
HSC
(z/y detected, point source)
VIKING & UKIDSS

Initial Color Selection(no g,r detection,red color in i-z / z-y)Multi-color Selection
1. Bayesian (CORE)
2. SED-fitting (BONUS)

Discovery!
Junk Removal &Visual InspectionSpectroscopic Follow-up

No photometric follow-up!
2016/01/21 Galaxy Coffee @ MPIA

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Published 100 z>6 qsos (Oct. 2016)
J0100+2802(z=6.3, Wu+15)J1120+0168(z=7.1, Mortlock+11)

optical NIR(z-band)without HSC

2016/10/25
初代星・初代銀河研究会2016@金沢
2017/06/07
銀河進化研究会@大阪大学

12/21
4/19

Published 100 z>6 qsos (Oct. 2016)
J0100+2802(z=6.3, Wu+15)

SDSS

PS1
J1120+0168(z=7.1, Mortlock+11)

UKIDSS
CFHQS

VIKING

DES
optical NIR(z-band)

HSC

withoutNow, we should go
deeperHSC& higher-z (z>7)

2016/10/25
初代星・初代銀河研究会2016@金沢
2017/06/07
銀河進化研究会@大阪大学

12/21
5/19

2015/12/04 Group Meeting @ MPIA

HSC & VIKING photometryBest-fit QSO model
Best-fit stellar model

2015/12/04 Group Meeting @ MPIA• Additional Slides

2017/06/07 銀河進化研究会@大阪大学

Yoshiki Matsuoka (NAOJ)

Surprisingly...

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

Yoshiki Matsuoka (NAOJ)

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

80Known z ≥ 6 quasars

5Spectroscopy done

55

Quasars at z ≥ 631

Galaxies at z ~ 68

[O III] emitters at z ~ 0.8

2Brown dwarfs

8Moving/transient

6GOPIRA symposium (NAOJ, Mitaka; Sep 26-28, 2016)

2017/06/07 銀河進化研究会@大阪大学