High Redshift Quasar Survey

Survey Science Group Workshop, 2013 High1 Resort

Yiseul Jeon, Myungshin Im, W.-K. Park, J. H. Kim, M. Karouzos, J.-W. Kim, S.-K. Lee, H. Jun, C. Choi,

D. Kim, D. Kim, J. Hong, M. Hyun, and Y. C. Taak

Center for the Exploration of the Origin of the Universe (CEOU), Astronomy Program, Dept. of Physics & Astronomy, Seoul National University

Contents

I. Introduction History of our Universe High Redshift Quasars

II. Method of Study Multi-wavelength Data Color Selection Current Status

III. Summary

I. Introduction

Neutral HydrogenRecombination

First Star/First Galaxy/First SMBHz ~ 20

Reionization z ~ 10

Robertson et al. 2010

BB Dark Age Reionization Galaxy Formation

Galaxy Formation

History of our Universe

Quasar - An energetic active galactic nucleus- Powered by an accretion disc

High Redshift Quasar- One of the brightest objects- Useful for investigating the early universe - >50 quasars at z>5 discovered

High Redshift Quasars

• Intrinsic Properties of early SMBHsMass Growth of SMBHs & Evolution of QLF

• Environmental Effect due to QuasarsReionization of IGM

Artist's impression of quasar GB1508+5714 (z=4.3)

1. Growth of Super Massive Black Holes

1. Growth of Super Massive Black Holes

1) SMBH at z~7SMBH of 109M⊙ already exists age ~0.8 Gyr

1. Growth of Super Massive Black Holes

1) SMBH at z~7 First SMBH already exists age < 1 Gyr→ must have formed at very early time.2) Redshift Desert at 5<z<6 Due to limitations of current selection technique

109M⊙ z~6 1010M⊙ z~5

Chiu et al. 2005

r-i

i-z

←z=5.5

←z=5.2

x10 increase during 0.5Gyr

1. Growth of Super Massive Black Holes

1) SMBH at z~7 First SMBH already exists age < 1 Gyr→ must have formed at very early2) Redshift Desert at 5<z<6 Due to limitations of current selectionCause of SMBH Growth unknown More samples required

Robertson et al. 2010

IGM attenuation (Madau 1996) ↓

2. Reionization of Intergalactic MediumBB Dark Age Reionization Galaxy Formation

2. Reionization of Intergalactic Medium

Gunn-Peterson trough

Fan et al. 2006

Robertson et al. 2010

z=6.13

z=5.93

z=5.83

Fan et al. 2006

Robertson et al. 2010

Willott et al. 2010

◇ SDSS main△ SDSS deep stripe● CFHQS

Quasar Luminosity Function at z~6

At z>10: First stars(e.g., Kashlinsky et al. 2005)

At z~6: Star Forming Galaxy vs. Quasar

At z<2.5: mostly by AGNs

(e.g., Haardt & Madau 1996)

?

3. Evolution of Quasar Luminosity Function

→ New technique with New Deep/Wide survey data

Limitations of Previous Studies Redshift Desert at 5<z<6 and Discovery of z~7 Quasar New selection technique Various Luminosity Range Deep Survey Data Larger Sample Size Wide Survey Data

Redshift Redshift M1450

SMBH Mass Growth HI Fraction in IGM QLF at z~6

II. Method of Study

Quasar candidate selection

i z Y J H K 3.6 4.5

e.g.) z~7 quasar (blue)i)z Drop-outii)Bluer Y-J than Brown Dwarf(green)iii)Power-law SED

+ QuasarsΔ Model Brown Dwarfs+ Star-forming galaxy + Passive Evolving Galaxy

Quasar candidate selection1. Match multi-wavelength catalogues2. Select quasar candidates using color-color

diagram3. Remove spurious objects by eyeball rejection4. Do photometry on original images5. Imaging follow-up 6. Spectroscopy of remaining candidates

Quasar candidate selection

Optical NIR IR

- SDSS - CFHTLS-Wide(a) - CQUEAN Is & Iz(b)

- UKIDSS LAS & DXS(c) - IMS(b)

- Spitzer Space Telescope Ch 1 & Ch 2

(a) 3 mag deeper than SDSS z-band(b) available only for CEOU(c) only accessible to UKIDSS collaboration

- Multi-wavelength catalogues

On-going High-z Quasar Survey of CEOU

Redshift

5—6 6 6 6 ~7

DataSDSS

UKIDSS LASCQUEAN Is & Iz

SDSSUKIDSS LAS

SEGUEBOAO JUKIRT J

CFHT MegaPipeIMS(UKIRT J/Y)UKIDSS DXS

SWIRE

FieldSDSS DR7

UKIDSS LAS DR7 SEGUE 2

ELAIS-N1, ELAIS-N2, Lockman Hole, EGS,

COSMOS, VIMOS

Area [deg2]

~4000 ~1000 ~130

Depth [AB]

z < 19.5 J < 19.2 zerr < 0.1 Jerr < 0.15 J < 22.5

Quasar Selection at 5<z<6

Redshift

5—6 6 6 6 ~7

Data

SDSSUKIDSS LAS

CQUEAN Is & Iz

SDSSUKIDSS LAS

SEGUEBOAO JUKIRT J

CFHT MegaPipeIMS(UKIRT J/Y)UKIDSS DXS

SWIRE

FieldSDSS DR7

UKIDSS LAS DR7 SEGUE 2

ELAIS-N1, ELAIS-N2, Lockman Hole, EGS,

COSMOS, VIMOS

Area [deg2]

~4000 ~1000 ~130

Depth [AB]

z < 19.5 J < 19.2 zerr < 0.1 Jerr < 0.15 J < 22.5

Redshift gap at 5<z<6:due to the limitations of current filter system

Quasar Selection at 5<z<6• Camera for QUasars in EArly uNiverse (CQUEAN)

with custom designed Is and Iz filters at McDonald 2.1m

<McDonald 2.1m>

←CQUEAN

• Spectroscopic Follow-up Observation 2.5 nights at KP-4m (2012B) 3 nights at KP-4m (2013A) 3 nights at NTT (2013A)

Quasar Selection at 5<z<6• 2.5 nights at KPNO 4-m telescope

<KPNO 4-m Jan. 2013 >

Quasar Selection at z~7

Redshift

5—6 6 6 6 ~7

DataSDSS

UKIDSS LASCQUEAN Is & Iz

SDSSUKIDSS LAS

SEGUEBOAO JUKIRT J

CFHT MegaPipeIMS (UKIRT J/Y)

UKIDSS DXSSWIRE

FieldSDSS DR7

UKIDSS LAS DR7 SEGUE 2

ELAIS-N1, ELAIS-N2, Lockman Hole, EGS,

COSMOS, VIMOS

Area [deg2]

~4000 ~1000 ~130

Depth [AB]

z < 19.5 J < 19.2 zerr < 0.1 Jerr < 0.15 J < 22.5

Mauna Kea @May 2009

Quasar Selection at z~7 The most distant known quasar at z=7.085 (Mortlock

et al. 2011)

Ongoing & Future Optical/Near-IR SurveysWillott et al. 2010

Intermediate-wide medium-deep survey is needed.UKIRT NIR Survey !

IMS FieldsField RA Dec

Area(deg2

)

Optical Coverage (mag/deg2)

NIR IR

XMM-LSS02:21:20

-04:30 11

CFHTLS-W1 (35 MegaPipe z-fields, z ~ 25AB/72deg2,i-band for many fields), NOAO DWS, Maidanak Y-band

UKIDSS DXS+UDS (3.75, JK)IMS (7.5, J)

SWIRE

CFHTLS-W2 08:54 -04:15 27CFHLTLS-W2 (19 MegaPipe z-fields, z~25AB/49 deg2)

IMS (27, YJ)

Lockman Hole

10:45:00

58:00 12

CFHT MegaPipe Archive (15 fields, i-data in limited area), Subaru (~18 fields, I = 26 AB, B=27AB)

UKIDSS DXS (6.75, JK)IMS (5.25, J)

SWIRE

EGS 14:17 54:30 38

CFHTLS-W3 (44 MegaPipe z-fields, z~25ABmag/49 deg2, i-band data too)

IMS (38.25, YJ)

ELAIS-N116:11:00

55:00 14

CFHT MegaPipe (9 fields, z~25AB mag)Subaru Deep I (18 fields (5 deg2)

UKIDSS DXS+UDS (9, JK)IMS (4.5, J)

SWIRE

ELAIS-N216:36:48

41:01:45

5CFHT MegaPipe (6 fields, z~25 AB mag), Subaru Deep I (18 fields (5 deg2)

IMS (5.25, J) SWIRE

VIMOS 22:17 00:20 25

CFHLTLS-W4 (20 MegaPipe z-fields, z~25AB/16 deg2, i-band data available too

UKIDSS DXS+UDS (9, JHK)IMS (15.75, YJ)

Quasar Selection at z~6

Redshift

5—6 6 6 6 ~7

DataSDSS

UKIDSS LASCQUEAN Is & Iz

SDSSUKIDSS LAS

SEGUEBOAO JUKIRT J

CFHT MegaPipeIMS(UKIRT J/Y)UKIDSS DXS

SWIRE

FieldSDSS DR7

UKIDSS LAS DR7 SEGUE 2

ELAIS-N1, ELAIS-N2, Lockman Hole, EGS,

COSMOS, VIMOS

Area [deg2]

~4000 ~1000 ~130

Depth [AB]

z < 19.5 J < 19.2 zerr < 0.1 Jerr < 0.15 J < 22.5

NIR spectrum by IRTF, SpeX

Redshift 5—6 6 6 6 ~7

DataSDSS

UKIDSS LASCQUEAN Is&Iz

SDSSUKIDSS LAS

SEGUEBOAO JUKIRT J

CFHT MegapipeUKIRT J

UKIDSS DXSSWIRE

FieldSDSS DR7

UKIDSS LAS DR7 SEGUE 2

ELAIS-N1, ELAIS-N2, Lockman Hole, EGS,

COSMOS, VIMOS

Area [deg2]

~2000 ~1000 ~40/200

Depth [AB]

z < 19.5 J < 19.2 zerr < 0.1 Jerr < 0.15 J < 22.5Color-Color Diagram

(1) From SEGUE data confirmed by HET and follow-up NIR spec. at IRTF (2) From UKIDSS LAS dataconfirmed by Magellan

Quasar Selection at z~6

Quasar candidate selection

Confirm as Quasar! Calculate redshift by identifying redshifted Lyman break and UV emission

lines Measure SMBH mass using UV emission lines such as CIV λ1549 Investigate Lyman alpha forest to understand the ionization state of IGM

- Spectroscopy of candidates

III. Summary

III. Summary

• Limitations of Previous High-z Quasar Survey 1. Growth of SMBH2. Reionization of IGM3. Evolution of quasar LF

• Deep/Wide Survey Data with New selection technique –SMBH evolution–IGM ionization process

• CQUEAN/UKIRT

• Thank you

On-going High-z Quasar Survey of CEOU

Redshift

5—6 6 6 6 ~7

DataSDSS

UKIDSS LASCQUEAN Is & Iz

SDSSUKIDSS LAS

SEGUEBOAO JUKIRT J

CFHT MegaPipeIMS(UKIRT J/Y)UKIDSS DXS

SWIRE

FieldSDSS DR7

UKIDSS LAS DR7 SEGUE 2

ELAIS-N1, ELAIS-N2, Lockman Hole, EGS,

COSMOS, VIMOS

Area [deg2]

~4000 ~1000 ~200

Depth [AB]

z < 19.5 J < 19.2 zerr < 0.1 Jerr < 0.15 J < 22.5

Published <5 24 17 1

Prediction*

(increasing)

~40 (x10)

<10100—102

(x50)100—101

(x10)*assuming continuous density evolution of the high-z quasar LF (Willott+10)

Redshift

SMBH Mass Growth

Redshift

5—6 6 6 6 ~7

Published <5 24 17 1

Prediction ~40 <10 100—102 100—101

< First SMBH >

①Accretion from Seed BH If BH mass increases by accretion with Eddington rate,

where tEdd = 0.45 Gyr and ε is the radiative effiency

From seed mass of 102M⊙, it takes 0.9 Gyr. And From 105M⊙, 0.5 Gyr. (Volonteri10)

Not enough for 109M⊙ at z~7

②By Galaxy Merger Possible from SAM in ΛCDM (Li+07)

< Vigorous growth at 5<z<6 > Existence of the most massive SMBH

Redshift Redshift

SMBH Mass Growth HI Fraction in IGM

Redshift

5—6 6 6 6 ~7

Published <5 24 17 1

Prediction ~40 <10 100—102 100—101

Abrupt transition?

(Fan+06)

Continuous process?

(Becker+07)

Redshift Redshift M1450

SMBH Mass Growth HI Fraction in IGM QLF at z~6

Redshift

5—6 6 6 6 ~7

Published <5 24 17 1

Prediction ~40 <10 100—102 100—101

Also, QLF of 5<z<6 and z~7

→ Our research will contribute towards the understanding of the evolution of SMBHs and the IGM ionization state at the early Universe.