High Redshift Quasar Survey
description
Transcript of High Redshift Quasar Survey
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.