infrared medium-deep survey myungshin im 1, soojong pak 2, won-kee park 1,3, ji hoon kim 1, jae-woo...

Infrared Medium-deep Survey

Myungshin Im1, Soojong Pak2, Won-Kee Park1,3, Ji Hoon Kim1, Jae-Woo Kim1, Seong-Kook J. Lee1, Marios Karouzos1, Yiseul Jeon1, Changsu Choi1, Hyunsung Jun1, Dohyeong Kim1, Jueun Hong1, Duho Kim1, Minhee Hyun1, Yongmin Yoon1, Yoon Chan Taak1, Yongjung Kim1, Giseon Baek2, Hyeonju Jeong2, Juhee Lim2, Eunbin Kim2, Nahyun Choi2, Hye-In Lee2, K. M. Bae2, &

Seunghyuk Chang4 & IMS Team1CEOU/Astronomy Program, Dept. of Physics & Astronomy, Seoul National University, Seoul

151-742, KOREA, 2School of Space Research, Kyung Hee University, Suwon 446-741, KOREA, 3Korea Astronomy and Space Science Institute, Daejeon 305-348, KOREA, 4Samsung

Electronics, Suwon, Gyeonggi-do 443-370, KOREA

2014. 11. 03 - 11. 07 The 6th KIAS Workshop

Infrared Medium-deep Survey

• Imaging survey at J < 23 AB mag, 120 deg2 of 7 fields (additional Y-band data for a limited area)

• Follow-up NIR imaging of high redshift objects selected from 2000+ deg2

• Imaging observations with UKIRT, McDonald 2.1m, since 2010

• Follow-up spectroscopy with Magellan and 4-m class telescopes

• ~30 members from SNU, KHU, KASI, KNU, ASIAA, NCU, Subaru, JPL, …


McDonald 2.1-m with CQUEAN(grizY, is/iz)

UKIRT 3.9-m (zYJHK)

Key Scientific QuestionsSupermassive Black Holes

(109 – 1010 M⊙) at z < 7(Fan et al. 2005; Mortlock et al.

2011)

When and how did they emerge?

Re-ionization State of IGM?

Quasars at 5 < z < 7.5

Massive clusters at z > 1!(Foley et al. 2011 + many)

How did galaxies evolve?LCDM universe OK?

Halo mass/galaxy relation?

Massive clusters at z > 1

First stars at z ~ 11.5?(Planck results +)

Death of massive stars?

GRBs and SNe


High Redshift Objects Are Red

QSO at z=7

Galaxy at z=2

Brown dwarf

NIR imaging is

essential


Survey Design : How Many, How Deep?

1 .How faint?

2. How many?

3. What wavelength?

0.01 to 1 per 1 sq. degree

23 AB 등급

0.9 – 1 μm or longer: J or Y-band

Quasars and galaxy clusters at high redshift

Im et al. (2002)2014. 11. 03 - 11. 07 The 6th KIAS Workshop

QSO LF(Willott et al. 2010)

~L3

IMS Fields: Total ~ 120 deg2

Field RA Dec Area

(deg2)

Optical Coverage (mag/deg2) NIR Coverage IR coverage

XMM-LSS 02:21:20 -04:30 5 CFHTLS-W1 (35 MegaPipe z-fields, z ~ 25AB/72deg2), NOAO DWS, Maidanak Y-band

UKIDSS DXS+UDS (2.6/8.75)

SWIRE (9.2)

CFHTLS-W2 08:54 -04:15 49 CFHLTLS-W2 (19 MegaPipe z-fields, z~25AB/49 deg2), COSMOS HST (1.8 deg2)

No NIR yet

Lockman Hole

10:45:00 58:00 15 CFHT MegaPipe Archive (15 fields), Subaru (~18 fields, I = 26 AB, B=27AB)

UKIDSS DXS (1/8.75)

SWIRE (11)

EGS 14:17 54:30 49 CFHTLS-W3 (44 MegaPipe z-fields, z~25ABmag/49 deg2)

No NIR yet IRAC GTO data, AKARI 15 micron

ELAIS-N1 16:11:00 55:00 9 CFHT MegaPipe (9 fields, z~25AB mag)

Subaru Deep I (18 fields (5 deg2)


SWIRE (9.2)

ELAIS-N2 16:36:48 41:01:45

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

No NIR yet SWIRE(4.8)

SA22 22:17 00:20 16 CFHLTLS-W4 (20 MegaPipe z-fields, z~25AB/16 deg2


None


Science Highlights

• High redshift quasars

• High redshift galaxy clusters/galaxies

• Transient objects (GRBs, TDE, SNe, etc)


SMBH Mass Evolution

AKARI points(Jun, H., MI, 2014 submitted)

z ~ 5.5 z > 6.5

?

Fast growth fromstellar mass BHs

Slow growth withheavy BH seeds


• 1010 M⊙ at z ~ 5 (1.2 Gyr), and a few x 109 M⊙ at z ~ 6.4 (0.95 Gyr)• Emergence of SMBHs [Lbol/LEdd ~ 1 high accretion rate; Hot dust-poor (e.g., Jun & Im 2013)]

• What was happening at z ~ 5.5 and z > 7 (only one z=7 QSO so far)?• Bias for high accretion rate objects?

Faint quasars at z > ~6

• SMBHs with low accretion?

• Budget of IGM ionizing photon


Willott et al. (2010)

z~5.5 Quasars

Identification of z ~ 5.5 QSOs is difficult with SDSS filters


Chiu et al. 2005

High Redshift Quasar Selection @z=5.5 and z=6.5With Special Filters


CQUEAN, Camera for QUasars in EArly

uNiverse

• Kyungheee Univ.(S. Pak)/SNU

• NIR sensitive (~1 micron)

• Custom is and iz filters - tailored for high-z QSO selection

• Focal Reducer (3x, 5’ x 5’)

• Auto-guiding system

• Installed on the 2.1m at McDonald Observatory

• ~30 nights/year for high redshift quasar survey


Park, Pak, MI et al. (2012)

Quasars at 5 < z < 5.5


Park, Pak, MI, et al. (2012)Jeon et al. 2014, in prep.

Spectroscopic confirmation of QSOs at z ~ 5.5 and z ~ 6

Lyα

z = 5.3 z = 5.0

z = 6.0 Spectroscopic identification of 8 QSOs at z = 5 – 6 (all with 3-4m class telescopes)

More spectroscopy to come (BH mass, IGM study)


Jeon, Y., MI, et al. 2014, in prep.

Faint Quasar Candidates at z ~ 6


9 candidates z(AB) ~ 22.5 magfrom 90 deg2

g r i z Y J

Selection of Quasars at z ~ 7

• Y,J-band coverage + I,z data

Quasar at z ~ 7

Brown dwarf


Evolution of Quasars at z > 7?

• Several candidates Rapid evolution of quasars at z > 7


High Redshift Clusters

• > 100s clusters at z < 1: Good agreement with CDM universe

• Clusters at z > 1 (Overzier et al. 2008, Kang & Im 2009; Matsuda et al. 2011; Capak et al. 2011,…; 1 < z < 5.3)

• Some find very massive clusters at z ~ 1.5 trouble with CDM universe?


http://www.spitzer.caltech.edu/uploaded_files/graphics/fullscreen_graphics/0006/5426/ssc2011-02a_Sm.jpg

High Redshift Clusters and Galaxy Evolution

• Reversal of SFR-density relation: Difficult to explain with models, controversial, what is the origin?

• IMS: Large number of galaxies and clusters (120 deg2 vs. ~1 deg2)


Reversal (Elbaz et al. 2007) No reversal (Ziparo et al. 2014) versus

Hig

h S

F

High density

z=0

z=1

z=1

Search for High Redshift Clusters


3.6 – 4.5 micron

z -

J

Multi-wavelength data Photometric redshift or color-color diagram

Redshift bin Identify over-dense area


Cluster at z=1.1

1000 candidates identified

For galaxies at z =1,

Difference in galaxy properties are due to mass, not environmentNo reversal in SFR-density relation for massive galaxies

SFR quenching due to environ. at z < 1 (reversal in SFR-density rel).


SDSS (z=0) IMS (z=1)

Jae-Woo Kim, MI, et al. 2014

Fraction of Quiescent GalaxyAt z > 1.4, mass dependent (not environment)

At z < 1.4, environment becomes important


log (M*/M⊙) ≥ 9.1 log (M*/M⊙) ≥ 10.0

Passiv

e

fracti

on

(N

passiv

e/N

tota

l)Seong-Kook Lee, MI, et al. 2014

Red: ClusterBlue: Field

GRB, Transients

Tidal disruption event: Swift J1644+57(Burrows et al. 2011, Nature)

Long-term (2+ years) monitoring results(Yoon et al. 2014; Im et al. 2014)

Christmas Burst, GRB 101225A(Thone et al. 2011, Nature)

CQUEAN riz data helpsdetermine the black body radiatoin afterglow


Swift J1644+57Long-term Light Curve

Before host subtraction∝ t-0.4

After host subtraction∝ t-1.1

( c.f. TD ∝ t-5/3 )


Swift J1644+57Host Galaxy + BH Mass

• Log(MBH/M⊙) ~ 6.8 ± 0.5

χ2=1.318

Yongmin Yoon, MI, et al. 2014, in prep.


Summary• Infrared Medium-deep Survey

- 120 deg2 imaging in J and Y (23 AB mag)

- CQUEAN imaging of high redshift objects

- Transient follow-up

• 8 quasars at z=5.5 – 6.0 • 1000+ of z > 1 cluster candidates: environment vs

internal mechanism• GRBs/TDE/SNe


infrared medium-deep survey myungshin im 1, soojong pak 2, won-kee park 1,3, ji hoon kim 1, jae-woo...

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