Infrared Medium-deep Survey Myungshin Im 1, Soojong Pak 2, Won-Kee Park 1,3, Ji Hoon Kim 1, Jae-Woo Kim 1, Seong-Kook J. Lee 1, Marios Karouzos 1, Yiseul Jeon 1, Changsu Choi 1, Hyunsung Jun 1, Dohyeong Kim 1, Jueun Hong 1, Duho Kim 1, Minhee Hyun 1, Yongmin Yoon 1, Yoon Chan Taak 1, Yongjung Kim 1, Giseon Baek 2, Hyeonju Jeong 2, Juhee Lim 2, Eunbin Kim 2, Nahyun Choi 2, Hye-In Lee 2, K. M. Bae 2, & Seunghyuk Chang 4 & IMS Team 1 CEOU/Astronomy Program, Dept. of Physics & Astronomy, Seoul National University, Seoul , KOREA, 2 School of Space Research, Kyung Hee University, Suwon , KOREA, 3 Korea Astronomy and Space Science Institute, Daejeon , KOREA, 4 Samsung Electronics, Suwon, Gyeonggi-do , KOREA The 6th KIAS Workshop

Infrared Medium-deep Survey Imaging survey at J < 23 AB mag, 120 deg 2 of 7 fields (additional Y-band data for a limited area) Follow-up NIR imaging of high redshift objects selected from deg 2 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, … The 6th KIAS Workshop McDonald 2.1-m with CQUEAN (grizY, is/iz) UKIRT 3.9-m (zYJHK)

Key Scientific Questions Supermassive Black Holes (10 9 – 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 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 The 6th KIAS Workshop

High Redshift Objects Are Red QSO at z=7 Galaxy at z=2 Brown dwarf NIR imaging is essential The 6th KIAS Workshop

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) The 6th KIAS Workshop QSO LF (Willott et al. 2010) ~L 3

IMS Fields: Total ~ 120 deg 2 FieldRADecArea (deg 2 ) Optical Coverage (mag/deg 2 )NIR CoverageIR coverage XMM-LSS02:21:20-04:305CFHTLS-W1 (35 MegaPipe z- fields, z ~ 25AB/72deg 2 ), NOAO DWS, Maidanak Y-band UKIDSS DXS+UDS (2.6/8.75) SWIRE (9.2) CFHTLS-W208:54-04:1549CFHLTLS-W2 (19 MegaPipe z- fields, z~25AB/49 deg2), COSMOS HST (1.8 deg2) No NIR yet Lockman Hole 10:45:0058:0015CFHT MegaPipe Archive (15 fields), Subaru (~18 fields, I = 26 AB, B=27AB) UKIDSS DXS (1/8.75) SWIRE (11) EGS14:1754:3049CFHTLS-W3 (44 MegaPipe z- fields, z~25ABmag/49 deg2) No NIR yetIRAC GTO data, AKARI 15 micron ELAIS-N116:11:0055:009CFHT MegaPipe (9 fields, z~25AB mag) Subaru Deep I (18 fields (5 deg2) UKIDSS DXS+UDS (1.7/8.75) SWIRE (9.2) ELAIS-N216:36:4841:01:4 5 6CFHT MegaPipe (6 fields, z~25 AB mag), Subaru Deep I (18 fields (5 deg2) No NIR yetSWIRE(4.8) SA2222:1700:2016CFHLTLS-W4 (20 MegaPipe z- fields, z~25AB/16 deg2 UKIDSS DXS+UDS (3.5/8.75) None The 6 th KIAS Workshop

Science Highlights High redshift quasars High redshift galaxy clusters/galaxies Transient objects (GRBs, TDE, SNe, etc) The 6th KIAS Workshop

SMBH Mass Evolution AKARI points (Jun, H., MI, 2014 submitted) z ~ 5.5z > 6.5 ? Fast growth from stellar mass BHs Slow growth with heavy BH seeds The 6th KIAS Workshop M ⊙ at z ~ 5 (1.2 Gyr), and a few x 10 9 M ⊙ at z ~ 6.4 (0.95 Gyr) Emergence of SMBHs [L bol /L Edd ~ 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 The 6th KIAS Workshop Willott et al. (2010)

z~5.5 Quasars Identification of z ~ 5.5 QSOs is difficult with SDSS filters The 6th KIAS Workshop Chiu et al. 2005

High Redshift Quasar and z=6.5 With Special Filters The 6th KIAS Workshop

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 The 6th KIAS Workshop Park, Pak, MI et al. (2012)

Quasars at 5 < z < The 6th KIAS Workshop 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 = 5.3z = 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) The 6th KIAS Workshop Jeon, Y., MI, et al. 2014, in prep.

Faint Quasar Candidates at z ~ The 6th KIAS Workshop 9 candidates z(AB) ~ 22.5 mag from 90 deg 2 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 The 6th KIAS Workshop

Evolution of Quasars at z > 7? Several candidates  Rapid evolution of quasars at z > The 6th KIAS Workshop

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? The 6th KIAS Workshop

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 deg 2 vs. ~1 deg 2 ) The 6th KIAS Workshop Reversal (Elbaz et al. 2007)No reversal (Ziparo et al. 2014) versus High SF High density z=0 z=1

Search for High Redshift Clusters The 6th KIAS Workshop 3.6 – 4.5 micron z - J Multi-wavelength data  Photometric redshift or color-color diagram  Redshift bin  Identify over-dense area

The 6th KIAS Workshop Cluster at z=1.1  1000 candidates identified

For galaxies at z =1, Difference in galaxy properties are due to mass, not environment No reversal in SFR-density relation for massive galaxies SFR quenching due to environ. at z < 1 (reversal in SFR-density rel) The 6th KIAS Workshop SDSS SDSS (z=0)IMS (z=1) Jae-Woo Kim, MI, et al. 2014

Fraction of Quiescent Galaxy At z > 1.4, mass dependent (not environment) At z < 1.4, environment becomes important The 6th KIAS Workshop log (M * /M ⊙ ) ≥ 9.1 log (M * /M ⊙ ) ≥ 10.0 Passive fraction (N passive /N total ) Seong-Kook Lee, MI, et al Red: Cluster Blue: Field

GRB, Transients Tidal disruption event: Swift J (Burrows et al. 2011, Nature) Long-term (2+ years) monitoring results (Yoon et al. 2014; Im et al. 2014) Christmas Burst, GRB A (Thone et al. 2011, Nature) CQUEAN riz data helpsdetermine the black body radiatoin afterglow The 6th KIAS Workshop

Swift J Long-term Light Curve Before host subtraction ∝ t -0.4 After host subtraction ∝ t -1.1 ( c.f. TD ∝ t -5/3 ) The 6th KIAS Workshop

Swift J Host Galaxy + BH Mass Log(M BH /M ⊙ ) ~ 6.8 ± 0.5 χ 2 =1.318 Yongmin Yoon, MI, et al. 2014, in prep The 6th KIAS Workshop

IMS Preliminary Data Release (click IMS banner) u.php?id=starthttp://astro.snu.ac.kr/~exact/dokuwiki4/dok u.php?id=start J-band and Y-band Catalogs for Elais-N1, Elais-N2, and SA22 fields are available (About 30 deg 2 ) The 6th KIAS Workshop

Summary Infrared Medium-deep Survey deg 2 imaging in J and Y (23 AB mag) - CQUEAN imaging of high redshift objects - Transient follow-up 8 quasars at z=5.5 – of z > 1 cluster candidates: environment vs internal mechanism GRBs/TDE/SNe The 6th KIAS Workshop