FMOS Extremely Red Universe II. Extremely Red Universe Probed with FMOS Toru Yamada (NAOJ)

Targets for FMOS Extremely-Red Objects Multi-wavelength sample NIR-selected sample Suprime-Cam/UKIDSS DXS 10 deg2 Imaging SurveyWide-field optical imaging at the two northern DXS fields(Lockman Hole, ELIAS N1) with Suprime-Camw/ T.Futamase, M.Kajisawa, T.Kodama, H.Matsuhara, K.Ohta, K.Sekiguchi, Y.Taniguchi, K.Umetzu, and T.Wada and UKIDSS DXS team

UKIDSS DXS ( Edge sans talk) Northern Fields Lockman Hole ELIAS N1

K

Lockman Hole (11h)ELIAS N1 Field Configuration: TBD Suprime-Cam Wide-Field Imaging Survey I < 26 mag 10 deg2 (40 FOV of Scam ) 10 nightsBkg:SWIRE

ERO / HERO selected in UKIDSS DXS Trivial targets for FMOSThey may be: Old Passive Galaxies at z=1-3 Dusty Star-Forming Galaxy at z > 1 Dusty AGN at High and Intermediate Redshift

~104 Dusty EROs

Mannucci (2001) This works at z~1.5(But maybe not at z~2)

ERO / HERO selected in UKIDSS DXS Trivial targets for FMOSThey may be: Old Passive Galaxies at z=1-3 Dusty Star-Forming Galaxy at z > 1 Dusty AGN at High and Intermediate Redshift

IJK SED/photometric redshifte.g., I-K>4 (for K=21, I > 25 data is needed) J-K>2

Passive Old Galaxies at 1 < z < 3Model SED:Kodama et al. (1998)Coma Metal SequencemodelsConspicuous red colorsat z=1-3

Number Density and Spatial Distribution of Old Passive Galaxies Color Selection Pure photometric easy to observe, easy to model Oldest galaxies are always Reddest at any redshift tracing morphological transformation is very difficult Wide Field Fair sample of the universe Search for rare objects (massive clusters, ULIRG) High statistical accuracy FMOS Confirmation/Calibration of Redshift Distribution Constraint for stellar formation epoch of the oldest galaxies Study galaxy formation bias using the oldest galaxies Search for massive clusters or their progenitors at z=1-3

53W002 fieldModel: z(obs)=2.4Yamada et al. 2001K=20J-K=2Franx et al. (2003) HDF-SKs < 22.5 5L*

Results at z~1 from SXDSSXDS: B

1.3Subaru Suprime Cam 1.2 deg2B(28.) V(26.) R(27.) I(26.5) z(25.5)XMM 100 ksec (center) 50 ksec x 6

SXDS z-band selected objectsColor distributionZ-selected objects0.8 < i-z < 1.2

Old Passive Galaxies in SXDS Field (zAB

Redshift Distribution of the Obejects Selected by Color CriteriaFor Old Passive GalaxiesZ < 22All

Redshift DisributionVs. magnitude and colors 5L*, zf=5 5L*, zf=3

FMOS 10h simulated spectra for 1Gyr EllipticalObserved at z=2 H=21 (K~20)H=22 (K~21)

Finding Proto-Clusters at z=1-3 Massive Clusters (or their high-z progenitors) Are Rare !Lx ~ 2 x 1044 erg/s => 10-7 Mpc-3Z=0 X-ray LF of clusters ~10 clusters w/ Lx > 1044 erg/s at z=0

~100 clusters w/ Lx > 1043 erg/s at z=0

10 sq. deg.1 < z < 3Need Large Area !

Proto-cluster at z=3.1 (Steidel et al. 1998) Suprime-Cam 7h narrow-band imaging @497 nm Hayashino, Matsuda, Tamura, TY et al. 2004 2 x 10-17 erg/s/cm2EWobs > 170 emittersabsorbersA sample ofextended objectsProto-cluster seen in Ly Emission Line

Selection of extended emitters (II)Matsuda, TY, et al. (2004)d~30kpc 35 objects !16 arcsec2>7 in isophotal aperture robust !

25S00 blob1S00 blob2

Weak Lensing Cluster Search Umetsu et al.

SummaryWe are conducting Suprime-Cam/UKIDSS DXS 10 deg2 Imaging Survey

Two Northern Field (Lockman Hole, ELIAS N1)

1st run 2 nights in March 2004 Scheduled 2nd run 5 nights in April/May 2004 Proposed

UKIDSS DXS J 104 dusty starbursts at z > 1 => Old Passive Galaxies at z=1-3

FMOS Spectroscopy SF/AGN activities in dusty ERO/HERO Number density of old passive galaxies at z=1-3 Identification of clusters/proto-clusters at z =1-3

Image credits: ALMA websiteImage credits: ALMA website