MOIRCS and FMOS for cluster studies Ichi Tanaka Astronomical Institute, Tohoku University MOIRCS and FMOS for cluster studies

Contents: 1.Intruduction and the current status of MOIRCS 2.MOIRCS and FMOS 3.Distant cluster studies as a target of FMOS-MOIRCS joint project

1. Intruduction and Current Status of MOIRCS

MOIRCS: Multi-Object Infrared Camera and Spectrograph for Subaru T. Ichikawa C. Tokoku R. Suzuki Y. Katsuno T. Nishimura & K. Omata/ M. Konishi/ T. Yoshikawa et al. & K. Omata/ M. Konishi/ T. Yoshikawa et al.

F.O.V 4' × 7' Observing Mode Imaging / MOS (cooled slits / Grizm) Optimized wavelength um Spectral Resolution 500 ～ ”slit Detector HAWAII-2 (HgCdTe) x 2 Pixel Size 18 um Image Scale arcsec/pixel Readout noise / Q.E. <10e - (TBD) / ~60% Slits about 50 slits per mask Slit Capacity ~24 Expected effeciency Imaging: 0.34 Spectroscopy: 0.20 Limiting Magnitude Imaging （ 1 hr 、 S/N=10 ） J=23.8, H=23.1, K=22.3 Spectroscopy （ R=500, 4 hr, S/N=5) J=21.3, H=20.8, K=20.0 Performance of MOIRCS

(From GOODS 6hr Ks data) Large FOV: CISCO versus MOIRCS

This is the MOIRCS view! 4' x 7'

Slit mask exchange unit Main dewar Support structure Peripherals optics detector Suzuki et al. Subaru UM 2002 Components of MOIRCS

Support Structure/ Connector Main Dewer Optical Unit/ Bench/ Filter/ Grism Slit Exchanging Unit Peripherals Detector

Inside is Cooled to 77K The Design of MOIRCS --- dual camera & spectrograph system Light MOS plate exchanging unit Front View Side View detector Cooler Filters/ Grism Focal Plane

OPTICAL Rayout of MOIRCS

4 arcmin. The area that lower chip doesn't use. 4 arcmin. 1 arcmin. 4 arcmin. Thre Relation of the MOIRCS FOV on Cassegrain Focus (~6'  The area that upper chip doesn't use.

4 arcmin. Unusable detector area (imaging) ~30 arcsec Object on the center is devided Imaging modeSpectrograph mode Usable for Spectroscopy!

Cooled mask slot / robotic mask in-out mechanism Max 50 slitlets / 24 masks available for a night MOIRCS is the MOS in zJHK!

zJ R500HK R500 Grisms: R=500 gratings for zJ / HK wavebands R=1300 for J,H,K bands

Mask Dewar with the exclusive cooler (cooled to 150K) can hold 24 slit masks Linear Actuator （ can handle 0.01mm accuracy ） Gate Valve Mask Dewar is detachable. Useful for efficient mask exchange! Slit Mask Exchanging Unit

◎ Procedure 1 ． Setting mask, vacuuming, cool down 2 ． Rotate corrousel for selecting mask 3.Gate valve opens, grab a mask by robot arm 4. pick up a mask, rotate, set to the focal plane 5. Close Gate valve, start obs. Room temperature test is successful (~15minutes.) Slit mask exchanging mechanism

First Light is soon. Current plan: early March, 2004 !!! MOIRCS Science Workshop: Feb. 27/28 in Sendai !!! Registeration deadline … Jan. 31, 2004 A planned GT science will be intensively introduced and discussed on WS. Contributions are greatly welcomed!

2. MOIRCS and FMOS Comparison for scientific purpose

MOIRCS and FMOS FMOS: R= zJH with OHS 400 in 30' FOV. MOIRCS: R= zJHK <50 in 4'x7' FOV. FMOS … sparsely distributed targets => e.g. Field Objects MOIRCS … high density region => e.g. Clusters ECHIDNA Rayout

MOIRCS and FMOS FOCAS F.O.V. Suprime-Cam F.O.V. MOIRCS FOV FMOS: Good match to Suprime-Cam --- photo-z MOIRCS: Good match to FOCAS --- optical spectroscopy

For General Field Survey MOIRCS & FOCAS … pensil beam survey for whole galaxies [rest optical spectra for all galaxies, but still large cosmic variance] FMOS & SpCam-WFCAM … much less cosmic variance [good for large-scale clustering, global cosmic SFR history, & follow-up of the rare objects (sub-mm sources/ EROs/ AGNs) but needs a careful target selection by photo-z] For Studies of Cluster environment … FMOS-MOIRCS joint observation is most efficient! *** Only FMOS can do an efficient follow-up of SupCam 30'x30'data ***

3. Distant Cluster Sudies as a Target of FMOS-MOIRCS Joint Project

Distant Clusters of Galaxies Topic: Star-formation activities in cluster environment Large-scale clustering and star-formation Early-epoch of clusters How the star-formation activities has ceased in clusters? What is the relationship between the dynamical evolution of clusters and the galaxy evolution in clusters? What properties do massive cluster galaxies have in their very young epoch?

SFR measurement: H  H  lines) … MOIRCS/FMOS  absorption (continuum for z>1 FMOS OHS! ) High density regions … MOIRCS (z>1); FOCAS(z<1) Galaxies in the outskirts of clusters … FMOS Structure, cluster dynamics : often >10Mpc … FMOS! … no efficient way to do optical spectroscopy for faint galaxies! Complex cluster merger ・・・ < a few Mpc … MOIRCS For understanding galaxy evolution in cluster environment …

A supercluster at z=0.54 Connolly et al. (1996) Suprime-Cam data by the PISCES project (Kodama et al.) known clusters at z=0.54 Galaxies with photometric redshift~0.54 Galaxies with pectroscopic redshift~0.54

CL 0016

A supercluster search for a large QSO group at z=1.1 Area A. Area B. Area C. Our observed area by Suprime-Cam (i', z') 2 degrees LQG10 … group of 23 QSOs at z~1.1 (Crampton et al. 1989) : LSS at z~1.1? Pilot works by Tanaka et al. (2000,2001), Yamada et al. (1997)

Results Area AArea B i’-z’ color selection for old red glalaxies at z=1.1 … some hint for superstructure associated with LQG10 Density enhancement mildly traces QSO distribution

C-M Diagram Comparison with Passive Evolution Model by Kodama & Arimoto more likely to be at z~1.1

Area A. Area B. Area C. ? highest density peaks ・・・ MOIRCS/FOCAS is good Others … only sparsely distributed The whole structure / galaxy properies at the outskirts of clusters ==> ONLY FMOS can access!

Example of the hottest X-ray cluster RXJ S-Z by Komatsu et al. (2001) Redshift by Cohen &Kneib (2002) SupCam data by Miyazaki (private) Substructure? 47 spectra … still not enough

Distant clusters …. More complex! Examples of two clusters at z=0.8 Gioia et al. (1999) PISCES project (Subaru press relase 2003)

Summary MOIRCS will soon achieve First Light (Workshop on Feb.) FMOS, MOIRCS & Suprime-Cam can make up a good inter-collaborative project for intensive studies of cluster environments at z>1.