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MOIRCS and FMOS for cluster studies
Ichi Tanaka
Astronomical Institute, Tohoku University
MOIRCSMOIRCS and and FMOSFMOS for cluster studiesfor 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. IchikawaT. Ichikawa
C. TokokuC. Tokoku
R. SuzukiR. Suzuki
Y. KatsunoY. Katsuno
T. NishimuraT. 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 0.8 - 2.5 um
Spectral Resolution 500 ~ 1300 (2000) @ 0.5”slit
Detector HAWAII-2 (HgCdTe) x 2
Pixel Size 18 um
Image Scale 0.117 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
opticsdetector
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
LightMOS plate
exchanging unit
Front View
Side View
detector
Cooler
Cooler
Filters/Grism
Focal Plane
OPTICAL Rayout of MOIRCS
4 arcmin.
Unusable detector area (imaging)
~30 arcsec
Object on the center is devided
Imaging mode Spectrograph 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 R500 HK 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
◎Procedure1 . 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 FMOSComparison
for scientific purpose
MOIRCS and FMOSFMOS: R=700 - 2400 zJH with OHS 400 in 30' FOV.
MOIRCS: R=500 - 1300 zJHK <50 in 4'x7' FOV.
FMOS … sparsely distributed targets => e.g. Field ObjectsMOIRCS … 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:
HHlines) …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=0.54Connolly et al. (1996)
Suprime-Cam data by the PISCES project (Kodama et al.)
known clusters at z=0.54
Galaxies with photometric redshift~0.54Galaxies 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 A Area 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
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 1347.5-1145
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 27-28 Feb.)
• FMOS, MOIRCS & Suprime-Cam can make up a good inter-collaborative project for intensive studies of cluster
environments at z>1.