MOIRCS and FMOS for cluster studies

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

• Intruduction and the current status of MOIRCS
• MOIRCS and FMOS
• Distant cluster studies as a target of
  FMOS-MOIRCS
• joint project

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1.Intruduction and Current Status of MOIRCS
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MOIRCSMulti-Object Infrared Camera and
Spectrograph for Subaru
T. Ichikawa
T. Nishimura
C. Tokoku
R. Suzuki
Y. Katsuno
K. Omata/ M. Konishi/ T. Yoshikawa et al.
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Performance of MOIRCS
F.O.V 4' 7'
Observing Mode Imaging / MOS (cooled slits / Grizm)
Optimized wavelength 0.8 - 2.5 um
Spectral Resolution 500 1300 (2000) _at_ 0.5slit
Detector HAWAII-2 (HgCdTe) x 2
Pixel Size 18 um
Image Scale 0.117 arcsec/pixel
Readout noise / Q.E. lt10e- (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/N10) J23.8, H23.1, K22.3 Spectroscopy(R500, 4 hr, S/N5) J21.3, H20.8, K20.0
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Large FOV CISCO versus MOIRCS
(From GOODS 6hr Ks data)
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This is the MOIRCS view!
4' x 7'
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Components of MOIRCS
Suzuki et al. Subaru UM 2002
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Optical Unit/ Bench/ Filter/ Grism
Slit Exchanging Unit
Peripherals
Support Structure/ Connector
Main Dewer
Detector
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The Design of MOIRCS --- dual camera
spectrograph system
Light
MOS plate exchanging unit
Focal Plane
Cooler
Filters/Grism
Cooler
detector
Front View
Side View
Inside is Cooled to 77K
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OPTICAL Rayout of MOIRCS
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Thre Relation of the MOIRCS FOV on Cassegrain
Focus (6' f)
The area that lower chip doesn't use.
4 arcmin.
1 arcmin.
4 arcmin.
The area that upper chip doesn't use.
4 arcmin.
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Imaging mode
Spectrograph mode
Object on the center is devided
4 arcmin.
Usable for Spectroscopy!
Unusable detector area (imaging) 30 arcsec
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MOIRCS is the MOS in zJHK!
Cooled mask slot / robotic mask in-out
mechanism Max 50 slitlets / 24 masks available
for a night
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Grisms
R500 gratings for zJ / HK wavebands R1300 for
J,H,K bands
zJ R500
HK R500
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Slit Mask Exchanging Unit
Linear Actuator (can handle 0.01mm accuracy)
Gate Valve Mask Dewar is detachable.
Mask Dewar with the exclusive cooler (cooled to
150K) can hold 24 slit masks
Useful for efficient mask exchange!
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Slit mask exchanging mechanism
?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.
(15minutes.)
Room temperature test is successful
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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!
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2. MOIRCS and FMOSComparisonfor scientific
purpose
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MOIRCS and FMOS
FMOS R700 - 2400 zJH with OHS 400 in 30'
FOV. MOIRCS R500 - 1300 zJHK lt50
in 4'x7' FOV.
ECHIDNA Rayout
FMOS sparsely distributed targets gt e.g. Field
Objects MOIRCS high density region gt e.g.
Clusters
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MOIRCS and FMOS
Suprime-Cam F.O.V.
FOCAS F.O.V.
MOIRCS FOV
FMOS Good match to Suprime-Cam ---
photo-z MOIRCS Good match to FOCAS ---
optical spectroscopy
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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

Only FMOS can do an efficient follow-up of
SupCam 30'x30'data
For Studies of Cluster environment
FMOS-MOIRCS joint observation is most efficient!
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3. Distant Cluster Sudies as a Target of
FMOS-MOIRCS Joint Project
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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?
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For understanding galaxy evolution in cluster
environment

• SFR measurement
• Ha, Hb, OII (lines) MOIRCS/FMOS
• Hd absorption (continuum for zgt1 FMOS OHS!)
• High density regions MOIRCS (zgt1) FOCAS(zlt1)
• Galaxies in the outskirts of clusters FMOS

• Structure, cluster dynamics often gt10Mpc FMOS!
• no efficient way to do optical spectroscopy
  for faint galaxies!
• Complex cluster merger lt a few Mpc MOIRCS

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A supercluster at z0.54Connolly et al. (1996)
known clusters at z0.54
Galaxies with pectroscopic redshift0.54
Galaxies with photometric redshift0.54
Suprime-Cam data by the PISCES project (Kodama et
al.)
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CL 0016
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A supercluster search for a large QSO group at
z1.1
LQG10 group of 23 QSOs at z1.1 (Crampton et
al. 1989) LSS at z1.1? Pilot works by Tanaka
et al. (2000,2001), Yamada et al. (1997)
Area A.
Area C.
Our observed area by Suprime-Cam (i', z')
Area B.
2 degrees
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Results
i-z color selection for old red glalaxies at
z1.1 some hint for superstructure associated
with LQG10
Area A
Area B
Density enhancement mildly traces QSO distribution
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C-M Diagram
Comparison with Passive Evolution Model by
Kodama Arimoto
more likely to be at z1.1
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highest density peaks MOIRCS/FOCAS is
good Others only sparsely distributed The whole
structure / galaxy properies at the outskirts of
clusters gt ONLY FMOS can access!
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Example of the hottest X-ray cluster RXJ
1347.5-1145
Redshift by Cohen Kneib (2002)
SupCam data by Miyazaki (private)
Substructure? 47 spectra still not enough
S-Z by Komatsu et al. (2001)
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PISCES project (Subaru press relase 2003)
Distant clusters . More complex! Examples of two
clusters at z0.8
Gioia et al. (1999)
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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 zgt1.