Transcript Document
FMOS
: 400 Object Fibre-Based Spectrograph at Prime Focus of SUBARU TELESCOPE (
F
ibre
M
ulti-
O
bject
S
pectrograph)
SPECIFICATIONS
FOV 30 arcminφ Wavelength Coverage 0.9
～
1.8μ
ｍ（
J,H-band
）
(OH airglow-suppresion capability) Diameter of Fibres 100μ
ｍ
1.25arcsecφ Spectral Resolution R
＝
λ/δλ
～
2400 (high res. mode)
～
700 (low res. mode) Limiting Mag.
（
1h integr. S/N
＝５） ～
22.3 mag in J
～
20.9 mag in H
FMOS Science Overview
(G.Dalton)
•
Need for a survey spectrograph at NIR wavelengths
•
Successor to 2dF and SDSS
•
Urgently needed for follow up of UKIDSS and later VISTA-IR surveys
•
SUBARU is the only telescope that provides the necessary focal station for such an instrument
•
With FMOS & the UKIDSS DXS we may be able to make a robust determination of the nature of Λ --Just need to measure velocity dispersions for about 1000 clusters with z~1.5
Numbers of possible observing programmes will be proposed or presented in the FMOS-WS in Jan. 13-14, 2004 in Kyoto.
Fabrication in Progress
Prime Focus Unit : (New)
PFU
Housing, Instr. Rotator, and Wire twister S/H camera, AG camera, and Focus adjuster
Kyoto University
Designed, Fabricated, and Tested in Kyoto
Fibre Positioner
: ECHIDNA
AAO
i) Tube Piezo-based Actuators ii) Actuator Module (22 x 2 lines x 20 mod.) iii) Fibre Bundles for Autoguiding (7 bundles x 2 lines) iv) Focal Plane Imager v) Housing, Control Electronics & Software
Lifting frame Electronic Enclosure Echidna positioner assembly Main structural plate FPI Guide system
Crane hook The FMOS Echidna system PFU assembly Corrector
FMOS Prime Focus Corrector designed and fabricated in AAO
Fibre Channel/Connector/Slit-Assy
Durham University
The Cabling Design
Echidna positioner
• 2 cables, 2 connectors and 2 slit units. • Modular cable and connector design
2 Spectrographs
Two Spectrographs and Camra Systems Kyoto University University of Oxford
Optical Design of IRS Identical Optical Design for two Spectrographs
Schmidt Plate
Optical Design of IRS
Grating 1 0.9
-- Entrance slit OH 1.8
μm an line of 400 fibres
Mask Mirror
VPH Grating Detector
Mochida Schmidt
Camera Lens Unit (
IRS-CAM
)
Why OH Suppression?
Because the IR sky is disgusting!
Can work between the lines, but then we start anything useful with this wonderful wide field!
Sky subtracted Sky subtracted
Natural OH + Object
T=1200 sec
OH suppressed sky
T=800 sec T=3200 sec
Both-side Aspheric Off-axis Schmidt Plate
(Mochida Schmidt)
Light
Aspheric This aspheric plates will be grinded with the ELID grinding method.
Normal Schmidt Plate
（
A Part of 70cmφ Schmidt
）
IRS Camera
@
Rutherford Appleton Laboratory
IRS Camera
@
Kyoto University
IRS-CAM
Two Spectrographs and Camra Systems Kyoto University University of Oxford
IRS-CAM
New room/floor is being built in the dome of Subaru
FMOS Science Workshop -- Program
http://www.kusastro.kyoto-u.ac.jp/~ohta/fmosws/program.html
Jan 13 (Tue):
FMOS overview
10:00-10:40 T. Maihara(Kyoto): FMOS overview and current status 10:40-10:55 N. Tamura (Durham): Expected performance 1 (spectrum) 10:55-11:10 M .Akiyama (Suabru): Expected performance 2 (on chip)
Galactic Astronomy
11:10-11:40 P. Lucas (Hertfordshire): FMOS and UKIDSS Galactic Astronomy 11:40-12:10 M. Ishii (NAOJ): Spectral Classification of YSO clusters with FMOS (12:10-12:40 FMOS Kyoto Lab tour )
Extragalactic Astronomy
13:45-14:15 C. Ikuta (NAOJ): Metal-Rich Populations in A Metal-Poor Galaxy 14:15-14:45 T. Kodama (NAOJ): Study of distant clusters through PISCES spectroscopic follow-up 15:00-15:30 A. Edge (Durham): SDSS-2dF Luminous Red Galaxy Survey and the prospects for its UKIDSS-FMOS counterpart 15:30-16:00 T. Yamada (NAOJ): Extremely-Red Universe with FMOS II. Suprime-Cam/UKIDSS 10 sq. degree Imaging Survey 16:00-16:30 I. Tanaka (NAOJ/Tohoku Univ.): Distant clusters with MOIRCS and FMOS 16:30-17:00 C. Simpson (Durham): OHS observations of vigorous star formation in a bulge-dominated ERO, and the need for spectroscopic classification of EROs 17:00-17:30 K. Sekiguchi (Subaru): Observing galaxy mass assembly at z > 1 in the SXDF (18:00-20:00 Conference Dinner)
Jan 14 09:30-10:00 N. Arimoto et al. (NAOJ): Proto-Ellipticals @ z>2 10:00-10:10 H. Hanami (Iwate U.): Short comment 10:10-10:40 N. Tamura (Durham): Passive Ellipticals(TBD) 10:40-11:10 O. Almaini (Edinburgh): The UKIDSS Ultra-Deep Survey: Mapping The Early Stages of Galaxy Formation 11:10-11:40 G. Dalton (Oxford): The Post-2dF/WMAP Era of Cosmology - A New Canvas for FMOS Surveys 11:40-12:10 K. Glazebrook (Johns Hopkins Univ.): FMOS detection of cosmic sound 12:10-12:30 K. Ohta (Kyoto Univ.): A Survey with FMOS: Galaxy Evolution (TBD) 13:30-14:00 M. Akiyama (Subaru): FMOS surveys of AGN/QSOs : Growth of Massive Black Holes 14:00-14:30 S. Croom (AAO): Prospects for infrared AGN surveys 14:30-15:00 R. Sharp (IoA): Multi-object spectroscopy in the Near IR with the CIRPASS spectrograph
Discussion
15:15-16:15 Discussion on method of observations and data reduction kick off by I. Lewis(Oxford), S. Croom (AAO) AAO proposal by G. Frost (AAO) 16:15-17:15 General Discussions (1) How to use GT (how much GT?) (2) Large survey program (3) UK time? Collaboration with UK/Japan? Poster papers: PFU design : Kimura (Kyoto Univ.) Software design : S. Eto (Kyoto Univ.) UK spectrograph system : I. J. Lewis (Univ. Cambridge) Fibre system : N. Tamura (Univ. Durham) Echidna system : G. Frost (AAO)
System Throughput Assessment ================================================== Wavelength (microns) 1 1.25
1.65
------------------------------------------------------------------------------------- Atmosphere (zenith = 1.0) Central Obstruction Primary Mirror (Al) Corrector BSM51Y glass /MgF2 0.99
0.95
0.85
0.91
0.99
0.95
0.90
0.96
0.99
0.95
0.93
0.93
Throughput to focal plane 0.72
0.81
0.81
================================================== Fibre attenuation (dB/km) 2.50
1.30
0.80
------------------------------------------------------------------------------------ Fibre Surface 0.96
0.96
0.96
Fibre transmission GRIN lens transmission GRIN les AR coating 0.99
0.95
0.98
1.00
0.95
0.98
1.00
0.95
0.98
Alignment losses 0.96
0.96
0.96
GRIN lens AR coating GRIN lens transmission Fibre Transmission Fibre Surface 0.98
0.95
0.99
0.98
0.98
0.95
1.00
0.98
0.98
0.95
1.00
0.98
MOS fibre system throughput 0.77
0.78
0.78
==================================================
AR coating (single pass) Overcoated Silver reflectivity Gold reflectivity 0.97
0.97
0.97
--------------------------------------------------------------------------------- Spectrograph Collimator(Ag) 0.97
0.98
0.98
Schmidt 1 bulk transmission Schmidt1 (2 passes=4 surfaces) 0.98
0.98
0.99
Grating (unpolarised light) 0.99
0.97
0.82
1.00
0.98
0.84
1.00
0.98
0.68
Flat (protected Ag 2 passes) Spectrograph Collimator (Ag) Mask Mirror (gold) Spectrograph Collimator (Ad) Schmidt 2 bulk transmission Schmidt 2 (2 surfaces) 0.94
0.97
0.97
0.97
0.96
0.98
0.97
0.98
0.96
0.98
0.97
0.98
0.99
0.99
1.00
Aperture stop (for f/4.7) 0.90
0.90
0.90
VPH Grating 0.70
0.70
0.70
---------------------------------------------------------------------------------- OHS Throughput (low res) 0.42
0.45
0.37
---------------------------------------------------------------------------------- OHS Throughput (High res) 0.59
0.65
0.53
================================================
Camera Window (2 surfaces) Camera (12 surfaces) Camera +window bulk transm.
0.99
0.93
1.00
0.99
0.95
1.00
1.00
0.97
1.00
Red cutoff (side 1) 0.97
0.98
0.97
--------------------------------------------------------------------------------- Camera throughput 0.89
0.93
0.94
================================================ Total Spectrogr (low res) 0.37
0.42
0.35
Total Spectrogr (high res) 0.53
0.60
0.50
INGRID QE FMOS HAWAII-2 QE 0.52
0.67
0.56
0.71
0.57
0.72
================================================ Total System (low res) 0.14
0.19
0.16
Total system (high res) 0.20
0.27
0.23
================================================
Summary for plotting (low res) ========================================== Wavelength 1 1.25
1.65
----------------------------------------------------------------------- Throughput to focal plane 0.72
0.81
0.81
MOS fibre system throughput OHS Throughput Camera throughput Total Spectrograph Throughput Detector Q.E. 0.77
0.42
0.89
0.37
0.67
0.78
0.45
0.93
0.42
0.71
0.78
0.37
0.94
0.35
0.72
Total System Throughput 0.14
0.19
0.16
==========================================
Summary for plotting (high res) ========================================= Wavelength 1 1.25
1.65
--------------------------------------------------------------------- Throughput to focal plane 0.72
0.81
0.81
MOS fibre system throughput 0.77
0.78
0.78
0.53
OHS Throughput Camera throughput 0.89
Total Spectrograph Throughput Detector Q.E. Total System Throughput 0.59
0.93
0.53
0.67
0.20
0.65
0.94
0.60
0.71
0.27
0.50
0.72
0.23
==========================================