FMOS : 400 Object Fibre-Based Spectrograph at Prime Focus of SUBARU TELESCOPE

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FMOS : 400 Object Fibre-Based Spectrograph at Prime Focus of SUBARU TELESCOPE (Fibre Multi-Object Spectrograph) SPECIFICATIONS FOV 30 arcminφ Wavelength Coverage 0.9 1.8μ m( J,H-band (OH airglow-suppresion capability) Diameter of Fibres 100μ 1.25arcsecφ Spectral Resolution

description

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 ) - PowerPoint PPT Presentation

Transcript of FMOS : 400 Object Fibre-Based Spectrograph at Prime Focus of SUBARU TELESCOPE

Page 1: FMOS   :  400 Object Fibre-Based Spectrograph               at Prime Focus of SUBARU TELESCOPE

FMOS : 400 Object Fibre-Based Spectrograph

at Prime Focus of SUBARU TELESCOPE

(Fibre Multi-Object Spectrograph) 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

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• 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.

FMOS Science Overview (G.Dalton)

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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

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Fibre Positioner : ECHIDNA

AAOi) 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

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Liftingframe

ElectronicEnclosure

Echidna positionerassembly

Mainstructural

plate

FPI

Guide system

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Crane hook

The FMOS-Echidna system

PFU assembly

Corrector

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FMOS Prime Focus Corrector designed and fabricated in AAO

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Fibre Channel/Connector/Slit-Assy

FROM ECHIDNA

Launch lens

LED on PCB

TO SPECTROGRAPH

Sub-connector Blocks

Receiver Lens

Removable Ferrule

Fixed Ferrule

Insertable Coupling Prisms

LED Coupling Lens

Durham University

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The Cabling Design

• 2 cables, 2 connectors

and 2 slit units.

• Modular cable

and connector design

Echidna positioner

2 Spectrographs

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Two Spectrographs and Camra Systems

Kyoto University

University of Oxford

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Optical Design of IRS

Mask Mirror

Mochida Schmidt

Schmidt Plate

Camera Lens Unit (IRS-CAM)

VPH Grating

Grating 10.9 --- 1.8 μm

an OH line  

Detector

Entrance slit of 400 fibres

Optical Design of IRSIdentical Optical Design for two Spectrographs

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Why OH Suppression?

Because the IR sky is disgusting!

Can work between the lines, but then we start to run out of pixels to do anything useful with this wonderful wide field!

T=1200 sec

T=800 sec

T=3200 sec

Natural OH + Object

OH suppressed sky

Sky subtracted

Sky subtracted

Sky subtracted

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Both-side Aspheric Off-axis Schmidt Plate (Mochida Schmidt)

Aspheric This aspheric plates will be grinded with the ELID grinding method.

Light

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Normal Schmidt Plate

( A Part of 70cmφ Schmidt )

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IRS Camera

@Rutherford Appleton Laboratory

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IRS Camera

@Kyoto University

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Two Spectrographs and Camra Systems

Kyoto University

University of Oxford

IRS-CAMIRS-CAM

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New room/floor is being built in the dome of Subaru

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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 )

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Extragalactic Astronomy

13:45-14:15 C. Ikuta (NAOJ): Metal-Rich Populations in A Metal-Poor Galaxy14:15-14:45 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)

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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

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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)

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System Throughput Assessment==================================================Wavelength (microns) 1 1.25 1.65--------------------------------------------------------------------------------------

Atmosphere (zenith = 1.0) 0.99 0.99 0.99Central Obstruction 0.95 0.95 0.95Primary Mirror (Al) 0.85 0.90 0.93Corrector BSM51Y glass /MgF2 0.91 0.96 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 0.96Fibre transmission 0.99 1.00 1.00GRIN lens transmission 0.95 0.95 0.95GRIN les AR coating 0.98 0.98 0.98

Alignment losses 0.96 0.96 0.96GRIN lens AR coating 0.98 0.98 0.98GRIN lens transmission 0.95 0.95 0.95Fibre Transmission 0.99 1.00 1.00Fibre Surface 0.98 0.98 0.98MOS fibre system throughput 0.77 0.78 0.78==================================================

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AR coating (single pass) 0.99 1.00 1.00Overcoated Silver reflectivity 0.97 0.98 0.98

Gold reflectivity 0.97 0.97 0.97----------------------------------------------------------------------------------Spectrograph Collimator(Ag) 0.97 0.98 0.98Schmidt 1 bulk transmissionSchmidt1 (2 passes=4 surfaces) 0.98 0.98 0.99

Grating (unpolarised light) 0.82 0.84 0.68

Flat (protected Ag 2 passes) 0.94 0.96 0.96Spectrograph Collimator (Ag) 0.97 0.98 0.98

Mask Mirror (gold) 0.97 0.97 0.97Spectrograph Collimator (Ad) 0.97 0.98 0.98Schmidt 2 bulk transmissionSchmidt 2 (2 surfaces) 0.99 0.99 1.00

Aperture stop (for f/4.7) 0.90 0.90 0.90VPH 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================================================

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Camera Window (2 surfaces) 0.99 0.99 1.00

Camera (12 surfaces) 0.93 0.95 0.97Camera +window bulk transm. 1.00 1.00 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 0.52 0.56 0.57FMOS HAWAII-2 QE 0.67 0.71 0.72

================================================

Total System (low res) 0.14 0.19 0.16

Total system (high res) 0.20 0.27 0.23================================================

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Summary for plotting (low res)==========================================Wavelength 1 1.25 1.65------------------------------------------------------------------------Throughput to focal plane 0.72 0.81 0.81MOS fibre system throughput 0.77 0.78 0.78OHS Throughput 0.42 0.45 0.37Camera throughput 0.89 0.93 0.94Total Spectrograph Throughput 0.37 0.42 0.35Detector Q.E. 0.67 0.71 0.72Total System Throughput 0.14 0.19 0.16==========================================

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Summary for plotting (high res)=========================================Wavelength 1 1.25 1.65----------------------------------------------------------------------Throughput to focal plane 0.72 0.81 0.81MOS fibre system throughput 0.77 0.78 0.78OHS Throughput 0.59 0.65 0.53Camera throughput 0.89 0.93 0.94Total Spectrograph Throughput 0.53 0.60 0.50Detector Q.E. 0.67 0.71 0.72Total System Throughput 0.20 0.27 0.23==========================================