1 / 31

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

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 ）

yoland
Télécharger la présentation

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

An Image/Link below is provided (as is) to download presentation Download Policy: Content on the Website is provided to you AS IS for your information and personal use and may not be sold / licensed / shared on other websites without getting consent from its author. Content is provided to you AS IS for your information and personal use only. Download presentation by click this link. While downloading, if for some reason you are not able to download a presentation, the publisher may have deleted the file from their server. During download, if you can't get a presentation, the file might be deleted by the publisher.

E N D

Presentation Transcript

  1. FMOS : 400Object Fibre-Based Spectrograph at Prime Focus of SUBARU TELESCOPE (Fibre Multi-Object Spectrograph) SPECIFICATIONS FOV30 arcminφ Wavelength Coverage 0.9～1.8μｍ（J,H-band） (OH airglow-suppresion capability) Diameter of Fibres 100μｍ 1.25arcsecφ Spectral Resolution R ＝λ/δλ～2400(high res. mode) ～ 700 (low res. mode) Limiting Mag. （1h integr.S/N＝５） ～ 22.3 magin J ～ 20.9 magin H

  2. 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.

  3. 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

  4. 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

  5. FMOS Prime Focus Corrector designed and fabricated in AAO

  6. Durham University Fibre Channel/Connector/Slit-Assy

  7. The Cabling Design Echidna positioner • 2 cables, 2 connectors and 2 slit units. • Modular cable and connector design 2 Spectrographs

  8. Two Spectrographs and Camra Systems Kyoto University University of Oxford

  9. Identical Optical Design for two Spectrographs Grating 1 Schmidt Plate VPH Grating Detector Optical Design of IRS Optical Design of IRS 0.9 ---1.8 μm an OH line Entrance slit of 400 fibres Mask Mirror Mochida Schmidt Camera Lens Unit (IRS-CAM)

  10. Why OH Suppression? Because the IR sky is disgusting! Natural OH + Object Can work between the lines, but then we start to run out of pixels to do anything useful with this wonderful wide field! Sky subtracted T=1200 sec OH suppressed sky Sky subtracted T=800 sec Sky subtracted T=3200 sec

  11. Both-side Aspheric Off-axis Schmidt Plate (Mochida Schmidt) Light This aspheric plates will be grinded with the ELID grinding method. Aspheric

  12. Normal Schmidt Plate （A Part of 70cmφ Schmidt）

  13. IRS Camera @Rutherford Appleton Laboratory

  14. IRS Camera @Kyoto University

  15. Kyoto University University of Oxford IRS-CAM Two Spectrographs and Camra Systems IRS-CAM

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

  17. FMOS Science Workshop -- Program http://www.kusastro.kyoto-u.ac.jp/~ohta/fmosws/program.html Jan 13 (Tue): FMOS overview10:00-10:40 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 Astronomy11:10-11:40 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 )

  18. 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)

  19. Jan 14 09:30-10:00 N. Arimoto et al. (NAOJ):Proto-Ellipticals @ z>210:00-10:10 H. Hanami (Iwate U.):Short comment10:10-10:40 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

  20. 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)

  21. System Throughput Assessment ================================================== Wavelength (microns) 1 1.25 1.65 -------------------------------------------------------------------------------------- Atmosphere (zenith = 1.0) 0.99 0.99 0.99 Central Obstruction 0.95 0.95 0.95 Primary Mirror (Al) 0.85 0.90 0.93 Corrector 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 0.96 Fibre transmission 0.99 1.00 1.00 GRIN lens transmission 0.95 0.95 0.95 GRIN les AR coating 0.98 0.98 0.98 Alignment losses 0.96 0.96 0.96 GRIN lens AR coating 0.98 0.98 0.98 GRIN lens transmission 0.95 0.95 0.95 Fibre Transmission 0.99 1.00 1.00 Fibre Surface 0.98 0.98 0.98 MOS fibre system throughput 0.77 0.78 0.78 ==================================================

  22. AR coating (single pass) 0.99 1.00 1.00 Overcoated Silver reflectivity 0.97 0.98 0.98 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) 0.82 0.84 0.68 Flat (protected Ag 2 passes) 0.94 0.96 0.96 Spectrograph Collimator (Ag) 0.97 0.98 0.98 Mask Mirror (gold) 0.97 0.97 0.97 Spectrograph Collimator (Ad) 0.97 0.98 0.98 Schmidt 2 bulk transmission Schmidt 2 (2 surfaces) 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 ================================================

  23. Camera Window (2 surfaces) 0.99 0.99 1.00 Camera (12 surfaces) 0.93 0.95 0.97 Camera +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 0.57 FMOS 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 ================================================

  24. 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 0.77 0.78 0.78 OHS Throughput 0.42 0.45 0.37 Camera throughput 0.89 0.93 0.94 Total Spectrograph Throughput 0.37 0.42 0.35 Detector Q.E. 0.67 0.71 0.72 Total System Throughput 0.14 0.19 0.16 ==========================================

  25. 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 OHS Throughput 0.59 0.65 0.53 Camera throughput 0.89 0.93 0.94 Total Spectrograph Throughput 0.53 0.60 0.50 Detector Q.E. 0.67 0.71 0.72 Total System Throughput 0.20 0.27 0.23 ==========================================

More Related