Current Status of FMOSand

Schedule Toward the Common Use

Naruhisa Takato

What is FMOS?Fibre Multi-Object Spectrograph

• wavelength coverage: 0.9 – 1.8 um• FOV: φ30 ‘• 400 multiplicity• OH – airglow suppression• spectral resolution: R=500 & 2200• expected limiting magnitude: ( 1 hour, S/N=5) J = 22.3, H = 20.9

A Quick History of FMOS

• 2000 : project approved design and development of - Fibre positioner (Echidna): AAO - Prime Focus Unit (PIR): Kyoto/NAOJ - Spectrograph IRS1: Kyoto/NAOJ, IRS2: Oxford, RAL (UK) - F5 fibre: Durham (UK)

A Quick History of FMOS

• 2005/07, 10 1st and 2nd PIR test on telescope

- Corrector was offseted/tilted, but could not correct it because corrector could move only along 1-axis and…- PIR cable wrapper broken mechanically

Cable wrapper and corrector moving mechanism were re-designed and newly fabricated.

Photo: M. Kimura

IRS１（ Univ. Kyoto) IRS２（ UK)

TUE-IR / Subaru

F5 fibre installation

Current Active Members

• Hawaii M. Akiyama, N. Tamura, M. Kimura, P. Tait, N. Takato• Kyoto F. Iwamuro, T. Maihara, K. Ohta• Oxford Univ., Univ. Durham, Rutherford Appleton Lab. (UK)• Anglo Australian Observatory (AU)

Progress in FMOS engineering Obs.

- Coma aberration can be canceled by adjusting corrector lens using SH wavefront measurement- optics: 0.3-0.5 arcsec, - actural image size (incl. seeing): 0.8-1”- telescope distortion modeling: 0.8” rms => 6 stars were acquired at the same time in AG fiber- Obtained Sky spectrum

Stellar images in AG fibre

A Tentative Schedule Toward Open Use

• 2007/12 : PIR test on the telescope (I)(II)• 2008/01 : Echidna test on the telescope (I)• 2008/02: refine Echidna and Spectrograph control on the telescope(II)• 2008/05: IRS1,2 test (I)• 2008/06: IRS1,2 test (II)• 2008/08-: tune-up the total system• 2008/12? - : start GT?• 2009/06 : provide maintenance document• 2009/08??: start Open Use

… need stable instrument for open use