FMOS: Fiber Multi Object Spectrograph

Introduction

FMOS is a fiber-fed multi-object spectrograph. The Echidna fiber positioner system configures 400 fibers with an accuracy of 0.2 arcsec rms in the 30-arcmin diamter field of view at the Subaru prime focus and these fibers are extracted as spectra by the two spectrographs (IRS1 & IRS2). A mask mirror is installed in these spectrographs for OH airglow suppression (OHS). The spectral coverage is from 0.9 μm to 1.8 μm. This is observed at one exposure entirely with R=600 in the Low Resolution mode (LR), while it is divided into four bands ("J-short", "J-long", "H-short" & "H-long") with a ~0.25 μm coverage and one of them is observed at one exposure with R=2200 in the High Resolution mode (HR).

!! Important notes for S11B observers !! The Spine-to-object (S2O) allocation software is still updated from time to time for bug-fix and upgrade. The latest version has been ready to try since Jun 30, 2011. However, due to the recent incident of the telescope, unfortunately, the engineering observations in July and August were both canceled, and we have not been able to confirm yet if S2O files created by the latest version work in actual observation. Accordingly, we request S11B observers to download an older version (20101007 version) from the link below and prepare s2o files using it. In fact, there are several known issues on this version, but workarounds are available for most of them. S2O files created by this version have been working in observations. Spine-to-Object (S2O) allocation software (20101007 version) for Linux and Mac OS X (10.4 or higher). An HTML user manual is available in the "doc" directory. Several examples of catalogs are also available in the "examples" directory. Known issues on this 20101007 version Note that there will be an engineering observation in Sep 2011, so the latest version of S2O software may be available for observers whose observations have been scheduled later in S11B. In S11B, HR as well as LR will be available on IRS1, while IRS2 will still be operated only in LR.

Contents

• System Overview
• Basic Instrument Parameters
• Notable characteristics
• Time variation of spectral throughput in several fibers
• Nonlinear time variation of bias component on the IRS2 detector
• Observation
• Planning observation
• Observation procedure
• Data acquisition for flat fielding and calibration
• Operation of high resolution mode [Important for S11B and S12A applicants/observers]
• Performance
• Measured system throughput
• Guideline of sensitivity
• Spectra from engineerng observations
• FMOS spectrum simulator
• Information for PIs
• Proposal checklist
• Observation checklist
• Preparation for an OPE file
• Text file
• PDF file (NOTE: Supplementary information is available therein).
• List of OH airglow masks
• Spine ID and spectrum ID matchup
• FIBRE-pac: FMOS data reduction package

Candidate target fields for FMOS Guaranteed Time Observation (GTO)

!! Important !! High priority fields in S11B are shown by red colors.

• Candidate fields for studying evolution of galaxies and AGNs
• Subaru XMM-Newton Deep Survey (or UKIDSS Ultra Deep Survey) (2h18m, -5d)
• UKIDSS Deep Extragalatic Survey
• XMM-LSS (2h25m, -4.5d)
• Lockman Hole (10h57m, +57.6d)
• Elais N1 (16h10m, +54d)
• VIMOS 4 (22h17m, +0.3d) [SSA22]
• COSMOS (10h0m, 2.2d)
• GOODS-N and its flanking field (12h37h, 62d)
• DEEP-II AEGIS (14h20m, 53d)
• SSA22 (22h17m, +0.3d)

• Candidate fields for design study of future BAO surveys
• Subaru XMM-Newton Deep Survey (or UKIDSS Ultra Deep Survey) (2h18m, -5d)
• Subaru Deep Field (13h24m, 27.5d)
• CFHT Legacy Survey Wide [4 patches]
• W1:(02h18m,-7.0d) [on the XMM LSS field]
• W2:(08h54m,-4.3d)
• W3:(14h17m,+54.5d) [on the Groth Strip]
• W4:(22h13m,+1.3d) [on the VVDS 22h & UKIDSS DXS fields]
• Red Cluster Survey 2 [13 patches]
• RCS0047:(00h47m,+0.6d)
• RCS0133:(01h33m,-0.2d)
• RCS0310:(03h10m,-14.3d)
• RCS0357:(03h57m,-8.8d)
• RCS1112:(11h12m,-5.9d)
• RCS1303:(13h03m,-1.2d)
• RCS1514:(15h14m,+9.9d)
• RCS1613:(16h13m,+55.0d) [on the Elais-N1]
• RCS2143:(21h41m,-0.1d)
• RCS2338:(23h38m,-9.1d)
• RCS2329:(23h26m,-1.3d) [on the DEEP2]
• RCS1645:(16h45m,+39.5d) [on the Elais-N2]
• RCS1040:(10h40m,+57.7d) [on the Lockman Hole]

• Candidate fields for studying IMF (This observations will be executed in 'niche' observing time.)
  • IC1848 (02h49m, +60.6d)
  • NGC1333 (03h29m, +31.3d)
  • IC348 (03h44m, +32.2d)
  • Pleiades (03h47m, +24.1d)
  • L1495 (04h14m, +28.1d)
  • LkHa101 (04h30m, +35.3d)
  • HeilesCloud2 (04h41m, +25.9d)
  • Trapezium (05h35m, -05.4d)
  • NGC2264 (06h41m, +09.9d)
  • RhoOph (16h28m, -24.5d)
  • SerpensCloud (18h30m, +01.3d)
  • S106 (20h27m, +37.4d)
  • NGC7538 (23h14m, +61.5d)

Further information

Questions regarding these pages should be directed to Naoyuki Tamura. Please note that all numbers on these pages are subject to change as the characteristics and performance of FMOS are better determined.

References

"The Fibre Multi-Object Spectrograph (FMOS) for Subaru Telescope"

Kimura, M., et al. 2010, Publication of The Astronomical Sciety of Japan, Vol. 62, 1135.

"FIBRE-pac: FMOS image-based reduction package"

Iwamuro, F., et al. 2011, Publication of The Astronomical Sciety of Japan, in press (arXiv.1111.6746)

"FMOS: the fiber multiple-object spectrograph: Part VI. Onboard performances and results of the engineering observations"

Iwamuro, F. et al. 2008, Proc. of SPIE, Vol. 7014, 26

"Performance of Echidna fiber positioner for FMOS on Subaru"

Akiyama, M., et al. 2008, Proc. of SPIE, Vol. 7018, 94

"Echidna: the engineering challenges"

Brzeski, J., et al. 2004, Proc. of SPIE, Vol. 5492, 1228

"Integration, commissioning, and performance of the UK FMOS spectrograph"

Dalton, G., et al. 2008, Proc. of SPIE, Vol. 7014, 127

"Design and construction of the fibre system for FMOS"

Murray, G., et al. 2008, Proc. of SPIE, Vol. 7014, 186

"Cryogenic tests of volume-phase holographic gratings: results at 100 K"

Tamura, N. et al. 2006, Applied Optics, Vol. 45, 5923

Last updated: Jan 30, 2012