Fibre Multi-Object Spectrograph (FMOS) for the Subaru Telescope

Kimura, Masahiko; Maihara, Toshinori; Iwamuro, Fumihide; Akiyama, Masayuki; Tamura, Naoyuki; Dalton, Gavin; Takato, Naruhisa; Tait, Philip J.; Ohta, Kouji; Eto, Shigeru; Mochida, Daisaku; Elms, Brian; Kawate, Kaori; Kurakami, Tomio; Moritani, Yuki; Noumaru, Junichi; Ohshima, Norio; Sumiyoshi, Masanao; Yabe, Kiyoto; Brzeski, Jurek; Farrell, Tony; Frost, Gabriella; Gillingham, Peter; Haynes, Roger; Moore, Anna; Müller, Rolf; Smedley, Scott; Smith, Greg; Bonfield, D. G.; Brooks, C.B.; Holmes, A.; Lake, Emma Curtis; Lee, Hanshin; Lewis, Ian; Froud, Tim R.; Tosh, Ian; Woodhouse, Guy F.W.; Blackburn, Colin; Dipper, N. A.; Murray, Graham J.; Sharples, R. M.; Robertson, David J.

doi:10.1093/pasj/62.5.1135

Cited by 109 publications

(65 citation statements)

References 31 publications

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“…IR-selected sources were targeted in two pointings (0.5 deg 2 ) located within the COSMOS field with FMOS as part of the Guaranteed time observations program. The FMOS instrument (Kimura et al 2010) consists of 400 1.2 arcsec diameter fibres which can be placed within a 30 arcmin diameter field of view. We used the low-resolution mode (R ∼ 600), allowing instantaneous coverage of both the J and H band (0.9 < λ < 1.8 µm), with cross-beam switching, i.e.…”

Section: Fmos Observations and Emission-line Measurementsmentioning

confidence: 99%

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FMOS near-IR spectroscopy ofHerschel-selected galaxies: star formation rates, metallicity and dust attenuation atz∼ 1

Roseboom

Bunker²,

Sumiyoshi

et al. 2012

Monthly Notices of the Royal Astronomical Society

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We investigate the properties (e.g. star formation rate, dust attenuation, stellar mass and metallicity) of a sample of infrared (IR) luminous galaxies at z ∼ 1 via near‐IR spectroscopy with Subaru‐FMOS. Our sample consists of Herschel SPIRE and Spitzer MIPS selected sources in the COSMOS field with photometric redshifts in the range of 0.7 < zphot < 1.8, which have been targeted in two pointings (0.5 deg2) with FMOS. We find a modest success rate for emission‐line detections, with candidate Hα emission lines detected for 57 of 168 SPIRE sources (34 per cent). By stacking the near‐IR spectra we directly measure the mean Balmer decrement for the Hα and Hβ lines, finding a value of 〈E(B − V)〉 = 0.51 ± 0.27 for 〈LIR〉 = 1012 L⊙ sources at 〈z〉 = 1.36. By comparing star formation rates estimated from the IR and from the dust‐uncorrected Hα line we find a strong relationship between dust attenuation and star formation rate. This relation is broadly consistent with that previously seen in star‐forming galaxies at z ∼ 0.1. Finally, we investigate the metallicity via the N2 ratio, finding that z ∼ 1 IR‐selected sources are indistinguishable from the local mass–metallicity relation. We also find a strong correlation between dust attenuation and metallicity, with the most metal‐rich IR sources experiencing the largest levels of dust attenuation.

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Section: Fmos Observations and Emission-line Measurementsmentioning

confidence: 99%

“…Here we investigate the rest-frame optical-to-far-IR properties of a sample of Herschel 1 (Pilbratt et al 2010) sources which were targeted for near-IR spectroscopy with FMOS (Kimura et al 2010).…”

Section: Introductionmentioning

confidence: 99%

FMOS near-IR spectroscopy ofHerschel-selected galaxies: star formation rates, metallicity and dust attenuation atz∼ 1

Roseboom

Bunker²,

Sumiyoshi

et al. 2012

Monthly Notices of the Royal Astronomical Society

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“…This configuration with a large distance between fibers and the metrology camera allows us to take all fiber images in one shot, although the possible disturbing effects of the air between them merits careful attention. In 2012 December this "dome seeing" effect was measured at Subaru telescope by using the basically same configuration but actually backilluminated FMOS 27 fibers and a commercial-based CCD camera Atik 450 set at the common-use Cassegrain container ( Figure 11). It was concluded that to average out the short-timescale image instability on fiber positions due to the "dome seeing" effects an exposure time of around 1 second or so rather than shorter ones is optimal.…”

Section: Metrology Cameramentioning

confidence: 85%

Progress with the Prime Focus Spectrograph for the Subaru Telescope: a massively multiplexed optical and near-infrared fiber spectrograph

et al. 2014

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The Prime Focus Spectrograph (PFS) is an optical/near-infrared multi-fiber spectrograph with 2394 science fibers, which are distributed in 1.3 degree diameter field of view at Subaru 8.2-meter telescope. The simultaneous wide wavelength coverage from 0.38 μm to 1.26 μm, with the resolving power of 3000, strengthens its ability to target three main survey programs: cosmology, Galactic archaeology, and galaxy/AGN evolution. A medium resolution mode with resolving power of 5000 for 0.71 μm to 0.89 μm also will be available by simply exchanging dispersers. PFS takes the role for the spectroscopic part of the Subaru Measurement of Images and Redshifts (SuMIRe) project, while Hyper Suprime-Cam (HSC) works on the imaging part. HSC's excellent image qualities have proven the high quality of the Wide Field Corrector (WFC), which PFS shares with HSC. The PFS collaboration has succeeded in the project Preliminary Design Review and is now in a phase of subsystem Critical Design Reviews and construction.To transform the telescope plus WFC focal ratio, a 3-mm thick broad-band coated microlens is glued to each fiber tip. The microlenses are molded glass, providing uniform lens dimensions and a variety of refractive-index selection. After successful production of mechanical and optical samples, mass production is now complete. Following careful investigations including Focal Ratio Degradation (FRD) measurements, a higher transmission fiber is selected for the longest part of cable system, while one with a better FRD performance is selected for the fiber-positioner and fiber-slit components, given the more frequent fiber movements and tightly curved structure. Each Fiber positioner consists of two stages of piezo-electric rotary motors. Its engineering model has been produced and tested. After evaluating the statistics of positioning accuracies, collision avoidance software, and interferences (if any) within/between electronics boards, mass production will commence. Fiber positioning will be performed iteratively by taking an image of artificially backilluminated fibers with the Metrology camera located in the Cassegrain container. The camera is carefully designed so that fiber position measurements are unaffected by small amounts of high special-frequency inaccuracies in WFC lens surface shapes.Target light carried through the fiber system reaches one of four identical fast-Schmidt spectrograph modules, each with three arms. All optical glass blanks are now being polished. Prototype VPH gratings have been optically tested. CCD production is complete, with standard fully-depleted CCDs for red arms and more-challenging thinner fully-depleted CCDs with blue-optimized coating for blue arms. The active damping system against cooler vibration has been proven to work as predicted, and spectrographs have been designed to avoid small possible residual resonances.

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“…The light passing through the turbulence will deviate from its original position on the camera sensor. In order to understand such effect, a series of tests were executed with Subaru FMOS 4 instrument under different conditions. The details are discussed in the following section:…”

Section: Metro Logy System Analysismentioning

confidence: 99%

Metrology camera system of prime focus spectrograph for Subaru telescope

Reiley

Wang

Chou

et al. 2018

Ground-Based and Airborne Instrumentation for Astronomy VII

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The Prime Focus Spectrograph (PFS) is a new optical/near-infrared multi-fiber spectrograph designed for the prime focus of the 8.2m Subaru telescope. The metrology camera system of PFS serves as the optical encoder of the COBRA fiber motors for the configuring of fibers. The 380rnm diameter aperture metrology camera will locate at the Cassegrain focus of Subaru telescope to cover the whole focal plane with one SOM pixel Canon CMOS sensor. The metrology camera is designed to provide the fiber position information within 5µrn error over the 45cm focal plane. The positions of all fibers can be obtained within 1 s after the exposure is finished. This enables the overall fiber configuration to be less than 2 minutes.

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Fibre Multi-Object Spectrograph (FMOS) for the Subaru Telescope

Cited by 109 publications

References 31 publications

FMOS near-IR spectroscopy ofHerschel-selected galaxies: star formation rates, metallicity and dust attenuation atz∼ 1

FMOS near-IR spectroscopy ofHerschel-selected galaxies: star formation rates, metallicity and dust attenuation atz∼ 1

Progress with the Prime Focus Spectrograph for the Subaru Telescope: a massively multiplexed optical and near-infrared fiber spectrograph

Metrology camera system of prime focus spectrograph for Subaru telescope

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