The FMOS Facility for the SUBARU telescope
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Transcript of The FMOS Facility for the SUBARU telescope
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The FMOS Facility for the SUBARU telescope
Gavin Dalton
Oxford/RAL
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Overview of Fibre Multi Object Spectrograph project for the Subaru telescope
Masayuki Akiyama
(Subaru Telescope, NAOJ)
on behalf of FMOS team (P.I. Toshinori Maihara)
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FMOS: instrument overview
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FMOS: project overview
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FMOS: prime-focus corrector
• Prime-focus corrector designed and fabricated by AAO
• Three BSM51Y design with F/2.0 and 30arcmin diameter FoV.
• Image quality optimized between 0.9-1.8micron
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• If we put 400 magnetic buttons with fibres (like 2dF) on the prime-focus of the Subaru telescope, it would be like,,,
• So we need new fibre positioning method for FMOS…
FMOS: fibre positioner
145mm
= 30arcmin
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FMOS:Echidna: 1998 Birth of Echidna concept
• Concept by Peter Gillingham (AAO) shown at SPIE@Kona
• Tiling the focal plane with 400 of them = 7mm x 7mm each
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FMOS:Echidna:Long-term development effort
• 1998 Echidna with “Nano-motor”
• 2000 Echidna with “ball-spine” design
• 1999 Echidna with “inch-worm” design
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FMOS:Echidna: 2001 Final design fixed
“Stick-and-slip” motion with sawtooth voltage signal
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FMOS:Echidna: Under testing in Hilo
• Focal plane with 480 fibres.
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FMOS:Echidna: Under testing in Hilo
• Focal plane imager.
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FMOS:Echidna: Under testing in Hilo
• Positioner unit
• SEE ECHIDNA THE MOVIE !!
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Movies
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FMOS:Echidna: test results so far
• Focal plane imaging camera tested. Positions of 400 fibres in 154mm FoV can be measured with 2-3micron r.m.s. accuracy.
• Configuration accuracy of 10micron (corresponds to 0.12 arcsec. Fibre core is 100micron, i.e. 1.2”) can be achieved for >95% of the 400 fibres with 7 iterations in 11minutes.
• Fibre tip is 30micron r.m.s. from the focal plane.
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FMOS: prime-focus unit (PIR)
• New prime focus unit with • instrument focusing unit (Z-movement)• corrector lens adjustment mechanism (XY-movement)• cable wrapping unit
for FMOS is constructed by Kyoto Univ. and Mitsubishi.
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FMOS:PIR+Echidna under testing NOW
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FMOS: fibre train with connector
• Fibre trains with• 120mm 200 fibres/slit• strain relief boxes• F2/F5 conversion air connector• fibre back illumination system
was designed and fabricated in Durham.
• F2-side fibre
• F5-side fibre
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FMOS: fibre train with connector
FROM ECHIDNA
Launch lens
LED on PCB
TO SPECTROGRAPH
Sub-connector Blocks
Receiver Lens
Removable Ferrule
Fixed Ferrule
Insertable Coupling Prisms
LED Coupling Lens
N.B. some of the tolerances on these lenses turn out to be difficult!
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Mapping direction
24 furcation tubes carry 480 fibres (20 in each)
from F P to connector (Launch side.) Each head
consists of 6 sub -con nectors, 2 tubes feed each. T he elem ents are arranged in dual colum ns of
20. Cabling length: 7.6 m .
Rows of circles represent the entire spine array (m inus fiducals and guide fibres.)
Packing is hexagonal.
R/ G/ B → Telescope fiel d of vi ew (2 00 spines) seen by spectrograph I
T /Y / M → Telescope fiel d of view (2 00 spines) seen by spectrograph II No co lour → Redundant area outside field (80 spines) Numbers at left show active fibres present in each row.
The l enslet -coupled fibres are removable, so elements on this side are interchangeable (purple.)
Populated elements in the receiver -side correspond to the 400 spines within the telescope field ONLY (CO L O U R circles.) Redundant s pines ( No colour in ECHIDN A field) are not coupled to the spectrogr aph. The contiguous mapping is conserved .
24 furcation tubes carry 400 fibre s (7, 11, 13, 15 etc.) Length: 7 m (approx.)
20 co nduits continue, carrying 400 fibres (20 each) through into the Nasmyth strain relief box, & then on, into the spectrograph slit units. Length: 40 m& 3 m (approx.)
ECHIDNA – Focal plane
Connector heads (Launch side)
Conne ctor heads (Receiver side)
Nasmyth strain relief
unit s
Slit unit (20 output blocks , 10 in each slit, (20 fibres per
block )
7 11 13 15 17 18 19 20 20 20 20 20 20 20 20 20 20 19 18 17 15 13 11 7
Top end strain relief
unit s
How to map ECHIDNA to spectrographs?
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FMOS: fibre train with connector
A lot of attention has been paid to cable management!
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The FMOS Spectrographs
Gavin Dalton
Oxford/RAL
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• 2 bench-mounted spectrographs (total slit length is ~700 arcseconds).
• Optics cooled to ~200K, with articulated cryogenic cameras
• OH suppression by masking lines at intermediate focus.
• Full ZYJH wavelength coverage in 4 shots at suppression resolution
• Full coverage in 1 shot through redispersing VPH grating
Spectrograph outline
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Can work between the lines, but then we start to run out of pixels to do anything useful with this wonderful wide field!
Because the IR sky is rather nasty…
Why OH Suppression?
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Accomodation Issues
•No space for systems of this size in any convenient location
•Extra floor added to Subaru enclosure on IR side above the Nasmyth platform
•Limited access (spectrogaphs must be assembled in situ)
•Cost…
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Spectrograph Design
Mask Mirror M2H & M2J
Collimator M1
Fold Mirror
Reflection GratingG1 (used in+1 order) Corrector Plate
S1
Corrector Plate S2
VPH Grating G2 (used in+1 order)
300mm Dewar Window
Camera System
Hawaii-II Detector Y
X
Z
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Predicted performance
0.00
0.20
0.40
0.60
0.80
1.00
1.20
0.8 1.3 1.8
Throughput to FocalPlane
Fibre System
FMOS Spectrograph
Camera Throughput
Total SpectrographThroughput
Detector QE
Total SystemThroughput
Low Res SystemThroughput
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Installation (two weeks ago)
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Installation (two weeks ago)
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Installation (two weeks ago)
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FMOS Commissioning Schedule
Near future mile-stones (first discussions on this project were 01/97!)
• 2007/10 Transfer IR prime-focus unit (PIR) and Echidna fibre positioner to summit
• 2007/12 Engineering observations of IR prime-focus unit•Check image quality•Check Auto-Guiding/Shack Hartmann system
• 2008/01 Engineering observation of Echidna fibre positioner•Check positioning accuracy (spectrographs available)
• 2008/02 Start engineering observation with two spectrographs
• 2008/?? Open use observation with shared risk mode/GTO
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So what can we do?
• 20 nights GTO: Galaxy evolution survey, ~15000 ‘good’ spectra from e.g. UDS (Interesting possibility would be to cover the DEEP2 AEGIS area?).
• Opportunity for a large programme (few x 105 redshifts). –See Totani’s talk.
• Whatever else comes up?
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