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STATUS REPORT OF FPC

STATUS REPORT OF FPC. SPICA Task Force Meeting March 29, 2010 MATSUMOTO, Toshio (SNU). Concept of FPC. FPC consists of two instruments FPC-G : Focal plane guiding camera FPC-S : Near infrared camera for scientific observation FPC-S has a back up function of FPC-G

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STATUS REPORT OF FPC

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  1. STATUS REPORT OF FPC SPICA Task Force Meeting March 29, 2010 MATSUMOTO, Toshio (SNU)

  2. Concept of FPC FPC consists of two instruments FPC-G: Focal plane guiding camera FPC-S: Near infrared camera for scientific observation FPC-S has a back up function of FPC-G FPC-G and S must have a same FOV and pixel scale with same detector. 1K x 1K InSb array (25mm pixel) ROIC developed for MIRI/JWST by Raytheon 5 arc-minutes FOV for 1 frame 0.3 arc-second FOV for 1 pixel (~diffraction limit at 5mm)

  3. Detector proposed by Raytheon • Format:                         1024 x 1024 active (plus two columns of reference pixels) • Pixel Pitch:                       25 μm • Input Circuit:                     SFD (source follower per detector) • Active Fill Factor:                 > 98% • Spectral Response:               0.4-5.3 μm • Average Quantum Efficiency:     > 90% (1 - 5 μm) • Typical Response Uniformity:   ≤ 5% (1σ) • Average Dark Current:           ≤ 0.02 e-/sec at 30 K • Read Noise:                       25 ~ 30 e- for single CDS (~20 e- for 0.4 Hz eadout) • Power Dissipation:                 0.5 mW (0.4 Hz readout), 1.2 mW ( 1Hz readout) • Well Capacity:                   2x105e- • Outputs:                         4 • Reset Modes                   Global Reset or reset by Row pair • Operating temperature >10 K

  4. Optical design of FPC-G • Optical axes of lens group are shifted to improve off axis image • 7 lenses with 4 aspherical surfaces • Lens materials are ordinary used ones • Spot size ( I and z band) is typically 10 mm. • Maximum size is ~35 mm at a far end from the telescope axis • Distortion effect can be corrected by interpolation formula.

  5. Structure of FPC-G Weight ~ 4kg (Support structure and FPA are not included) Cross sectional view of FPC-G

  6. Performance of FPC-G Required accuracy of the determination of centroid: 0.05 arcsec Wavelength band: I band (0.8 mm) Detection limit: 18.6 mag (1Hz read out, 25s) Number of stars in 1 frame: ~12 stars (GSCII Catalog) FPC-G can achieve required accuracy Power dissipation 1.2 mW (1 Hz readout), 0.5 mW (0.4 Hz readout)

  7. Optical design of FPC-S FPC-S covers wavelength range from 0.5 mm to 5 mmone more optical element a little longer than previous design (520 mm)

  8. Spot diagram for white light (0.8-5 mm) Typical spot size 24 mm Max spot size 31 mm For monochromatic light 2-5mm max spot size ~34 mm 0.8-2mm max spot size ~42 mm Distortion effect can be corrected by interpolation formula. Error of centroid for 4’x4’ field is average:0.03”, Max 0.06” Error of centroid for 5’x5’ field is average:0.07”, Max 0.37”

  9. Structure of FPC-S Weight ~ 6kg (Support structure and FPA are not included) Filter wheel 10 positions (blank, diffuser, 8 filters)

  10. New mode: LVF Spectroscopy • Three LVFs (Linear Variable Filter) are installed on the filter wheel cf. 0.8-1.6, 1.4-2.8, 2.5-5 • LVF has transmission depending on the physical position (scanning direction). Wavelength coverage is factor 2 Wavelength resolution is ~ 50. http://www.lwecorp.com/product-literature/lvf_ds_co_ae_042506.pdf • Slit less spectroscopy at the wavelength range from 0.8 to 5 mm • Combined with slow scan, surface spectroscopy can be done efficiently for diffuse extended source ← 5 arc-minute → LVF 0.8mm 1.6 mm Scan direction ↓

  11. Expected performance of FPC-S • Assumed parameters Telescope 3-m aperture (7m2) Efficiency 0.5 (Optical + quantum efficiency) Read out noise 20 e- image size 4 pixels • 3s detection limit for point sources (100 sec integration, R~5) 26.3mag(AB) for all bands Vega magnitude J(1.25mm) H(1.6mm) K(2.2mm) L(3.5mm) M(5.0mm) 25.5 24.8 24.4 23.4 23.0 Photon noise becomes dominant for integration time longer than 100 sec 3s detection limit for surface brightness (100sec integration, R~5) 81 nW.m-2.sr-1 • 3s detection limit fro LVF mode, R~50, integration time ~t Point sources, Fl 3.4x10-16.l-2.t-1 W.m-2.mm-1 Extended source, l.Fl8.1x104.l-1.t-1nW.m-2.sr-1 Line intensity for point source 6.84x10-18.l-1.t-1W.m-2 Line intensity for extended source 1.62x103.l-1.t-1nW.m-2.sr-1

  12. Comparison with JWST • Larger field of view JWST 2.2x4.4 arcmin FPC-SPICA 5x5 arcmin • Much larger throughput x 20 of JWST • Capability of surface spectroscopy • New science that can not be done with JWST will be possible

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