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UES: Utrecht Echelle Spectrograph

UES: Utrecht Echelle Spectrograph. High-resolution spectrograph on the 4.2m WHT (1992- 2002 ) 50,000 < R < 80,000 Spectral range 300-1100nm Cross-dispersion, (3 prisms) + 2 diffraction gratings. GTC. HORUS.

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UES: Utrecht Echelle Spectrograph

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  1. UES: Utrecht Echelle Spectrograph • High-resolution spectrograph on the 4.2m WHT (1992- 2002 ) 50,000 < R < 80,000 • Spectral range • 300-1100nm • Cross-dispersion, • (3 prisms) • + 2 diffraction • gratings

  2. GTC

  3. HORUS • Abundances everywhere (stars, clusters, comets, nebulae, ISM, planets…) • Follow-up faint metal-poor stars • Transmission spectroscopy of planets • Precision radial velocities (if ultra-stable): planets, asteroseismology • …

  4. Optical elements + detector 4k x 4k Fairchildt Collimator Prisms (3) Gratings (2) Camera 5

  5. UES optical design 3m 3m 6

  6. HORUS optical design 7

  7. pre-optics Microlense arrays (Amus) 50mm fibers (UV050125140, Ceramoptep) 8

  8. Acquisition arm 9

  9. Coupling to OSIRIS inside OSIRIS 10

  10. Design Image sliced on the Nasmyth focus into 12 square 357 µm (0.43 arcsec) microlenses feeding 50 µm diameter fibers 2 calibration fibers 4 sky fibers

  11. Light enclosed in fibers 66% 19% 84% at 1” 6% 57% at 1.5” 38% at 2”

  12. Performance • R ~ 50,000 (1.5-3.5 Å/mm and FWHM ~ 3 pixel) 16% throughput on blaze (0.4 original × 0.65 fiber × 0.8 pre-optics × 0.90 folds × 0.84@1”) • New detector is larger (40962 15 µm) • 40 mm (Δx limited by corr. plate) 61 mm (Δy CCD) • ~ 1-2 m/s long-term precision 370-570 nm contiguous 570-900 nm partially (estimated)

  13. 10ºC<T<20ºC T stability GTC foundations ≈ 0.3 K T variations damped by x5 Data (T, RH) being taken since February 2012    Coudé room

  14. Isolating structure Al 3.15 x 2.5 x 2 m (38.4 m2) stability +/- 0.1K Ref. temperature TBD Δ T = 10ºC implies losses 110w 250w chiller, 20l/min Environment

  15. Vacuum chamber • Stainless steel AISI 304 • 2.9m x 1.6m (1.5m Ø) • mass 1320 Kg • 4 isomatic dampers • Thermal transmission (238w/K): • conduction: 96w/K • convection: 140w/K • radiation (net): 2w/K

  16. All optical elements at a constant temperature 3 hangers to join bench and chamber (G10). Thermal transmission (6w/K): Conduction: 5.3w/K Convection: NA (pressure under 200 mTorr) Radiation (net): 0.7w/K Optical bench

  17. HORUS data reduction and analysis software • Basic processing: bias, flatfielding • Extraction: standard, optimal, perfectionism • Calibration: flux (rough), wavelength (critical) • RVs: cross-correlation, template matching, research! • Spectral classification: stars, galaxies, clusters • Stellar parameters: Teff, logg, [Fe/H], micro, [α /Fe] …

  18. HORUS-P

  19. HORUS-P

  20. The 2 UES gratings 21

  21. Zooming-in 22

  22. Science CCD Lab data

  23. Science Lab data Na-Ar Na-Ne Th-Ar

  24. Lab studies • Stability with temperature • Stability with image • Spectrophotometric precision • Solar center-to-limb variation Shift (pixels) Frame #

  25. HORUS • Estimates indicate 2 years of work and 350 000 euros needed • Have used internal (IAC) funding for design studies and some components (200 000 euros for detector from Spectral Instruments + about 15000 euros recently for design, fibers and other hardware) • IAC internal (Severo Ochoa) funding secured (200 000 euros) • Vacuum chamber is delayed: internal review + funding issues • Attractive alternative is to take it under a simplified form to GTC while vacuum-chamber development continues

  26. HORUS • Most high-resolution science projects do not require extreme stability • Pre-optics can be optimized for poor seeing conditions that GTC cannot use effectively now • HORS can use Nasmyth platform: it fits and with a shorter length (reduced losses) • Essentially ready to go!

  27. HORUS: tentative schedule • Basic instrument completion: June-September 2013 (cover, lab fiber link, Fold 2) • Lab tests: Nov-Dec 2013 • GTC Fiber link, acquisition arm: January –February 2014 • Calibration Unit: March-May 2014 • Comissioning: June-July 2014

  28. Thanks! • Juan Calvo, Ramon Garcia Lopez, Felix Gracia, Rafael Rebolo, Vicente Sanchez, Samuel Santana, Fabio Tenegui (IAC) • Chuck Henderson, Basil Blank (PulseRay) • Fred Hearty (Univ. Virginia)

  29. HORUS issues • Wavelength calibration: can use ICM? otherwise a supply from IACUB) • CCD had faulty electronics: now solved • CCD cryocooler: can be stored in isolated cabinet • Fiber-fed. Fibers in hand. Several fiber links produced for lab tests • Acquisition electronics: working, if too simple • Missing folder: on lease from P. L. Palle (solar lab at Teide Observatory) calibration unit is needed (ThAr hollow-cathode + power

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