HARMONI: A single field, wide band, integral-field spectrograph for the E-ELT

1. HARMONI: A single field, wide band, integral-field spectrograph for the E-ELT Matthias Tecza for the HARMONI team, includingNiranjan Thatte (PI),Fraser Clarke,Roland Bacon, Santiago Arribas,Evencio Mediavilla, Gary Rae, Roger Davies

2. HARMONI: A single field, wide band, integral-field spectrograph for the E-ELT HARMONI is a proposed optical-NIR, adaptive optics assisted, integral field spectrograph designed to exploit the early-light capabilities of the European ELT Phase A study: March ‘08 — Dec ‘09

3. Exoplanets (Coronagraphy) High-z Kinematics Stellar Outflows High-z LAE Morse, Davidson Genzel et al. 06, Förster Schreiber et al. 06 Chauvin et al. 2004 Rhoads et al. 2005 E-ELT instrument road mapSandro D’Odorico, Marseille Nov’06 • Proven instrument concept delivering high quality science • Early spectroscopic follow up faint sources discovered in deep imaging surveys (e.g. JWST), which is only possible with an ELT • Narrow field-of-view matched to early AO capabilities — near-diffraction limited over a small field • Single object mode rather than survey mode (à la MUSE) • Oxford pre-study of an instrument concept (Apr - Sep ‘07) • £70k award from STFC RAS, 9th May 2008

4. SPIFFI/SINFONI NIR: 1.0-2.5µm ≈ 2000 spectra R ≈ 2000 - 4000 0.25” - 0.025” 8”x8” - 0.8”x0.8” VLT/SINFONI AO module SWIFT I/z: 0.65-1.0µm ≈ 4000 spectra R ≈ 4000 0.235” - 0.08” 22”x10” - 7.5”x3.5” Palomar 5m / PALAO Single-Field Wide-Band Spectrograph (SFWBS) • Primary mode • Integral Field • Medium Spectral Resolution • NIR • GLAO & LTAO/MCAO • Optional modes • Visible-red wave bands • Primary mode • Integral Field • Medium Spectral Resolution • NIR • GLAO & LTAO/MCAO • Optional modes • Visible-red wave bands • High Spectral Resolution RAS, 9th May 2008

5. 2nd mirror stack Light loss at boundary slicer stack Principle of the Image Slicer(used in SINFONI, GNIRS, NIFS) input from telescope preserves pupil of input beam located in telescope focal plane output to spectrometer RAS, 9th May 2008

6. slicer entrance pupil re-imaged telescope pupil re-imaged slicer stack f=d mini-pupil d Image Slicer with de-magnification from pre-optics flat slicer mirrors flat pupil mirrors • lens mosaic • creates tele-centric exit slit • de-magnifies slicer stack RAS, 9th May 2008

7. 360mm 180mm SWIFT slicer • ≈4000 spectra • 44 slices, 91 pixel long • 0.47mm slice width • ≈4:1 de-magnification • Twin exit slits, ≈115mm length • Flat slice and pupil mirrors • Lenses for de-magnification RAS, 9th May 2008

8. from telescope/AO flatpupilmirrors re-imaging mirrors Study-slicer Top view flatslicingmirrors RAS, 9th May 2008

9. reimagingmirrors Study-slicer Side view to spectrograph flatpupilmirrors flatslicingmirrors from telescope/AO RAS, 9th May 2008

10. Single slicer • ≈4,000 spaxels • 44 slices, 88 pixel long • 1.3mm slice width • 10:1 de-magnification • Exit slit length ≈260mm • Flat slice and pupil mirrors • Mirrors for de-magnification (cf lenses in SWIFT) RAS, 9th May 2008

11. Two slicers: 8000 spectra RAS, 9th May 2008

12. 230mm Full slicer 260mm 57.2mm • Four exit slits • 4:1 aspect ratio on slicer due to 2:1 anamorphic pre-optics • 2:1 aspect ratio on sky • 176 x 88 pixels • Maximum spaxel scale of 50mas • 8.8” x 4.4” FoV • Smaller spaxel scales (eg. 5mas) through scale changing pre-optics 470mm RAS, 9th May 2008

13. Study-slicer design advantages • No field splitting in pre-optics • No re-imaging like MUSE • High throughput • Flat slicer and pupil mirrors • Aberrations are equal for all slices • All mirror design • Fully achromatic for wide waveband coverage • Very efficient use of detector real estate • ≈95% spectrum packing factor RAS, 9th May 2008

14. Conceptual spectrograph design • f/6 Collimator • 1500mm focal length • 120mm x 240mm beam • 3 mirror design, 2 fold mirrors • 700mm mirror segments • Grating (VPH) • 200mm x 250mm • f/1.8 Camera (from KMOS) • 420mm focal length • ±5˚ field • 6 lens design • Ø 150-300mm lenses • 2 HAWAII2 detectors • 3.5m x 2.5m x 1.0m RAS, 9th May 2008

15. Phase A Study Developments • Addition of field splitter at telescope focus allows simplification of optics and layout (4 separated slicers, easier pre-optics design). • Presently studying completely reflective pre-optics solution for wide wavelength coverage, which would also allow dichroic split at disperser. • Doubling the number of detectors to 16x 2K2 detectors (4K spectral length) seems feasible. Beyond that cameras get very challenging. RAS, 9th May 2008

16. HARMONI in context • No study of such an instrument for E-ELT carried out so far, although IRIS is part of TMT first-light suite • Currently no other visible wavelength spectroscopic capability planned for E-ELT (except for CODEX) • Preliminary ESO estimate of 9M€ hardware costs. RAS, 9th May 2008

17. HARMONI EAGLE IRIS NIRSpec Spectral Discovery Space MUSE RAS, 9th May 2008

18. Mapping: 35,000 spectra MUSE90,000 spectra EAGLE Single IFU: 441 spectra HARMONI, 16,000 spectra IRIS, 4096 spectra Spatial Discovery Space NIRSpec, 900 spectra RAS, 9th May 2008

19. Phase A Study Plan • Phase 1: March ‘08 — January ‘09 • We are conducting a scientific-technical trade-off to determine optimal instrument parameters in line with the instrument science cases developed by the science working group. At the end of phase 1 we will arrive at a single instrument concept to take forward into phase 2 • Investigate scientific drivers for optional modes: high spectral resolution (R≈15,000) and bluer minimum wavelength (0.6µm) • 2 science team meetings to date • Phase 2: February ‘09 — November ‘09 • We will detail the chosen instrument concept to an advanced conceptual design, together with a suggested management pathway to realise a complete instrument inline with E-ELT requirements. • Study review: December ‘09 RAS, 9th May 2008

20. Phase A Study Milestones RAS, 9th May 2008

21. Baseline Instrument Specifications RAS, 9th May 2008