HARMONI:%20A%20single%20field,%20wide%20band,%20integral-field%20spectrograph%20for%20the%20E-ELT

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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

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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

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E-ELT instrument road mapSandro DOdorico,
Marseille Nov06
INSTRUMENT OBS.MODES FOCUS /AO WAVE RANGE(µm) FIELD PIXEL SIZE(mas) ?/d? PROMINENT SCIECE CASES REF STUDY
DL, NIR Imager imaging Nasm./LTAO , MCAO 0.9-2.5 gt30 4 wide, n. bands all ONIRICA _at_ OWL
Narrow Field Spectrograph spectroscopy Nasm./SCAO , LTAO 0.6-2.5 1/ 10 20 / 50 3000, 20000 all Not studied
High ResolutionVis Spectrograph spectroscopy Coude/ GLAO 0.4 -0.8 Point source 150000 C2, C7 CODEX
Planetary Imager Spectrograph imaging, spectroscopy Nasm/ EXAO 0.6-1.75 2 V 4 H gt Nyquist gt15 S3, S9 EPICS
NIR MOS Spectroscopy multiplex.20 Grav. Inv./ MOAO 0.8-2.5 gt 5 30 - 50 3000, 10000 C4, C10 WFSPEC, MOMSI
NIR MOS ,DL Spectroscopy multiplex 20 Grav. Inv. or Nas/MCAO 0.8-2.5 gt30 10 - 30 3000 , 20000 G4, G9 MOMSI
MIR Imager imaging (limited spectroscopy Nas or IF/ SCAO or LTAO Mar-20 30 6 - 20 w-n bands, S3, S9, S5, G9, C10 MIDIR
Narrow Field Spectrograph spectroscopy Nasm./SCAO , LTAO 0.6-2.5 1/ 10 20 / 50 3000, 20000 all Not studied

• 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

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• SPIFFI/SINFONI
• NIR 1.0-2.5µm
• 2000 spectra
• R 2000 - 4000
• 0.25 - 0.025
• 8x8 - 0.8x0.8
• VLT/SINFONI AO module

• SWIFT
• I/z 0.65-1.0µm
• 4000 spectra
• R 4000
• 0.235 - 0.08
• 22x10 - 7.5x3.5
• Palomar 5m / PALAO

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Initial instrument requirements

• Wavelength range
• Near-infrared 1-2.5µm
• Wide wave band favours slicer over lenslets à la
  Tiger
• Spectral resolving power
• R 4000
• one band (J, H, K) at a time
• Spaxel size and field-of-view
• 5mas to 50mas spaxel size
• 1-5 field-of-view
• 16,000 spectra (or 8 HAWAII 2k2 detectors)
• 128 x 128 square field
• 88 x 176 21 rectangular field
• Focus on slicer design
• Initially based on SWIFT de-magnifying image
  slicer design

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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
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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

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SWIFT slicer

• 4000 spectra
• 44 slices, 91 pixel long
• 0.47mm slice width
• 41 de-magnification
• Twin exit slits, 115mm length
• Flat slice and pupil mirrors
• Lenses for de-magnification

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Study-slicer
Top view
flatslicingmirrors
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Study-slicer
Side view
to spectrograph
flatpupilmirrors
flatslicingmirrors
from telescope/AO
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Single slicer

• 4,000 spaxels
• 44 slices, 88 pixel long
• 1.3mm slice width
• 101 de-magnification
• Exit slit length 260mm
• Flat slice and pupil mirrors
• Mirrors for de-magnification (cf lenses in
  SWIFT)

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Two slicers 8000 spectra
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Full slicer
260mm
57.2mm

• Four exit slits
• 41 aspect ratio on slicer due to 21 anamorphic
  pre-optics
• 21 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
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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

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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

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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.

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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.

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Spectral Discovery Space
MUSE
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Spatial Discovery Space
NIRSpec, 900 spectra
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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 (R15,000) 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

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Phase A Study Milestones
Milestone Date Location
Kick-off meeting 1st April 2008 Videocon
Sience team meeting 1 12th Mar 2008 Oxford
Consortium meeting 1 7th May 2008 Oxford
Science team meeting 2 8th May 2008 Oxford
Progress meeting 1 19th May 2008 Garching
Consortium meeting 2 15th July 2008 Oxford
Progress meeting 2 15th Sep 2008 Oxford
Science team meeting 3 16th Sep 2008 Oxford
Progress meeting 3 15th November
Phase 1 review 15th January (tbc) Garching
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Baseline Instrument Specifications
Field of view 5-10?, likely 21 format 100x200 spaxels
Spatial pixel scales At least 3 50 mas, 4 mas, 15 mas(TBD)
Wavelength range 0.8-2.4µm, visible extension
Spectral resolution 4000, 20000(?)
Simultaneous ? coverage 2K-4K spectra possible At least single band at medium/high res goal entire spectral range at once
IFU technology Image slicer? (best fill factor on detector)
Throughput gt35 average, incl. detector Q.E. (similar to SINFONI)
AO performance GLAO 3-5x gain in EE in 50 mas spaxel (abs. value 3.7 at K with GLAO!) LTAO K-60, J-20, NGS-19th mag. MCAO K-50(uniform), NGS-19th/20th
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The E-ELT focal stations

• HARMONI