ADASS XVII - September, Software Modelling of IFU Spectrometers Nuria P. F. Lorente UK Astronomy Technology Centre Royal Observatory, Edinburgh, UK Alistair C. H. Glasse, Gillian S. Wright (UK ATC, JWST-MIRI), Suzanne Ramsay Howat (UK ATC, KMOS), Chris J. Evans (UK ATC, EELT)

ADASS XVII - September, Why do we need instrument simulators?

ADASS XVII - September, Why do we need instrument simulators? l Increasing scale and complexity of telescopes and instruments with time

ADASS XVII - September, Why do we need instrument simulators? l Increasing scale and complexity of telescopes and instruments with time l We need to know how design and construction changes may potentially affect the science we can do with the instrument

ADASS XVII - September, Why do we need instrument simulators? l Increasing scale and complexity of telescopes and instruments with time l We need to know how design and construction changes may potentially affect the science we can do with the instrument l Development of data reduction and analysis software requires test data

ADASS XVII - September, Why do we need instrument simulators? l Increasing scale and complexity of telescopes and instruments with time l We need to know how design and construction changes may potentially affect the science we can do with the instrument l Development of data reduction and analysis software requires test data l An understanding of the data products will help in designing effective calibration strategies

ADASS XVII - September, Why do we need instrument simulators? l Increasing scale and complexity of telescopes and instruments with time l We need to know how design and construction changes may potentially affect the science we can do with the instrument l Development of data reduction and analysis software requires test data l An understanding of the data products will help in designing effective calibration strategies l Synthetic data products are an effective communication tool in a distributed scientific and engineering environment

ADASS XVII - September, JWST-MIRI MRS Launch in 2013 Positioned at L2 4 instruments on board

ADASS XVII - September, JWST-MIRI MRS Launch in 2013 Positioned at L2 4 instruments on board Collaborative project between Consortium of 21 institutes under ESA NASA Imager, coronograph, low-resolution spectrometer, IFU medium resolution spectrometer

ADASS XVII - September, JWST-MIRI MRS 4 spectral channels (5 – 28 microns) FoV 3.70x3.70arcsec – 7.74x7.93 arcsec Spectral resolution ~3000 One IFU slicer per channel All channels are observed simmultaneously Dichroic filters divide each IFU channel into 3 sub- bands Data from pairs of channels are captured on two 1024x1024 pixel detectors Expected sensitivity 1.21e-20 Wm^-2, 6.4microns, 5.610e-20 W^m-2 at 22.5 microns

ADASS XVII - September, Specsim: Modelling the Field of View Specsim GUI

ADASS XVII - September, Specsim: Modelling the Field of View Specsim GUI Sky Background

ADASS XVII - September, Specsim: Modelling the Field of View Specsim GUI Sky Background Targets

ADASS XVII - September, Specsim: Modelling the Field of View Specsim GUI Sky Background Targets

ADASS XVII - September, Specsim: Modelling the Field of View Specsim GUI Sky Background Targets

ADASS XVII - September, Specsim: Modelling the Field of View Specsim GUI Sky Background Targets Sky Model

ADASS XVII - September, Specsim: Modelling the IFU Spectrometer

ADASS XVII - September, Specsim: Modelling the IFU Spectrometer Transmission Function Definitions

ADASS XVII - September, Specsim: Modelling the IFU Spectrometer Transmission Function Definitions

ADASS XVII - September, Specsim: Modelling the IFU Spectrometer Transmission Function Definitions Cosmic Rays Noise Exposure Length

ADASS XVII - September, Specsim: Modelling the IFU Spectrometer Transmission Function Definitions Cosmic Rays Noise Exposure Length

ADASS XVII - September, JWST-MIRI MRS Modelling Observations of a YSO (Glasse et al., in prep. 2007)

ADASS XVII - September, JWST-MIRI MRS Modelling Observations of a YSO (Glasse et al., in prep. 2007) Spitzer IRS spectrometer (Lahuis et al., 2006)

ADASS XVII - September, "IRS46 at 875 pc" N_TARGETS 1 { "Dither_A" N_CONT N_BROAD N_NARROW “NL1" “NL2"... } JWST-MIRI MRS Modelling Observations of a YSO (Glasse et al., in prep. 2007) Spitzer IRS spectrometer (Lahuis et al., 2006)

ADASS XVII - September, "IRS46 at 875 pc" N_TARGETS 1 { "Dither_A" N_CONT N_BROAD N_NARROW “NL1" “NL2"... } JWST-MIRI MRS Modelling Observations of a YSO (Glasse et al., in prep. 2007) Spitzer IRS spectrometer (Lahuis et al., 2006) Point source Black-body continuum CO2 Gaussian absorption feature, and silicate spectrum 360 narrow absorption lines (HCN etc.)

ADASS XVII - September, "IRS46 at 875 pc" N_TARGETS 1 { "Dither_A" N_CONT N_BROAD N_NARROW “NL1" “NL2"... } JWST-MIRI MRS Modelling Observations of a YSO (Glasse et al., in prep. 2007) Spitzer IRS spectrometer (Lahuis et al., 2006) Specsim synthetic spectrum Point source Black-body continuum CO2 Gaussian absorption feature, and silicate spectrum 360 narrow absorption lines (HCN etc.)

ADASS XVII - September, JWST-MIRI MRS Modelling Observations of a YSO (Glasse et al., in prep. 2007) Simulated detector image Simulated white-light images

ADASS XVII - September, VLT - KMOS NIR multi-object IFU spectrometer 3 identical channels 8 IFUs per channel 14 slices of 14 pixels per IFU 3 spectrographs 2048 x 2048 pixel detector images

ADASS XVII - September, VLT - KMOS “Emission line galaxy with 3 lines” N_TARGETS1 { “Galaxy continuum” N_CONT N_BROAD0 N_NARROW0 } “Emission line – different extent” N_CONT0 N_BROAD0 N_NARROW “Line1” “Line2” “Line3” }

ADASS XVII - September, VLT - KMOS White-light image of the galaxy Image of the galaxy at the wavelength of the emission line Portion of the detector image Note the spectral line and the galaxy continuum

ADASS XVII - September, Simulated field of view E-ELT Investigating the effect of adaptive optics on image quality

ADASS XVII - September, Simulated field of view E-ELT Seeing-limited PSF Investigating the effect of adaptive optics on image quality

ADASS XVII - September, Simulated white-light image, with no AO correction E-ELT Seeing-limited PSF Investigating the effect of adaptive optics on image quality

ADASS XVII - September, Simulated field of view Ground-layer correction PSF E-ELT Investigating the effect of adaptive optics on image quality

ADASS XVII - September, Simulated white-light image with ground-layer correction Ground-layer correction PSF E-ELT Investigating the effect of adaptive optics on image quality

ADASS XVII - September, Simulated field of view Laser Tomography PSF E-ELT Investigating the effect of adaptive optics on image quality

ADASS XVII - September, Simulated white-light image with laser-tomography correction E-ELT Laser Tomography PSF Investigating the effect of adaptive optics on image quality

ADASS XVII - September, E-ELT Seeing-limited field Ground layer correction only Laser-tomography Investigating the effect of adaptive optics on image quality