1. ADASS XVII - September, 2007 1 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)

2. ADASS XVII - September, 2007 2 Why do we need instrument simulators?

3. ADASS XVII - September, 2007 3 Why do we need instrument simulators? l Increasing scale and complexity of telescopes and instruments with time

4. ADASS XVII - September, 2007 4 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

5. ADASS XVII - September, 2007 5 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

6. ADASS XVII - September, 2007 6 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

7. ADASS XVII - September, 2007 7 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

8. ADASS XVII - September, 2007 8 JWST-MIRI MRS Launch in 2013 Positioned at L2 4 instruments on board

9. ADASS XVII - September, 2007 9 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

10. ADASS XVII - September, 2007 10 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

11. ADASS XVII - September, 2007 11 Specsim: Modelling the Field of View Specsim GUI

12. ADASS XVII - September, 2007 12 Specsim: Modelling the Field of View Specsim GUI Sky Background

13. ADASS XVII - September, 2007 13 Specsim: Modelling the Field of View Specsim GUI Sky Background Targets

14. ADASS XVII - September, 2007 14 Specsim: Modelling the Field of View Specsim GUI Sky Background Targets

15. ADASS XVII - September, 2007 15 Specsim: Modelling the Field of View Specsim GUI Sky Background Targets

16. ADASS XVII - September, 2007 16 Specsim: Modelling the Field of View Specsim GUI Sky Background Targets Sky Model

17. ADASS XVII - September, 2007 17 Specsim: Modelling the IFU Spectrometer

18. ADASS XVII - September, 2007 18 Specsim: Modelling the IFU Spectrometer Transmission Function Definitions

19. ADASS XVII - September, 2007 19 Specsim: Modelling the IFU Spectrometer Transmission Function Definitions

20. ADASS XVII - September, 2007 20 Specsim: Modelling the IFU Spectrometer Transmission Function Definitions Cosmic Rays Noise Exposure Length

21. ADASS XVII - September, 2007 21 Specsim: Modelling the IFU Spectrometer Transmission Function Definitions Cosmic Rays Noise Exposure Length

22. ADASS XVII - September, 2007 22 JWST-MIRI MRS Modelling Observations of a YSO (Glasse et al., in prep. 2007)

23. ADASS XVII - September, 2007 23 JWST-MIRI MRS Modelling Observations of a YSO (Glasse et al., in prep. 2007) Spitzer IRS spectrometer (Lahuis et al., 2006)

24. ADASS XVII - September, 2007 24 "IRS46 at 875 pc" N_TARGETS 1 { "Dither_A" 0 0.485 1.01 N_CONT 2 0 0.015 700.0 0 0.002 160.0 N_BROAD 2 0 -0.001 15.2 0.30 1 -0.014 N_NARROW 360 12.02300 -0.245 “NL1" 12.03510 -0.023 “NL2"... } JWST-MIRI MRS Modelling Observations of a YSO (Glasse et al., in prep. 2007) Spitzer IRS spectrometer (Lahuis et al., 2006)

25. ADASS XVII - September, 2007 25 "IRS46 at 875 pc" N_TARGETS 1 { "Dither_A" 0 0.485 1.01 N_CONT 2 0 0.015 700.0 0 0.002 160.0 N_BROAD 2 0 -0.001 15.2 0.30 1 -0.014 N_NARROW 360 12.02300 -0.245 “NL1" 12.03510 -0.023 “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.)

26. ADASS XVII - September, 2007 26 "IRS46 at 875 pc" N_TARGETS 1 { "Dither_A" 0 0.485 1.01 N_CONT 2 0 0.015 700.0 0 0.002 160.0 N_BROAD 2 0 -0.001 15.2 0.30 1 -0.014 N_NARROW 360 12.02300 -0.245 “NL1" 12.03510 -0.023 “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.)

27. ADASS XVII - September, 2007 27 JWST-MIRI MRS Modelling Observations of a YSO (Glasse et al., in prep. 2007) Simulated detector image Simulated white-light images

28. ADASS XVII - September, 2007 28 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

29. ADASS XVII - September, 2007 29 VLT - KMOS “Emission line galaxy with 3 lines” N_TARGETS1 { “Galaxy continuum” 10.0 0.0 2.0 0.6 50 N_CONT1 00.000003 2500.0 N_BROAD0 N_NARROW0 } “Emission line – different extent” 10.0 0.0 2.0 1.0 140.0 N_CONT0 N_BROAD0 N_NARROW3 1.190.0“Line1” 1.760.0“Line2” 2.2100.0“Line3” }

30. ADASS XVII - September, 2007 30 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

31. ADASS XVII - September, 2007 31 Simulated field of view E-ELT Investigating the effect of adaptive optics on image quality

32. ADASS XVII - September, 2007 32 Simulated field of view E-ELT Seeing-limited PSF Investigating the effect of adaptive optics on image quality

33. ADASS XVII - September, 2007 33 Simulated white-light image, with no AO correction E-ELT Seeing-limited PSF Investigating the effect of adaptive optics on image quality

34. ADASS XVII - September, 2007 34 Simulated field of view Ground-layer correction PSF E-ELT Investigating the effect of adaptive optics on image quality

35. ADASS XVII - September, 2007 35 Simulated white-light image with ground-layer correction Ground-layer correction PSF E-ELT Investigating the effect of adaptive optics on image quality

36. ADASS XVII - September, 2007 36 Simulated field of view Laser Tomography PSF E-ELT Investigating the effect of adaptive optics on image quality

37. ADASS XVII - September, 2007 37 Simulated white-light image with laser-tomography correction E-ELT Laser Tomography PSF Investigating the effect of adaptive optics on image quality

38. ADASS XVII - September, 2007 38 E-ELT Seeing-limited field Ground layer correction only Laser-tomography Investigating the effect of adaptive optics on image quality