Software Modelling of IFU Spectrometers

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) ADASS XVII - September, 2007

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

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

4. Why do we need instrument simulators? • Increasing scale and complexity of telescopes and instruments with time • We need to know how design and construction changes may potentially affect the science we can do with the instrument ADASS XVII - September, 2007

5. Why do we need instrument simulators? • Increasing scale and complexity of telescopes and instruments with time • We need to know how design and construction changes may potentially affect the science we can do with the instrument • Development of data reduction and analysis software requires test data ADASS XVII - September, 2007

6. Why do we need instrument simulators? • Increasing scale and complexity of telescopes and instruments with time • We need to know how design and construction changes may potentially affect the science we can do with the instrument • Development of data reduction and analysis software requires test data • An understanding of the data products will help in designing effective calibration strategies ADASS XVII - September, 2007

7. Why do we need instrument simulators? • Increasing scale and complexity of telescopes and instruments with time • We need to know how design and construction changes may potentially affect the science we can do with the instrument • Development of data reduction and analysis software requires test data • An understanding of the data products will help in designing effective calibration strategies • Synthetic data products are an effective communication tool in a distributed scientific and engineering environment ADASS XVII - September, 2007

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

9. JWST-MIRI MRS • Collaborative project between • Consortium of 21 institutes under ESA • NASA • Imager, coronograph, low-resolution spectrometer, IFU medium resolution spectrometer • Launch in 2013 • Positioned at L2 • 4 instruments on board 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 ADASS XVII - September, 2007

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

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

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

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

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

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

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

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

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

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

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

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

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

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

25. JWST-MIRI MRS Modelling Observations of a YSO Spitzer IRS spectrometer (Lahuis et al., 2006) "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" ... } Point source Black-body continuum CO2 Gaussian absorption feature, and silicate spectrum 360 narrow absorption lines (HCN etc.) (Glasse et al., in prep. 2007) ADASS XVII - September, 2007

26. JWST-MIRI MRS Modelling Observations of a YSO Spitzer IRS spectrometer (Lahuis et al., 2006) Specsim synthetic spectrum "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" ... } Point source Black-body continuum CO2 Gaussian absorption feature, and silicate spectrum 360 narrow absorption lines (HCN etc.) (Glasse et al., in prep. 2007) ADASS XVII - September, 2007

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

29. “Emission line galaxy with 3 lines” • N_TARGETS 1 • { • “Galaxy continuum” • 0.0 0.0 2.0 0.6 50 • N_CONT 1 • 0 0.000003 2500.0 • N_BROAD 0 • N_NARROW 0 • } • “Emission line – different extent” • 0.0 0.0 2.0 1.0 140.0 • N_CONT 0 • N_BROAD 0 • N_NARROW 3 • 1.1 90.0 “Line1” • 1.7 60.0 “Line2” • 2.2 100.0 “Line3” • } VLT - KMOS ADASS XVII - September, 2007

30. VLT - KMOS • White-light image of the galaxy • Portion of the detector image • Note the spectral line and the galaxy continuum • Image of the galaxy at the wavelength of the emission line ADASS XVII - September, 2007

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

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

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

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

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

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

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

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