adass xvii - september, 2007 1 software modelling of ifu spectrometers nuria p. f. lorente uk...
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ADASS XVII - September, 20071
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, 20073
Why do we need instrument simulators?
Increasing scale and complexity of telescopes and instruments with time
ADASS XVII - September, 20074
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, 20075
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, 20076
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, 20077
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, 20078
JWST-MIRI MRS
• Launch in 2013
• Positioned at L2
• 4 instruments on board
ADASS XVII - September, 20079
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, 200710
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, 200713
Specsim: Modelling the Field of ViewSpecsim GUI
Sky Background
Targets
ADASS XVII - September, 200714
Specsim: Modelling the Field of ViewSpecsim GUI
Sky Background
Targets
ADASS XVII - September, 200715
Specsim: Modelling the Field of ViewSpecsim GUI
Sky Background
Targets
ADASS XVII - September, 200716
Specsim: Modelling the Field of ViewSpecsim GUI
Sky Background
Targets
Sky Model
ADASS XVII - September, 200718
Specsim: Modelling the IFU Spectrometer
Transmission Function Definitions
ADASS XVII - September, 200719
Specsim: Modelling the IFU Spectrometer
Transmission Function Definitions
ADASS XVII - September, 200720
Specsim: Modelling the IFU Spectrometer
Transmission Function Definitions
Cosmic RaysNoise
Exposure Length
ADASS XVII - September, 200721
Specsim: Modelling the IFU Spectrometer
Transmission Function Definitions
Cosmic RaysNoise
Exposure Length
ADASS XVII - September, 200722
JWST-MIRI MRS
Modelling Observations of a YSO
(Glasse et al., in prep. 2007)
ADASS XVII - September, 200723
JWST-MIRI MRS
Modelling Observations of a YSO
(Glasse et al., in prep. 2007)
Spitzer IRS spectrometer (Lahuis et al., 2006)
ADASS XVII - September, 200724
"IRS46 at 875 pc"N_TARGETS 1{"Dither_A"0 0.485 1.01N_CONT 20 0.015 700.00 0.002 160.0N_BROAD 20 -0.001 15.2 0.301 -0.014N_NARROW 36012.02300 -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)
ADASS XVII - September, 200725
"IRS46 at 875 pc"N_TARGETS 1{"Dither_A"0 0.485 1.01N_CONT 20 0.015 700.00 0.002 160.0N_BROAD 20 -0.001 15.2 0.301 -0.014N_NARROW 36012.02300 -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.)
ADASS XVII - September, 200726
"IRS46 at 875 pc"N_TARGETS 1{"Dither_A"0 0.485 1.01N_CONT 20 0.015 700.00 0.002 160.0N_BROAD 20 -0.001 15.2 0.301 -0.014N_NARROW 36012.02300 -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.)
ADASS XVII - September, 200727
JWST-MIRI MRS
Modelling Observations of a YSO
(Glasse et al., in prep. 2007)
1B
2B
3B4B1B
2B
3B4B
Simulated detector image Simulated white-light images
ADASS XVII - September, 200728
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, 200729
VLT - KMOS“Emission line galaxy with 3 lines”
N_TARGETS 1
{
“Galaxy continuum”
1 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”
1 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”
}
ADASS XVII - September, 200730
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, 200731
Simulated field of view
E-ELT Investigating the effect of adaptive optics on image quality
ADASS XVII - September, 200732
Simulated field of view
E-ELT
Seeing-limited PSF
Investigating the effect of adaptive optics on image quality
ADASS XVII - September, 200733
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, 200734
Simulated field of view
Ground-layer correction PSF
E-ELT Investigating the effect of adaptive optics on image quality
ADASS XVII - September, 200735
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, 200736
Simulated field of view
Laser Tomography PSF
E-ELT Investigating the effect of adaptive optics on image quality
ADASS XVII - September, 200737
Simulated white-light image with laser-tomography correction
E-ELT
Laser Tomography PSF
Investigating the effect of adaptive optics on image quality