Alistair C. H. Glasse, Gillian S. Wright (UK ATC, JWST-MIRI),. Suzanne Ramsay ... ADASS XVII - September, 2007. 3. Why do we need instrument simulators?
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)
1 ADASS XVII - September, 2007
Why do we need instrument simulators?
2 ADASS XVII - September, 2007
Why do we need instrument simulators? z
Increasing scale and complexity of telescopes and instruments with time
3 ADASS XVII - September, 2007
Why do we need instrument simulators? z z
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
4 ADASS XVII - September, 2007
Why do we need instrument simulators? z z
z
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
5 ADASS XVII - September, 2007
Why do we need instrument simulators? z z
z z
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
6 ADASS XVII - September, 2007
Why do we need instrument simulators? z z
z z z
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
7 ADASS XVII - September, 2007
JWST-MIRI MRS
• Launch in 2013 • Positioned at L2 • 4 instruments on board
8 ADASS XVII - September, 2007
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
9 ADASS XVII - September, 2007
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 subbands • 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
10 ADASS XVII - September, 2007
Specsim: Modelling the Field of View Specsim GUI
11 ADASS XVII - September, 2007
Specsim: Modelling the Field of View Specsim GUI
Sky Background
12 ADASS XVII - September, 2007
Specsim: Modelling the Field of View Specsim GUI
Targets
Sky Background
13 ADASS XVII - September, 2007
Specsim: Modelling the Field of View Specsim GUI
Targets
Sky Background
14 ADASS XVII - September, 2007
Specsim: Modelling the Field of View Specsim GUI
Targets
Sky Background
15 ADASS XVII - September, 2007
Specsim: Modelling the Field of View Specsim GUI
Targets
Sky Background Sky Model
16 ADASS XVII - September, 2007
Specsim: Modelling the IFU Spectrometer
17 ADASS XVII - September, 2007
Specsim: Modelling the IFU Spectrometer
Transmission Function Definitions 18 ADASS XVII - September, 2007
Specsim: Modelling the IFU Spectrometer
Transmission Function Definitions 19 ADASS XVII - September, 2007
Specsim: Modelling the IFU Spectrometer
Cosmic Rays Noise Exposure Length
Transmission Function Definitions 20 ADASS XVII - September, 2007
Specsim: Modelling the IFU Spectrometer
Cosmic Rays Noise Exposure Length
Transmission Function Definitions 21 ADASS XVII - September, 2007
JWST-MIRI MRS Modelling Observations of a YSO
(Glasse et al., in prep. 2007) 22 ADASS XVII - September, 2007
JWST-MIRI MRS Modelling Observations of a YSO
Spitzer IRS spectrometer (Lahuis et al., 2006)
(Glasse et al., in prep. 2007) 23 ADASS XVII - September, 2007
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" ... }
ADASS XVII - September, 2007
(Glasse et al., in prep. 2007) 24
JWST-MIRI MRS Modelling Observations of a YSO
Spitzer IRS spectrometer (Lahuis et al., 2006) Point source
CO2 Gaussian absorption feature, and silicate 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" ... }
ADASS XVII - September, 2007
Black-body continuum
360 narrow absorption lines (HCN etc.) (Glasse et al., in prep. 2007) 25
JWST-MIRI MRS Modelling Observations of a YSO
Spitzer IRS spectrometer (Lahuis et al., 2006) Point source
CO2 Gaussian absorption feature, and silicate 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" ... }
Specsim synthetic spectrum
ADASS XVII - September, 2007
Black-body continuum
360 narrow absorption lines (HCN etc.) (Glasse et al., in prep. 2007) 26
JWST-MIRI MRS Modelling Observations of a YSO
1B 3B
4B
2B
Simulated detector image
Simulated white-light images
(Glasse et al., in prep. 2007) 27 ADASS XVII - September, 2007
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
28 ADASS XVII - September, 2007
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 0
1
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”
}
29 ADASS XVII - September, 2007
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
30 ADASS XVII - September, 2007
E-ELT
Investigating the effect of adaptive optics on image quality
Simulated field of view 31 ADASS XVII - September, 2007
E-ELT
Investigating the effect of adaptive optics on image quality
Seeing-limited PSF
Simulated field of view 32 ADASS XVII - September, 2007
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
33
E-ELT
Investigating the effect of adaptive optics on image quality
Ground-layer correction PSF
Simulated field of view 34 ADASS XVII - September, 2007
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
35
E-ELT
Investigating the effect of adaptive optics on image quality
Laser Tomography PSF
Simulated field of view 36 ADASS XVII - September, 2007
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
37
E-ELT
Investigating the effect of adaptive optics on image quality
• Seeing-limited field
• Ground layer correction only
• Laser-tomography 38 ADASS XVII - September, 2007
