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, 20072

Why do we need instrument simulators?

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, 200711

Specsim: Modelling the Field of ViewSpecsim GUI

ADASS XVII - September, 200712

Specsim: Modelling the Field of ViewSpecsim GUI

Sky Background

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, 200717

Specsim: Modelling the IFU Spectrometer

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

ADASS XVII - September, 200738

E-ELT

• Seeing-limited field

• Ground layer correction only

• Laser-tomography

Investigating the effect of adaptive optics on image quality