MUSE Exposure Time Calculator

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Legacy version P95-phase2 (December 2014)
Provided for reference only!

This is not the normal ETC version www.eso.org/observing/etc

Optical AO Integral-Field Spectroscopy Mode Version 5.0.1

Description.

F.A.Q

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Target Flux Distribution

Target Spatial Distribution:

Infinitely Extended Source

Extended Uniform Source

Finite diameter:

arcsec (max 30)

Sersic profile

Radius inside which half of the luminosity is : If below 0".1 , a point source is assumed	arcsec (max 15)
Strength of decrease (0.5 to 10, 4=deVaucouleurs) :

Point Source

Distance from target center at which the S/N or exp.time must be computed:
Irrelevant for Infinitely Extended Source.
For other profiles, distance must be below source radius + 7".5 .

arcsec

Target Spectral Distribution and Brightness:

Uniform (constant with wavelength)

Target Magnitude and Mag.System:

=		Vega
		AB

Magnitudes are given per arcsec2 for extended
sources, and as the integral photometry for
point sources and Sersic profiles.

Magnitudes refer to the redshifted spectrum.

Blackbody:

Temperature : K

Template Spectrum:

Redshift
z =

Upload Spectrum:

Supported formats: FITS images and two-column ASCII,
with wavelength in nm units and ascending order,
and a flux unit proportional to erg/cm2/s/A.
The spectrum will be scaled to the given magnitude.

Single Line :

Lambda:	nm
Flux:	10-16 erg/s/cm2 (per arcsec2 for extended sources)
FWHM:	nm (minimum 0.25 nm)

Background Source Flux Distribution

Background Source Spatial Distribution:

None

Infinitely Extended Source

Extended Uniform Source

Finite diameter:

arcsec (max 30)

Sersic profile

Radius inside which half of the luminosity is : If below 0".1 , a point source is assumed	arcsec (max 15)
Strength of decrease (0.5 to 10, 4=deVaucouleurs) :

Point Source

Distance from background object center at which the S/N or exp.time must be computed:
Irrelevant for Infinitely Extended Source.
For other profiles, distance must be below source radius + 7".5 .

arcsec

Background Source Spectral Distribution and Brightness:

Uniform (constant with wavelength)

Background Source Magnitude and Mag. System:

=		Vega
		AB

Magnitudes are given per arcsec2 for extended
sources, and as the integral photometry for
point sources and Sersic profiles.

Magnitudes refer to the redshifted spectrum.

Blackbody:

Temperature : K

Template Spectrum:

Redshift
z =

Upload Spectrum:

Supported formats: FITS images and two-column ASCII,
with wavelength in nm units and ascending order,
and a flux unit proportional to erg/cm2/s/A.
The spectrum will be scaled to the given magnitude.

Single Line :

Lambda:	nm
Flux:	10-16 erg/s/cm2 (per arcsec2 for extended sources)
FWHM:	nm (minimum 0.25 nm)

Instrument Setup

Instrument Mode:
Number of coadded spatial pixels:
Number of coadded spectral pixels:

Sky Conditions

Moon Phase:	Days from new Moon
Airmass:

Seeing

This column: Values to be filled

This column: Outputs computed by the ETC and provided for information

WFM:

PSF fwhm at VLT focal plane:	arcsec
At the wavelength:	nm

Unit Telescope Seeing: arcsec. Supported UT seeing range: 0.45-1.9. NOTE! Use this UT seeing in the phase I proposal!
DIMM seeing (at given airmass):	arcsec
DIMM seeing (at Zenith):	arcsec
Probability of DIMM seeing:	%

Observation Setup

Reference Wavelength:	λref= nm. The numeric results will refer to this wavelength.
Wavelength range to plot:	λmin= nm λmax= nm

User provides S/N ratio and NDIT --- ETC returns DIT User provides S/N ratio and DIT --- ETC returns NDIT User provides NDIT and DIT --- ETC returns S/N ratio
S/N =	NDIT =	DIT = sec

The total exposure time is the product of DIT (Detector Integration Time) by NDIT (number of DITs). This exposure time does not take into account instrument and telescope overheads.

On submission the model can generate the following:

Plots: Toggle All / No Plots

	Peak Pixel values

	Target Spectrum, per Spectral Bin	Target Spectrum, per Spectral Pixel
		Sky Emission per Pixel
	Sky Transmission
	S/N per Spectral Bin	S/N per Pixel
	System Efficiency (excl.atmosphere)
	Target Input Spectrum in Physical Units
	Target Ensquared Energy

	Background Object per Spectral Bin	Background Object per Spectral Pixel
	Background Object Input Spectrum in Physical Units
	Background Object Ensquared Energy

FITS files: Toggle All / No FITS files

	PSFs (seven FITS files) at the interpolated seeings, at the seven reference wavelengths of the database

	Target Object (one FITS file)
	Target Images (seven FITS files) at the seven reference wavelengths of the database, ie. the Target convolved by the PSFs

	Background Object (one FITS file)
	Background Object Images (seven FITS files) at the seven reference wavelengths of the database, ie. the Background Object convolved by the PSFs