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E-ELT Spectroscopic Exposure Time Calculator

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This ETC is for E-ELT Spectroscopy. A detailed description is available in the E-ELT Spectroscopy ETC document.
For imaging, use the E-ELT Imaging ETC.

E-ELT Spectroscopic Mode Version 5.0.0
 
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Target Input Flux Distribution

Uniform (constant with wavelength)
Blackbody: T= K
Spectral Type (Pickles Model): (only U-K bands)
MARCS Stellar Model: [130nm - 20.0μm]


Target Brightness :
Vega mag = The input spectrum will be scaled to have this magnitude in the selected system.
AB mag
Flux mJy The input spectrum will be scaled have to this flux at the observing wavelength (λref) chosen below.

The magnitude or flux is given per square arcsec for extended sources.

Spatial Distribution:
Point Source
Extended Source


Telescope Setup

Observatory Site:
Telescope Diameter:

Sky Conditions

Seeing: arcsec (FWHM in V band)
Airmass:

Instrument Setup

AO Mode:  
Observing wavelength: band (λref):
λref: nm
The numeric results will refer to λref and the wavelength range of the graphs will be centered there.
Radius of circular S/N ref. area:
.i.e. over which the S/N is calculated.
mas (on the sky) DLC=1.22 λ/D is the radius of the diffraction limited PSF core for a D=42m telescope.
Number of spectra on the detector:
i.e. number of spatial elements (spaxel) in the S/N ref. area
Spectral resolution R=λ/Δλ: IMPORTANT: please consult the documentation when using R>100,000

Results

S/N ratio: S/N = DIT = sec
Exposure Time: NDIT =

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.


Plots: Toggle All / No Plots

Resultant spectrum including sky
Object Spectrum only
Sky Emission Spectrum
Sky Transmission Spectrum
S/N as a function of wavelength
System Efficiency and Wavelength Range
Input spectrum in physical units
 
Detailed S/N info
   

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