Input Flux Distribution

 Uniform (constant with wavelength)
 Blackbody: T =		 Kelvin
 Template Spectra:	
O5V   (Kurucz)
 O5V (Pickles)
 O9V (Pickles)
B1V   (Kurucz)
B2IV  (Pickles)
B3V   (Kurucz)
B8V   (Kurucz)
B9III (Pickles)
B9V (Pickles)
A0III (Pickles)
 A0V (Pickles)
A1V   (Kurucz)
F0V   (Kurucz)
G0    (Pickles)
G2V   (Kurucz)
K2V   (Pickles)
K7V   (Pickles)
M2V   (Pickles)
Planetary Nebula
HII Region (ORION)
Elliptical Galaxy
S0 Galaxy
Sa Galaxy
Sb Galaxy
Starburst Galaxy 1
Starburst Galaxy 2
Starburst Galaxy 3
Starburst Galaxy 4
Starburst Galaxy 5
Starburst Galaxy 6
E Galaxy (GALEV)
QSO
  Redshift Z = 

  Object Magnitude:       		Band: 
U
B
V
R
I


Magnitudes are given per square arcsec for extended sources. Note that some template spectra are 
defined over a limited wavelength range and may not allow calculations for all instrument configurations. 

The object magnitude is not taken into account for the following single line source
 Single line
	Wavelength:         nm
	Flux:               10-16 ergs/s/cm2 (per arcsec2 for extended sources)
	FWHM:               nm (Minimum value: 0.50)

Spatial Distribution:	 Point Source		 Extended Source
Sky Conditions
Days From New Moon: 
0 days3 days
7 days10 days
14 days
 Airmass:    Seeing:  arcsec
The sky brightness is determined by the moon phase and the instrument efficiency according to this table.

Instrumental Setup

Mirrors (3 aluminium coated mirrors): 65.00 % at 670 nm

Instrument optics : fixed

Results

 S/N:			Value    Plotting range  %
Exposure Time (s):	Value    Plotting range  %
On submission the model can generate the following graphs:
 
 Object Spectrum
 Sky Spectrum
 Input spectrum in physical units
 Signal-to-noise
 Total Efficiency and Wavelength Range
 2D simulated image



           











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