Input Flux Distribution

 



 Continuum (Flat Spectra)
 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)
GALEV Elliptical Galaxy
GALEV Sa Galaxy
GALEV Sb Galaxy
GALEV Sc Galaxy
GALEV Sd Galaxy
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
QSO
  Redshift Z = 

   Single line
	Wavelength:         nm
	Flux:               10-16 ergs/s/cm2 (per arcsec2 for extended sources)
	FWHM:               nm (Minimum value: 0.50)

 Object Magnitude:       		Band: 
U
B
V
R
I

 For De Vaucouleurs and Exponential profiles, the Projected Semi-Major Axis is intended
 as the Effective Radius along the slit.

Grism:             
	LR-Red - 751 nm (with OS-Red)
	LR-Blue - 482 nm (with OS-Blue)
	MR - 708 nm (with GG475)
	HR-Blue(new) - 402 nm (no OS filter)
	HR-Red - 740 nm (with GG475)
	HR-Orange - 631 nm (with GG435)

Slit:       width    length in arcsecs 

Detector: 
             
                High Gain
              
                

 S/N:			Value    Plotting range  %
 Exposure Time (s):	Value    Plotting range  %

  Flat Field Accuracy: 0.0  

On submission the model can generate the following graphs:
 
 Object Spectrum
 Sky Spectrum at central row
 Total spectrum (object+sky) at central row
 Input spectrum in physical units
 Total Efficiency and Wavelength Range
 Signal to noise versus wavelength

 2D simulated image