&NL_MODEL		
!model_type='global average' :  mu is set to 1/sqrt(3) and f to 0.5 			    
!model_type='dayside average' : mu is set to 1/sqrt(3) and f to 1
!model_type='no average' : f and mu are set manually below
!lim_type= 'fixed TAU' : onlt taulim is considered (see below)
!lim_type= 'fixed P' : only Plim is considered (see below)
!-------------------------------------------------------
 model_type = 'global average',
 lim_type = 'fixed TAU'/
&NL_PLIM
! This is the limit pressure in cgs units (only for lim_type='fixed P')
!-------------------------------------------------------
 plim=8d6/
&NL_TAULIM
! This is the limit optical depth (only for lim_type='fixed tau')
!-------------------------------------------------------
 taulim=1d4/
&NL_MEAN
!This is valid only if 'no average' is choosen
!mu is the angle between the vertical and the substellar point mu=1 is the substellar point
!f is used for averaged (see model_type). For a given column atmosphere model at an angle mu, f=1
!-------------------------------------------------------
mu=1
ff=1/
&NL_COEFF_TYPE
!COEFF can be either "AUTO" to use the coefficients of Parmentier2013 or "USER" for user defined coefficients.If "AUTO" is choosen, the values of beta,gp,betav,gammav1,gammav2 are ignored.
!TiO is used only if COEFF are "AUTO". "TiO" is a solar composition atmosphere whereas if "NoTiO" is choosen, the TiO/VO is removed.
!STAR can only be "SUN" for now. As a future extension atmospheric coefficient specific for MDwarfs will be available.
 ALBEDO="AUTO"
 COEFF="AUTO"
 TiO="TIO" 
 STAR="SUN"/
&NL_COEFF
!A is the albedo of the planet, used only if ALBEDO="USER"
!betav determine the repartition of the stellar flux between the two visible bands. For betav=1 only the first visible band is considered. For betav=0 only the second band is considered
!gamma1 is the ratio between the visible opacity in the first visible band and the thermal opacity.
!gamma2 is the ratio between the visible opacity in the second visible band and the thermal opacity.
!beta sets the relative width of the lines in the thermal wavelenght. For 0<beta<0.5 correspond to opacities with line shape. 0.5<beta<1 correspond to oapcities with gap shapes.
!gp is the ratio of the thermal Planck mean opacity to the Rosseland mean opacity. Gp=1 correspond to grey thermal opacities.
 A=0.
 betav=0.
 gammav1=10
 gammav2=0.15
 beta=0.9
 gp=1.0001/  
&NL_NATM
!n_atm is the number of point for the atmospheric output. It doesn't affect the radius calculations.
 n_atm=100/
&NL_Radius
!photo_radius calculates of the photospheric radius if YES
!chord_radius calculates the transit radius if YES
!Rchord_precision='approximate' consider the opacity constant between the photospheric and the transit radius
!Rchord_precision='exact' perform an exact calculation for the transit radius. This can be very long and generally changes less than 1% from the approximate calculation.
!Ngamma=1 calculates the transit radius in the fist visible band
!Ngamma=2 calculates the transit radius in the second visible band
 photo_radius='YES'
 chord_radius='YES'
 Rchord_precision='approximate'
 Ngamma=1/