0.1             ! COSPOL0BS=COS(POLAR) ; FOR OBSERVER
3               ! NSUN ; NUMBER OF SUNS
0.2      00.    ! {COSPOLSUN, AZIMUTH}={COS(POLAR), AZIMUTH[deg]} ; FOR SUN(1), NSUN ROWS ARE NEEDED
0.2      90.    ! {COSPOLSUN, AZIMUTH}={COS(POLAR), AZIMUTH[deg]} ; FOR SUN(2), NSUN ROWS ARE NEEDED
0.2     180.    ! {COSPOLSUN, AZIMUTH}={COS(POLAR), AZIMUTH[deg]} ; FOR SUN(3), NSUN ROWS ARE NEEDED
2000000000      ! NPH
1.D-6           ! WEIGHTMIN
1.D0            ! DXSLAB 
1.D0            ! TAU 
0.99D0          ! SSA 
0.1D0           ! ALBGR 
'./phF_L13.txt' ! FILE WITH SCATTERING MATRIX ELEMENTS, THETAD, A1,A3,B1,B2 
1800            ! NTHETAD 
4000            ! NTHETAI 

NOTES
-----

ANGLES. REFERRING TO FIGURE 5 OF GARCIA MUÑOZ & MILLS, A&A, 2014:
	* POLAR ANGLES ARE DEFINED WITH RESPECT TO THE UPWARDS DIRECTION.
	* AZIMUTH = AZIOBS - AZISUN. 

NSUN IS THE NUMBER OF SIMULTANEOUS SUNS CONSIDERED IN THE SIMULATION. 
	
NPH IS THE TOTAL NUMBER OF PHOTONS TO FINISH THE SIMULATION

WEIGHTMIN IS THE PHOTON'S RESIDUAL WEIGHT BELOW WHICH IT IS CONSIDERED THAT THE PHOTON
DOES NOT CONTRIBUTE FURTHER TO THE OUTPUT SOLUTION. 

DXSLAB IS THE GEOMETRICAL THICKNESS OF THE ATMOSPHERIC SLAB.

TAU IS THE OPTICAL THICKNESS OF THE ATMOSPHERIC SLAB.

SSA IS THE SINGLE SCATTERING ALBEDO OF THE MEDIUM.

ALBGR IS THE GROUND ALBEDO, ASSUMING LAMBERTIAN REFLECTION AT THE BOTTOM BOUNDARY.

'./phF_hazeL.txt' (OR SIMILAR) IS THE PATH+FILE NAME OF THE FILE THAT CONTAINS
THE ELEMENTS OF THE SCATTERING MATRIX. THIS FILE MUST CONTAIN 5 COLUMNS OF LENGTH
NTHETAD+1. FROM LEFT TO RIGHT, THE COLUMNS STAND FOR: 
	SCATTERING ANGLE // A1 // A3 // B1 // B2.

NTHETAI CONTROLS THE ANGULAR RESOLUTION IN THE FTHETA FUNCTION. 
NTHETAI MUST BE LARGE WHEN THE SCATTERING PROPERTIES OF THE MEDIUM ARE COMPLEX. 
ALL THE CALCULATIONS SHOWN IN THE MANUSCRIPT ADOPT NTHETAI=1000, EXCEPT FOR THE L=60 
PARTICLES FROM TABLES D9-D16 IN WHICH CASE, NTHETAI=4000.