The description of parameters rarely used:  &HParam data
----------------------------------------------------------

<<AnihiE>>   real*8 
 If E(positron) $<$ AnihiE, annihilation is considered. 

<<AtmosFile>>   character*100 
 path to the atmospheric data as in 'Cosmos/Data/Atmos/stdatmos2.d' 

<<BackAngLimit>>   real*8 
 If the cosine of the angle between a particle and the primary becomes smaller than 
 this value, the particle is discarded. See also BorderHeighH. If you give a value 
 less than -1.0, such rejection will never happen. Default is -1.0 

<<BaseErg>>   real*8 
 See BaseTime. The default is 1000 (GeV). 

<<BasePower>>   real*8 
 See BaseTime. Default is 1.0 

<<BorderHeightH>>   real*8 
 If a particle goes higher than this, discard it. This should be larger than 
 HeightOfInj or 0. 
 If 0, it is adjusted to be the same as HeightOfInj. NOTE: For upgoin primary cases, you have 
 to set this one explicitly. 

<<BorderHeightL>>   real*8 
 If a particle reaches this hight, call observation routine. No further tracking is done. 
 This is for neutrino observation. See ObsPlane. 

<<Cekaon>>   real*8 
 Obsolute 

<<Ceneuc>>   real*8 
 \verb| p -> n ; n-> p; p~->n~; n~->p~| prob. 

<<Cepic0>>   real*8 
 Obsolute 

<<Charge2heavyG>>   integer 
 charge of heavy $\rightarrow$ heavy group index conversion array. 

<<Code2heavyG>>   integer 
 particle code $\rightarrow$ heavy group index conversion array. 

<<Code2massN>>   integer 
 particle code $\rightarrow$ mass number conversion array. 

<<Deltkp>>   real*8 
 k-p xsection increases as $E^{Deltkp}$ (E$>$ 100GeV) 

<<Deltpip>>   real*8 
 pi-p xsection increases as $E^{Deltpip}$ (E$>$ 100GeV) 

<<Deltpp>>   real*8 
 p-p xsection increases as $E^{Deltpp}$(E$>$ 100GeV) 

<<DpmFile>>   character*70 
 control card to specify the dpmjet execution conditions. If ' ', 
 Cosmos/Data/DPM/atmos.inp is assumed. 

<<Ecrit>>   real*8 
 Critical energy in GeV. \newline 
 Employed only when calculating air shower size in the hybrid 
 air shower generation. The value would be dependent on the 
 experimental purpose. The default value, 81 MeV, is bit too 
 small in many applications (The air shower size is overestimated). 
 Comparisons of sizes by the hybrid method and by the full Monte 
 Carlo tell that \newline 
 $N_e$ (full 3-D M.C) $ < N_e$ (hybrid AS with $E_c=81$ MeV ) $ < N_e$ (full 1-D M.C) 
 $ {\ \lower-1.2pt\vbox{\hbox{\rlap{$<$}\lower5pt\vbox{\hbox{$\sim$}}}}\ } 
 N_e$(hybrid AS with $E_c={76}$ MeV) at around shower maximum. 
 Hybrid AS is always essentially 1-D. 

<<Efermi>>   real*8 
 If Kinetic E $<$ Efermi, Fermi Momentum is considered for Nucleus target.\\ 

<<Elund2>>   real*8 
 obsolete (from v6.0) 

<<Elund3>>   real*8 
 obsolete (from v6.0). 

<<Elund>>   real*8 
 obsolete (from v6.0) 

<<EndLevel2>>   integer 
 Don't worry. This is system use. 

<<EndLevel>>   integer 
 Used for skeleton/flesh-out job. In a normal job, system default value 0 is reset by 
 the system to be the max number of observation levels. (=NoOfSites). Its real use is in such a 
 skeleton/flesh-out job that one first follows the particles up to some high depth and later chooses 
 events and flesh them out to deeper depths. In such a skeleton-making job, the user must give the 
 depth list which is used flesh-out job, too. In the skeleton job, particle tracking is terminated 
 at the level specified by EndLevel. In such a flesh-out job, the user must give a larger value 
 or 0 to EndLevel 

<<ErrorOut>>   integer 
 Error output logical dev number. 

<<Es>>   real*8 
 Modified scattering constant. 19.3d-3 GeV 

<<Eta2Pi0>>   real*8 
 eta/pi0 ratio. this is used to see the effect due to non-decay of pi0 
 at very high energies. Only source of h.e gamma can be eta and LPM may work 
 for them. default is 0.2 

<<EthinRatio>>   real*8 
 if ThinsSamplig 
= F, thin sampling is performed if the energy of a particle is 
 $<$ EthinRatio * PrimaryEnergy(/nucleon) (=Ethin) ( EtinRatio$>$ 0). 
 If EthinRatio $<$ 0, Ethin will be |EthinRatio| (GeV). 

<<EventNo>>   integer 
 cumulative event number counter.(excluding discarded ones due to cutoff). 

<<EventsInTheRun>>   integer 
 Counter for event number in the run. Internal use. 
 (excluding discarded ones due to cutoff). 

<<ExactThick>>   logical 
 If T, a given length is converted into thickness with best accuracy even for very 
 inclined trajectory by using numerical integration. 

<<FragmentTbl>>   real*8 
 tbl(i,j)=$<$Number$>$ of frag. j when a heavy of heavy group index i 
 breaks up at air. 

<<Generate2>>   character*16 
 don't touch this. for skeleton/flesh use. 

<<GeomagFile>>   character*70 
 IGRF or WMM file path which contains geomagnetic field expansion 
 coefficients. Their format is the same one as given in their web 
 page. If ' ' (default), Cosmos/Data/Geomag/igrf is used. 

<<HeavyG2charge>>   integer 
 heavy group index $\rightarrow$ charge of heavy conversion array. 

<<HeavyG2code>>   integer 
 heavy group index $\rightarrow$ particle code conversion array. 

<<HeavyG2massN>>   integer 
 heavy group index $\rightarrow$ mass number conversion array. 

<<HeavyG2symbol>>   character*4 
 heavy group index $\rightarrow$ 'Fe' etc conversion array. 

<<HowGeomag>>   integer 
 if 1, no magnetic field until first coll. \newline 
 2, mag.f always exists. If Reverse not=0, use this. \newline 
 11, same as 1 but mag.f is const. \newline 
 12, same as 2 but mag.f is const. \newline 
 21, same as 1 but mag.f is const. \newline 
 22, same as 2 but mag.f is const. \newline 
 31, same as 1 but mag.f is dependent on the position. \newline 
 const value is the one at deepest observation plane. for 11,12 or should be given by 
 MagN, MagE, MagD for 21, 22. For normal applications, 11 is good. 
 If no magnetic field is applied, energy loss by dE/dx is considered.(bef.4.92, 
 and aft. 5.14) 

<<HowIntNuc>>   integer 
 If 0, the number of interacting nucleons among a projectile heavy nucleus is 
 determined as the number of first collision of each interacting nucleon inside 
 the nucleus. If 1, the number is determined as the total number of collisions 
 including successive interactions. Default is 1. (There is uncertaninity in 
 interpretation of the formula; value 1 gives larger number of interacting 
 nucleons.) 

<<InclusiveFile>>   character*100 
 The path to the inclusive data file, xdist.d. Default is 
 "../Contrib/Inclusive/xdist.d" 

<<IncreaseXsec>>   real*8 
 how the xsection increases. 1.0$\rightarrow$ power of E 

<<KEminObs2>>   real*8 
 Don't touch this. skeleton/flesh use. 

<<KnockOnRatio>>   real*8 
 KnockOnRatio* KEminoObs is used instead of RecoilKineMinE if KnockOnRatio $<$1. 

<<Knockon>>   logical 
 Obsolete. Don't use this. See RecoilKineMinE 
 and KnockonRatio. 

<<Kpicns>>   real*8 
 See Kpilog. 0.077 

<<Kpilog>>   real*8 
 K$_{ch}/\pi_{ch}$=(Kpilog*log(ss+.069)+Kpicns)*exp(-8/s') where ss(GeV**2)= 
 effective s. s'(GeV**2)=s - 4.63. See also Kpicns. 

<<LamorDiv>>   real*8 
 In the geomagnetic field, a charged particle can travel almost streight 
 in (Lamor Radius)/LamorDiv. Default is 5. For AMS like tracking 20 may be needed. 

<<LpmBremEmin>>   real*8 
 The LPM effect is taken into account for bremsstrahlung when LpmEffect is .true. 
 and the electron energy is higher than this. 

<<LpmPairEmin>>   real*8 
 The LPM effect is taken into account for pair creation when LpmEffect is .true. 
 and the gamma energy is higher than this. 

<<LundPara>>   integer 
 To control Lund program. LundPara(1) is set to kfr(7); kfr(7)=1 is for Frititof 
 hard scattering. 2 is for Pythia H.S. 2 gives higher multiplicity but shape is 
 strange. Default is 1. LundPara(2) is set to kfr(12): 1 by for OPAL hard scattering 
 parameterization. 2 by DELPHI. Default is 2. (2 gives bit higher PT). LundPara(3) 
 $>$ 0 $\Rightarrow$ Pythia message will appear. LundPara(4) $>$ 0 Fritiof 
 message; both on ErrorOut. LundPara(5) =0 $\Rightarrow$ All kaons collisions 
 are treated as pi- in Fritiof, else they are treated by adhoc model as they are. 

<<MagBrem>>   integer 
 If 0, no magnetic bremsstrahlung is considered. \newline 
 if 1 and Ee $>$ MagBremEmin, energy loss due to magnetic brems is considered \newline 
 if 2 and Ee $>$ MagBremEmin, real sampling of gamma is performed. \newline 
 (note, actually upsilon is referred further). 
 if generate='as' with really high energy primaries, WaitRatio 
 must be made small so that WaitRatio*E0 $\sim$ MagBremEmin 

<<MagBremEmin>>   real*8 
 E $>$ this, magnetic bremsstrahlung by electrons may be considered. However, if 
 MagBrem = 0, not considered at all \newline 
 MagBrem = 1, total energy loss due to brems is considered. \newline 
 MagBrem = 2, gamma energy is sampled actually. \newline 
 If upsilon (Ee/m * B/Bcr) is small, the effective treatment will be 
 the same as MagBrem = 0 case. 

<<MagChgDist>>   real*8 
 Distance where mag. can be seen as const.(m) at sea level 

<<MagD>>   real*8 
 See HowGeomag (in Tesla) 

<<MagE>>   real*8 
 See HowGeomag (in Tesla) 

<<MagN>>   real*8 
 See HowGeomag (in Tesla) 

<<MagPair>>   integer 
 If 0, no magnetic pair creation is considered. \newline 
 if 1 and Eg > MagPairEmin, real sampling is tried. 
 (note, actually upsilon is referred further). To see these magnetic effects, 
 HowGeoMag=2 and HightOfInj $\sim$ 5000 km are desirable. 

<<MagPairEmin>>   real*8 
 E $>$ this, magnetic pair creation by gamma may be considered. However, if 
 MagPair = 0, not considered at all. \newline 
 MagPair = 1, pair creation is sampled. \newline 
 However, again, actual occurrence will be dependent on the angle between 
 B and photon direction. 

<<MaxComptonE>>   real*8 
 Above this energy, Compton scattering is neglected. 

<<MaxPhotoE>>   real*8 
 Above this energy, photoelectric effect is neglected. 

<<Moliere>>   integer 
 0$\rightarrow$ use Gaussian approx always (with air density change and 
 energy loss effect)\newline 
 1$\rightarrow$ use Moli\`ere scattering for non-electrons (default)\newline 
 2$\rightarrow$ use Moli\`ere scattering for all charged particles.\newline 
 If negative, anglular-correlated displacement is made to be 0 since Moli\`ere 
 theory cannot give it. (if $>0$, we use Gaussian approximation for correlation). 

<<MuBr>>   integer 
 parameter similar to MuNI but for bremsstrahlung by muons. 

<<MuNI>>   integer 
 0$\rightarrow$ nuclear interaction of muon is completely neglected \newline 
 1$\rightarrow$ energy loss by n.i is subsumed in dE/dx of muons as a continuous energy loss. Let v= 
 Etransfer/Emu, the loss here is Int(vc:vmax) of (Emu vdsigma/dv). (vc $\sim$0, vmax$\sim$1). \newline 
 2$\rightarrow$ (Default value). similar to 1 but as the continuous loss only v $<$ vmin=10$^{-3}$ of 
 fractional muon energy is subsumed (Int(vc: vmin) of (Emu vdsigma/dv)). The portion 
 of loss by v$>$vmin is treated as a stocastic process. However, the product from the 
 n.i itself is neglected \newline 
 3$\rightarrow$ the same as 2, but the n.i is explicitly included to produce a number of particles. 
 The n.i is treated as a photo-nucleus interaction. 

<<MuPr>>   integer 
 parameter similar to MuNI but for pair creation by muons. 

<<Mudirp>>   real*8 
 \verb| DD~| \# enhancement factor. D is only for prompt muon. 

<<MulLow>>   integer 
 if 1, QCD predicted multiplicity law is used in the adhoc model else UA5 
 parametalization is used. Default is 1. (from v5), 
 0.6135exp(23/18sqrt(2log(roots/0.3))) is QCD jet prediction. 
 7.2roots**0.254 -7 is UA5 data. The branch point is set at roots = 900 GeV. 
 (I have adjusted 0.6135 so that 900 GeV is the b.p) 

<<NoOfSites2>>   integer 
 No of Sites for particle observation; not to be touched; for skeleton/flesh use. 

<<OffsetHeight>>   real*8 
 The vertical offset height from the deepest detector. 
 The primary is directed to this height above the detector. 
 If ObsPlane is 3 (spherical), not used. 

<<PathLimit>>   real*8 
 If the sum of (path/beta) of a particle exceeds this, it is judged as dead. 
 (to avoid infinite cyclotron loop). However, for normal applications, 
 this will not be effective because of BackAnglLimit. See Reverse. 
 TimeStructure should be T if Reverse 
= 0 and PathLimit is to be effective. 

<<PrevEventNo>>   integer 
 The event number already finished. System use for Cont job. 
 (excluding discarded ones due to cutoff). 

<<PtAvFrag>>   real*8 
 $<$Pt$>$ of heavy fragments. 

<<PtAvNonInteNuc>>   real*8 
 $<$Pt$>$ of non interacting nucleons. 

<<RatioToE0>>   real*8 
 In the A.S generation, hadronic interactions are followed down to at 
 least RatioToE0 * E0/nucleon energy. 

<<RecoilKineMinE>>   real*8 
 Recoil Kinetic Min Energy above which the recoil (=knock-on process) 
 is treated. Below this energy, the effect is included as continuous 
 energy loss. Used only if KnockOnRatio $>$ 1. 
 See also KnockOnRatio. 

<<Reverse>>   integer 
 0$\rightarrow$ Normal tracking. \newline 
 1$\rightarrow$ incident is tracked to a direction opposite to the given one. 
 the incident is charge-conjugated. 
 All interactions are ignored. (Use when to make cut-off table or to see 
 a given particle (say, observed anti proton) can go out of Earth. \newline 
 2$\rightarrow$ same as 1 but energy gain (not loss) is taken into account 
 TimeStructure should be T if Reverse 
= 0. See BackAnglLimit. 

<<SeedFileDev>>   integer 
 logical device number of SeedFile. 

<<SucInt>>   integer 
 The number of successive interactions inside A is affected by this parameter.\newline 
 If $0\rightarrow$ old formula (before uv3.500) is used, which give rather 
 smaller number ($<Nsuc>$ in Air = 1.7 for 30 mb pp), \newline 
 if $1\rightarrow$ new one $<Nsuc>=2.2$ for 30 mb pp). \newline 
 Default is 0 (from V5.00 again). 

<<SucPw>>   real*8 
 In the 2nd, 3rd,.. collision of a nucleon inside a nucleus, the collision is 
 made to be more elastic than normal one. The leading particle spectrum is 
 sampled from x**SucPw dx. SucPw should be in 1 to 2. 

<<TempDev>>   integer 
 Logical Dev. number for temporary disk use. 

<<TraceDev>>   integer 
 Logical dev \# for TraceDir/trace1,2,.... 

<<Truncc>>   real*8 
 coeff. for truncating path. 

<<Truncn>>   real*8 
 coeff. for truncating path. 

<<Truncx>>   real*8 
 coeff. for truncating path. 

<<UpsilonMin>>   real*8 
 Magnetic bremsstralhung is considered only if upsilon $>$ UpsilonMin. 

<<UseRungeKutta>>   integer 
 How to calculate deflection by the geomagnetic field. Let L be the distance 
 the particle travels. \newline 
 0$\rightarrow$Don't use RungeKutta method. Use the solution assuming the constant B, which 
 is exact if B is const. Since the particle path is made short, this is 
 enough for normal cases where particles are inside the atmosphere.(default) \newline 
 In every case below, if the particle height is $<$ 30km 
 (= cheight in ccomPathEnd.f), the same method as 0 is used. \newline 
 1$\rightarrow$ Use the Euler method. Time needed is 20% more than the 0 case. 
 As B, use the value at L/2 point obtained by using the current direction. \newline 
 2$\rightarrow$ mixture of 1 and Runge-Kutta-Gill method. If gradient of B is large, RKG is 
 employed. This needs $\sim$4 times more cpu time than case of 1 when making a 
 cutoff table. The step size of RKG is $\sim$1/10 of the Lamore radius. \newline 
 3$\rightarrow$ The same as 2 but use the Runge-Kutta-Fehlberg method instead of RKG. 
 Step size is automattically adjusted ($\sim$1/20 $\sim$1/30 of Lamor radius) \newline 
 4$\rightarrow$ As a middle point, use the point obtained by assuming the constant B at 
 initial point. If grad B is still large, use RKG. \newline 
 5$\rightarrow$ The same as 4 but us RKF instead of RKG. \newline 
 6$\rightarrow$ Use always RKG \newline 
 7$\rightarrow$ Use always RKF. This takes very long time.(50 times of 0). \newline 

<<UserHookc>>   character*100 
 array size is MAX\_USERHOOKC(=5). Usage is left for the user. To get the i-th 
 component, the use may 'call cqUHookc(i, cv)' in the userHook routine, 
 where cv is a character variable to receive the data. 

<<UserHooki>>   integer 
 array size is MAX\_USERHOOKI(=10). Usage is left for the user. To get the i-th 
 component, the use may 'call ccqUHooki(i, iv)' in the userHook rouitne, 
 where iv is an integer varialbe to receive the data. 

<<UserHookr>>   real*8 
 array size is MAX\_USERHOOKR(=10). Usage is left for the user. To get the i-th 
 component, the use may 'call cqUHookr(i, rv)' in the userHook routine, 
 where rv is a real*8 variable to receive the data. 

<<X0>>   real*8 
 Radiation length in kg/m$^2$ for air. Normally the user should not touch this. 

<<XaxisFromSouth>>   real*8 
 Angle between the horizontal detector X-axis and the south(deg). + is counter 
 clockwise. If $|$XaxisFromSouth$| > 360$, it is computed so that the direction is 
 to the magnetic east at the deepest observation point. Default is 361. 

