tphysvar goft(const tphysvar logT, const tphysvar logrho, const cube gofttab)
{
// uses the log(T), because the G(T) is also stored using those values.
typedef CGAL::Delaunay_triangulation_2<K> Delaunay_triangulation;
typedef CGAL::Interpolation_traits_2<K> Traits;
typedef K::FT Coord_type;
typedef K::Point_2 Point;
std::map<Point, Coord_type, K::Less_xy_2> function_values;
typedef CGAL::Data_access< std::map<Point, Coord_type, K::Less_xy_2 > > Value_access;
tgrid grid=gofttab.readgrid();
tphysvar tempgrid=grid[0];
tphysvar rhogrid=grid[1];
tphysvar goftvec=gofttab.readvar(0);
// put the temperature and density grid from the gofttab into the CGAL data structures
vector<Point> delaunaygrid;
Point temporarygridpoint;
tphysvar::const_iterator tempit=tempgrid.begin();
tphysvar::const_iterator rhoit=rhogrid.begin();
tphysvar::const_iterator goftit=goftvec.begin();
for (; tempit != tempgrid.end(); ++tempit)
{
temporarygridpoint=Point(*tempit,*rhoit);
delaunaygrid.push_back(temporarygridpoint);
function_values.insert(std::make_pair(temporarygridpoint,Coord_type(*goftit)));
++rhoit;
++goftit;
}
Value_access tempmap=Value_access(function_values);
// compute the Delaunay triangulation
Delaunay_triangulation DT;
DT.insert(delaunaygrid.begin(),delaunaygrid.end());
tphysvar g;
int ng=logT.size();
// the reservation of the size is necessary, otherwise the vector reallocates in the openmp threads with segfaults as consequence
g.resize(ng);
cout << "Doing G(T) interpolation: " << flush;
// If MPI is available, we should divide the work between nodes, we can just use a geometric division by the commsize
int commrank,commsize;
#ifdef HAVEMPI
MPI_Comm_rank(MPI_COMM_WORLD,&commrank);
MPI_Comm_size(MPI_COMM_WORLD,&commsize);
#else
commrank = 0;
commsize = 1;
#endif
int mpimin, mpimax;
// MPE_Decomp1d decomposes a vector into more or less equal parts
// The only restriction is that it takes the vector from 1:ng, rather than 0:ng-1
// Therefore, the mpimin and mpimax are decreases afterwards.
MPE_Decomp1d(ng,commsize, commrank, &mpimin, &mpimax);
mpimin--;
mpimax--;
boost::progress_display show_progress((mpimax-mpimin+1)/10);
#ifdef _OPENMP
#pragma omp parallel for schedule(dynamic)
#endif
for (int i=mpimin; i<mpimax; i++)
{
Point p(logT[i],logrho[i]);
// a possible linear interpolation
// see http://www.cgal.org/Manual/latest/doc_html/cgal_manual/Interpolation/Chapter_main.html#Subsection_70.3.3
// make sure to use small interpolation file. If not, this takes hours!
std::vector< std::pair< Point, Coord_type > > coords;
Coord_type norm = CGAL::natural_neighbor_coordinates_2(DT, p,std::back_inserter(coords)).second;
Coord_type res = CGAL::linear_interpolation(coords.begin(), coords.end(),
norm,
Value_access(function_values));
g[i]=res;
// let's not do nearest neighbour
// it is much faster than the linear interpolation
// but the spacing in temperature is too broad too handle this
/*Delaunay_triangulation::Vertex_handle v=DT.nearest_vertex(p);
Point nearest=v->point();
std::pair<Coord_type,bool> funcval=tempmap(nearest);
g[i]=funcval.first;*/
// This introduces a race condition between threads, but since it's only a counter, it doesn't really matter.
if ((i-mpimin)%10 == 0) ++show_progress;
}
cout << " Done!" << endl << flush;
return g;
}
cube emissionfromdatacube(cube datacube)
{
// construct the G(T) using CHIANTI tables
int ng=datacube.readngrid();
int nvars=5; // G(T), width, vx, vy, vz
// take the last 3 from datacube
cube emission(nvars, ng);
tgrid grid=datacube.readgrid();
emission.setgrid(grid);
emission.settype(emisscube);
// copy velocity vectors
for (int i=2; i<nvars; i++)
{
tphysvar velcomp=datacube.readvar(i);
emission.setvar(i,velcomp);
};
tphysvar logrho = log10(datacube.readvar(0));
tphysvar T = datacube.readvar(1);
tphysvar logT = log10(T);
// writearray(logT,"empty");
string ion="";// better to be aia for AIA tables this will be checked for correct table [DY]
double lambda0=.0;
double atweight=1;
cube gofttab=readgoftfromchianti(chiantifile,ion,lambda0,atweight);
// fit the G(T) function to the data points
tphysvar fittedgoft=goft(logT,logrho,gofttab);
// calculate the line width at each data point
tphysvar fittedwidth=linefwhm(T,lambda0,atweight);
// calculate the maximum of the emission profile at each grid point
// The emission in the CHIANTItables is calculated with the sun_coronal.abund file
// There are 2 cases:
// - we are doing spectroscopic calculations: the fittedemission should normalised with the alphaconst, and if a different abundance is used, we should renormalise to the new abundance
// - we are doing intensity calculations (for e.g. AIA): the tables are already in the correct units, and the fittedemission needs to only be multiplied with 1.
double normaliseconst=1.;
double abundratio=1.;
if (lambda_pixel>1) // for spectroscopic study
{
cout << "This code is configured to do spectroscopic modelling" << endl;
// tphysvar fittedwidth=linefwhm(T,lambda0,atweight);
normaliseconst=1./alphaconst;
if (abundfile != string("/empty"))
{
ifstream abundfilestream (abundfile);
cout << "Reading abundances from " << abundfile << "... " << flush;
double abundnew=abundfromchianti(abundfilestream, ion);
cout << "Done!" << endl << flush;
istringstream standardabundfile (______chiantitables_sun_coronal_abund_string);
double abundold=abundfromchianti(standardabundfile,ion);
abundratio=abundnew/abundold;
}
}
if (lambda_pixel==1) // for imaging study
{
if (atoi(ion.c_str())!=int(lambda0+0.5))
{// check if it is AIA GOFT table
cout << "GOFT table is not correct!" << endl;
exit(EXIT_FAILURE);
}
fittedwidth=T/T;// =1.0
}
// Spectral modelling: ne^2 [cm^-3] * G(ne,Te) [erg cm^3 s^1] = emis [erg cm^-3 s^-1]
// for integration *[cm] [D.Y 12 Nov 2014]
// AIA modelling: Temperature response function K(ne,Te)[cm^5 DN S^-1]*ne[cm^-3]=emis [DN cm^-1 s^-1];
// for integration *[cm] [D.Y 12 Nov 20
// cout << "normaliseconst" <<normaliseconst << endl;
// cout << "abundratio"<<abundratio<<endl;
tphysvar fittedemission=normaliseconst*abundratio*pow(10.,2.*logrho)*fittedgoft;
fittedemission=fittedemission/fittedwidth;
// load the emission and width into the emission-cube variable
emission.setvar(0,fittedemission);
emission.setvar(1,fittedwidth);
return emission;
};
