Creates a macro that computes the N_gamma for each pressure steps #86
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… TRestAxionSolarQCDFlux
…or N_gamma for vacuum and for each of the pressure steps from TRestAxionField::GetMassDensityScanning
for more information, see https://pre-commit.ci
francandon
changed the title
Co-authored-by: Javier Galan <javier.galan@unizar.es>
Co-authored-by: Javier Galan <javier.galan@unizar.es>
Co-authored-by: Javier Galan <javier.galan@unizar.es>
Co-authored-by: Javier Galan <javier.galan@unizar.es>
for more information, see https://pre-commit.ci
macros/REST_Axion_PlotNgamma.C
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| TRestAxionSolarQCDFlux* sFlux = new TRestAxionSolarQCDFlux("fluxes.rml", "Gianotti"); | ||
| sFlux->Initialize(); | ||
| TH1F* spec1 = sFlux->GetEnergySpectrum(); | ||
| spec1->Rebin(20000 / n_ma); |
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You could simply multiply spec1 bins by the results of the axion-photon probability at each energy.
TH1D *convoluted = spec1->Clone();
for( int n = 0; n < spec1->GetNbinsX(); n++ )
{
double en = convoluted->GetBinCenter(n+1);
// Get probability for `en` --> Paxion
convoluted->SetBinContent(n+1, convoluted->GetBinContent(n+1) * Paxion );
}
// Then calculate the integral of convoluted
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That’s great, I’ll change that as soon as I can. I had to rebin the spectrum because I was using this method of storing the Probabilty values in a histogram, and then multiply, then, both histograms needs to be the same size.
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ok, but you can just compute the probability for the binning given in the energy spectrum, as in the example I give previously.
macros/REST_Axion_PlotNgamma.C
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| // Create a vector for saving the integrals that corresponds to the Number of photones | ||
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| double energy_step = (E_a_max - E_a_min) / n_ma; |
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The energy step could be the binning of spec1.
macros/REST_Axion_PlotNgamma.C
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| TH1F* ng = new TH1F(); | ||
| *ng = (*spec1) * (*vac); | ||
| double integral = ng->Integral(ng->FindBin(0), ng->FindBin(20)); | ||
| n_photons[i] = integral * 0.2 * 0.8 * 14 * 60 * 60; |
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Give variable names to the numbers so that we know what they are.
…he definition of the factors that multiply the integral and redefine the pressure step as the bin size of the solar spectra
for more information, see https://pre-commit.ci
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I close this PR since changes have been already included in the in #88. In any case we should move towards a future |
Creates a macro called
REST_Axion_PlotNgamma.Cthat computes the number of photons vs axion mass for vacuum and for each of the pressure steps thatTRestAxionField::GetMassDensityScanningcomputes.