<jupyter_start><jupyter_text>Comparing Phoenix Spectra Plot Phoenix aces and Phoenix BT-Settl for same parametersAlso AMES Dusty Cond.  FORMAT OF THE SPECTRA OUTPUT FILESYou can find the  pre-computed grids, also accessible via links onthe bottom part of the simulator presentation page, or using this link:http://phoenix.ens-lyon.fr/Grids/The file names contain the main parameters of the models:lte{Teff/10}-{Logg}{[M/H]}a[alpha/H].GRIDNAME.7.spec.gz/bz2/xzis the synthetic spectrum for the requested effective temperature(Teff),surface gravity (Logg), metallicity by log10 number density withrespect to solar values ([M/H]), and alpha element enhencement relative     to solar values [alpha/H]. The model grid is also mentioned in the name.Spectra are provided in an ascii format (\*.7.gz):column1: wavelength in Angstroemcolumn2: 10\*\*(F_lam + DF) to convert to Ergs/sec/cm\*\*2/Acolumn3: 10\*\*(B_lam + DF) i.e. the blackbody fluxes of same Teff in same units.Additional columns, obtained systematically when computing spectra using thePhoenix simulator, give the information to identify atomic and molecularlines. This information is used by the idl scripts lineid.pro and plotid.pro which are provided in the user result package.     With the stacked ascii format (\*.spec.gz files ) we have rather:line1: Teff logg [M/H] of the modelline2: number of wavelengthsline3: F_lam(n) X 10\*\*DF , n=1,number of wavelengthslineX: B_lam(n) X 10\*\*DF , n=1,number of wavelengths<jupyter_code>from mingle.utilities.phoenix_utils import load_starfish_spectrum



def comparison_plot(name, teff, logg, feh):
    
    pars = teff, logg, feh

Artucus = [4300, 1.50, -0.5]
HD30501 = [5200, 4.5, 0.0]
ACES_bottom = [2300, 4.5, 0.0]
Sun = [5800, 4.5, 0.0]



comparison_plot("Sun", *Sun)




comparison_plot("ACES_bottom", *ACES_bottom)



comparison_plot("Artucus", *Artucus)




comparison_plot("HD30501", *HD30501)<jupyter_output><empty_output>
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