./bayesed (openmpi v1.8.8 is required for mpirun) [OPTIONS] -i inputfile
OPTIONS:
-a, --ann ARG1[,ARGn] Select ann model by name
e.g. -a id,bc03_pr_exp_ch_calzetti,iscalable
-ak, --aknn ARG1[,ARGn] Select aknn model by name
e.g. -ak id,bc03_pr_exp_ch_calzetti,iscalable,k,f_run,eps,iRad
-bb, --blackbody ARG1[,ARGn] black body spectrum
e.g. --blackbody id,bb,iscalable,w_min,w_max,Nw
-gb, --greybody ARG1[,ARGn] grey body spectrum
e.g. --greybody id,gb,iscalable,ithick,w_min,w_max,Nw
-h, -help, --help, --usage Display usage instructions
-i, --input ARG1[,ARGn] Input file containing observed photometric SEDs with given unit(0 for flux in uJy, 1 for AB magnitude)
e.g. -i 0,observation/ULTRAVISTA/ULTRAVISTA0.txt
-k, --knn ARG1[,ARGn] Select knn model by name
e.g. -k id,bc03_pr_exp_ch_calzetti,iscalable,k,f_run
-L, --luminosity ARG1[,ARGn] compute luminosity between w_min and w_max in rest-frame
e.g. --luminosity w_min,wmax
-pw, --powerlaw ARG1[,ARGn] power law spectrum
e.g. --powerlaw id,pw,iscalable,w_min,w_max,Nw
-s, --sampling ARG1[,ARGn] IS,mmodal,ceff,nlive,efr,tol,updInt,Ztol,seed,fb,resume,outfile,logZero,maxiter,acpt_min for MultiNest.
e.g. --sampling 1,0,0,400,0.3,0.1,1000,-1e90,1,0,0,0,-1e90,100000,0.01 (default)
-sfh, --sfh ARG1[,ARGn] Select a SFH for the csp model
e.g. -sfh id,itype_sfh,itruncated,itype_ceh
-ssp, --ssp ARG1[,ARGn] Select a ssp model for the csp model
e.g. -ssp id,ynII,iscalable,k,f_run,eps,iRad,iT0,iT1,iT2
-t, --template ARG1[,ARGn] Use template SED with the given name
e.g. -t id,M82,iscalable
--check Print all inputs and their category.
--cl ARG1[,ARGn] output estimates at confidence levels e.g. --cl 0.68,0.95 (default)
--cosmology ARG1[,ARGn] e.g. --cosmology 70,0.7,0.3 (default)
--ebv ARG1[,ARGn] set the global value of E(B-V) of MW for all objects
e.g. --ebv 0
--export ARG Exports all options including the default values of unset ones.
e.g. --export out.txt
--ext ARG1[,ARGn] select extinction curve
e.g. --ext id,ext_law[0-7]
0:Starburst(Calzetti+2000,FAST)
1:Milky Way (Cardelli+1989,FAST)
2:Star-forming(Noll+2009,FAST)
3:MW(Allen+76,hyperz)
4:MW(Fitzpatrick+86,hyperz)
5:LMC(Fitzpatrick+86,hyperz)
6:SMC(Fitzpatrick+86,hyperz)
7:SB(Calzetti2000,hyperz)
--filters ARG Set the file containing the definition of filters
e.g. --filters filter/filters.txt
--filters_selected ARG Set all used filters in the observation and select those needed
e.g. --filters_selected filter/filters_selected.txt
--flux_max ARG maximum allowed observational flux in microJy
e.g. --flux_max 1e99 (default)
--flux_min ARG minimum allowed observational flux in microJy
e.g. --flux_min 0 (default)
--gsl_integration_qag ARG1[,ARGn] set epsabs,epsrel,limit for gsl_integration_qag
e.g. --gsl_integration_qag 0,0.01,500 (default)
--import ARG1[,ARGn] Import one or more files that contain command line options and use # as comment char.
e.g. --import in.txt
--IGM ARG1[,ARGn] --IGM [0-5]
Select the model for intergalactic medium attenuation
0:None
1:Madau (1995) model (default)
2:Meiksin (2006) model
--load_priors ARG load priors from .hist files for all objects
e.g. --load_priors priors_root
--nzbin ARG Number of bins used to sample the prior of redshift.
e.g. --nzbin 20 (default)
--NNF ARG1[,ARGn] The MAXITER and toler used in nonnegative quadratic programming.
e.g. --NNF 10000,0 (default)
--NfilterPoints ARG e.g. --NfilterPoints 30 (default)
--outdir ARG output dir for all results
e.g. --ourdir result/ (default)
--output_PCs ARG output the amplitude of first N PCs
e.g. --output_PCs 0 (default)
--output_model_absolute_magnitude output model absolute magnitude of best fit
--output_model_apparent_magnitude output model apparent magnitude of best fit
--output_model_flux output model flux of best fit
--output_pos_obs output posterior estimation of observables
--rename ARG rename the model
--save_bestfit Save the best fitting result
--save_pos_sfh ARG Save the posterior distribution of model SFH with given Ngrid
e.g. --save_pos_sfh 100
--save_pos_spec Save the posterior distribution of model spectra (Warning,require memory of size nSamples*Nwavelengths!)
--save_priors save priors as .hist files for all objects
--save_sample_obs save posteriori sample of observables
--save_sample_par Save the posterior sample of parameters
--save_sample_spec Save the posterior sample of model spectra
--save_summary Save the summary file
--select_sample ARG1[,ARGn] select a subsample with given conditions
e.g. --select_sample Nvalid_photo_min,Nvalid_spectra_min,SNR_min
--sys_err_model ARG1[,ARGn] fractional systematic error of model
e.g. --sys_err_model 0,0 (default)
--sys_err_obs ARG1[,ARGn] fractional systematic error of obs
e.g. --sys_err_obs 0,0 (default)
--test_priors test priors by setting the loglike for observational data to be zero
--w_max ARG maximum allowed observational wavelength in micron
--w_min ARG minimum allowed observational wavelength in micron
--zrange ARG1[,ARGn] set the global value of z_min and z_max used for the fitting of all objects
e.g. --zrange 0,6