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wdinput.dat
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wdinput.dat
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# MCMC run parameters
fit = 1 # actually fit (1), or just plot model as specified (0)
nburn = 2000 # number of steps to use in burn-in phase
nprod = 1000 # number of steps to use in production phase
nwalkers = 200 # must be even multiple of npars (npars = 4)
nthread = 6 # number of CPU threads to use
scatter = 0.10 # fractional scatter to add to starting ball of parameters
flat = 0 # Is the chain file flattened, or 3D?
thin = 1 # amount to thin MCMC chain by before calculating best fit
# All model parameters have both a starting value and a prior
# priors are specified by type, val1, val2
# type can be one of 'gauss', 'uniform' or 'log_uniform'
# if type = 'gauss', val1 and val2 represent mean and standard deviation of prior
# if type = 'uniform' or 'log_uniform', val1 and val2 represent the limits of prior
# # # # # # # # # # # # # # #
# Initial Model Parameters #
# # # # # # # # # # # # # # #
# WD temp
# log g (model grid runs from 7 to 9.5, so within this as minimum)
teff = 20000 uniform 5000 90000.0
logg = 7.5 uniform 7.01 9.49
# Redenning E(B-V).
# If you don't know anything, should range from 0 to max galactic extinction
# at this position -> https://irsa.ipac.caltech.edu/applications/DUST/
ebv = 0.01 uniform 0.00 0.0137
# Parallax prior and initial guess from Gaia
# -> http://gea.esac.esa.int/archive/
plax = 2.4041 gauss 2.4041 0.1564
syserr = 0.03 # systematic error to add to all fluxes (in %)
# Name of chain file
chain = ../hierarchical_FinalFit/chain_prod.txt
# Now we want a mapping of filter names in chain file to
# photometric systems. Possible photometric systems are:
# HCAM - fluxes are in HiPERCAM natural photometric system
# UCAM_SDSS - fluxes in UCAM natural system, SDSS-like filters
# UCAM_SUPER - fluxes in UCAM natural system, super-SDSS filters
# USPEC - fluxes in USPEC natural system
# SDSS - fluxes in SDSS photometric system
["photometric_systems"]
'u' = 'SDSS'
'g' = 'SDSS'
'i' = 'SDSS'
'kg5' = 'USPEC'