(doc:yamlconf)= # YAML config file A full sample of `CONAN` **.yaml** config file is given below: ```{code-block} yaml :lineno-start: 1 # ========================================== CONAN YAML Configuration ========================================== # This is a template YAML configuration file for CONAN v3.3.12 # PRIORS: Fix-'F(val)', Norm-'N(mu,std)', Uni-'U(min,start,max)', TruncNorm–'TN(min,max,mu,std)', LogUni-'LU(min,start,max)' general: n_planet : 1 # number of planets in system photometry: light_curves: filepath : Notebooks/WASP-127/WASP127_LC_RV/../data/ # Light curve data directory names : [lc6bjd.dat, WASP-127_S9.dat] # List of LC filenames (must be in lc_filepath directory) filters : [R, T] # List of Filter names for each LC (for wavelength-dependent analysis) wavelength_um: [0.6, 0.8] # Central wavelengths in microns for each filter supersampling: [None, 30] # Supersampling factors for long-cadence data (None for no supersampling, number for subdivision factor) clip_outliers: [c1:W11C5n1, c1:W5C4.2n1] # Outlier clipping settings for each LC (format: 'c[columns]:W[width]C[sigma]n[iterations]', None for no clipping)) scale_columns: [med_sub, None] # Data column rescaling (med_sub=subtract median, rs0to1=rescale 0-1, rs-1to1=rescale -1 to 1, None=no rescaling) spline : [None, None] # Spline decorrelation setup for each LC (None for no spline) apply_jitter : [y, y] # Whether to fit jitter term for each light curve ('y'=yes, 'n'=no) baseline: # Baseline model configuration - polynomial orders for each data column of each LC offset: [y, y] # Fit offset term ('y'=yes, 'n'=no) col0 : [0, 0] # Time trend (0=none, 1=linear, 2=quadratic) col3 : [0, 0] # Column 3 decorrelation order col4 : [0, 0] # Column 4 decorrelation order col5 : [2, 0] # Column 5 decorrelation order col6 : [1, 0] # Column 6 decorrelation order col7 : [0, 0] # Column 7 decorrelation order col8 : [0, 0] # Column 8 decorrelation order sinusoid: names: [] # Light curve names to apply sinusoidal decorrelation trig : [] # Trigonometric function: 'sin', 'cos', or 'sincos' n : [] # Number of harmonics par : [] # Data column to decorrelate against P : [] # Period of sinusoid amp : [] # Amplitude of sinusoid x0 : [] # Phase offset gp: # Gaussian Process configuration - lc_name : WASP-127_S9.dat # list of LC names to apply GP. 'same' to fit same gp parameters for the LCs, 'all' for all LCs. filter name to apply GP to can also be given. kernel : [mat32] # list of GP kernel type: mat32, mat52, exp, cos, sho, etc. use tuple to specify combination of more than one kernel e.g. (mat32, exp) par : [col0] # Data column for GP independent variable h1_amp : ['LU(20,400,4000)'] # GP amplitude prior h2_len_scale: ['LU(0.007,0.4,5)'] # GP length scale prior h3_other : [None] # Third hyperparameter (kernel-dependent) h4_period : [None] # Fourth hyperparameter (for periodic kernels) operation : [] # Kernel combination operation ('+' or '*') gp_pck : ce # GP package: 'ce'=celerite, 'ge'=george, 'sp'=spleaf limb_darkening: # Limb darkening coefficients (using Kipping parameterization) filters: [R, T] # list of unique filter names to q1 : ['N(0.4239,0.0253)', 'N(0.2978,0.0159)'] # list of linear LD coefficients prior for each LC q2 : ['N(0.3969,0.0166)', 'N(0.3784,0.0135)'] # list of quadratic LD coefficients prior for each LC tdv: # Transit depth variation between filters fit_ddfs : n # Fit depth variations ('y'=yes, 'n'=no) drprs : 'U(-0.5,0,0.5)' # Depth variation prior. deviation of radius ratio from the reference values in planet_parameters (Uniform: min, start, max) div_white: n # Divide by white light curve ttv: # Transit timing variations fit_ttvs : n # Fit TTVs ('y'=yes, 'n'=no) dt : 'U(-0.125, 0, 0.125)' # prior for the deviation of transit times from the expected values baseline : 0.25 # Baseline fraction around transit per_LC_T0 : False # Fit one T0 per LC file vs per transit include_partial: True # Include partial transits in analysis phase_curve: # Phase curve and secondary eclipse modeling filters : [R, T] # list of filter names D_occ : ['F(0)', 'F(0)'] # prior for the observed Occultation depth in ppm Fn : [None, None] # prior for the Nightside flux in ppm (None = no phase curve, just transit and/or occultation) ph_off : [None, None] # prior for the Phase offset in degrees A_ev : ['F(0)', 'F(0)'] # prior for the semi amplitude of ellipsoidal variation (EV) in ppm f1_ev : ['F(0)', 'F(0)'] # prior for fraction amplitude of EV signal. values should range between 0 and 1. A_db : ['F(0)', 'F(0)'] # prior for semi-amplitude of Doppler boosting in ppm. pc_model: [cosine, cosine] # Phase curve model: 'cosine' or 'lambert' custom_LC_function: # Custom light curve function (for non-standard models) function : None # custom function name x : None # Independent variable func_pars : None # dictionary of argument priors to pass to the custom function. e.g {A: 'F(1.2)', B:'N(3,0.5)'} extra_args : None # dictionary of extra arguments to pass to the custom function op_func : None # operation function to apply to the output of custom function and transit model to obtain the desired model. replace_LCmodel: False # replace the transit model with the custom model contamination: # contamination due to flux from other sources in aperture filters : [R, T] # list of filter names contam_factor: ['F(0)', 'F(0)'] # contamination fraction: flux of contaminants/ flux of target within the aperture auto_decorr: # Automatic decorrelation - finds best baseline model using statistical comparison get_decorr : False # Set to True to automatically find best decorrelation parameters delta_bic : -5 # BIC improvement threshold for parameter selection (more negative = more conservative) exclude_cols: [] # Column numbers to exclude from decorrelation analysis exclude_pars: [] # Specific parameters to exclude (e.g., ['A3', 'B4']) enforce_pars: [] # Parameters to always include in decorrelation # ==== RADIAL VELOCITY CONFIGURATION ==== radial_velocity: rv_curves: filepath : Notebooks/WASP-127/WASP127_LC_RV/../data/ # Radial velocity data directory rv_unit : km/s # unit for radial velocity data: m/s or km/s names : [rv1.dat, rv2.dat] scale_columns: [med_sub, med_sub] # Data column rescaling (med_sub=subtract median, rs0to1=rescale 0-1, rs-1to1=rescale -1 to 1, None=no rescaling) spline : [None, None] # c{column_no}:d{degree}K{knot_spacing} e.g. c0:d3K2 or c0:d3K2|c4:d3K2 for two dimensional apply_jitter : [y, y] # Whether to fit jitter term for each light curve ('y'=yes, 'n'=no) baseline: gammas: ['N(-9.229240663524008,0.1)', 'N(-9.210554832958305,0.1)'] # systemic velocity priors col0 : [2, 0] col3 : [1, 0] col4 : [1, 0] col5 : [0, 0] gp: - rv_name : None # RV filename (None = no GP) kernel : None # GP kernel type par : None # Independent variable column h1_amp : None # GP amplitude h2_len_scale: None # GP length scale h3_other : None # Third hyperparameter h4_period : None # Fourth hyperparameter h5_der_amp : None # Derivative amplitude (for activity) error_col : None # Error column for multi-dimensional GP operation : # Kernel operation gp_pck : n # GP package ('n' = none) custom_RV_function: # custom RV function function : None # custom function name x : None # Independent variable func_pars : None # dictionary of argument priors to pass to the custom function. e.g {A: 'F(1.2)', B:'N(3,0.5)'} extra_args : None # dictionary of extra arguments to pass to the custom function op_func : None # operation function to apply to the output of custom function and transit model to obtain the desired model. replace_RVmodel: False # Replace standard RV model auto_decorr: # Automatic decorrelation for RV data get_decorr : False # Automatically find best RV decorrelation delta_bic : -5 # BIC threshold for parameter selection exclude_cols: [] # Columns to exclude from decorrelation exclude_pars: [] # Parameters to exclude enforce_pars: [] # Parameters to enforce planet_parameters: rho_star : 'N(0.565,0.035)' # Stellar density prior (g/cm³) - alternative to duration parameterization Duration : None # Transit duration (alternative to rho_star) - set to None if using rho_star RpRs : ['U(0.05,0.108,0.17)'] # prior Planet-to-star radius ratio. make into list for multiplanet Impact_para : ['U(0,0.29,1)'] # pripr on impact parameter, list for multiplanet T_0 : ['N(6776.621239999775,0.001)'] # Mid-transit time (BJD) Period : ['F(4.17806203)'] # Orbital period (days) Eccentricity: ['F(0)'] # prior on eccentricity. list for multiplanet omega : ['F(90)'] # prior on argument of periastron (degrees: 0-360) sesinw : None # prior on sqrt(e)sinw. alternative to eccentricity/omega secosw : None # prior on sqrt(e)cosw. alternative to eccentricity/omega K : ['U(0,0.01,0.05)'] #prior on RV semi amplitude. in same unit as rv data stellar_parameters: #stellar paramters. only used to convert radius and mass to actual units radius_rsun : 'N(1.33, 0.03)' #stellar radius in Rsun mass_msun : 'N(0.95, 0.02)' # stellar mass in Msun input_method: Rrho # Method for stellar parameter input: 'Rrho' uses radius+density, 'Mrho' uses mass+density # ==== SAMPLING CONFIGURATION ==== fit_setup: sampler : dynesty # Sampling algorithm: 'dynesty' (nested sampling) or 'emcee' (MCMC) number_of_processes : 10 # Number of CPU cores for parallel processing # === EMCEE Parameters (if sampler='emcee') === emcee_number_steps : 2000 # Chain length emcee_number_chains : 64 # Number of walkers emcee_burnin_length : 500 # Burn-in steps to discard emcee_move : stretch # Move algorithm: 'stretch', 'demc', 'snooker' # === Dynesty Parameters (if sampler='dynesty') === dynesty_nlive : 100 # Number of live points dynesty_dlogz : 0.1 # Stopping criterion (evidence tolerance) dynesty_nested_sampling : static # 'static' or 'dynamic' force_nlive : False # Force nlive even if < ndim*(ndim+1)/2 # === Advanced Options === leastsq_for_basepar : n # Use least-squares for baseline fitting light_travel_time_correction: n # Apply light travel time correction # Prior limits (set to 'auto' for automatic determination from data) lc_jitter_loglims : auto # Log jitter limits for light curves rv_jitter_lims : auto # Jitter limits for RV data lc_basecoeff_lims : auto # Baseline coefficient limits (LC) rv_basecoeff_lims : auto # Baseline coefficient limits (RV) # Multi-dimensional GP options (for spleaf package) apply_lc_gpndim_jitter : n # Jitter for each GP dimension (LC) apply_rv_gpndim_jitter : n # Jitter for each GP dimension (RV) apply_lc_gpndim_offset : n # Offset for each GP dimension (LC) apply_rv_gpndim_offset : n # Offset for each GP dimension (RV) # ============ END OF FILE ============================================ ``` There are 6 main sections: `general`: specify the number of planets to model in the LC and RV models. `photometry`: define the setup for the lightcurves. can be excluded if no lightcurves to analyse. `radial_velocity`: define the setup for the rvs. Can be excluded if no rv files to analyse. `planet_parameters`: define priors for fitting the planet's orbit and physical parameters `stellar_parameters`: give stellar radius and mass to use post-fit to convert planet radius and mass to actual punits. when fitting a phase curve or occultation, the stellar radius is also used to compute the light-travel-time delay. `fit_setup`: specify the desired sampling strategy and other options.