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MAUVE_MasterConfig_v5.4.2_sn40.yaml
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MAUVE_MasterConfig_v5.4.2_sn40.yaml
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# This is a test config file
GENERAL :
RUN_ID : # Name of the analysis run. A subdirectory of this name within the output directory will be created. This identifier further serves as a prefix to all output files.
INPUT : # Input file for this analysis run. The specified path is relative to the input path given in defaultDir.
OUTPUT : . # Output directory. The output of this run will be collected in a subdirectory named RUN_ID. The specified path is relative to the output path given in defaultDir.
REDSHIFT : # Initial guess on the redshift of the system [in z]. Spectra are shifted to rest-frame, according to this redshift.
PARALLEL: True # Use multiprocessing [True/False]
NCPU : 16 # Number of cores to use for multiprocessing
LSF_DATA : 'lsf_MUSE-WFM' # Path of the file specifying the line-spread-function of the observational data. The specified path is relative to the configDir path in defaultDir.
OW_CONFIG : True # Ignore configurations from previous runs which are saved in the CONFIG file in the output directory [True/False]
OW_OUTPUT : False # Overwrite any output files already present in the current output directory [True/False]
# Read data module
READ_DATA :
METHOD : 'MUSE_WFM' # Name of the routine in readData/ (without .py) to be used to read-in the input data.
DEBUG : FALSE # Switch to activate debug mode [True/False]: Pipeline runs on one, central line of pixels. Keep in mind to clean output directory after running in DEBUG mode!
ORIGIN : 219,219 # Origin of the coordinate system in pixel coordinates: x,y (Indexing starts at 0).
LMIN_TOT : 4750 # Spectra are shortened to the rest-frame wavelength range defined by LMIN_TOT and LMAX_TOT. Note that this wavelength range should be longer than all other wavelength ranges supplied to the modules [in Angst.]
LMAX_TOT : 7050
LMIN_SNR : 4800 # Rest-frame wavelength range used for the signal-to-noise calculation [in Angst.]
LMAX_SNR : 7000
EBmV : # Enter the E(B-V) value for the galaxy here (or use null for no Galactic dust correction)
# Spatial masking module
SPATIAL_MASKING :
METHOD : 'default' # Name of the routine in spatialMasking/ (without .py) to perform the tasks. Set 'False' to turn off module. Set 'default' to use the standard GIST implementation.
MIN_SNR : 3 # Spaxels below the isophote level which has this mean signal-to-noise level are masked.
MASK : # File containing a spatial mask (Set 'False' to not include a file).
# Spatial binning module
SPATIAL_BINNING :
METHOD : 'voronoi' # Name of the routine in spatialBinning/ (without .py) to perform the tasks. Set 'False' to turn off module. Set 'voronoi' to use the standard GIST implementation, exploiting the Voronoi tesselation routine of Cappellari & Copin (2003).
TARGET_SNR : 40.0 # Target signal-to-noise ratio for the Voronoi binning
COVARIANCE : 0.0 # Correct for spatial correlations of the noise during the Voronoi binning process according to the empirical equation SNR /= 1 + COVAR_VOR * np.log10(NSPAXEL) with NSPAXEL being the number of spaxels per bin (see e.g. Garcia-Benito et al. 2015).
# Prepare spectra module
PREPARE_SPECTRA :
METHOD : 'default' # Name of the routine in prepareSpectra/ (without .py) to perform the tasks. Set 'False' to turn off module. Set 'default' to use the standard GIST implementation.
VELSCALE : 53 # Spectral sampling of the logarithmically rebinned spectra [in km/s]; e.g. velscale = dLambda*C / mean(wave), with the spectral sampling of the linearly binned spectra dLambda, the speed of light C, and the mean wavelength of the spectrum mean(wave).
# Stellar kinematics module
KIN :
METHOD : 'ppxf' # Name of the routine in stellarKinematics/ (without .py) to perform the tasks. Set 'False' to turn off module. Set 'ppxf' to use the standard GIST implementation, exploiting the pPXF routine of Cappellari & Emsellem (2004).
SPEC_MASK : 'specMask_KIN' # File to define wavelength ranges to be masked during the stellar kinematics fit. The specified path is relative to the configDir path in defaultDir.
LMIN : 4800 # Rest-frame wavelength range used for the stellar kinematics analysis [in Angst.]
LMAX : 7000
SIGMA : # Initial guess of the velocity dispersion of the system [in km/s]
MOM : 4 # Number of kinematic moments to be extracted
ADEG : 12 # Degree of the additive Legendre polynomial. Set '-1' to not include any additive polynomials
MDEG : 0 # Degree of the multiplicative Legendre polynomial. Set '0' to not include any multiplicative polynomials
REDDENING : null # As opposed to None. Initial guess on the stellar reddening E(B-V), in order to measure the stellar reddening. Note: This cannot be used together with multiplicative polynomials.
MC_PPXF : 0 # Number of Monte-Carlo simulations to extract errors on the stellar kinematics. Formal errors are saved in any case.
LSF_TEMP : 'lsf_MILES' # Path of the file specifying the line-spread-function of the spectral templates. The specified path is relative to the configDir path in defaultDir.
TEMPLATE_SET : 'miles' # options are 'miles' or 'IndoUS' or 'walcher'
LIBRARY : 'MILES_EMLINES/' # options are 'MILES/', 'miles_ssp_ch/', 'IndoUS', and 'Walcher/'
NORM_TEMP : 'LIGHT' # Normalise the spectral template library to obtain light- or mass-weighted results [LIGHT / MASS]
DOCLEAN : True # use pPXF clean routine which performs 3-sigma clipping based on the best-fit model [True / False]
# Continuum Cube module
CONT :
METHOD : 'ppxf' # Name of the routine in stellarKinematics/ (without .py) to perform the tasks. Set 'False' to turn off module. Set 'ppxf' to use the standard GIST implementation, exploiting the pPXF routine of Cappellari & Emsellem (2004).
SPEC_MASK : 'specMask_KIN' # File to define wavelength ranges to be masked during the stellar kinematics fit. The specified path is relative to the configDir path in defaultDir.
LMIN : 4800 # Rest-frame wavelength range used for the stellar kinematics analysis [in Angst.]
LMAX : 7000
SIGMA : # Initial guess of the velocity dispersion of the system [in km/s]
MOM : 4 # Number of kinematic moments to be extracted
MDEG : 8 # Degree of the multiplicative Legendre polynomial. Set '0' to not include any multiplicative polynomials
REDDENING : null # As opposed to None. Initial guess on the stellar reddening E(B-V), in order to measure the stellar reddening. Note: This cannot be used together with multiplicative polynomials.
MC_PPXF : 0 # Number of Monte-Carlo simulations to extract errors on the stellar kinematics. Formal errors are saved in any case.
LSF_TEMP : 'lsf_MILES' # Path of the file specifying the line-spread-function of the spectral templates. The specified path is relative to the configDir path in defaultDir.
TEMPLATE_SET : 'miles' # options are 'miles' or 'IndoUS' or 'walcher'
LIBRARY : 'MILES_EMLINES/' # options are 'MILES/', 'miles_ssp_ch/', 'IndoUS', and 'Walcher/'
NORM_TEMP : 'LIGHT' # Normalise the spectral template library to obtain light- or mass-weighted results [LIGHT / MASS]
DOCLEAN : True # Keyword to turn on/off the sigma clipping. Set to 'False' for testing.
# Emission line fitting module
GAS :
METHOD : 'ppxf' # options are 'ppxf', 'gandalf' or 'MAGPI_gandalf' Name of the routine in emissionLines/ (without .py) to perform the tasks. Set 'False' to turn off module. Set 'gandalf' to use the standard GIST implementation, exploiting the pyGandALF routine of Sarzi et al. (2006).
SPEC_MASK : 'specMask_GAS'
LEVEL : 'BIN' # Set 'BIN' to perform the analysis bin-by-bin, 'SPAXEL' for a spaxel-by-spaxel analysis, and 'BOTH' to perform a spaxel-by-spaxel analysis that is informed by a previous bin-by-bin analysis.
LMIN : 4800 # Rest-frame wavelength range used for the emission-line analysis [in Angst.]
LMAX : 7000
ERRORS : 0 # Derive errors on the emission-line analysis (0 No / 1 Yes). Note: Due to limitations in pyGandALF, this is currently not possible. We expect a new pyGandALF version to be published soon.
REDDENING : False # Include the effect of reddening by dust in the pyGandALF fit. Put in the form 0.1,0.1 without any spaces. If you intend to use multiplicative polynomials instead, set REDDENING to 'False' and add a MDEG keyword in the GAS section to set the polynomial order. Additive polynomials cannot be used with pyGandALF.
MDEG : 8 # Degree of the multiplicative Legendre polynomial. Set '0' to not include any multiplicative polynomials.
FIXED : True # Fix the stellar kinematics to the results obtained with the stellar kinematics module [True / False]
MOM : 2 # Gas moments. Set to 2 for V and sigma. Higher orders not yet tested
EBmV : null # As opposed to None. De-redden the spectra for the Galactic extinction in the direction of the target previously to the analysis. Use e.g. EBmV = A_v / 3.2
EMI_FILE : 'emissionLinesPHANGS.config' # Emission line set-up file for emline fittet. The specified path is relative to the configDir path in defaultDir.
LSF_TEMP : 'lsf_MILES' # Path of the file specifying the line-spread-function of the spectral templates. The specified path is relative to the configDir path in defaultDir.
TEMPLATE_SET : 'miles' # options are 'miles' or 'IndoUS'
LIBRARY : 'MILES_EMLINES/' # options are 'MILES_EMLINES/' (contains asmaller subset of templates sim to that used by PHANGS) 'MILES/', 'miles_ssp_ch', or 'IndoUS'
NORM_TEMP : 'LIGHT' # Normalise the spectral template library to obtain light- or mass-weighted results [LIGHT / MASS]
# Star formation histories module
SFH :
METHOD : 'ppxf' # Name of the routine in starFormationHistories/ (without .py) to perform the tasks. Set 'False' to turn off module. Set 'ppxf' to use the standard GIST implementation, exploiting the pPXF routine of Cappellari & Emsellem (2004).
LMIN : 4800 # Rest-frame wavelength range used for the star formation histories analysis [in Angst.]
LMAX : 7000
SPEC_MASK : 'specMask_SFH' # File to define wavelength ranges to be masked during the star formation histories analysis. The specified path is relative to the configDir path in defaultDir.
SPEC_EMICLEAN : False # Keyword (True/False) to enable/disable the use of emission line cleaned spectra from the Emission Line Fitting Module.
MOM : 4 # Number of kinematic moments to be extracted. If you use FIXED = True, this should be same number of moments used to extract the stellar kinematics before. Otherwise the parameter can be set independently.
MDEG : 12 # Degree of the multiplicative Legendre polynomial. Set '0' to not include any multiplicative polynomials. Note that additive Legendre polynomials cannot be used for this module.
REGUL_ERR : 0.1 # Regularisation error for the regularised run of pPXF. Note: Regularisation = 1 / REGUL_ERR
NOISE : 1. # Set a wavelength independent noise vector to be passed to pPXF.
FIXED : True # Fix the stellar kinematics to the results obtained with the stellar kinematics module [True / False]. If 'False', please provide an initial guess on the velocity dispersion of the systems [in km/s] by adding the parameter SIGMA.
MC_PPXF : 0 # Added to add the option of running MC on the SFH module
LSF_TEMP : 'lsf_MILES' # Path of the file specifying the line-spread-function of the spectral templates. The specified path is relative to the configDir path in defaultDir.
TEMPLATE_SET : 'miles' # options are 'miles' or 'IndoUS (not recc.)'
LIBRARY : 'MILES_safe/' # options are 'MILES/', 'miles_ssp_ch/', or 'IndoUS/'
NORM_TEMP : 'LIGHT' # Normalise the spectral template library to obtain light- or mass-weighted results [LIGHT / MASS]
DOCLEAN : True # use pPXF clean routine which performs 3-sigma clipping based on the best-fit model [True / False]
# Line strenghts module
LS :
METHOD : 'default' # Name of the routine in lineStrengths/ (without .py) to perform the tasks. Set 'False' to turn off module. Set 'default' to use the standard GIST implementation, exploiting the routines of Kuntschner et al. (2006) and Martin-Navarro et al. (2018).
TYPE : 'SPP' # Set 'LS' to only measure line strength indices, or 'SPP' to also match these indices to stellar population properties.
LS_FILE : 'lsBands.config' # File to define the wavelength band of the line strength indices to be measured. The specified path is relative to the configDir path in defaultDir.
CONV_COR : 8.4 # Spectral resolution [in Angst.] at which the line strength indices are measured.
SPP_FILE : 'MILES_KB_LIS8.4.fits' # File providing predictions on line strength indices for a set of single stellar population models
MC_LS : 30 # Number of Monte-Carlo simulations in order to obtain errors on the line strength indices. Note: This must be turned on.
NWALKER : 10 # Number of walkers for the MCMC algorithm (used for the conversion of indices to population properties)
NCHAIN : 100 # Number of iterations in the MCMC algorithm (used for the conversion of indices to population properties)
LSF_TEMP : 'lsf_MILES' # Path of the file specifying the line-spread-function of the spectral templates. The specified path is relative to the configDir path in defaultDir.
TEMPLATE_SET : 'miles' # options are 'miles' or 'IndoUS'
LIBRARY : 'MILES_safe/' # options are 'MILES/', 'miles_ssp_ch/', or 'IndoUS/'
NORM_TEMP : 'LIGHT' # Normalise the spectral template library to obtain light- or mass-weighted results [LIGHT / MASS]