Files for running the beast on XSEDE

metal_xsede/beast_settings_LMC_mastergrid.txt

@@ -0,0 +1,256 @@
+import numpy as np
+
+from astropy import units
+
+# BEAST imports
+from beast.physicsmodel.stars import isochrone
+from beast.physicsmodel.stars import stellib
+from beast.physicsmodel.dust import extinction
+from beast.observationmodel.noisemodel import absflux_covmat
+
+#from extra_filters import make_integration_filter, make_top_hat_filter
+
+#-----------------------------------------------------------------
+# User inputs                                   [sec:conf]
+#-----------------------------------------------------------------
+# Parameters that are required to make models
+# and to fit the data
+#-----------------------------------------------------------------
+# AC == authomatically created
+# indicates where user's input change is NOT necessary/recommeded
+#-----------------------------------------------------------------
+
+# project : string
+#   the name of the output results directory
+project = "mastergrid_LMC"
+
+# name of the survey
+#  used for the creation of the unique name for each source
+surveyname = 'METAL'
+
+# filters : list of strings
+#   full filter names in BEAST filter database
+filters = [
+    'HST_WFC3_F225W',
+    'HST_WFC3_F275W',
+    'HST_WFC3_F336W',
+    'HST_WFC3_F475W',
+    'HST_ACS_WFC_F475W',
+    'HST_WFC3_F814W',
+    'HST_ACS_WFC_F814W',
+    'HST_WFC3_F110W',
+    'HST_WFC3_F128N',
+    'HST_WFC3_F160W'
+]
+
+# basefilters : list of strings
+#   short names for filters
+basefilters = []
+
+# obs_colnames : list of strings
+#   names of columns for filters in the observed catalog
+#   need to match column names in the observed catalog,
+#   input data MUST be in fluxes, NOT in magnitudes
+#   fluxes MUST be in normalized Vega units
+obs_colnames = [ f.upper() + '_RATE' for f in basefilters ]
+
+# obsfile : string
+#   pathname of the observed catalog
+obsfile = " "
+
+#------------------------------------------------------
+# Artificial Star Test Input File Generation Parameters
+#------------------------------------------------------
+
+# ast_models_selected_per_age : integer
+# Number of models to pick per age (Default = 70).
+ast_models_selected_per_age = 70  # NOT USED in flux bin method
+
+# ast_bands_above_maglimit : integer
+# Number of filters that must be above the magnitude limit
+# for an AST to be included in the list (Default = 3)
+ast_bands_above_maglimit = 3  # NOT USED in flux bin method
+
+# ast_n_flux_bins : integer
+# The number of flux bins into which the dynamic range of the
+# model grid in each filter is divided
+ast_n_flux_bins = 40
+
+# ast_n_per_flux_bin : integer
+# Minimum number of model seds that need to fall into each bin
+ast_n_per_flux_bin = 50
+
+# ast_realization_per_model : integer
+# Number of Realizations of each included AST model
+# to be put into the list. (Default = 20)
+ast_realization_per_model = 1  # for the toothpick model (NOT truncheon)
+
+
+# ast_maglimit : float (single value or array with one value per filter)
+# (1) option 1: [number] to change the number of mags fainter than
+#                  the 90th percentile
+#               faintest star in the photometry catalog to be used for
+#                  the mag cut.
+#               (Default = 1)
+# (2) option 2: [space-separated list of numbers] to set custom faint end limits
+#               (one value for each band).
+ast_maglimit = [1.]  # NOT USED for this production run
+
+# ast_with_positions :  (bool,optional)
+# If True, the ast list is produced with X,Y positions.
+# If False, the ast list is produced with only magnitudes.
+ast_with_positions = True
+
+# ast_source_density_table :  (string,optional)
+# Name of source density table from tools/create_source_density_map.py
+# If supplied, the ASTs will be repeated for each source density bin in the table
+ast_density_table = None
+# ast_source_density_table = 'data/b15_4band_det_27_A_sourcedens_map.hd5'
+
+#ast_N_bins : (int, optional)
+#Number of source or background bins that you want ASTs repeated over
+ast_N_bins = 4
+
+
+# ast_pixel_distribution : float (optional)
+# (Used if ast_with_positions is True), minimum pixel separation between AST
+# position and catalog star used to determine the AST spatial distribution
+ast_pixel_distribution = 10.0
+
+# ast_reference_image : string (optional, but required if ast_with_positions
+# is True and no X and Y information  is present in the photometry catalog)
+# Name of the reference image used by DOLPHOT when running the measured
+# photometry.
+ast_reference_image = " "
+
+# ast_coord_boundary : None, or list of two arrays (optional)
+# If supplied, these RA/Dec coordinates will be used to limit the region
+# over which ASTs are generated.  Input should be list of two arrays, the
+# first RA and the second Dec, ordered sequentially around the region
+# (either CW or CCW).
+ast_coord_boundary = None
+
+
+#-------------------------------------------
+#Noise Model Artificial Star Test Parameters
+#-------------------------------------------
+
+# astfile : string
+#   pathname of the AST files (single camera ASTs)
+astfile = " "
+
+# ast_colnames : list of strings
+#   names of columns for filters in the AST catalog (AC)
+ast_colnames = np.array(basefilters)
+
+# noisefile : string
+#   create a name for the noise model
+noisefile = project + '/' + project + '_noisemodel.hd5'
+
+# absflux calibration covariance matrix for HST specific filters (AC)
+absflux_a_matrix = absflux_covmat.hst_frac_matrix(filters)
+
+#-------------------------------------------
+#Grid
+#-------------------------------------------
+
+# n_subgrid : integer
+#     Number of sub-grids to use (1 means no subgrids).  These are
+#     useful when the physics model grid is too large to read into
+#     memory.
+n_subgrid = 10
+
+################
+
+### Distance/Velocity
+
+# Distances: distance to the galaxy [min, max, step] or [fixed number]
+# (Shaefer 2008, Haschke et al 2012)
+distances = [40, 60, 2.5]
+distance_prior_model = {'name': 'flat'}
+
+# Distance unit (any length or units.mag)
+distance_unit = units.kpc
+
+# velocity of galaxy
+# (van der Marel et al 2002)
+velocity = 262.2 * units.km / units.s
+
+################
+
+### Stellar grid definition
+
+# log10(Age) -- [min,max,step] to generate the isochrones in years
+#   example [6.0, 10.13, 1.0]
+logt = [6.0, 10.13, 0.1]
+age_prior_model = {'name': 'flat'}
+
+# note: Mass is not sampled, instead the isochrone supplied
+#       mass spacing is used instead
+mass_prior_model = {"name": "kroupa"}
+
+# Metallicity : list of floats
+#   Here: Z == Z_initial, NOT Z(t) surface abundance
+#   PARSECv1.2S accepts values 1.e-4 < Z < 0.06
+# the master grid is log Z = -2.1 to 0.3 in steps of 0.3
+# the PARSEC models have Z_sun = 0.0152
+z = (
+    10 ** np.array([-2.1, -1.8, -1.5, -1.2, -0.9, -0.6, -0.3]) * 0.0152
+).tolist()
+met_prior_model = {"name": "flat"}
+
+# Isochrone Model Grid
+#   Current Choices: Padova or MIST
+#   PadovaWeb() -- `modeltype` param for iso sets from ezpadova
+#      (choices: parsec12s_r14, parsec12s, 2010, 2008, 2002)
+#   MISTWeb() -- `rotation` param (choices: vvcrit0.0=default, vvcrit0.4)
+#
+# Default: PARSEC+CALIBRI
+oiso = isochrone.PadovaWeb()
+# Alternative: PARSEC1.2S -- old grid parameters
+#oiso = isochrone.PadovaWeb(modeltype='parsec12s', filterPMS=True)
+# Alternative: MIST -- v1, no rotation
+#oiso = isochrone.MISTWeb()
+
+# Stellar Atmospheres library definition
+osl = stellib.Tlusty() + stellib.Kurucz()
+
+################
+
+### Dust extinction grid definition
+extLaw = extinction.Generalized_RvFALaw(ALaw=extinction.Generalized_DustExt(curve='F19'), BLaw=extinction.Generalized_DustExt(curve='G03_SMCBar'))
+#extLaw = extinction.Gordon16_RvFALaw()
+
+# A(V): dust column in magnitudes
+#   acceptable avs > 0.0
+#   example [min, max, step] = [0.0, 10.055, 1.0]
+avs = [0.01, 10.0, 0.05]
+av_prior_model = {'name': 'flat'}
+#av_prior_model = {'name': 'lognormal',
+#                  'max_pos': 2.0,
+#                  'sigma': 1.0,
+#                  'N': 10.}
+
+# R(V): dust average grain size
+#   example [min, max, step] = [2.0,6.0,1.0]
+rvs = [2.0, 6.0, 0.5]
+rv_prior_model = {'name': 'flat'}
+#rv_prior_model = {'name': 'lognormal',
+#                  'max_pos': 2.0,
+#                  'sigma': 1.0,
+#                  'N': 10.}
+
+# fA: mixture factor between "MW" and "SMCBar" extinction curves
+#   example [min, max, step] = [0.0,1.0, 0.25]
+fAs = [0.0, 1.0, 0.2]
+fA_prior_model = {'name': 'flat'}
+#fA_prior_model = {'name': 'lognormal',
+#                  'max_pos': 0.5,
+#                  'sigma': 0.2,
+#                  'N': 10.}
+
+################
+
+# add in the standard filters to enable output of stats and pdf1d values
+# for the observed filters (AC)
+add_spectral_properties_kwargs = dict(filternames=filters)