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fast.param
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fast.param
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#... FAST V1.0: parameter file .........................................
#--- GENERAL INFORMATION -----------------------------------------------
#
# Please read this parameter file in detail, you can find all relevant
# information here. Note that you have to adjust your input catalogs
# accordingly, otherwise FAST will not work properly!
#
# o Requirements:
# - ~2.0 Gb memory (or more depending on the grid size)
# - idl (make sure IDL is properly installed, with IDL_DIR defined)
#
# o The main (example_phot or example_spec) directory should contain
# the following files:
# - Parameter file
# - [CATALOG].cat If you fit broadband photometry
# - [CATALOG].zout If you input photometric redshifts
# - [CATALOG].translate If you input a translate file
# - [FILTERS_RES] If you fit broadband photometry
# - [SPECTRUM].spec If you fit spectra
#
# o FAST can be run from the command line in the example directory.
# The first argument is the parameter file. Default is 'fast.param'
# $ ../fast
# $ ../fast my_fast.param
#
#-----------------------------------------------------------------------
#--- BROADBAND PHOTOMETRIC INFORMATION ---------------------------------
#
# o [CATALOG].cat (similar as for eazy):
# - Example catalog: hdfn_fs99.cat
# - FAST recognizes columns with names {id,ID,z_spec,F[n],E[n],
# TOT[n]} with n the number of the filter
# - Column names in the original header or in the translate file
# that have no flux information cannot start with "F" or "E"
# - If z_spec is not given or any negative value, no z_spec is assumed
# - Give -99 if the object has no coverage in a certain band
#
# o [CATALOG].zout (preferably generated with eazy):
# - Example catalog: hdfn_fs99.zout
# - If NAME_ZPHOT is not defined, FAST reads columns with labels "z_phot"
# as best-fit photometric redshifts "l68/l95/l99" and "h68/h95/h99"
# for the confidence intervalst
# - If input photo-z is a negative value, the galaxy will not be fitted
# - If [CATALOG].zout is not available, and no z_specs are given in
# [CATALOG].cat, then the redshifts are allowed to float
# - You can also read in spectroscopic redshifts from [CATALOG].zout.
# The corresponding column should be labeled "z_spec". However, if you
# list them in [CATALOG].cat, FAST will ignore those in [CATALOG].zout
#
# o [CATALOG].translate:
# - Example file: hdfn_fs99.translate
# - Translates the column names in [CATALOG].cat to the required
# F[n],E[n],etc formats
# - Will only be used when available
#
# o AB_ZEROPOINT: m_AB = AB_ZEROPOINT - 2.5*log(F[n]) (Default: 25.)
# - Default: AB_ZEROPOINT = 25.
# - fluxes in microjanskys: AB_ZEROPOINT = 23.93
# - fluxes in erg sec^{-1} cm^{-2} Hz^{-1}: AB_ZEROPOINT = -48.57
#
# o FILTERS_RES: similar as for eazy
#
# o FILTER_FORMAT: tells the program in the response curves provided in
# filters_res file are determined for energy-counting (=0) or photon-
# counting (=1) detectors (Default: 1)
#
# o TEMP_ERR_FILE: Template error function. The photometric errors are
# in rest-frame multiplied by this function. Note that this function
# will not change the spectroscopic uncertainties.
#
# o NAME_ZPHOT: Header name of the column in your [CATALOG].zout file
# that you want to use for your photometric redshifts. If not defined,
# FAST will look for 'z_phot'
#
#-----------------------------------------------------------------------
CATALOG = 'hdfn_fs99'
AB_ZEROPOINT = 25.
FILTERS_RES = '../Filters/FILTER.RES.v6.R300'
FILTER_FORMAT = 1
TEMP_ERR_FILE = '../Template_error/TEMPLATE_ERROR.fast.v0.2'
NAME_ZPHOT = 'z_m2'
#--- SPECTROSCOPIC INFORMATION -----------------------------------------
#
# o SPECTRUM:
# - Example file: "1030_gnirs.spec"
# - The file should have the following format:
# # bin wl tr F[id1] E[id1] F[id2] E[id2] ...
# - bin: number of the bin in which the spectral element falls
# - wl: wavelength is in Angstrom
# - tr: transmission of spectral element, choose from 1 (not-masked)
# or 0 (masked). No intermediate values are allowed (yet).
# The total transmission of the bin cannot be zero, so you can
# only mask certain parts within a bin
# - (e)fl: in 10^-19 ergs s-1 cm-2 Angstrom-1 (if AUTO_SCALE=0)
# - id: should be an integer
# - If you want to fit spectra and photometry at the same time, only
# the objects for which both spectra AND photometry are provided
# will be fit. Note that when you fit only one or a few galaxies
# from the same field, you can feed the full photometric catalog,
# and FAST will find the corresponding photometry.
# - Photometric redshifts are ignored when spectra are included.
# - The value -99 as a non-detection is NOT recognized for spectra.
# - It is advisable to keep the wavelength spacing constant and in
# small steps, as in the example input file!
#
# o AUTO_SCALE: This option automatically scales the spectrum using the
# broadband photometry as provided in the [CATALOG].cat file. The
# error on the scaling is taken into account when deriving the
# confidence intervals. The photometric bands used to scale the
# spectrum are not included in the fit. The scaling factor will be
# stored in the grid file, thus you have to set "SAVE_CHI_GRID" to "1"
#
#-----------------------------------------------------------------------
SPECTRUM = ''
AUTO_SCALE = 0 # 0 / 1
#--- OUTPUT INFORMATION -----------------------------------------------
#
# o OUTPUT_DIR: output directory for results
#
# o OUTPUT_FILE: output file for results.
# If not given: [CATALOG]_[SPECTRUM].fout
#
# o N_SIM: The number of monte carlo simulations used to calibrate the
# confidence levels. If zero or not defined, only best-fit values will
# be given.
#
# o C_INTERVAL: Percentage of confidence intervals, choose from 68% (1
# sigma), 95% (2 sigma), or 99% (3 sigma)
#
# o BEST_FIT: output best-fit SPS model
#
#-----------------------------------------------------------------------
OUTPUT_DIR = ''
OUTPUT_FILE = ''
N_SIM = 0
C_INTERVAL = 68 # 68 / 95 / 99 or [68,95] etc
BEST_FIT = 1 # 0 / 1
#--- CHOOSE STELLAR POPULATIONS LIBRARY --------------------------------
#
# o LIBRARY_DIR: directory containing the stellar population libraries
# of the form: ised_[SFH].[resolutions].
# The binaries in these directories are of the following form:
# [library]_[resolution]_[imf]_z[metallicity]_ltau[ltau/yr].ised
#
# o All binary inputs are made using "csp_galaxev"
# ("galaxev" software by Bruzual & Charlot 2003) on the SSP models
# "bc2003_[RESOLUTION]_[metal]_[IMF]_ssp.ised" and assuming no dust
# law (and no recycling of gas ejected by stars for exponentially
# declining star formation history)
#
# o LIBRARY: choose from Bruzual & Charlot 2003 ('bc03'),
# Maraston 2005 ('ma05'), and FSPS by Conroy et al. ('co11')
#
# o RESOLUTION: Choose 'hr' for spectral fitting, and 'pr' (photometric
# resolution) or 'lr' for medium and broadband filters. Not all
# resolutions are standard available for all SFHs or libraries or IMFs
#
# o IMF (stellar initial mass function), choose from
# - 'ch'(abrier)
# - 'sa'(lpeter)
# - 'kr'(oupa)
#
# o SFH: parametrization of the star formation history (SFH), choose from
# - 'exp': exponentially declining SFH; sfr ~ exp(-t/tau)
# - 'del': delayed exponentially declining SFH; sfr ~ t exp(-t/tau)
# - 'tru': truncated SFH, with constant star formation between
# t_onset and t_onset+tau
# For all SFH you can specify the range tau in the grid
#
# o DUST_LAW: parametrization of the dust attenuation curve. You can
# choose from the following options
# - 'calzetti': Calzetti (2000) dust law
# - 'mw': Milky Way, following parametrization by Cardelli et al. (1989)
# - 'kc': Kriek & Conroy (2013). Average dust law. We use the
# parametrization by Noll et al. with E_B = 1 and delta = -0.1
# - 'noll': For this law you have to parametrize E_b and delta.
# You can only pick one value for each, arrays are not allowed.
#
# o MY_SFH: if you define this option, FAST will not fit a range of
# star-formation histories, but just one model (so LOG_TAU_XXX will
# be ignored). For this option you can only read in one custom star
# formation history, for which you have to make the ISED file
# yourself using "csp_galaxev". The naming of the ised file has to
# be as follows:
# [library]_[resolution]_[imf]_z[metallicity]_[MY_SFH].ised
# This file needs to be placed directly in 'LIBRARY_DIR'
#
#-----------------------------------------------------------------------
LIBRARY_DIR = '../Libraries/'
LIBRARY = 'co09' # 'bc03' / 'ma05' / 'co11'
RESOLUTION = 'pr' # 'pr' / 'lr' / 'hr'
IMF = 'ch' # 'ch' / 'sa' / 'kr'
SFH = 'del' # 'exp' / 'del' / 'tru'
DUST_LAW = 'kc' # 'calzetti' / 'mw' / 'kc' / 'noll'
# E_B = 1 # only define for 'noll' dust law
# delta = -0.2 # only define for 'noll' dust law
MY_SFH = ''
#--- DEFINE GRID -------------------------------------------------------
#
# o Choose only values for tau and metallicity that are in your library.
# Otherwise extend your library.
#
# o If EAZY is used, make sure Z_MIN, Z_MAX are similar.
#
# o METAL: the options differ per stellar population library
# ma05: Z=0.001, Z=0.01, Z=0.02 [solar], and Z=0.04
# bc03: Z=0.004, Z=0.008, Z=0.02 [solar], and Z=0.05
# co11: Z=0.0008, Z=0.0031, Z=0.0096, Z=0.019 [solar], and Z=0.03
# You can choose more than one by defining an array.
#
# o If a grid has already been made for a specific LIBRARY, RESOLUTION,
# IMF, tau, age, z, A_v, metallicity, and filter set and/or spectral
# elements, the grid will be automatically read from the "tmp"
# directory.
#
# o NO_MAX_AGE: By default (0), ages that exceed the age of the universe
# are not allowed. However, when NO_MAX_AGE is put to 1 you can have
# older ages.
#
#-----------------------------------------------------------------------
LOG_TAU_MIN = 8.5 # log [yr]
LOG_TAU_MAX = 10. # log [yr]
LOG_TAU_STEP = 0.5 # log [yr], min 0.1
LOG_AGE_MIN = 8.0 # log [yr]
LOG_AGE_MAX = 10.0 # log [yr]
LOG_AGE_STEP = 0.2 # log [yr]
NO_MAX_AGE = 0 # 0 / 1
Z_MIN = 0.01 # Cannot be 0.
Z_MAX = 6.00
Z_STEP = 0.05
Z_STEP_TYPE = 0 # 0: Z_STEP, 1: Z_STEP*(1+z)
A_V_MIN = 0. # [mag]
A_V_MAX = 3. # [mag]
A_V_STEP = 0.1 # [mag]
METAL = [0.019] # [0.0096,0.019,0.03]
#--- COSMOLOGY ---------------------------------------------------------
#
#-----------------------------------------------------------------------
H0 = 70.0 # Hubble constant
OMEGA_M = 0.3 # Omega matter
OMEGA_L = 0.7 # Omega lambda
#--- SAVE INTERMEDIATE PRODUCTS ----------------------------------------
#
# - SAVE_CHI_GRID: if "1" then the temporary grid per objects will be
# saved as an idl ".save" file in the "tmp" directory. This option
# slows down the program.
#
#-----------------------------------------------------------------------
SAVE_CHI_GRID = 0 # 0 / 1