FAST++ aborts while running with JWST filters

I am trying to run FAST++ on some JWST photometry and every time I run the parameter file it always aborts.

I use the new FILTERS.RES file from EAZY that includes the JWST filters.

Here is the parameter file (most of them are the default parameters and I use absolute paths):

#... FAST++ V1.2: 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++ may not work properly!
#
# o Requirements:
#   - about 30 MB of free RAM memory
#   - at least one CPU core
#
# o The current directory should contain the following files:
#   - This parameter file
#   - [CATALOG].cat        If you fit broadband photometry
#   - [CATALOG].zout       If you input photometric redshifts
#   - [CATALOG].lir        If you input infrared luminosities
#   - [CATALOG].translate  If you input a translate file
#   - [SPECTRUM].spec      If you fit spectra
#
# o FAST++ runs from the command line.
#   The first argument is the parameter file. Default is 'fast.param'
#   $ fast++
#   $ fast++ my_fast.param
#
# o VERBOSE: set to 0 to disable output in the terminal (except for
#   warnings and errors, which are always shown)
#
# o PARALLEL: sets which part of the code should be executed in parallel.
#    - 'none': (default) no parallelization, the code will execute on
#      one CPU.
#    - 'generators': each model will be generated and adjusted to the
#      photometry in a separate thread. Good when you have a huge number
#      of models and very few galaxies to fit. Will fallback to 'models'
#      if a model cache exists.
#    - 'models': each model will be adjusted to the photometry in a
#      separate thread, but models are generated in the main thread only.
#      Good when you have many models and few galaxies to fit, or when
#      the models were already generated and cached on the disk.
#    - 'sources': the input catalog will be split into equal parts, and
#      each part will be analyzed in a separate thread. Good when you
#      have few models but lots of galaxies.
#
# o N_THREAD: sets the maximum number of threads the program can use at
#   once. This should be close to (or equal to) the number of available
#   cores on your CPU, or one less than the number of nodes available on a
#   cluster. Setting this to zero will disable parallelization. Note that,
#   to enable parallel execution, you also need to change PARALLEL to
#   something other than 'none'.
#
# o MAX_QUEUED_FITS: sets the maximum number of fits that are queued and
#   waiting to be executed by the worker threads. Increasing this value
#   will make the code run faster, but will also increase memory usage.
#   For a run on a desktop computer with no more than 10 threads, a value
#   of 1000 provides a good compromise; larger values do not improve
#   performances significantly (no more than 10%).
#
#-----------------------------------------------------------------------

VERBOSE         = 1         # 0 / 1
PARALLEL        = 'generators'    # 'none', 'generators', 'models', or 'sources'
N_THREAD        = 4         # 0, 1, 2, 3, 4, etc
MAX_QUEUED_FITS = 10000

#--- 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
#   - If z_spec is not given or any negative value, no z_spec is assumed
#   - Give a negative error or "NaN" 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 intervals
#   - If input photo-z is a negative value, the photo-z will be ignored
#   - 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: AB_ZEROPOINT = 23.9
#   - fluxes in micro Janskys: AB_ZEROPOINT = 23.9
#   - fluxes in erg sec^{-1} cm^{-2} Hz^{-1}: AB_ZEROPOINT = 48.6
#
# 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.
#
# 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'
#
# o FORCE_ZPHOT: if set to 1, tells the program to treat the photometric
#   redshifts as spectroscopic redshifts.
#
# o BEST_AT_ZPHOT: if set to 1, tells the program to force the best-fit
#   solution to match the photometric redshift obtained by EAzY, but the
#   confidence intervals will still account for the uncertainty on the
#   redshift (note that these intervals may not be centered on the best-
#   fit solution if this option is enabled).
#
# o ZPHOT_CONF: tells which confidence interval of the photometric
#   redshifts should be used to limit the grid for each galaxy.
#   Redshifts outside of this confidence interval will not be considered.
#
# o USE_LIR: if set to 1 and [CATALOG].lir exists, FAST++ will read
#   infrared luminosities from this file and use them to constrain the
#   fit. Must contain columns: id, lir and elir. The observed luminosities
#   (given in units of total solar luminosity) are compared to the
#   modelled difference of bolometric luminosity before and after dust
#   attenuation is applied to the model. This can help break degeneracies,
#   but requires that the redshift is well known. The file can contain a
#   fourth column, labelled 'log', which is a 0/1 flag that determines if
#   the LIR value is given in log10 units or in natural units. This
#   changes the way the uncertainty is interpreted: with log=0 the
#   uncertainty is assumed to be Gaussian (additive), but with log=1 the
#   uncertainty is assumed to be log-normal (multiplicative). Therefore
#   when log=1, the 'elir' column must contain the 1-sigma uncertainty on
#   log10(LIR).
#
#-----------------------------------------------------------------------

CATALOG        = '/Users/nikhilgaruda/Documents/Astronomy_Research/G165/fast/img_fam'
AB_ZEROPOINT   = 0.
FILTERS_RES    = '/Users/nikhilgaruda/Documents/Astronomy_Research/G165/Photometry/EAZYpy/eazy/data/filters/FILTER.RES.latest'
FILTER_FORMAT  = 1
TEMP_ERR_FILE  = ''
NAME_ZPHOT     = 'z_m1'
FORCE_ZPHOT    = 0          # 0 / 1
BEST_AT_ZPHOT  = 0          # 0 / 1
ZPHOT_CONF     = 68         # 68 / 95 / 99
USE_LIR        = 0          # 0 / 1

#--- SPECTROSCOPIC INFORMATION -----------------------------------------
#
# o SPECTRUM:
#   - Example file: "1030_gnirs.spec"
#   - The file should have the following format:
#     # bin wl_low wl_low F[id1] E[id1] F[id2] E[id2] ...
#   - bin: ID of the bin in which the spectral element falls
#   - wl_low: lower wavelength of the spectral element in Angstrom
#   - wl_up: upper wavelength of the spectral element in Angstrom
#   - (e)fl: in 10^-19 ergs s-1 cm-2 Angstrom-1 (these units do not
#     matter if AUTO_SCALE is set to 1)
#   - id[.]: should be an ID in the flux catalog
#   - Missing values can be signaled with negative errors or "NaN".
#
# o AUTO_SCALE: This option automatically adjusts the spectrum to the
#   model separately from the rest of the photometry. The spectrum thus
#   does not participate in determining the best amplitude of the
#   model, but still participates in the chi2. This can account for
#   uncertain flux calibration of the spectrum, and will emphasize more
#   the features of the spectrum rather than it's absolute flux level.
#   Note that when this feature is enabled, the template error function,
#   if used, will not be applied to the spectral data.
#
# o APPLY_VDISP: Velocity dispersion of the spectral templates. Setting
#   this parameter to a non-zero value will broaden the templates with
#   a fixed velocity dispersion before the fit. This is only relevant
#   when fitting spectra, and has an impact on performances (a couple
#   seconds of extra delay), so it is disabled by default.
#
#-----------------------------------------------------------------------

SPECTRUM       = ''
AUTO_SCALE     = 0          # 0 / 1
APPLY_VDISP    = 0          # km/s

#--- 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 determine 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 in the 'best_fits' directory
#
# o BEST_FROM_SIM: use the median of the Monte Carlo simulation as
#   best-fit instead of the model with the smallest chi squared on
#   the original (unperturbed) photometry.
#
# o INTERVAL_FROM_CHI2: use the chi2 grid directly to compute confidence
#   intervals on the fit parameters, instead of using Monte Carlo
#   simulation. This will force setting 'SAVE_BESTCHI' to a value large
#   enough to encompass the chosen confidence intervals.
#
# o SAVE_SIM: save the best-fit parameters for each Monte Carlo
#   simulation for all sources in the "best_fits" directory.
#
# o SFR_AVG: output the SFR as the average of the 'SFR_AVG' last million
#   years. If set to zero (the default) FAST++ will output the
#   instantaneous SFR.
#
# o INTRINSIC_BEST_FIT: if BEST_FIT=1, setting this option to 1 will also
#   output the intrinsic best-fit SED of the galaxy, as it would be seen
#   without dust obscuration. This intrinsic SED is saved as a third
#   column in the best-fit SED file.
#
# o BEST_SFHS: if set to 1, the program will output the best-fit star
#   formation history along with the best fit SEDs. If Monte Carlo
#   simulations are enabled, the confidence intervals of the SFH will
#   also be written.
#
# o SFH_OUTPUT_STEP: if BEST_SFHS=1, sets the time step of the output SFH
#   in million years. The default is 10 Myr.
#
# o SFH_OUTPUT: 'sfr' will output the evolution of the star formation rate
#   with time, while 'mass' will show the total stellar mass (including
#   mass loss).
#
# o REST_MAG: list of filter ID to use to compute rest-frame magnitudes.
#   These absolute magnitudes are then given at 10pc in the AB system,
#   using AB_ZEROPOINT, and are not corrected for attenuation.
#
# o CONTINUUM_INDICES: file listing the continuum indices (absorption
#   line equivalent-width, Dn4000, ...) to compute from each model
#   spectrum. See examples in the "share/continuum_indices" directory.
#
# o SFH_QUANTITIES: list of SFH quantities to compute for each model.
#   These quantities are computed directly on the SFH functional form
#   of each model, and are thus non-parametric. Available quantites:
#    - 'tsf': shortest time interval over which 68% of SFR took place
#             (= duration of star formation).
#    - 'past_sfr': average SFR during the above time interval
#                  (= mean past SFR).
#    - 'sfr'X : average SFR over the last 'X' Myr.
#    - 'brate'X : 'sfr'X / 'past_sfr' (= birth-rate parameter).
#    - 'tquench'X : elapsed time since the SFR dropped below a factor
#                   'X' of the 'past_sfr' (= time since quenching).
#    - 'tform'X : elapsed time since the galaxy had formed 'X'% of its
#                 current mass (= time since formation).
#
# o OUTPUT_COLUMNS: define here what columns to write in [CATALOG].fout
#   Available columns: id, metal, lage, Av, lmass, lsfr, lssfr, lldust,
#   llion, lmform and chi2. If using the "standard" FAST templates, two
#   additional columns are available: ltau and la2t. If using custom SFH,
#   you can also choose any of your custom SFH parameter. Rest-frame
#   magnitudes specified in 'REST_MAG' are also available, the format is
#   "M[...]" where "[...]" is the filter ID. If this variable is set to
#   an empty array (default), then all available parameters are written
#   in the file (except lldust, llion, and lmform).
#
#-----------------------------------------------------------------------

OUTPUT_DIR         = '/Users/nikhilgaruda/Documents/Astronomy_Research/G165/fast/OUTPUT'
OUTPUT_FILE        = ''
N_SIM              = 100
C_INTERVAL         = [68 ,95]           # 68 / 95 / 99 or [68,95] etc
BEST_FIT           = 1             # 0 / 1
BEST_FROM_SIM      = 0             # 0 / 1
INTERVAL_FROM_CHI2 = 0             # 0 / 1
SAVE_SIM           = 1             # 0 / 1
SFR_AVG            = 0             # 0, 100 Myr, 300 Myr etc
INTRINSIC_BEST_FIT = 0             # 0 / 1
BEST_SFHS          = 1             # 0 / 1
SFH_OUTPUT_STEP    = 1           # 10 Myr, 100 Myr etc
SFH_OUTPUT         = 'sfr'         # 'sfr' or 'mass'
REST_MAG           = []            # [140,142,161] for UVJ colors
CONTINUUM_INDICES  = ''
SFH_QUANTITIES     = ['tsf','past_sfr','sfr10','brate10','tquench10','tform50']            # ['tquench10','tform50','brate10', ...]
OUTPUT_COLUMNS     = ['id','Av','lmass','lsfr', 'metal', 'chi2']            # ['id','Av','lmass','lsfr', ...]

#--- 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'
#
# o CUSTOM_SFH: if you define this option, FAST++ will build a grid of
#   templates on the fly using SSP models, instead of reading the
#   composite models from "csp_galaxev". You can therefore fit any
#   star formation history. The SFH must be a mathematical expression
#   which returns the SFR as a function of the time 't' since the galaxy
#   was born (the unit of the SFR doest not matter). Custom grid parameters
#   can be referenced in this function (see below) but not the age or the
#   dust attenuation.
#
# o CUSTOM_PARAMS: when using CUSTOM_SFH, define here the names of your
#   grid parameters (e.g., log_tau). For each of these parameters you
#   must provide the _MIN, _MAX and _STEP values, as for the other
#   grid parameters.
#
# o CUSTOM_SFH_LOOKBACK: changes the meaning of the time 't' in the SFH
#   expression, so that 't' refers to the lookback time. The instant t=0
#   then refers to the moment where the galaxy is observed, and larger
#   values correspond to earlier times in the past. This is equivalent
#   to substituting 't' for '10^lage - t' in the SFH expression.
#
#-----------------------------------------------------------------------

LIBRARY_DIR         = '/Users/nikhilgaruda/Documents/Documents/Astronomy_Research/Software/fastpp/share/libraries/'
LIBRARY             = 'co11'         # 'bc03' / 'ma05' / 'co11'
RESOLUTION          = 'hr'           # '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              = ''
CUSTOM_SFH          = ''             # '(1 + t)^alpha'
CUSTOM_PARAMS       = []             # ['alpha', ...]
CUSTOM_SFH_LOOKBACK = 0              # 0 / 1
# ALPHA_MIN         = -2             # define these for each parameter
# ALPHA_MAX         = 2              # define these for each parameter
# ALPHA_STEP        = 0.1            # define these for each parameter

#--- 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, A_v_bc, metallicity, and filter set and/or
#   spectral elements, the grid will be automatically read from the cache
#   unless the NO_CACHE option is set to "1". This option will also
#   prevent the code from writing this cache in the first place.
#
# o DIFFERENTIAL_A_V: By default (0), all stars suffer the same amount
#   of extinction by dust. If DIFFERENTIAL_A_V is set to "1", young
#   stars will be place under a thicker screen of dust, as controlled by
#   A_V_BC_MIN, A_V_BC_MAX, A_V_BC_STEP, and LOG_BC_AGE_MAX.
#
# o LOG_BC_AGE_MAX: When DIFFERENTIAL_A_V is set to "1", stars in their
#   birth cloud will be given extra attenuation. Only stars younger than
#   LOG_BC_AGE_MAX are considered to be in their birthcloud. The default
#   of 10 Myr is taken from Charlot&Fall (2001).
#
# 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     = 0.05            # log [yr]
NO_MAX_AGE       = 0              # 0 / 1
Z_MIN            = 0.01           # Cannot be 0.0
Z_MAX            = 14.00
Z_STEP           = 0.01
Z_STEP_TYPE      = 1              # 0: Z_STEP, 1: Z_STEP*(1+z)
A_V_MIN          = 0.             # [mag]
A_V_MAX          = 3.             # [mag]
A_V_STEP         = 0.1            # [mag]
A_V_BC_MIN       = 0.             # [mag]
A_V_BC_MAX       = 0.             # [mag]
A_V_BC_STEP      = 0.1            # [mag]
DIFFERENTIAL_A_V = 0              # 0 / 1
LOG_BC_AGE_MAX   = 7.0            # log [yr]
METAL            = [0.02]         # [0.0096,0.019,0.03]
NO_CACHE         = 1              # 0 / 1

#--- COSMOLOGY ---------------------------------------------------------
#
#-----------------------------------------------------------------------

H0             = 70.0               # Hubble constant
OMEGA_M        = 0.3                # Omega matter
OMEGA_L        = 0.7                # Omega lambda
NO_IGM         = 0                  # 0 / 1

#--- SAVE INTERMEDIATE PRODUCTS ----------------------------------------
#
# o SAVE_CHI_GRID: if "1" then the chi2 grid for all objects will be
#   saved in a ".grid" file in the output directory.
#
# o SAVE_BESTCHI: if anything else than "0", the models with a chi2
#   less than SAVE_BESTCHI different from the best chi2 will be
#   saved in a ".grid" file in the "best_chi2" directory, for each
#   object separately. This will occupy less disk space than the
#   SAVE_CHI_GRID option. Usual values are "1" to have 68% chance of
#   including the "true" model, "2.71" for 90% and "6.63" for 99%.
#   SAVE_CHI_GRID and SAVE_BESTCHI can be enabled together.
#
#-----------------------------------------------------------------------

SAVE_CHI_GRID  = 1          # 0 / 1
SAVE_BESTCHI   = 1          # 1 (68%) / 2.71 (90%) / 6.63 (99%) / etc

Here is the error I get while running the program:

❯ ./fast++ /Users/nikhilgaruda/Documents/Astronomy_Research/G165/fast/fast.param

note: this is FAST++ version '1.3.0-ecf74e2'
note: using instantaneous SFRs
note: applying Madau+1995 IGM absorption
note: computing SFH quantities: {tform50, tsf, past_sfr, tquench10, sfr10, brate10}
note: reading fluxes from '/Users/nikhilgaruda/Documents/Astronomy_Research/G165/fast/img_fam.cat'
note: using column translation file '/Users/nikhilgaruda/Documents/Astronomy_Research/G165/fast/img_fam.translate'
note: ... translated 16 column names
note: reading filters from '/Users/nikhilgaruda/Documents/Astronomy_Research/G165/Photometry/EAZYpy/eazy/data/filters/FILTER.RES.latest'
note: found 417 filters in the database, will use 8 of them
note: reading fluxes...
note: fitting 2 sources with 8 fluxes each
note: reading photometric redshifts from '/Users/nikhilgaruda/Documents/Astronomy_Research/G165/fast/img_fam.zout'
note: define grid...
note: fitting a grid of 599912 templates (ntau=4,nmetal=1,nage=41,nav=31,navbc=1,nz=118)
note: identify zspecs and redshift bounds in the grid...
note: initializing chi2 grid on disk... (expected size 77.8084 MB)
libc++abi: terminating due to uncaught exception of type std::length_error: vector
[1]    47262 abort      ./fast++ /Users/nikhilgaruda/Documents/Astronomy_Research/G165/fast/fast.para

cschreib / fastpp

FAST++ aborts while running with JWST filters #17