mistfit 0.7.2

Fit MIST models using MiniMINT with dynesty nested sampling (photometry + spectroscopic constraints).

Nested Sampling MIST fitter

Nested-sampling stellar-parameter fits using dynesty + minimint (MIST isochrones with extinction).

This package provides a single public function, fit_stars_with_minimint, which takes an astropy.table.Table containing photometry (and optionally spectroscopy, parallax, and reddening priors), and returns the same table with posterior summaries appended. A simple CLI is also included.

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Citation

If this tool is used in a publication, please cite dynesty, minimint, and Cavieres (in prep).

Quick start

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Installation & requirements

• Python ≥ 3.9 recommended
• Dependencies: numpy, scipy, matplotlib (headless OK), astropy, dynesty, minimint, corner (optional, for debug corner plots)

Install with pip (example):

pip install mistfit

Python example

from astropy.table import Table
from mistfit import fit_stars_with_minimint

if __name__ == "__main__":
    tab = Table.read("xshooter_with_phot_gaia_minimint.fits")
    out = fit_stars_with_minimint(
        tab,
        output_path="xshooter_nested",
        nlive=5000,
        processes=8,
        debug=True,
    )

CLI

# run a nested fit on an input catalog (FITS/ECSV supported by Astropy)
mistfit /path/to/input_table.fits \
  --outdir /path/to/out \
  --nlive 5000 \
  --dlogz 0.01 \
  --procs 8 \
  --debug

The outputs are written to --outdir: --outdir will be created if it doesn’t exist; results are saved as fit_results.fits (or .ecsv fallback).

• Updated table with appended posterior columns: fit_results.fits (or .ecsv if FITS types conflict)
• If --debug, per-star folders with runplot.png, traceplot.png, corner.png, optional isochrone_check.png, and summary.json.

Helpful commands:

mistfit --help

module form (works even without the console script on PATH)

python -m mistfit.cli --help

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Input table format

Minimum requirement: ≥ 3 photometric bands recognized by minimint and their per-band uncertainties, using the naming conventions below. Each row corresponds to one star. A source_id column is recommended (used to name per-star debug folders), but not required.

Column names and uncertainty suffixes

• Photometric band columns use the minimint band names (see list below). Examples: Gaia_G_EDR3, DECam_g, 2MASS_Ks.

• The uncertainty column for a quantity <NAME> is discovered by trying these suffixes (first match wins):

  • <NAME>_ERR, <NAME>_ERRMAG, <NAME>_SIG, <NAME>_E

  Examples: DECam_g_ERR, Gaia_BP_EDR3_ERR, Teff_ERR, PARALLAX_E.

Supported photometric bands (subset)

The code auto-detects any of the following present in your table (case-sensitive): Bessell_I, PS_z, 2MASS_Ks, SkyMapper_u, Gaia_RP_MAW, Gaia_RP_DR2Rev, Gaia_BP_EDR3, PS_w, PS_r, SDSS_g, SkyMapper_v, Bessell_V, PS_y, SDSS_r, Bessell_U, Gaia_BP_DR2Rev, WISE_W1, PS_i, Tycho_V, SDSS_i, WISE_W4, Gaia_G_EDR3, Gaia_RP_EDR3, SkyMapper_r, Gaia_BP_MAWb, SDSS_z, Tycho_B, Bessell_B, DECam_i, Gaia_G_DR2Rev, DECam_Y, 2MASS_J, Kepler_Kp, DECam_u, GALEX_FUV, GALEX_NUV, PS_open, SDSS_u, DECam_r, SkyMapper_g, SkyMapper_z, PS_g, Kepler_D51, DECam_g, Bessell_R, DECam_z, Hipparcos_Hp, WISE_W2, TESS, 2MASS_H, WISE_W3, SkyMapper_i, Gaia_G_MAW, Gaia_BP_MAWf.

Gaia special case: If all three Gaia EDR3 bands (Gaia_G_EDR3, Gaia_BP_EDR3, Gaia_RP_EDR3) are present and have uncertainties, a color-dependent extinction law is used for those bands; otherwise fixed extinction coefficients from the table below are used.

Optional spectroscopy and priors

• Effective temperature: Teff with Teff_ERR (or any allowed suffix). A minimum systematic floor of 100 K is added internally.
• Surface gravity: logg with logg_ERR. A minimum 0.1 dex floor is added.
• Metallicity prior: Either FEH_CAL or FEH with matching error column. A minimum 0.1 dex floor is added. If neither is present, [Fe/H] is free within global bounds.
• Parallax prior: PARALLAX with PARALLAX_ERR. Optional zero-point correction in PARALLAX_ZPC is added to PARALLAX before use. Only positive effective parallaxes are used; otherwise the sampler falls back to a wide distance prior.
• Reddening prior: EBV with optional EBV_ERR. If EBV is present without an error, an uncertainty of 0.3 mag is assumed.

Photometry error floor

For each band’s magnitude uncertainty, a 0.1 mag systematic floor is added internally.

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How the fit works (parameters & priors)

The sampler explores a 5D parameter vector:

• Mass [M☉], prior ~ Salpeter (α = 2.35) within [0.1, 5.0] and model’s maximum mass for the chosen age/metallicity
• log10(Age/yr) uniform in [5.0, 10.1139]
• [Fe/H]: truncated normal around the provided prior (if any), else uniform in [-2.9, 0.9]
• Distance [pc]: from parallax prior if provided; otherwise log-uniform in [1e3, 2e5]
• E(B−V): uniform in [EBV_MIN, EBV_MAX], default [0.0, 1.5], or tightened to ±5σ around the EBV prior (clipped to [0, 1.5]).

Likelihood combines photometry (with extinction and distance modulus) and, when available, spectroscopic terms for Teff and logg.

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Behavior in common scenarios

• Photometry-only mode: Triggered when both Teff and logg are not simultaneously available with errors. The fit still runs using photometry (and any priors) and reports posteriors. This is the default for most catalog-only use cases.

• Missing parallax: No PARALLAX prior → distance prior becomes wide log-uniform [1e3, 2e5] pc. If PARALLAX is present but ≤0 after adding PARALLAX_ZPC, it is ignored and the wide prior is used.

• Missing EBV: No EBV column → E(B−V) prior is uniform over the global ebv_range (default [0.0, 1.5]). If EBV exists without an error, we assume EBV_ERR = 0.3 mag and set the prior to ±5σ around that value (clipped to [0, 1.5]).

• Photometry naming mismatches: Columns must exactly match supported minimint band names. If your catalog uses different names, rename columns before running (see snippet below).

• Gaia extinction: If Gaia triplet (G,BP,RP) is available with errors, a color-dependent law is iteratively applied; otherwise scalar A_λ/E(B−V) coefficients are used.

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Outputs

For each star, the following columns are appended:

• mass_p16, mass_p50, mass_p84, mass_multimodal
• logage_p16, logage_p50, logage_p84, logage_multimodal
• feh_p16, feh_p50, feh_p84, feh_multimodal
• dist_pc_p16, dist_pc_p50, dist_pc_p84, dist_multimodal
• ebv_p16, ebv_p50, ebv_p84, ebv_multimodal
• lnZ, lnZ_err (Bayesian evidence and its uncertainty from dynesty)

Multimodality flags are binary and computed by KDE peak counting on the 1D posterior for each parameter (requires ≥200 samples; peak prominence ≳ 5% of max). 1 indicates multiple significant modes.

If debug=True, per-star artifacts are saved under output_path/<source_id>/:

• runplot.png, traceplot.png, corner.png
• isochrone_check.png (only if Gaia G and Teff are present)
• summary.json containing mode, bands used, p50 values, and lnZ

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Extinction coefficients (A_λ / E(B−V))

When not using the Gaia color-dependent law, these coefficients are applied:

• Gaia EDR3: G=0.83627×3.1, BP=1.08337×3.1, RP=0.63439×3.1
• DECam: g=3.451, r=2.646, i=2.103, z=1.575, Y=1.515
• SDSS: u=4.871, g=3.560, r=2.681, i=2.400, z=1.899
• 2MASS: J=0.987, H=0.531, Ks=0.164
• SkyMapper: u=5.017, v=4.750, g=3.651, r=3.032, i=2.325, z=1.790
• WISE: W1=W2=W3=W4=0.0
• Johnson–Cousins/Bessell: U=5.47, B=4.32, V=3.31, R=2.68, I=1.85

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Tuning & performance

• nlive: Initial live points for dynesty’s dynamic sampler (nlive_init). Larger values better resolve multi-modality and tails, at higher cost. Typical: 2000–8000.
• dlogz: Evidence tolerance (dlogz_init). Smaller is more thorough.
• processes: Number of processes in an internal multiprocessing.Pool. One nested run is executed per star, but dynesty also parallelizes within a run.
• random_seed: Seeds the RNG for reproducibility across stars.
• ebv_range: Global E(B−V) bounds when no star-specific EBV prior is available.

Checkpoints (*_checkpoint.h5) are written only if debug=True.

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End-to-end minimal schema examples

Photometry-only (Gaia + DECam)

Required (any ≥3 bands with errors):

source_id
Gaia_G_EDR3, Gaia_G_EDR3_ERR
Gaia_BP_EDR3, Gaia_BP_EDR3_ERR
Gaia_RP_EDR3, Gaia_RP_EDR3_ERR
DECam_g, DECam_g_ERR

Optional priors:

EBV, EBV_ERR
PARALLAX, PARALLAX_ERR, PARALLAX_ZPC
FEH (or FEH_CAL), FEH_ERR

Photometry + spectroscopy

Add:

Teff, Teff_ERR
logg, logg_ERR

Renaming helper (example)

# Suppose your catalog has G_BP, G_RP, G (Gaia EDR3). Rename to minimint names:
for old, new in {
    'phot_g_mean_mag': 'Gaia_G_EDR3',
    'phot_bp_mean_mag': 'Gaia_BP_EDR3',
    'phot_rp_mean_mag': 'Gaia_RP_EDR3',
}.items():
    if old in tab.colnames and new not in tab.colnames:
        tab.rename_column(old, new)
# Likewise ensure error columns exist with one of the accepted suffixes.

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API reference

fit_stars_with_minimint(
    table: astropy.table.Table,
    output_path: str,
    nlive: int = 3000,
    dlogz: float = 0.01,
    processes: int = 4,
    debug: bool = False,
    random_seed: int = 42,
    ebv_range: tuple[float, float] = (0.0, 1.5),
) -> Table

Returns the input Table with posterior and diagnostic columns appended, and writes an updated table to output_path.

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Notes & caveats

• Photometric/spectroscopic errors get minimum floors (0.1 mag, 100 K, 0.1 dex) to account for systematics.
• Distance prior reverts to broad log-uniform if parallax is unusable (non-positive after ZP correction).
• Evidence (lnZ) can be compared between phot-only vs spec+phot runs for model comparison, but be mindful of different likelihood terms.
• Multimodality flags are heuristic; inspect posteriors/plots for complex cases.

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License

Do whatever you want, fully open source