Let's start

Fill in the parameter list with your data

Stellar observables

Enter with stellar observed parameters together with their 1σ errors (here assumed to be Gaussian):
Effective temperature: T eff = ± K
Metallicity: [Fe/H] = ± dex
Logarithm of surface gravity: logg = ± dex
Luminosity: L = ± L/L
Parallax1: ϖ = ± mas
Asteroseismic parameters:
Frequency of maximum oscillation power: νmax = ± μHz
Large frequency separation2: Δν = ± μHz
Period spacing3: ΔP = ± s

1 Parallax is only taken into consideration when using method 1 step. See more details here.
2 For PARSEC models, Δν are computed using scaling relation, while for MESA models, they are computed from the calculations of individual radial-mode frequencies. Read more here.
3 ΔP is only taken into consideration for MESA models.
NOTE: if you do not have a given input parameter, fill in the form with -99.9.

Photometric systems

Choose among the available photometric systems, briefly described here:

  and     to update the table bellow.

Keep the header and enter apparent magnitudes in the following order:

Stellar models

Select the set of evolutionary tracks:

Mass-loss on RGB using the Reimers formula with η Reimers =

Solar values: Δν = μHz, νmax = μHz

Bayesian priors

Select the Bayesian priors:
Flat prior for age in the interval from yr to yr.
Prior on mass -- initial mass function:
Prior on evolutionary stage:


Select the Bayesian method: