Models included

In order to estimate an age for a white dwarf a chain of models have to be used. Here are the models included in \(\texttt{wdwarfdate}\).

\(\texttt{wdwarfdate}\)
Models Included	Cooling Models	Cooling tracks from the Montreal White Dwarf Group available online (Berdard et al. 2020): Thick H layer (DA) Thin H layer (non-DA)
	IFMR	Marigo et al. (2020) Cummings et al. (2018) MIST and PARSEC based. Salaris et al. (2009) Williams et al. (2009)
	Stellar evolution models	MESA Isochrones available online (Choi et al. 2016 and Dotter 2016): \([{\rm Fe/H}] = -4.00, -1.00, 0.00, 0.50\) \({\rm v/vcrit} = 0.0, 0.4\) \([\alpha/{\rm Fe}] = 0\)

Constraints

We summarize here the most important constraints when using \(\texttt{wdwarfdate}\). For a complete discussion see Kiman et al. 2022.

Combining the limitation of the cooling tracks with the restrictions of the IFMR, the values for which \(\texttt{wdwarfdate}\) can estimate a total age are \(1,500 \lesssim T_{\rm eff} \lesssim 90,000\,{\rm K}\) and \(7.9 \lesssim \log g \lesssim 9.3\).
Given that the cooling tracks assume single star evolution and C/O core for the white dwarfs, the best range of final masses to use \(\texttt{wdwarfdate}\) is \(0.45-1.1\,{\rm M}_{\odot}\), because outside this range objects are not likely to have evolved as a single star.