H-rich white dwarfs at these effective temperatures and surface gravities [e.g. @holberg06] appear to be broadly consistent with the SDSS photometry for DA1 and DA2 (Table \[phot\]).

           SDSS            $T_{\rm eff}$    $B_{\rm dip}$(MG)   $z_{\rm off}({\rm R}_{\rm WD})$   inclination (${}^\circ$)   $M$(M$_{\odot}$)    $\tau_{c}$ (Myr)
  ----------------------- ---------------- ------------------- --------------------------------- -------------------------- ------------------ ---------------------
   J092646.88$+$132134.5    9500$\pm$500      210$\pm$25.1              -0.09$\pm$0.01                  21.8$\pm$7.9          0.62$\pm$0.10     726$^{+140}_{-107}$
   J150746.80$+$520958.0   18000$\pm$1000     65.2$\pm$0.3              -0.39$\pm$0.03                  36.4$\pm$4.1          0.99$\pm$0.05      321$^{+47}_{-40}$
       \[magnetic\]                                                                                                                            

The energy distributions of the DAH components DAH1 and DAH2 have been compared to a grid of model spectra for HFMWDs. These were calculated with a radiative transfer code for magnetised, high gravity atmospheres. The code calculates both theoretical flux (Stokes $I$) and polarization (Stokes $V$) spectra, for a given temperature and pressure structure ($T_{\rm eff}$, $\log g$) and a specific magnetic field vector with respect to the line of sight and the normal on the surface of the star [see @jordan92; @jordan93]. However, as no polarization information is available from our datasets, our analysis has been limited to the flux spectra (Stokes parameter $I$). For computational efficiency, we have made use of our existing three-dimensional grid of synthetic spectra. This grid spans the effective temperature range $7000\,{\rm K}\le T_{\rm eff} \le 50000\,{\rm K}$ in 14 steps, 