We developed an orbit-superposition method for edge-on barred galaxies and evaluated its capability to recover the bar pattern speed $\rm\Omega_p$. We selected three simulated galaxies (Au-18, Au-23, and Au-28) with known pattern speeds from the Auriga simulations and created MUSE-like mock data sets with edge-on views (inclination angles $\theta_{ \rm T}\ge85^\circ$) and various bar azimuthal angles $\varphi_{ \rm T}$. For mock data sets with side-on bars ($\varphi_{ \rm T}\ge50^\circ$), the model-recovered pattern speeds $\rm\Omega_p$ encompass the true pattern speeds $\rm\Omega_T$ within the model uncertainties ($1\sigma$ confidence levels, $68\%$) for 10 of 12 cases. The average model uncertainty within the $1\sigma$ confidence levels is equal to $10\%$. For mock data sets with end-on bars ($\varphi_{ \rm T}\le30^\circ$), the model uncertainties of $\rm\Omega_p$ depend significantly on the bar azimuthal angles $\varphi_{ \rm T}$, with the uncertainties of cases with $\varphi_{ \rm T}=10^\circ$ approaching $\sim30\%$. However, by imposing a stricter constraint on the bar morphology ($p_{ \rm bar}\le0.50$), the average uncertainties are reduced to $14\%$ , and $\rm\Omega_p$ still encompass $\rm\Omega_T$ within the model uncertainties for three of four cases. For all the models that we create in this paper, the $2\sigma$ ($95\%$) confidence levels of the model-recovered pattern speeds $\rm\Omega_p$ always cover the true values $\rm\Omega_T$.
Categories: astro-ph.GA