A multiwavelength light curve analysis of the very fast nova V1723 Sco

We have analyzed multiwavelength light curves of the very fast nova V1723 Sco, based on our fully self-consistent nova explosion models. The time-stretching method gives the distance modulus in the $V$ band of $(m-M)_V = 15.3\pm 0.2$. Then the absolute $V$ magnitude reaches $M_{V,\rm max}= m_{V, \rm max} - (m-M)_V= 6.77 - 15.3\pm 0.2 = -8.5\pm 0.2$. Using our fully self-consistent nova outburst model combined with the optically thick winds on a $1.25 ~M_\odot$ white dwarf accreted by a mass accretion rate of $\dot{M}_{\rm acc}=1\times 10^{-9} ~M_\odot$ yr$^{-1}$, we successfully reproduce the overall $V$ light curve with a free-free emission model as well as the supersoft X-ray light curve with a blackbody approximation model. The epoch of the first GeV gamma-ray detection is almost coincident with the epoch of our model $V$ peak. This supports the shock formation mechanism that a strong shock arises soon after the optical $V$ maximum far outside the WD photosphere. We conclude that the shocked shell is optically thin.