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We present the first results from a detailed analysis of a new, long($\sim100$ ks) XMM-Newton observation of the narrow-line Seyfert 1 galaxy PG1404$+$226 which showed a large-amplitude, rapid X-ray variability by a factorof $\sim7$ in $\sim10$ ks with an exponential rise and a sharp fall in thecount rate. We investigate the origin of the soft X-ray excess emission andrapid X-ray variability in the source through time-resolved spectroscopy andfractional root-mean-squared (rms) spectral modeling. The strong soft X-rayexcess below 1 keV observed both in the time-averaged and time-resolved spectrais described by the intrinsic disk Comptonization model as well as therelativistic reflection model where the emission is intensive merely in theinner regions ($r_{\rm in}<1.7 r_{\rm g}$) of an ionized accretion disk. Wedetected no significant UV variability while the soft X-ray excess flux variestogether with the primary power-law emission (as $F_{{\rm primary}}\proptoF_{{\rm excess}}^{1.54}$), although with a smaller amplitude, as expected inthe reflection scenario. The observed X-ray fractional rms spectrum isapproximately constant with a drop at $\sim0.6$ keV and is described by anon-variable emission line component with the observed energy of $\sim0.6$ keVand two variable spectral components: a more variable primary power-lawemission and a less variable soft excess emission. Our results suggest the`lamppost geometry' for the primary X-ray emitting hot corona which illuminatesthe innermost accretion disk due to strong gravity and gives rise to the softX-ray excess emission.

Large-amplitude rapid X-ray variability in the narrow-line Seyfert 1 galaxy PG 1404$+$226