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We present the variability study of the lowest-luminosity Seyfert 1 galaxyNGC 4395 based on the photometric monitoring campaigns in 2017 and 2018. Using22 ground-based and space telescopes, we monitored NGC 4395 with a $\sim$5minute cadence during a period of 10 days and obtained light curves in the UV,V, J, H, and K/Ks bands as well as the H$\alpha$ narrow-band. The RMSvariability is $\sim$0.13 mag on \emph{Swift}-UVM2 and V filter light curves,decreasing down to $\sim$0.01 mag on K filter. After correcting for continuumcontribution to the H$\alpha$ narrow-band, we measured the time lag of theH$\alpha$ emission line with respect to the V-band continuum as${55}^{+27}_{-31}$ to ${122}^{+33}_{-67}$ min. in 2017 and ${49}^{+15}_{-14}$to ${83}^{+13}_{-14}$ min. in 2018, depending on the assumption on thecontinuum variability amplitude in the H$\alpha$ narrow-band. We obtained noreliable measurements for the continuum-to-continuum lag between UV and V bandsand among near-IR bands, due to the large flux uncertainty of UV observationsand the limited time baseline. We determined the AGN monochromatic luminosityat 5100\AA\ $\lambda L_\lambda = \left(5.75\pm0.40\right)\times10^{39}\,\mathrm{erg\,s^{-1}}$, after subtracting the contribution of thenuclear star cluster. While the optical luminosity of NGC 4395 is two orders ofmagnitude lower than that of other reverberation-mapped AGNs, NGC 4395 followsthe size-luminosity relation, albeit with an offset of 0.48 dex($\geq$2.5$\sigma$) from the previous best-fit relation of Bentz et al. (2013).

Variability and the size-luminosity relation of the intermediate mass AGN in NGC 4395