Broad Band Photometric Reverberation Mapping of NGC 4395

Abstract

We present results of broad band photometric reverberation mapping (RM) to measure the radius of the broad line region, and subsequently the black hole mass (M${}_{\mathrm{BH}}$), in the nearby, low luminosity active galactic nuclei (AGN) NGC 4395. Using the Wise Observatory's 1m telescope equipped with the SDSS g${}^{\prime }$, r${}^{\prime }$ and i${}^{\prime }$ broad band filters, we monitored NGC 4395 for 9 consecutive nights and obtained 3 light curves each with over 250 data points. The g${}^{\prime }$ and r${}^{\prime }$ bands include time variable contributions from H$\beta$ and H$\alpha$ (respectively) plus continuum. The i${}^{\prime }$ band is free of broad lines and covers exclusively continuum. We show that by looking for a peak in the difference between the cross-correlation and the auto-correlation functions for all combinations of filters, we can get a reliable estimate of the time lag necessary to compute M${}_{\mathrm{BH}}$. We measure the time lag for H$\alpha$ to be $3.6\pm 0.8$ hours, comparable to previous studies using the line resolved spectroscopic RM method. We argue that this lag implies a black hole mass of M${}_{\mathrm{BH}}=(4.9\pm 2.6)\times 10^4$ \Msun .

References in corpus (1)

• Multiwavelength Monitoring of the Dwarf Seyfert 1 Galaxy NGC 4395. III. Optical Variability and X-ray/UV/Optical Correlations

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