The comparison of optical variability of broad-line Seyfert 1 and narrow-line Seyfert 1 galaxies from the view of Pan-STARRS

Abstract

By means of the data sets of the Panoramic Survey Telescope and Rapid Response System (Pan-STARRS), we investigate the relationship between the variability amplitude and luminosity at 5100 Å, black hole mass, Eddington ratio, $R_{\mathrm{Fe}\mathrm{II}}$ ( the ratio of the flux of Fe II line within 4435-4685 Å~to the broad proportion of $\mathrm{H}\beta$ line) as well as $R_{5007}$ (the ratio of the flux [O III] line to the total $\mathrm{H}\beta$ line) of the broad line Seyfert 1 (BLS1) and narrow line Seyfert 1 (NLS1) galaxies sample in g,r,i,z and y bands, respectively. We also analyze the similarities and differences of the variability characteristics between the BLS1 galaxies and NLS1 galaxies. The results are listed as follows. (1). The cumulative probability distribution of the variability amplitude shows that NLS1 galaxies are lower than that in BLS1 galaxies. (2). We analyze the dependence of the variability amplitude with the luminosity at 5100 Å, black hole mass, Eddington ratio, $R_{\mathrm{Fe}\mathrm{II}}$ and $R_{5007}$, respectively. We find significantly negative correlations between the variability amplitude and Eddington ratio, insignificant correlations with the luminosity at 5100 Å. The results also show significantly positive correlations with the black hole mass and $R_{5007}$, significantly negative correlations with $R_{\mathrm{Fe}\mathrm{II}}$ which are consistent with Rakshit and Stalin(2017) in low redshift bins (z<0.4) and Ai et al.(2010). (3). The relationship between the variability amplitude and the radio loudness is investigated for 155 BLS1 galaxies and 188 NLS1 galaxies. No significant correlations are found in our results.

arXiv comment10 pages, 5 figures, accepted by Astrophysics and Space Science, in Press

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