Abstract
The aim of this work was to find a correlation between the size of the BLR and the star formation rate. This research is based on the studies elaborated by Kaspi et al. (2000, ApJ, 533,631; 2005, ApJ, 629, 61), Maiolino et al. (2008, A&A, 468,979), Kennicutt (1998, ARAA, 36, 189) and Diamond-Stanic et al.(2012, ApJ, 746, 168). Kaspi et al. (2005, ApJ, 629, 61) using measures of mapping reverberation derived the size of the BLR and correlated this with the emission at 5100Å, λ Lλ(2-10 keV) and other emissions. On the other hand Maiolino et al. (2008, A&A, 468, 979) and Diamond-Stanic et al. (2012, ApJ, 746, 168), derived star formation rates (SFR) using observations in (7.7μm) and (11.3μm). For this study, we estimated the size of the BLR based on observations on hard X-rays, continuous emissions and recombination lines on the hydrogen atom of a sample of Active Nuclei. Besides, we determined the star formation rate based on observations of the emissions of PAHs for the same sample above and the adjustment equation was derived for the expected correlation. Using 17 Seyfert Galaxies with emission in PAH (11.3μm) obtained from IRS SL module (Spitzer Space Telescope Database) and 5100Å from the Nasa-IPAC Extragalactic Database (NED), we made a plot of R(BLR) versus the star formation rate (SFR). In the estimation of R(BLR) size, we used the R(BLR)∝Lα and for the SFR we use SFR∝LPAH. We found that the nuclear star formation rate (SFR) traced by the 11.3μm aromatic feature follows a relationship with the RBLR of the form SFR∝(RBLR0.7.
