On the Relationship between the Optical Emission‐Line and X‐Ray Luminosities in Seyfert 1 Galaxies

Abstract

We have explored the relationship between the [O III] λ5007 and the 2-10 keV luminosities for a sample of Broad-and Narrow-Line Seyfert 1 galaxies (BLSy1 and NLSy1, respectively). We find that both types of Seyferts span the same range in luminosity and possess similar [O III]/X-ray ratios. The NLSy1s are more luminous than BLSy1s, when normalized to their central black hole masses, which is attributed to higher mass accretion rates. However, we find no evidence for elevated [O III]/X-ray ratios in NLSy1s, which would have been expected if they had excess EUV continuum emission compared to BLSy1s. Also, other studies suggest that the gas in narrow-line regions (NLR) of NLSy1s and NLSy1s span a similar range in ionization, contrary to what is expected if those of the former are exposed to a stronger flux of EUV radiation. The simplest interpretation is that, like BLSy1s, a large EUV bump is not present in NLSy1s. However, we show that the [OIII]/X-ray ratio can be lowered as a result of absorption of the ionizing continuum by gas close to the central source, although there is no evidence that intrinsic line-of-sight absorption is more common among NLSy1s, as would be expected if there were a larger amount of circumnuclear gas. Other possible explanations include: 1) anisotropic emission of the ionizing radiation, 2) higher gas densities in the NLR of NLSy1s, resulting in lower average

The mid IR – hard X-ray correlation in AGN and its implications for dusty torus models

“…After converting their result to our Cosmology, we get L 2−10 keV = 1.5 × 10 42 erg s −1 and a column density of N H = (7.2 ± 1) × 10 21 cm −2 . Older observations by Malizia et al (1997);Turner et al (1997);Risaliti (2002); Risaliti et al (2002) and Kraemer et al (2004) are in good agreement with these numbers if one accounts for the different cosmological parameters used.…”

What controls the [O III] 5007 line strength in active galactic nuclei?

“…Interestingly, there is no significant correlation of CF and L / L Edd (taken from BL05; r S =−0.133, Pr = 0.41). Such a relation was suggested by BG92 as the physical mechanism driving the set of EV1 correlations (see also Kraemer et al 2004).…”

A MINOR MERGER CAUGHT IN THE ACT OF FUELING THE ACTIVE GALACTIC NUCLEUS IN Mrk 509

“…Using M BH = 1.43 × 10 8 M (Peterson et al 2004) we calculate an Eddington luminosity of L edd = 1.8 × 10 46 erg s −1 . With an X-ray luminosity of L 2-10keV = 1.17 × 10 44 erg s −1 (Kraemer et al 2004, and references therein) and a bolometric correction of 30 (Awaki et al 2001), we calculate a bolometric luminosity of L bol = 3.5 × 10 45 erg s −1 , and an Eddington ratio of L/L edd = 0.19 for Mrk 509. If we use the Kraemer et al (2004) …”

“…As part of a recent project to map the kinematics of the narrow line region (NLR) of Seyfert galaxies (Fischer et al 2013), we obtained WFC3 [O iii] and continuum (F550M) images of Mrk 509, a nearby (z = 0.0346, 1 ∼ 700 pc), highly luminous (L bol = 3.5 × 10 45 erg s −1 , Awaki et al 2001;Kraemer et al 2004) Type 1 AGNs, where we discovered an asymmetric filament adjacent to the nucleus, shown in Figure 1. The majority of the filament is a linear feature several kiloparsecs long to the west of the nucleus, stretching from northwest to southeast, and is most prominent at radii <2100 pc, inside the massive starburst ring which surrounds the AGN (although it does extend beyond the ring; Figure 1).…”