On the X-ray, optical emission line and black hole mass properties of local Seyfert galaxies !

By F. Panessa, L. Bassani, M. Cappi, Mauro Dadina, X. Barcons, F. J. Carrera, Luis C. Ho, K. Iwasawa. 2006

277 citations recorded by the source corpus.

We investigate the relation between X-ray nuclear emission, optical emission line luminosities and black hole masses for a sample of 47 Seyfert galaxies. The sample, which has been selected from the Palomar optical spectroscopic survey of nearby galaxies (Ho et al. 1997a, ApJS, 112, 315), covers a wide range of nuclear powers, from L2" 10keV # 10 43 erg/s down to very low luminosities (L2" 10keV # 10 38 erg/s). Best available data from Chandra, XMM-Newton and, in a few cases, ASCA observations have been considered. Thanks to the good spatial resolution available from these observations and a proper modeling of the various spectral components, it has been possible to obtain accurate nuclear X-ray luminosities not contaminated by o! -nuclear sources and/or di! use emission. X-ray luminosities have then been corrected taking into account the likely candidate Compton thick sources, which are a high fraction (>30%) among type 2 Seyferts in our sample. The main result of this study is that we confirm strong linear correlations between 2-10 keV, (OIII)! 5007, H" luminosities which show the same slope as quasars and luminous Seyfert galaxies, independent of the level of nuclear activity displayed. Moreover, despite the wide range of Eddington ratios (L/LEdd) tested here (six orders of magnitude, from 0.1 down to # 10 " 7 ), no correlation is found between the X-ray or optical emission line luminosities and the black hole mass. Our results suggest that Seyfert nuclei in our sample are consistent with being a scaled-down version of more luminous AGN.

Subfields: Astronomy and Astrophysics, Radiation

View Paper: https://www.semanticscholar.org/paper/5e6013ab64850625f32d28c21307a1b7a65af656

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In Astronomy and Astrophysics

1. D. M. Alexander
2. P. Hopkins
3. L. Hernquist
4. Mara Salvato
5. W. N. Brandt
6. A. Koekemoer
7. R. Hickox
8. H. Netzer

In Radiation

1. C. Ricci
2. Y. Ueda
3. Poshak Gandhi
4. M. Koss
5. B. Trakhtenbrot
6. Mara Salvato
7. M. Brightman
8. Luis C. Ho

Citations in the corpus

• Faint high-redshift AGN in the Chandra deep field south: the evolution of the AGN luminosity function and black hole demography (2011, background): “The fraction of these objects in the local Universe is high: 30–50% of the optically selected Seyfert 2 galaxies can be Compton thick (≈1/4−1/3 of the full AGN population, Risaliti et al. (1999), Panessa et al. (2006), a result confirmed by hard X-ray selection, see Malizia et al. 2009).”
• The subarcsecond mid-infrared view of local active galactic nuclei – II. The mid-infrared–X-ray correlation (2015, methodology): “Furthermore, Panessa et al. (2006) argue that the XMM-Newton data on this source is significantly contaminated by off-nuclear emission and thus not usable to extract information about the nucleus.”
• Resolving the mid-infrared cores of local Seyferts (2009, methodology): “From the raw [Oiii] λ5007 optical emission line measurement of Gu et al. (2006) along with the type-1<F2−10/F[OIII] > relation from Panessa et al. (2006), we deriveL2−10∼ 1.1×1042 erg s−1.”
• An X-ray view of 82 LINERs with Chandra and XMM-Newton data (2009, background): “Nearby examples of both Seyfert 2 (Maiolino et al., 1998; Risaliti et al., 1999; Page et al., 2003; Cappi et al., 2006; Panessa et al., 2006), and Seyfert 1 (Nandra et al., 2007) or PG-QSOs (Piconcelli et al., 2005; Jimenez-Bailon et al., 2005) have been studied.”
• BAT AGN Spectroscopic Survey. I. Spectral Measurements, Derived Quantities, and AGN Demographics (2017, background): “AGN with contradictory optical and X-ray classification So-called “naked” AGN candidates (Hawkins 2004; Panessa et al. 2006) are objects showing an optical spectrum with no detectable broad emission lines in the optical (Seyfert 2) and no obscuration in the X-rays (NH< 1020.5 cm−2).”
• On the origin of radio emission in radio-quiet quasars (2008, methodology): “Systematic analysis of radio (Ho & Ulvestad 2001) and X-ray (Panessa et al. 2006) observations is available for all 12 objects.”
• Biases in Virial Black Hole Masses: An SDSS Perspective (2007, result): “These Eddington ratio values are in good agreement with the typical Eddington ratios from X-ray selected AGN samples which cover the bolometric luminosity range Lbol ∼ 1041 − 1044 erg s−1 (e.g., Panessa et al. 2006; Babić et al. 2007; Ballo et al. 2007).”
• OBSCURATION-DEPENDENT EVOLUTION OF ACTIVE GALACTIC NUCLEI (2015, background): “These include optical (Risaliti et al. 1999; Cappi et al. 2006; Panessa et al. 2006; Akylas & Georgantopoulos 2009; Gilli et al. 2010; Vignali et al. 2010; Jia et al. 2013; Mignoli et al. 2013; Vignali et al. 2014), infrared (e.g. Fiore et al. 2008, 2009; Alexander et al. 2011; Brightman & Nandra…”
• Nuclear Activity in Nearby Galaxies (2008, methodology): “The incidence of X-ray cores in LINERs is somewhat lower than, but still compares favorably to, that found in Palomar Seyferts (∼ 90%), the vast majority of which now have suitable X-ray observations, as summarized in Cappi et al. (2006) and Panessa et al. (2006).”
• ONGOING AND CO-EVOLVING STAR FORMATION IN zCOSMOS GALAXIES HOSTING ACTIVE GALACTIC NUCLEI (2008, methodology): “6a), as shown by the solid line, is similar to previous studies based on a sample of low redshift AGN (e.g., Panessa et al. 2006) shown by the dotted line.”
• Towards a complete census of AGN in nearby Galaxies: a large population of optically unidentified AGN (2009, background): “32 µm luminosities of the mid-IR identified AGNs and a sample of well-studied local AGNs from Panessa et al. (2006) as a function of their [OIII] λ5007Å luminosity.”
• The active nuclei of z < 1.0 3CRR radio sources (2009, background): “For example, Panessa et al. (2006) tabulate 2–10 keV X-ray and [O III] luminosities for a sample of lowluminosity Seyferts and establish a correlation between the two which extends up to intermediate-luminosity Seyfert 1s and PG quasars.”
• X-ray variability of 104 active galactic nuclei - XMM-Newton power-spectrum density profiles (2012, result): “We have compared these luminosities with those for the same objects reported by González-Martı́n et al. (2009); Panessa et al. (2006); O’Neill et al. (2005, and references therein).”
• Unification of X-ray winds in Seyfert galaxies: from ultra-fast outflows to warm absorbers (2012, background): “Regarding Seyfert galaxies in particular, some authors suggested that the radiative efficiency for some of them could be slightly lower than that (Bian & Zhao 2003b; Panessa et al. 2006; Singh et al. 2011).”
• An extreme [O III] emitter at z = 3.2: a low metallicity Lyman continuum source (2015, background): “According to the empirical relation between the [O iii]λ5007 luminosity and the X-ray luminosity (e.g., Panessa et al. 2006), given the extreme [O iii]λ5007 emission the expected X-ray luminosity would be LX ∼ 1045erg s−1 if the [O iii]λ5007 emission is associated to an AGN.”
• The Coincidence of Nuclear Star Clusters and Active Galactic Nuclei (2008, methodology): “Both the Hα and [OIII] luminosities are known to be good indicators of the X-ray and bolometric luminosities of low-luminosity AGN of all types (Ho et al. 2001), including sources with significant absorption in the X-ray (Panessa et al. 2006).”
• Observational evidence for intermediate-mass black holes (2017, background): “9, right), a behavior typical of heavily obscured AGN (e.g., Panessa et al. 2006).”