A Survey of Seyfert AGN: Nuclear Gas Disks and Direct Black Hole Mass Estimates

Hicks, E. K. S.; Davies, Richard; Malkan, Matthew A.; Genzel, R.; Tacconi, L. J.

doi:10.1017/s1743921310006125

Cited by 1 publication

(1 citation statement)

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“…Several sources of uncertainties can be identified and are also partly discussed in Scharwächter et al (2013). (I) The spatial resolution should be such to allow a resolution at least 2.5 times the sphere of influence of the BH (Hicks et al, 2010), while that on IFU data for NGC 1275 can barely relove it. Even though improved by adaptive optics corrections, the resolution of IFU data in Scharwächter et al (2013) does not allow to resolve well enought the BH sphere of influence.…”

Section: Ngc 1275: Properties and Bh Mass Estimatementioning

confidence: 99%

NGC 1275: An Outlier of the Black Hole-Host Scaling Relations

Sani

Ricci

Franca

et al. 2018

Front. Astron. Space Sci.

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The active galaxy NGC 1275 lies at the center of the Perseus cluster of galaxies, being an archetypal BH-galaxy system that is supposed to fit well with the M BH -host scaling relations obtained for quiescent galaxies. Since it harbors an obscured AGN, only recently our group has been able to estimate its black hole mass. Here our aim is to pinpoint NGC 1275 on the less dispersed scaling relations, namely the M BH -σ ⋆ and M BH − L bul planes. Starting from our previous work , we estimate that NGC 1275 falls well outside the intrinsic dispersion of the M BH -σ ⋆ plane being 1.2 dex (in black hole mass) displaced with respect to the scaling relations. We then perform a 2D morphological decomposition analysis on Spitzer/IRAC images at 3.6 µm and find that, beyond the bright compact nucleus that dominates the central emission, NGC 1275 follows a de Vaucouleurs profile with no sign of significant star formation nor clear merger remnants. Nonetheless, its displacement on the M BH − L 3.6,bul plane with respect to the scaling relation is as high as observed in the M BH -σ ⋆ . We explore various scenarios to interpret such behaviors, of which the most realistic one is the evolutionary pattern followed by NGC 1275 to approach the scaling relation. We indeed speculate that NGC 1275 might be a specimen for those galaxies in which the black holes adjusted to its host.Keywords: AGN1, AGN2, black hole mass, scaling realtions, infrared, NGC 1275 OVERVIEWAlthough active galactic nuclei (AGN) are divided in many flavors, the Unified Model (Antonucci, 1993) explains these observational properties with a line-of-sight-dependent scenario, in which a dusty torus makes the emission anisotropic. Nowadays however there is growing observational evidence that type 1 AGN (AGN1) and type 2 (AGN2) are actually characterized by intrinsically different physical properties [e.g., different luminosity functions (La Franca et al., 2005;Ueda et al., 2015); accretion rates (Winter et al., 2010); intrinsic X-ray luminosity and black hole (BH) masses (Tueller et al., 2008)]. Thanks to our new virial relation based on unbiased physical quantities, i.e., hard X-ray luminosity and Paβ emission line FWHM, we have been able to measure, for the first time, with virial methods the supermassive black hole mass (M BH ) of AGN2 (La Franca et al., 2015Onori et al., 2017b), whose values have been up today estimated using scaling relations.Sani et al. NGC1275: Outlier of BH-Host RelationsThese relations are calibrated on AGN1 and are unlikely to hold also for all AGN2 (Graham, 2008). With direct virial masses for AGN2, we can investigate the relation between the M BH and the bulge properties, thus putting a missing piece to the AGN/galaxy coevolution puzzle. By selecting unbiased samples of type 1 and type 2 AGN, we have found that in the luminosity range 42.5 < log(L X /erg s −1 ) < 44.5, where the two distributions of main AGN types overlap, AGN2 show, on average, significantly smaller Paβ and HeI FWHM than AGN1 (1,970 km/s instead of 3,400 km/s). As expecte...

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Section: Ngc 1275: Properties and Bh Mass Estimatementioning

confidence: 99%