Virial M BH of AGN2 with deep NIR spectroscopy and the measure of the local M BH L 3.6,bul relation

Virial M BH of AGN2 with deep NIR spectroscopy and the measure of the local M BH L 3.6,bul relation 1 Università Roma Tre F. Ricci 1, F. Onori, F. La Franca 1, E. Sani, M. Brusa et al. Hidden Monsters, Dartmouth 8-12 August 2016 Federica Ricci (Roma Tre) Dartmouth 8-12 August 2016 1 / 13

Unified Model According to the Unified Model (Antonucci&Miller+85, Urry&Padovani+95), AGN1 and AGN2 are the same objects seen at different viewing angles However AGN1 and AGN2 show different luminosities (e.g. Lawrence&Elvis+82, La Franca+05, Ueda+03,+14) accretion rates (e.g. Winter+10) Eddington ratios (e.g. Lusso+12) Clustering properties (e.g. Hickox+11, Allevato+14, Lanzuisi+15, DiPompeo+16) Federica Ricci (Roma Tre) Dartmouth 8-12 August 2016 2 / 13

Direct measurement of the M BH Are we missing someone? Federica Ricci (Roma Tre) Dartmouth 8-12 August 2016 3 / 13

AGN-Galaxy coevolution Where the BH mass has been measured (mainly in AGN1) very important scaling relations with the bulge properties have been found, suggesting a strong link between the AGN and the host galaxy evolution. Ferrarese&Merritt+00; Gebhardt+00; Kormendy&Richstone+95, Marconi&Hunt+03; Sani+11; Magorrian+98; Haring&Rix+04 Are these relationships valid for AGN2 as well? At least more than half of the AGN are AGN2! Federica Ricci (Roma Tre) Dartmouth 8-12 August 2016 4 / 13

Virial M BH calibrations for AGN: Bulge host morphology dependence? If the scaling relation M BH σ changes according to the bulge host morphology, also the RM M BH changes. Are the SE virial relations changing as well? Federica Ricci (Roma Tre) Dartmouth 8-12 August 2016 5 / 13

Virial M BH calibrations for AGN: Bulge host morphology dependence? NIR virial relations based on the Paβ FWHM (but also Hα, Paα, HeI1.083µm) and the hard-x L 14 195 kev, therefore potentially able to work with low-l AGN1 and AGN2 Goal: see the BLR also in AGN2 F. Ricci, F. La Franca et al. A&A submitted Federica Ricci (Roma Tre) Dartmouth 8-12 August 2016 5 / 13

Project: measure BH masses of AGN2 in the SWIFT/BAT 70-month sample Selected in the 14-195 kev band no incompleteness in the Compton-thin AGN2 population no galaxy contamination in the hard-x L F. Onori, F. La Franca, F. Ricci, et al., MNRAS in press Additional 8 targets to be observed@lbt soon! Federica Ricci (Roma Tre) Dartmouth 8-12 August 2016 6 / 13

NIR Spectra F. Onori, F. La Franca, F. Ricci, et al., MNRAS in press Broad emission line component (in Paα, Paβ, HeI1.083µm) found in 13 AGN2 spectral line fitting! Federica Ricci (Roma Tre) Dartmouth 8-12 August 2016 7 / 13

Federica Ricci (Roma Tre) Dartmouth 8-12 August 2016 8 / 13

Fitting Results The broad lines in AGN2 are less wide and less intense than in AGN1 Comparison among the Paβ, HeI and Hα broad FWHM AGN1:FWHM 3356 ± 310 km/s EW 80±6 Å AGN2:FWHM 1970 ± 145 km/s EW 44±9 Å Federica Ricci (Roma Tre) Dartmouth 8-12 August 2016 9 / 13

Possible selection effects L X (a/b) and L X N H planes No dependence on galaxy orientation No dependence on the N H, but no BLR components found for logn H > 23.6 F. Onori, F. La Franca, F. Ricci et al. MNRAS in press Federica Ricci (Roma Tre) Dartmouth 8-12 August 2016 10 / 13

Results: M BH, λ Assuming the average (CB+PB) virial relation for all AGN2 AGN2 populate the low M BH end of the M BH L X plane AGN2 have lower M BH and higher λ than the RM AGN1 (of the same L X ) M BH (AGN1) - M BH (AGN2) 0.7 dex λ(agn2) -λ(agn1) 0.7 dex Federica Ricci (Roma Tre) Dartmouth 8-12 August 2016 11 / 13

Results: M BH, λ Assuming the pseudo bulge virial relation for AGN2 with log L X < 43 AGN2 populate the low M BH end of the M BH L X plane AGN2 have lower M BH and higher λ than the RM AGN1 (of the same L X ) The morphology of the host can have an impact on the measure of the M BH bulge/disk decomposition is crucial! Federica Ricci (Roma Tre) Dartmouth 8-12 August 2016 11 / 13

Results: the local M BH L 3.6,bul relation Where are our AGNs in this relation? We expect AGN2 to populate a region at lower masses Sani+11 Measured the bulge 3.6 µm luminosities using Spitzer data and GALFIT software: pure Sersic profile (ellipticals) add an exponential disc (lenticular S0 and spiral galaxies) additional Gaussian component (barred galaxies SB) nuclear point source to account for the emission of the AGN Federica Ricci (Roma Tre) Dartmouth 8-12 August 2016 12 / 13

Results: the local M BH L 3.6,bul relation Where are our AGNs in this relation? AGN2 are morphologically pseudobulges and follow the same M BH L 3.6,bul of the pseudobulges F. Ricci, E. Sani et al. in prep Federica Ricci (Roma Tre) Dartmouth 8-12 August 2016 12 / 13

Take home message Selected 41 AGN2 from SWIFT/BAT 70-month catalog NIR spectra obtained with LUCI@LBT, Xshooter@VLT and ISAAC@VLT Calibrated new NIR virial relations able to work also with AGN2 (and low-l AGN1) that take into account the bulge type of the host We found the BLR component of NIR emission lines (Paα, Paβ and HeI1.083µm) in 13 objects and measured the BH masses AGN2 have on average lower BH Masses and higher Eddington ratios than the AGN1 control population (with the same luminosity) AGN2 populate the, low mass, pseudo bulge, region of M BH L 3.6,bul relation AGN2 should be properly (separately from AGN1) taken into account to understand the AGN evolution Federica Ricci (Roma Tre) Dartmouth 8-12 August 2016 13 / 13

THANK YOU! Federica Ricci (Roma Tre) Dartmouth 8-12 August 2016 13 / 13

NIR virial relations No morphological classification? We have calibrated 2 NIR virial relations based on the Paβ FWHM which use either the X-ray or the Paβ luminosities less affected by reddening/absorption problems F. La Franca, F. Onori, F. Ricci et al. 2015 Federica Ricci (Roma Tre) Dartmouth 8-12 August 2016 13 / 13

New direct BH mass measures The IMBH NGC4395 (one of the smallest SMBH) and the AGN2 MCG-01-24-12 According to Galaxy/AGN evolution models very few IMBH at z 0 expected F. La Franca, F. Onori, F. Ricci et al. 2015 Federica Ricci (Roma Tre) Dartmouth 8-12 August 2016 13 / 13

Obscuration as a function of N H The BAT survey is unbiased up to N H 23.5 Federica Ricci (Roma Tre) Dartmouth 8-12 August 2016 13 / 13