Detection of faint broad emission lines in type 2 AGN – I. Near-infrared observations and spectral fitting

Onori, F.; Franca, F. La; Ricci, F.; Brusa, M.; Sani, E.; Maiolino, R.; Bianchi, S.; Bongiorno, A.; Fiore, F.; Marconi, A.; Vignali, C.

doi:10.1093/mnras/stw2368

Cited by 26 publications

(22 citation statements)

References 104 publications

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“…The sample has been extended with 4 AGN2 included in the Swift/BAT 70-month catalogue whose FWHM NIR lines, or spectra, were available in the literature. The spectral data, when available, have been fitted using the technique described in Onori et al (2017). In Table 1 we list the FWHM of the BLR components of the HeI and Paβ lines of the AGN2 sample (in the following called AGN2/BLR sample).…”

Section: Data and Samplesmentioning

confidence: 99%

“…Although based on few tens of objects, at face value our results imply that AGN2 have on average about 0.25 dex lower BLR FWHM, and 0.5 dex lower M BH (larger λ Edd ) than AGN1 of the same luminosity. In Onori et al (2017) we have investigated whether our FWHM measurements could be affected by some selection biases. No dependence was found in the sample where the BLR was measured on both the X-ray and NIR fluxes, on the orientation angle of the host galaxy or on the hydrogen column density, N H , measured in the X-ray band.…”

Section: Analysis Of Possible Selection Effectsmentioning

confidence: 99%

“…(top) we show the L 14−195 distribution of all the AGN1 included in the Swift/BAT 70-month catalogue (blue dashed line) as well as the distribution of the control sample of 33 AGN1 (blue dotted line). The average X-ray luminosity is logL 14−195 = 44.3 with a spread σ (logL 14−195 )=1.0 and logL 14−195 = 43.8 with a spread σ (logL 14−195 )=1.0, for the Swift/BAT AGN1 and the control sample of AGN1, respectively.3 COMPARISON BETWEEN THE AGN1 AND AGN2 POPULATIONSAs discussed byLandt et al (2008);Onori et al (2017);Ricci et al (2017), the most relevant NIR emission lines of the BLR (Paα, Paβ, HeI λ1.083 µm) have, within the errors, the same FWHM.…”

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confidence: 93%

“…-(12) bolometric luminosity and corresponding Eddington ratio, both calculated adopting the K-correction of Vasudevan & Fabian (2007). a) From Burtscher et al (2015) b) Measure of the FWHM of the Paα line from Cai et al (2010).c) The FWHM have been measured applying the fitting procedure described byOnori et al (2017) on the data published byRiffel et al (2006). d) From RamosAlmeida et al (2009).…”

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confidence: 99%

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Detection of faint broad emission lines in type 2 AGN – II. On the measurement of the black hole mass of type 2 AGN and the unified model

Onori

Ricci

Franca

et al. 2017

Monthly Notices of the Royal Astronomical Society: Letters

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We report the virial measurements of the BH mass of a sample of 17 type 2 AGN, drawn from the Swift/BAT 70-month 14-195 keV hard X-ray catalogue, where a faint BLR component has been measured via deep NIR (0.8-2.5 µm) spectroscopy. We compared the type 2 AGN with a control sample of 33 type 1 AGN. We find that the type 2 AGN BH masses span the 5< log(M BH /M ⊙ ) <7.5 range, with an average log(M BH /M ⊙ ) = 6.7, which is ∼ 0.8 dex smaller than found for type 1 AGN. If type 1 and type 2 AGN of the same X-ray luminosity log(L 14−195 /erg s −1 ) ∼ 43.5 are compared, type 2 AGN have 0.5 dex smaller BH masses than type 1 AGN. Although based on few tens of objects, this result disagrees with the standard AGN unification scenarios in which type 1 and type 2 AGN are the same objects observed along different viewing angles with respect to a toroidal absorbing material.

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Section: Data and Samplesmentioning

confidence: 99%

Section: Analysis Of Possible Selection Effectsmentioning

confidence: 99%

mentioning

confidence: 93%

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confidence: 99%

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Detection of faint broad emission lines in type 2 AGN – II. On the measurement of the black hole mass of type 2 AGN and the unified model

Onori

Ricci

Franca

et al. 2017

Monthly Notices of the Royal Astronomical Society: Letters

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“…A large number of works have already been carried out studying pointed X-ray observations (e.g., Winter et al 2009b;Ricci et al 2010;Tazaki et al 2011Tazaki et al , 2013Kawamuro et al 2016b;Tanimoto et al 2016;Marchesi et al 2017;Oda et al 2017) and the multiwavelength properties of Swift/BAT AGNs. This includes radio (e.g., Burlon et al 2013;Wong et al 2016), far-IR (e.g., Meléndez et al 2014;Mushotzky et al 2014;Shimizu et al 2015Shimizu et al , 2016, mid-IR (e.g., Meléndez et al 2008;Weaver et al 2010;Ichikawa et al 2012Ichikawa et al , 2017, near-IR (e.g., Mushotzky et al 2008;Lamperti et al 2017;Onori et al 2017aOnori et al , 2017bRicci et al 2017d), optical (e.g., Vasudevan et al 2009;Koss et al 2010;Winter et al 2010;Ueda et al 2015), and γ-ray (e.g., Sambruna et al 2010;Teng et al 2011) studies, as well as works focused on the host galaxy properties (e.g., Koss et al 2011b), on variability (e.g., Shimizu & Mushotzky 2013;Soldi et al 2014), and on peculiar sources (e.g., Koss et al 2012;Hogg et al 2012;Smith et al 2014;Schawinski et al 2015). Moreover, NuSTAR has been observing Swift/BAT AGNs since its launch in the framework of a legacy survey (M. …”

Section: Introductionmentioning

confidence: 99%

BAT AGN Spectroscopic Survey. V. X-Ray Properties of the Swift /BAT 70-month AGN Catalog

Ricci

Trakhtenbrot

Koss

et al. 2017

ApJS

470

719

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Hard X-ray (10 keV) observations of active galactic nuclei (AGNs) can shed light on some of the most obscured episodes of accretion onto supermassive black holes. The 70-month Swift/BAT all-sky survey, which probes the 14-195 keV energy range, has currently detected 838 AGNs. We report here on the broadband X-ray (0.3-150 keV) characteristics of these AGNs, obtained by combining XMM-Newton, Swift/XRT, ASCA, Chandra, and Suzaku observations in the soft X-ray band ( 10  keV) with 70-month averaged Swift/BAT data. The nonblazar AGNs of our sample are almost equally divided into unobscured (N 10 cm H 22 2 < -) and obscured (N 10 cm H 22 2  -) AGNs, and their Swift/BAT continuum is systematically steeper than the 0.3-10 keV emission, which suggests that the presence of a high-energy cutoff is almost ubiquitous. We discuss the main X-ray spectral parameters obtained, such as the photon index, the reflection parameter, the energy of the cutoff, neutral and ionized absorbers, and the soft excess for both obscured and unobscured AGNs.

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Novel calibrations of virial black hole mass estimators in active galaxies based on X-ray luminosity and optical/near-infrared emission lines

Ricci¹,

Franca²,

Onori³

et al. 2017

A&A

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Context. Accurately weigh the masses of super massive black holes (BHs) in active galactic nuclei (AGN) is currently possible for only a small group of local and bright broad-line AGN through reverberation mapping (RM). Statistical demographic studies can be carried out considering the empirical scaling relation between the size of the broad line region (BLR) and the AGN optical continuum luminosity. However, there are still biases against low-luminosity or reddened AGN, in which the rest-frame optical radiation can be severely absorbed or diluted by the host galaxy and the BLR emission lines could be hard to detect. Aims. Our purpose is to widen the applicability of virial-based single-epoch (SE) relations to reliably measure the BH masses also for low-luminosity or intermediate/type 2 AGN that are missed by current methodology. We achieve this goal by calibrating virial relations based on unbiased quantities: the hard X-ray luminosities, in the 2-10 keV and 14-195 keV bands, that are less sensitive to galaxy contamination, and the full-width at half-maximum (FWHM) of the most important rest-frame near-infrared (NIR) and optical BLR emission lines. Methods. We built a sample of RM AGN having both X-ray luminosity and broad optical/NIR FWHM measurements available in order to calibrate new virial BH mass estimators. Results. We found that the FWHM of the Hα, Hβ and NIR lines (i.e. Paα, Paβ and He i λ10830) all correlate each other having negligible or small offsets. This result allowed us to derive virial BH mass estimators based on either the 2-10 keV or 14-195 keV luminosity. We took also into account the recent determination of the different virial coefficients f for pseudo and classical bulges. By splitting the sample according to the bulge type and adopting separate f factors (Ho & Kim 2014) we found that our virial relations predict BH masses of AGN hosted in pseudobulges ∼0.5 dex smaller than in classical bulges. Assuming the same average f factor for both population, a difference of ∼0.2 dex is still found.

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Detection of faint broad emission lines in type 2 AGN – I. Near-infrared observations and spectral fitting

Cited by 26 publications

References 104 publications

Detection of faint broad emission lines in type 2 AGN – II. On the measurement of the black hole mass of type 2 AGN and the unified model

Detection of faint broad emission lines in type 2 AGN – II. On the measurement of the black hole mass of type 2 AGN and the unified model

BAT AGN Spectroscopic Survey. V. X-Ray Properties of the Swift /BAT 70-month AGN Catalog

Novel calibrations of virial black hole mass estimators in active galaxies based on X-ray luminosity and optical/near-infrared emission lines

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