Orientation effects on spectral emission features of quasars

Bisogni, S.; Marconi, A.; Risaliti, G.

doi:10.1093/mnras/stw2324

Cited by 44 publications

(58 citation statements)

References 30 publications

(36 reference statements)

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“…In order to have the same BH masses at fixed σ ⋆ ∼ 185 km s −1 , the AGN2 should have a virial factor ∼7 times higher than the RM AGN1. However, as also discussed in Paper II, according to the AGN unified model, AGN2 are viewed at larger inclinations (more edge-on) than AGN1, and there are indications that the ffactor decreases with increasing inclination Pancoast et al 2014;Bisogni et al 2017). This would imply that an even smaller f -factor would probably be more appropriate for AGN2.…”

Section: Discussionmentioning

confidence: 65%

Detection of faint broad emission lines in type 2 AGNs – III. On the MBH-σ⋆ relation of type 2 AGNs

Ricci

Franca

Marconi

et al. 2017

Monthly Notices of the Royal Astronomical Society: Letters

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Type 2 active galactic nuclei (AGN) represent the majority of the AGN population. However, due to the difficulties in measuring their black hole (BH) masses, it is still unknown whether they follow the same BH mass-host galaxy scaling relations valid for quiescent galaxies and type 1 AGN. Here we present the locus of type 2 AGN having virial BH mass estimates in the M BH − σ ⋆ plane. Our analysis shows that the BH masses of type 2 AGN are ∼ 0.9 dex smaller than type 1 AGN at σ ⋆ ∼ 185 km s −1 , regardless of the (early/late) AGN host galaxy morphology. Equivalently, type 2 AGN host galaxies have stellar velocity dispersions ∼ 0.2 dex higher than type 1 AGN hosts at M BH ∼ 10 7 M ⊙ .

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Section: Discussionmentioning

confidence: 65%

Detection of faint broad emission lines in type 2 AGNs – III. On the MBH-σ⋆ relation of type 2 AGNs

Ricci

Franca

Marconi

et al. 2017

Monthly Notices of the Royal Astronomical Society: Letters

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“…We note that the measured [O III] and [O IV] fluxes could be underestimated if the NLR extends beyond the slit size of the instruments due to the closeness of the source. Finally, following Risaliti et al (2011) and Bisogni et al (2016), if we assume that the [O III] luminosity is an indicator of the intrinsic luminosity and is emitted isotropically, and that the underlying continuum is due to an optically thick accretion disk, then the observed [O III] EW (EW obs ) can give us an estimate of the orientation of the accretion disk. For an accretion disk that is observed with an inclination θ, we get EW obs = EW * / cos θ, where EW * is the EW as measured in a face-on configuration.…”

Section: Discussionmentioning

confidence: 99%

A Hard Look at NGC 5347: Revealing a Nearby Compton-thick AGN

Kammoun

Miller

Zoghbi

et al. 2019

ApJ

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Current measurements show that the observed fraction of Compton-thick (CT) AGN is smaller than the expected values needed to explain the cosmic X-ray background. Prior fits to the X-ray spectrum of the nearby Seyfert-2 galaxy NGC 5347 (z = 0.00792, D = 35.5 Mpc) have alternately suggested a CT and Compton-thin source. Combining archival data from Suzaku, Chandra, and -most importantly -new data from NuSTAR, and using three distinct families of models, we show that NGC 5347 is an obscured CTAGN (N H > 2.23×10 24 cm −2 ). Its 2-30 keV spectrum is dominated by reprocessed emission from distant material, characterized by a strong Fe Kα line and a Compton hump. We found a large equivalent width of the Fe Kα line (EW = 2.3 ± 0.3 keV) and a high intrinsic-to-observed flux ratio (∼ 100). All of these observations are typical for bona fide CTAGN. We estimate a bolometric luminosity of L bol 0.014 ± 0.005 L Edd. . The Chandra image of NGC 5347 reveals the presence of extended emission dominating the soft X-ray spectrum (E < 2 keV), which coincides with the [O III] emission detected in Hubble Space Telescope images. Comparison to other CTAGN suggests that NGC 5347 is broadly consistent with the average properties of this source class. We simulated XRISM and Athena/X-IFU spectra of the source, showing the potential of these future missions in identifying CTAGN in the soft X-rays.

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“…Finally, as is well known, the broad Hβ emission line shows some asymmetry. Accounting for it has been done in various ways in the literature: some authors include several Gaussian components to fit the broad Hβ lines (Shen et al 2011;Trakhtenbrot & Netzer 2012), others use a broken powerlaw with an asymmetric slope around the central wavelength which is then convolved with a Gaussian (Bisogni, Marconi & Risaliti 2017). In our case, we simply add one Gaussian in the region between the Hβ and the [OIII] lines.…”

Section: A Relation Between the Broad And Narrow Line Regionsmentioning

confidence: 99%

Black hole mass estimation for active galactic nuclei from a new angle

Baron

Ménard

2019

Monthly Notices of the Royal Astronomical Society

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The scaling relations between supermassive black holes and their host galaxy properties are of fundamental importance in the context black hole-host galaxy co-evolution throughout cosmic time. In this work, we use a novel algorithm that identifies smooth trends in complex datasets and apply it to a sample of 2 000 type I active galactic nuclei (AGN) spectra. We detect a sequence in emission line shapes and strengths which reveals a correlation between the narrow L([OIII])/L(Hβ) line ratio and the width of the broad Hα. This scaling relation ties the kinematics of the gas clouds in the broad line region to the ionisation state of the narrow line region, connecting the properties of gas clouds kiloparsecs away from the black hole to material gravitationally bound to it on sub-parsec scales. This relation can be used to estimate black hole masses from narrow emission lines only. It therefore enables black hole mass estimation for obscured type II AGN and allows us to explore the connection between black holes and host galaxy properties for thousands of objects, well beyond the local Universe. Using this technique, we present the M BH − σ and M BH − M * scaling relations for a sample of about 10 000 type II AGN from SDSS. These relations are remarkably consistent with those observed for type I AGN, suggesting that this new method may perform as reliably as the classical estimate used in non-obscured type I AGN. These findings open a new window for studies of black hole-host galaxy co-evolution throughout cosmic time.

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Orientation effects on spectral emission features of quasars

Cited by 44 publications

References 30 publications

Detection of faint broad emission lines in type 2 AGNs – III. On the MBH-σ⋆ relation of type 2 AGNs

Detection of faint broad emission lines in type 2 AGNs – III. On the MBH-σ⋆ relation of type 2 AGNs

A Hard Look at NGC 5347: Revealing a Nearby Compton-thick AGN

Black hole mass estimation for active galactic nuclei from a new angle

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