Black Hole Mass Estimation in Type 1 AGN: Hβ vs. Mg II Lines and the Role of Balmer Continuum

Kovačević-Dojčinović, Jelena; Marčeta-Mandić, Sladjana

doi:10.3389/fspas.2017.00007

Cited by 11 publications

(9 citation statements)

References 31 publications

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“…As we mentioned, the objects with R<0.5 have somewhat different certain optical characteristics (Popović & Kovačević 2011;Kovačević-Dojčinović & Popović 2015); which is believed to be caused by SB presence. However, as we obtained, on Fig.…”

Section: Comparison Between the Optical And Mir Sb/agn Diagnosticsmentioning

confidence: 82%

“…Additionally, to check the results based on the narrow lines (which are superposed with broad lines in the Type 1 AGNs), we considered a sample of 49 Type 2 AGNs. We carefully fit the optical spectra using methods described in Popović et al (2004), Kovačević et al (2010) and Kovačević-Dojčinović & Popović (2015). For fitting of MIR data we used deblendIRS code described in Hernán-Caballero et al (2015).…”

Section: Discussionmentioning

confidence: 99%

“…(iv) The weak correlation between the main optical (log([OIII]5007/HβNLR)) and MIR (RPAH) starburst estimators implies that the difference in the optical characteristics in the objects with log([OIII]5007/HβNLR)<0.5 and >0.5 (Popović & Kovačević 2011;Kovačević-Dojčinović & Popović 2015) may have a different reason than the star formation presence.…”

Section: Discussionmentioning

confidence: 99%

“…The detailed description of this multi-Gaussian model and the fitting procedure is given in Kovačević et al (2010) and Kovačević-Dojčinović & Popović (2015). The examples of the best fit in the λλ4000-5500Å and λλ6200-6950Å ranges are given in Figs.…”

Section: Model Of the Line Spectra In The Optical Rangementioning

confidence: 99%

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The optical versus mid-infrared spectral properties of 82 Type 1 AGNs: coevolution of AGN and starburst

Lakićević¹,

Kovačević-Dojčinović

2017

Monthly Notices of the Royal Astronomical Society

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We investigated the connection between the mid-infrared (MIR) and optical spectral characteristics in a sample of 82 Type 1 active galactic nuclei (AGNs), observed with Infrared Spectrometer on Spitzer (IRS) and Sloan Digital Sky Survey (SDSS, DR12). We found several interesting correlations between optical and MIR spectral properties: i) as starburst significators in MIR increase, the EWs of optical lines HβNLR and FeII, increase as well; ii) as MIR spectral index increases, EW([OIII]) decreases, while fractional contribution of AGN (RAGN) is not connected with EW([OIII]); iii) The log([OIII]5007/HβNLR) ratio is weakly related to the fractional contribution of polycyclic aromatic hydrocarbons (RPAHs). We compare the two different MIR and optical diagnostics for starburst contribution to the overall radiation (RPAH and BPT diagram, respectively). The significant differences between optical and MIR starburst diagnostics were found. The starburst influence to observed correlations between optical and MIR parameters is discussed.

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Section: Comparison Between the Optical And Mir Sb/agn Diagnosticsmentioning

confidence: 82%

Section: Discussionmentioning

confidence: 99%

Section: Discussionmentioning

confidence: 99%

Section: Model Of the Line Spectra In The Optical Rangementioning

confidence: 99%

See 2 more Smart Citations

The optical versus mid-infrared spectral properties of 82 Type 1 AGNs: coevolution of AGN and starburst

Lakićević¹,

Kovačević-Dojčinović

2017

Monthly Notices of the Royal Astronomical Society

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“…There are a number of papers discussing the Mg II λ2800Å line as the SMBH mass estimator (see e.g. Jonić et al 2016;Popović et al 2019;Vestergaard and Peterson 2006;Mediavilla et al 2019;Lira et al 2018;Onken and Kollmeier 2008;Wang et al 2009;Marziani et al 2013;Kovačević-Dojčinović et al 2017;Woo et al 2018;Bahk et al 2019). It seems that the Mg II line is one of the best UV lines for SMBH mass measurements, and it has been used for estimates of the SMBH masses of higher cosmological redshifted quasars.…”

Section: Mg II Linementioning

confidence: 99%

Broad spectral lines in AGNs and supermassive black hole mass measurements

Popović

2020

Open Astronomy

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The mass measurement of supermassive black holes (SMBHs) is a very complex task. Between several methods for SMBH mass measurements, some of them use the spectral lines, which indicate the motion of the emitting/absorbing material around an SMBH. Mostly, there is an assumption of virialization of line emitting gas in the region which is close to the central SMBH. In this paper we will give an overview of methods for the SMBH mass measurements using broad emission spectral lines observed in Type 1 AGNs. First we give the basic idea to use the parameters of broad lines to SMBH mass measurements. After that we give an overview of broad lines from X-ray (Fe kα) to the IR (Pashen and Brecket lines) which have been used for SMBH mass estimates. Additionally, we describe and discuss a new method for SMBH mass measurements using the polarization in the broad lines emitted from Type 1 AGNs.

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Microlensing of the broad emission lines in 27 gravitationally lensed quasars

Fian

Mediavilla²,

Motta³

et al. 2021

A&A

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Aims. We aim to study the structure and kinematics of the broad line region (BLR) of a sample of 27 gravitationally lensed quasars with up to five different epochs of observation. This sample is composed of ∼100 spectra from the literature plus 22 unpublished spectra of 11 systems. Methods. We measure the magnitude differences in the broad emission line (BEL) wings and statistically model the distribution of microlensing magnifications to determine a maximum likelihood estimate for the sizes of the C IV, C III], and Mg II emitting regions. Results. The BELs in lensed quasars are expected to be magnified differently owing to the different sizes of the regions from which they originate. Focusing on the most common BELs in our spectra (C IV, C III], and Mg II), we find that the low-ionization line Mg II is only weakly affected by microlensing. In contrast, the high-ionization line C IV shows strong microlensing in some cases, indicating that its emission region is more compact. Thus, the BEL profiles are deformed differently depending on the geometry and kinematics of the corresponding emitting region. We detect microlensing in either the blue or the red wing (or in both wings with different amplitudes) of C IV in more than 50% of the systems and find outstanding asymmetries in the wings of QSO 0957+561, SDSS J1004+4112, SDSS J1206+4332, and SDSS J1339+1310. This observation indicates that the BLR is, in general, not spherically symmetric and supports the existence of two regions in the BLR, one insensitive to microlensing and another that only shows up when it is magnified by microlensing. Disregarding the existence of these two regions, our estimate for Mg II, R1/2 = 67.3−15.7+3.8 √(M/M⊙) light-days, is in good agreement with previous results from smaller samples, while we obtain smaller sizes for the C III] and CIV lines, R1/2 = 31.0−4.0+1.9 √(M/M⊙) light-days and R1/2 = 15.5−3.9+0.8 √(M/M⊙) light-days, respectively.

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Black Hole Mass Estimation in Type 1 AGN: Hβ vs. Mg II Lines and the Role of Balmer Continuum

Cited by 11 publications

References 31 publications

The optical versus mid-infrared spectral properties of 82 Type 1 AGNs: coevolution of AGN and starburst

The optical versus mid-infrared spectral properties of 82 Type 1 AGNs: coevolution of AGN and starburst

Broad spectral lines in AGNs and supermassive black hole mass measurements

Microlensing of the broad emission lines in 27 gravitationally lensed quasars

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