Probing the Hot X-Ray Gas in the Narrow-line Region of Mrk 3

Bogdán, Ákos; Kraft, Ralph; Evans, D. A.; Andrade-Santos, Felipe; Forman, W.

doi:10.3847/1538-4357/aa8c76

Cited by 16 publications

(9 citation statements)

References 51 publications

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“…The expression above assumes that the Ionization Correction Factor (ICF) for the oxygen is equal to 1, even though ions with higher ionization states are observed in other spectral bands as, for instance, X-rays (e.g. Cardaci et al 2009Cardaci et al , 2011Bianchi et al 2010;Bogdán et al 2017), indicating that there could be a significant contribution of them. We point out this issue in the work by Pérez-Montero et al (2019).…”

Section: Te-methodsmentioning

confidence: 99%

Chemical abundances of Seyfert 2 AGNs – I. Comparing oxygen abundances from distinct methods using SDSS

Dors

Freitas-Lemes

Amôres

et al. 2019

Monthly Notices of the Royal Astronomical Society

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We compare the oxygen abundance (O/H) of the Narrow Line Regions (NLRs) of Seyfert 2 AGNs obtained through strong-line methods and from direct measurements of the electron temperature (T e -method). The aim of this study is to explore the effects of the use of distinct methods on the range of metallicity and on the mass-metallicity relation of AGNs at low redshifts (z 0.4). We used the Sloan Digital Sky Survey (SDSS) and NASA/IPAC Extragalactic Database (NED) to selected optical (3000 < λ(Å) < 7000) emission line intensities of 463 confirmed Seyfert 2 AGNs. The oxygen abundance of the NLRs were estimated using the theoretical Storchi-Bergmann et al. calibrations, the semi-empirical N 2O2 calibration, the bayesian H ii-Chi-mistry code and the T e -method. We found that the oxygen abundance estimations via the strongline methods differ from each other up to ∼ 0.8 dex, with the largest discrepancies in the low metallicity regime (12 + log(O/H) 8.5). We confirmed that the T e -method underestimates the oxygen abundance in NLRs, producing unreal subsolar values. We did not find any correlation between the stellar mass of the host galaxies and the metallicity of their AGNs. This result is independent of the method used to estimate Z.

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Section: Te-methodsmentioning

confidence: 99%

Chemical abundances of Seyfert 2 AGNs – I. Comparing oxygen abundances from distinct methods using SDSS

Dors

Freitas-Lemes

Amôres

et al. 2019

Monthly Notices of the Royal Astronomical Society

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“…The largest deviation is seen for Mrk 3, where the NLR is being externally fueled as the host galaxy tidally siphons cold gas from a neighboring companion galaxy. This complicates the gas geometry and leads to a more centrally concentrated and highly ionized NLR (Bogdán et al 2017;Gnilka et al 2020). In this case, the best-fit log (U) ≈−1.3 resides on the higher-ionization slope of the ionization diagram (see Figure 5), which is indistinguishable from log(U) ≈ −2.5 for [O III]/H β ≈ 15-20 without additional line ratios.…”

Section: Photoionization Models With Variable U(r)mentioning

confidence: 99%

Quantifying Feedback from Narrow Line Region Outflows in Nearby Active Galaxies. IV. The Effects of Different Density Estimates on the Ionized Gas Masses and Outflow Rates

Revalski

Crenshaw

Rafelski

et al. 2022

ApJ

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Active galactic nuclei (AGN) can launch outflows of ionized gas that may influence galaxy evolution, and quantifying their full impact requires spatially resolved measurements of the gas masses, velocities, and radial extents. We previously reported these quantities for the ionized narrow-line region outflows in six low-redshift AGN, where the gas velocities and extents were determined from Hubble Space Telescope long-slit spectroscopy. However, calculating the gas masses required multicomponent photoionization models to account for radial variations in the gas densities, which span ∼6 orders of magnitude. To simplify this method for larger samples with less spectral coverage, we compare these gas masses with those calculated from techniques in the literature. First, we use a recombination equation with three different estimates for the radial density profiles. These include constant densities, those derived from [S ii], and power-law profiles based on constant values of the ionization parameter (U). Second, we use single-component photoionization models with power-law density profiles based on constant U, and allow U to vary with radius based on the [O iii]/Hβ ratios. We find that assuming a constant density of n H = 102 cm−3 overestimates the gas masses for all six outflows, particularly at small radii where the outflow rates peak. The use of [S ii] marginally matches the total gas masses, but also overestimates at small radii. Overall, single-component photoionization models where U varies with radius are able to best match the gas mass and outflow rate profiles when there are insufficient emission lines to construct detailed models.

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“…They estimated the total mass and mass outflow rates of the emission-line gas to be M ≈ 3.7 × 10 5 M andṀ out ∼ 0.3 M yr −1 , respectively. Bogdán et al (2017) analysed Chandra/HETG spectra of the Seyfert 2 galaxy Mrk 3 and derived some constraints on the emission-line gas. Although there have been efforts to model the X-ray NLR using Chandra imaging (e.g., Bianchi et al 2010;Gonzalez-Martin et al 2010;Maksym et al 2019), there have not been any other attempts to generate detailed physical models using HETG spectra.…”

Section: General Backgroundmentioning

confidence: 99%

Mass outflow of the X-ray emission line gas in NGC 4151

Kraemer

Turner

Couto

et al. 2020

Monthly Notices of the Royal Astronomical Society

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We have analysed Chandra/High Energy Transmission Gratings spectra of the X-ray emission line gas in the Seyfert galaxy NGC 4151. The zeroth order spectral images show extended H-and He-like O and Ne, up to a distance r ∼ 200 pc from the nucleus. Using the 1st order spectra, we measure an average line velocity ∼ −230 km s −1 , suggesting significant outflow of X-ray gas. We generated Cloudy photoionisation models to fit the 1st order spectra; the fit required three distinct emission-line components. To estimate the total mass of ionised gas and the mass outflow rates, we applied the model parameters to fit the zeroth order emission-line profiles of Ne IX and Ne X. We determined the total mass of ≈ 5.4× 10 5 M . Assuming the same kinematic profile as that for the [O III] gas, derived from our analysis of Hubble Space Telescope/Space Telescope Imaging Spectrograph spectra, the peak X-ray mass outflow rate was ≈ 1.8 M yr −1 , at r ∼ 150 pc. The total mass and mass outflow rates are similar to those determined using [O III], implying that the X-ray gas is a major outflow component. However, unlike the optical outflows, the X-ray outflow rate does not drop off at r > 100 pc, which suggests that it may have a greater impact on the host galaxy.

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Probing the Hot X-Ray Gas in the Narrow-line Region of Mrk 3

Cited by 16 publications

References 51 publications

Chemical abundances of Seyfert 2 AGNs – I. Comparing oxygen abundances from distinct methods using SDSS

Chemical abundances of Seyfert 2 AGNs – I. Comparing oxygen abundances from distinct methods using SDSS

Quantifying Feedback from Narrow Line Region Outflows in Nearby Active Galaxies. IV. The Effects of Different Density Estimates on the Ionized Gas Masses and Outflow Rates

Mass outflow of the X-ray emission line gas in NGC 4151

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