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

Kraemer, S. B.; Turner, T. J.; Couto, Jullianna Denes; Crenshaw, D. M.; Schmitt, Henrique R.; Revalski, Mitchell; Fischer, Travis C.

doi:10.1093/mnras/staa428

Cited by 20 publications

(51 citation statements)

References 74 publications

(147 reference statements)

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“…where n H is the density of the [O III] gas from the photoionization models and σ is the velocity dispersion of the gas (see Paper I), which ranges from 3.4 × 10 1 to 6.6 × 10 2 km s −1 . For the X-ray wind, we assume log U = 0.0 (Turner et al 2003;Armentrout, Kraemer & Turner 2007;Kraemer et al 2015Kraemer et al , 2020, which is consistent with models of the NLR X-ray emission-line gas. Using the fact that…”

Section: Kinetic Energy Density Analysismentioning

confidence: 77%

Hubble Space Telescope[O iii] emission-line kinematics in two nearby QSO2s: a case for X-ray feedback

Falcão

Kraemer

Fischer

et al. 2021

Monthly Notices of the Royal Astronomical Society

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We present a dynamical study of the narrow-line regions in two nearby QSO2s. We construct dynamical models based on detailed photoionisation models of the emission-line gas, including the effects of internal dust, to apply to observations of large-scale outflows from these AGNs. We use Mrk 477 and Mrk 34 in order to test our models against recent HST STIS observations of [O III] emission-line kinematics, since these AGNs possess more energetic outflows than found in Seyfert galaxies. We find that the outflows within 500 pc are consistent with radiative acceleration of dusty gas, however the outflows in Mrk 34 are significantly more extended and may not be directly accelerated by radiation. We characterise the properties of X-ray winds found from the expansion of [O III]-emitting gas close to the black hole. We show that such winds possess the kinetic energy density to disturb [O III] gas at ∼ 1.8 kpc, and have sufficient energy to entrain the [O III] clouds at ∼ 1.2 kpc. Assuming that the X-ray wind possesses the same radial mass distribution as the [O III] gas, we find that the peak kinetic luminosity for this wind is 2 per cent of Mrk 34’s bolometric luminosity, which is in the 0.5 per cent - 5 per cent range required by some models for efficient feedback. Our work shows that, although the kinetic luminosity as measured from [O III]-emitting gas is frequently low, X-ray winds may provide more than one order of magnitude higher kinetic power.

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Section: Kinetic Energy Density Analysismentioning

confidence: 77%

Hubble Space Telescope[O iii] emission-line kinematics in two nearby QSO2s: a case for X-ray feedback

Falcão

Kraemer

Fischer

et al. 2021

Monthly Notices of the Royal Astronomical Society

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“…If it is not confined by an external medium, e.g., a lane of gas and dust in the host disk, it will rapidly thermally expand. As it does so, the density drops, and the ionisation state of the gas increases to the point where it becomes X-ray emission line gas (as suggested by Kraemer et al 2020). In this case, the outflows could be dominated by the X-ray emitting gas.…”

Section: Discussionmentioning

confidence: 91%

“…However, the presence of disturbed gas at larger radial distances (F2018), suggests that the AGN have an effect outside the outflow regions. One possibility is that this is the result of X-ray winds, which may form from thermal expansion of the [O III] gas (Fischer et al 2019;Kraemer et al 2020). We are currently exploring this scenario (Trindade Falcão et al, in preparation).…”

Section: Discussionmentioning

confidence: 99%

Hubble Space Telescope observations of [O iii] emission in nearby QSO2s: physical properties of the ionized outflows

Falcão

Kraemer

Fischer

et al. 2020

Monthly Notices of the Royal Astronomical Society

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We use Hubble Space Telescope (HST)/ Space Telescope Imaging Spectrograph (STIS) long-slit G430M and G750M spectra to analyse the extended [O III] λ5007 emission in a sample of twelve nearby (z >0.12) luminous (Lbol > 1.6 × 1045 erg s−1) QSO2s. The purpose of the study is to determine the properties of the mass outflows of ionised gas and their role in AGN feedback. We measure fluxes and velocities as functions of radial distances. Using Cloudy models and ionising luminosities derived from [O III] λ5007, we are able to estimate the densities for the emission-line gas. From these results, we derive masses of [O III]-emitting gas, mass outflow rates, kinetic energies, kinetic luminosities, momenta and momentum flow rates as a function of radial distance for each of the targets. For the sample, masses are several times 103M⊙ − 107M⊙ and peak outflow rates are 9.3 × 10−3M⊙ yr−1 to 10.3 M⊙ yr−1. The peak kinetic luminosities are 3.4 × 10−8 to 4.9 × 10−4 of the bolometric luminosity, which does not approach the 5.0 × 10−3 - 5.0 × 10−2 range required by some models for efficient feedback. For Mrk 34, which has the largest kinetic luminosity of our sample, in order to produce efficient feedback there would have to be 10 times more [O III]-emitting gas than we detected at its position of maximum kinetic luminosity. Three targets show extended [O III] emission, but compact outflow regions. This may be due to different mass profiles or different evolutionary histories.

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“…The details of the spectral fitting are given in Kraemer et al (2020). In summary, we generated grids of Cloudy photoionization models (Ferland et al 2017) over a range of values of ionization parameter, U , and column density, N H , using the default energy resolution.…”

Section: Observations and Analysismentioning

confidence: 99%

“…In contrast, Kallman et al (2014) performed a detailed photoionization analysis of HETG spectra of NGC 1068 and were able to derive estimates of the total mass and mass outflow rates of the emission-line gas M ≈ 3.7 × 10 5 M andṀ out ∼ 0.3 M yr −1 , respectively. Here we summarize the results of our analysis of the 240 ksec HETG observation of NGC 4151 (Kraemer et al 2020).…”

Section: Introductionmentioning

confidence: 99%

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

Kraemer¹,

Turner

Crenshaw

et al. 2019

Proc. IAU

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We have analyzed Chandra/High Energy Transmission Grating 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 photoionization models to fit the 1st-order spectra; the fit required three distinct emission-line components. To estimate the total mass of ionized gas (M) 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 an M ≍ 5.4 × 105Mʘ. 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 is approximately 1.8 Mʘ 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 emitting mass outflow rate does not drop off at r > 100pc, which suggests that it may have a greater impact on the host galaxy.

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

Cited by 20 publications

References 74 publications

Hubble Space Telescope[O iii] emission-line kinematics in two nearby QSO2s: a case for X-ray feedback

Hubble Space Telescope[O iii] emission-line kinematics in two nearby QSO2s: a case for X-ray feedback

Hubble Space Telescope observations of [O iii] emission in nearby QSO2s: physical properties of the ionized outflows

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

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