Quantifying Feedback from Narrow Line Region Outflows in Nearby Active Galaxies. II. Spatially Resolved Mass Outflow Rates for the QSO2 Markarian 34*

†

Revalski, Mitchell; Dashtamirova, Dzhuliya; Crenshaw, D. Michael; Kraemer, S. B.; Fischer, Travis C.; Schmitt, H. R.; Gnilka, Crystal L.; Schmidt, J.; Elvis, M.; Fabbiano, G.; Storchi‐Bergmann, Thaisa; Maksym, W. Peter; Gandhi, P.

doi:10.3847/1538-4357/aae3e6

Cited by 62 publications

(61 citation statements)

References 91 publications

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“…The maximum X-raẏ M out = 1.80±0.57 M yr −1 , as compared to 2.31±0.67 M yr −1 for the optical/UV gas. Note the latter is somewhat smaller than the ∼ 3 M yr −1 given in Revalski et al (2018b); this is due to the averaging of the velocity within the extraction bin. While the outflow rates are similar, the possibility of a greater extent for the X-ray outflows suggests that its importance in mass outflow, hence AGN feedback, may have not been fully appreciated, as we discuss in Section 5.…”

Section: Mass Outflow Rates In the Extended Gasmentioning

confidence: 71%

“…As shown in Crenshaw et al (2015) and Revalski et al (2018b), the optical outflows in NGC 4151 extend out to a distance of ∼ 150 parsecs. To compare the mass distribution of the X-ray emission-line gas to that of the optical/UV gas within the outflow region, we summed the X-ray masses from the same distances to the NE and SW of the nucleus.…”

Section: Estimating the Mass Of The Extended Gasmentioning

confidence: 73%

“…Although the NLR outflows are often massive (e.g., mass of ∼ 10 6 M , Collins et al 2009;Revalski et al 2018b), and may inject large amounts of kinetic energy and momentum into the interstellar medium (ISM) of the host galaxy (e.g., Revalski et al 2018a), they do not appear to be able to escape the inner kpc of the host galaxy bulge (Fischer et al 2018). This calls into question the effectiveness of AGN-driven outflows in feedback.…”

Section: General Backgroundmentioning

confidence: 99%

“…The line is clearly present in the spectra, as shown on Figure 1, however, it is at a minimum point in the continuum, hence the flux at this wavelength is dominated by the line emission. In the 20 count binning, the line flux is spread out in the bin, which makes it appear as continuum Computed M values at the same radial distances (SW and NE values summed) for the HETG analysis (black crosses), compared to those from the STIS optical/UV analysis (red asterisks), from Crenshaw et al (2015) and Revalski et al (2018b). The optical/UV points are summed to correspond with the HETG extraction bin sizes.…”

Section: Appendix A: Appendix Amentioning

confidence: 99%

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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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Section: Mass Outflow Rates In the Extended Gasmentioning

confidence: 71%

Section: Estimating the Mass Of The Extended Gasmentioning

confidence: 73%

Section: General Backgroundmentioning

confidence: 99%

Section: Appendix A: Appendix Amentioning

confidence: 99%

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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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“…Measurements are more accurate for the most nearby sources (e.g. Revalski et al 2018;Venturi et al 2018;Fluetsch et al 2019); however, these samples lack the most powerful AGN which are thought to be the most important for influencing galaxy evolution.…”

Section: Introductionmentioning

confidence: 99%

KASHz: No evidence for ionised outflows instantaneously suppressing star formation in moderate luminosity AGN at z ∼ 1.4–2.6

Scholtz

Harrison

Rosario

et al. 2020

Monthly Notices of the Royal Astronomical Society

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As part of our KMOS AGN Survey at High-redshift (KASHz), we present spatiallyresolved VLT/KMOS and VLT/SINFONI spectroscopic data and ALMA 870µm continuum imaging of eight z=1.4-2.6 moderate AGN (L 2−10kev = 10 42 −10 45 ergs s −1 ). We map [O iii], Hα and rest-frame FIR emission to search for any spatial anti-correlation between ionised outflows (traced by the [O iii] line) and star formation (SF; traced by Hα and FIR), that has previously been claimed for some high-z AGN and used as evidence for negative and/or positive AGN feedback. Firstly, we conclude that Hα is unreliable to map SF inside our AGN host galaxies based on: (i) SF rates inferred from attenuation-corrected Hα can lie below those inferred from FIR; (ii) the FIR continuum is more compact than the Hα emission by a factor of ∼ 2 on average; (iii) in half of our sample, we observe significant spatial offsets between the FIR and Hα emission, with an average offset of 1.4 ± 0.6 kpc. Secondly, for the five targets with outflows we find no evidence for a spatial anti-correlation between outflows and SF using either Hα or FIR as a tracer. This holds for our re-analysis of a famous z=1.6 X-ray AGN ('XID 2028') where positive and negative feedback has been previously claimed. Based on our results, any instantaneous impact on SF by ionised outflows must be subtle, either occurring on scales below our resolution, or on long timescales.

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Observations of AGN feeding and feedback on Nuclear, Galactic, and Extragalactic Scales

Crenshaw¹,

Gnilka²,

Fischer

et al. 2019

Proc. IAU

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We investigate the processes of active galactic nuclei (AGN) feeding and feedback in the narrow line regions (NLRs) and host galaxies of nearby AGN through spatially resolved spectroscopy with the Gemini Near-Infrared Integral Field Spectrograph (NIFS) and the Hubble Space Telescope’s Space Telescope Imaging Spectrograph (STIS). We examine the connection between nuclear and galactic inflows and outflows by adding long-slit spectra of the host galaxies from Apache Point Observatory. We demonstrate that nearby AGN can be fueled by a variety of mechanisms. We find that the NLR kinematics can often be explained by in situ ionization and radiative acceleration of ambient gas, often in the form of dusty molecular spirals that may be the fueling flow to the AGN.

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Quantifying Feedback from Narrow Line Region Outflows in Nearby Active Galaxies. II. Spatially Resolved Mass Outflow Rates for the QSO2 Markarian 34* †

Cited by 62 publications

References 91 publications

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

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

KASHz: No evidence for ionised outflows instantaneously suppressing star formation in moderate luminosity AGN at z ∼ 1.4–2.6

Observations of AGN feeding and feedback on Nuclear, Galactic, and Extragalactic Scales

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