The Nuclear Outflows and Feedback in the Seyfert 2 Galaxy Markarian 573

Schlesinger, K. J.; Pogge, Richard W.; Martini, Paul; Shields, J. C.; Fields, Dale L.

doi:10.1088/0004-637x/699/1/857

Cited by 28 publications

(48 citation statements)

References 39 publications

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“…Comparing our derived opening angle for Mrk 573 against the projected opening seen in HST images, as well as against opening angles given in previous works (Schlesinger et al 2009;Wilson & Tsvetanov 1994), our value is much larger and consistent with those of other recently studied Seyfert 2s, Mrk 3 and NGC 4151 (Das et al 2005;Crenshaw et al 2010a). …”

Section: Mrk 573: Discussionsupporting

confidence: 92%

“…One possible reason we see large radial velocities at distances > 2 ′′ is that they are due to emission from a rotating disk (Schlesinger et al 2009), which our modeling program does not account for. This suggestion immediately seems plausible as images like Figure 4.…”

Section: Mrk 573: Discussionmentioning

confidence: 88%

“…Previous analysis by Schlesinger et al (2009) used STIS long-slit spectra to map the kinematics across the NLR in a study of the outflow and feedback of Mrk 573. This study determined that shock ionized radiation is not significant in the disk.…”

Section: Incorporating the Host Diskmentioning

confidence: 99%

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Determining Inclinations of Active Galactic Nuclei Via Their Narrow-Line Region Kinematics

Fischer

2012

Publications of the Astronomical Society of the Pacific

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Active Galactic Nuclei (AGN) are axisymmetric systems to first order; their observed properties are likely strong functions of inclination with respect to our line of sight. However, except for a few special cases, the specific inclinations of individual AGN are unknown. We Imaging Spectrograph (STIS). Our studies indicate that NLR kinematics dominated by radial outflow can be fit with simple biconical outflow models that can be used to determine the inclination of the bicone axis, and hence the obscuring torus, with respect to our line of sight. We present NLR analysis of 52 Seyfert galaxies and resultant inclinations from models of 17 individual AGN with clear signatures of biconical outflow. From these AGN, we can for the first time assess the effect of inclination on other observable properties in radio-quiet AGN, including the discovery of a distinct correlation between AGN inclination and X-ray column density.

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Section: Mrk 573: Discussionsupporting

confidence: 92%

Section: Mrk 573: Discussionmentioning

confidence: 88%

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Determining Inclinations of Active Galactic Nuclei Via Their Narrow-Line Region Kinematics

Fischer

2012

Publications of the Astronomical Society of the Pacific

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“…It has long been known to show a biconical structure, bright arcs, and knots of line-emitting gas (Ferruit et al 1999;Quillen et al 1999) that are strongly aligned and interacting with a kiloparsec-scale low-power radio outflow (Pogge & De Robertis 1993;Falcke et al 1998;Ferruit et al 1999). Schlesinger et al (2009) have recently studied the STIS/Hubble Space Telescope (HST) spectrum, finding that the ENLR optical spectrum is consistent with photoionization by the AGN.…”

Section: Introductionmentioning

confidence: 99%

THE SOFT X-RAY AND NARROW-LINE EMISSION OF Mrk 573 ON KILOPARSEC SCALES

González‐Martín

Acosta–Pulido

Pérez-García

et al. 2010

ApJ

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We present a study of the circumnuclear region of the nearby Seyfert galaxy Mrk 573 using Chandra, XMM-Newton, and Hubble Space Telescope (HST) data. We have studied the morphology of the soft (<2 keV) X-rays comparing it with the [O iii] and Hα HST images. The soft X-ray emission is resolved into a complex extended region. The X-ray morphology shows a biconical region extending up to 12 arcsec (4 kpc) in projection from the nucleus. A strong correlation between the X-rays and the highly ionized gas seen in the [O iii]λ5007 Å image is reported. Moreover, we have studied the line intensities detected with the XMM-Newton Reflection Grating Spectrometer (RGS) and used them to fit the low-resolution EPIC/XMM-Newton and ACIS/Chandra spectra. The RGS/XMM-Newton spectrum is dominated by emission lines of C vi, O vii, O viii, Fe xvii, and Ne ix, among other highly ionized species. A good fit is obtained using these emission lines found in the RGS/XMM-Newton spectrum as a template for Chandra spectra of the nucleus and extended emission, coincident with the cone-like structures seen in the [O iii]/Hα map. The photoionization model Cloudy provides a reasonable fit for both the nuclear region and the cone-like structures showing that the dominant excitation mechanism is photoionization. For the nucleus the emission is modeled using two phases: a high ionization [log (U) = 1.23] and a low ionization [log (U) = 0.13]. For the high-ionization phase the transmitted and reflected components are in a 1:2 ratio, whereas for the low ionization the reflected component dominates. For the extended emission, we successfully reproduced the emission with two phases. The first phase shows a higher ionization parameter for the northwest (log (U) = 0.9) than for the southeast cone (log (U) = 0.3). Moreover, this phase is transmission dominated for the southeast cone and reflection dominated for the northwest cone. The second phase shows a low-ionization parameter (log (U) = −3) and is rather uniform for northwest and southeast cones and equally distributed in reflection and transmission components. In addition, we have also derived the optical/infrared spectral energy distribution (SED) of the nucleus from high spatial resolution images of Mrk 573. The nuclear optical/infrared SED of the nucleus has been modeled by a clumpy torus model. The torus bolometric luminosity agrees very well with the active galactic nucleus (AGN) luminosity inferred from the observed hard X-ray spectrum. The optical depth along the line of sight expected from the torus modeling indicates a high neutral hydrogen column density in agreement with the classification of the nucleus of Mrk 573 as a Compton-thick AGN.

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“…We have found that the kinematics of the NLR are dominated by radial outflow in the four nearby Seyferts that we have studied to date: NGC 4151 (Hutchings et al 1998;Das et al 2005), NGC 1068 (Crenshaw & Kraemer 2000;Das et al 2006), Mrk 3 (Ruiz et al 2001), and Mrk 573 (T. Fischer et al, in preparation; see also Schlesinger et al 2009). In order to compare our results with those from previous groundbased spectra, we use HST/STIS long-slit spectra that cover most of the NLR in NGC 1068 (Cecil et al 2002;Das et al 2006) and NGC 4151 (Das et al 2005).…”

Section: Constraints From Hst /Stis Observationsmentioning

confidence: 90%

Velocity Offsets Due to Mass Outflows in Active Galaxies

et al. 2009

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Abstract. We present a study of the radial velocity offsets between AGN-related narrow emission lines and host-galaxy emission and absorption lines in Seyfert galaxies with observed redshifts less than 0.043. We find that 35% of the Seyferts in the sample show [O iii] emission lines with blueshifts with respect to their host galaxies exceeding 50 km s −1 , whereas only 6% show redshifts this large, in qualitative agreement with most previous studies. We also find that a greater percentage of Seyfert 1 galaxies show blueshifts than Seyfert 2 galaxies. Using HST/STIS spatially-resolved spectra of the Seyfert 2 galaxy NGC 1068 and the Seyfert 1 galaxy NGC 4151, we generate geometric models of their narrow-line regions (NLRs) and inner galactic disks and show how these models can explain the blueshifted [O iii] emission lines in collapsed STIS spectra of these two Seyferts. We conclude that the combination of mass outflow of ionized gas in the NLR and extinction by dust in the inner disk (primarily in the form of dust spirals) is primarily responsible for the velocity offsets in Seyfert galaxies.

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The Nuclear Outflows and Feedback in the Seyfert 2 Galaxy Markarian 573

Cited by 28 publications

References 39 publications

Determining Inclinations of Active Galactic Nuclei Via Their Narrow-Line Region Kinematics

Determining Inclinations of Active Galactic Nuclei Via Their Narrow-Line Region Kinematics

THE SOFT X-RAY AND NARROW-LINE EMISSION OF Mrk 573 ON KILOPARSEC SCALES

Velocity Offsets Due to Mass Outflows in Active Galaxies

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