The Complex Circumnuclear Environment of the Broad-Line Radio Galaxy 3c 390.3 Revealed by Chandra Hetg

Tombesi, Francesco; Reeves, J. N.; Kallman, T. R.; Reynolds, C. S.; Mushotzky, R. F.; Braito, V.; Behar, E.; Leutenegger, Maurice A.; Cappi, M.

doi:10.3847/0004-637x/830/2/98

Cited by 13 publications

(11 citation statements)

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“…Sensitive X-ray observations of radio galaxies show evidence for winds in this class of sources, similar to those observed in Seyferts, which are radio-quiet as a class (Tombesi et al 2010a(Tombesi et al , 2013aGofford et al 2013). Warm absorbers (WA) have been reported in 3C 382, 3C 445, 3C 390.3 and 4C+74.26 (Ballantyne 2005;Reeves et al 2009Reeves et al , 2010Torresi et al 2010Torresi et al , 2012Tombesi et al 2016). Moreover, more extreme ultrafast outflows (UFOs) have also been reported in 3C 111, 3C 120, 3C 390.3, 3C 445, 4C+74.26, andCygnus A (Tombesi et al 2010b, 2011;Ballo et al 2011;Braito et al 2011;Gofford et al 2013;Reynolds et al 2015).…”

Section: Introductionmentioning

confidence: 60%

Feeding and Feedback in the Powerful Radio Galaxy 3C 120

Tombesi

Mushotzky

Reynolds

et al. 2017

ApJ

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We present the spectral analysis of a 200 ks observation of the broad-line radio galaxy 3C 120 performed with the high energy transmission grating (HETG) spectrometer on board the Chandra X-ray Observatory. We find (i) a neutral absorption component intrinsic to the source with column density of logN H = 20.67 ± 0.05 cm −2 , (ii) no evidence for a warm absorber with an upper limit on the column density of just logN H < 19.7 cm −2 assuming the typical ionization parameter logξ≃2.5 erg s −1 cm, the warm absorber may instead be replaced by (iii) a hot emitting gas with temperature kT ≃ 0.7 keV observed as soft X-ray emission from ionized Fe L-shell lines which may originate from a kpc scale shocked bubble inflated by the AGN wind or jet with a shock velocity of about 1,000 km s −1 determined by the emission line width, (iv) a neutral Fe Kα line and accompanying emission lines indicative of a Compton-thick cold reflector with low reflection fraction R ≃ 0.2, suggesting a large opening angle of the torus, (v) a highly ionized Fe XXV emission feature indicative of photoionized gas with ionization parameter logξ=3.75 +0.27 −0.38 erg s −1 cm and a column density of logN H > 22 cm −2 localized within ∼2 pc from the X-ray source, and (vi) possible signatures for a highly ionized disk wind. Together with previous evidence for intense molecular line emission, these results indicate that 3C 120 is likely a late state merger undergoing strong AGN feedback.

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Section: Introductionmentioning

confidence: 60%

Feeding and Feedback in the Powerful Radio Galaxy 3C 120

Tombesi

Mushotzky

Reynolds

et al. 2017

ApJ

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“…Warm absorbers are rarely found in the radio loud galaxies, much similar to the phenomenon that BAL outflows are detected mostly in radio quiet QSOs. WA outflows have been detected in radio-loud galaxies such as 3C 390.3, 3C 120, 3C 382, 3C 445 (Reeves et al 2009(Reeves et al , 2010Torresi et al 2010Torresi et al , 2012Tombesi et al 2016). This paucity in occurrence of WA in radio loud AGN may have deep implications on when the AGN creates an outflow and when it produces a jet (different modes of feedback).…”

Section: The Warm Absorbersmentioning

confidence: 99%

Ionized outflows from active galactic nuclei as the essential elements of feedback

et al. 2020

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Outflows from active galactic nuclei (AGN) are one of the fundamental mechanisms by which the central supermassive black hole interacts with its host galaxy. Detected in ≥ 50% of nearby AGN, these outflows have been found to carry kinetic energy that is a significant fraction of AGN power, and thereby give 'negative' feedback to their host galaxies. To understand the physical processes that regulate them, it is important to have a robust estimate of their physical and dynamical parameters. In this review we summarize our current understanding on the physics of the ionized outflows detected in absorption in the UV and X-ray wavelength bands. We discuss the most relevant observations and our current knowledge and uncertainties in the measurements of the outflow parameters. We also discuss their origin and acceleration mechanisms. The commissioning and concept studies of large telescope missions with high resolution spectrographs in UV/optical and X-rays along with rapid advancements in simulations offer great promise for discoveries in this field over the next decade.

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“…Using an XSTAR photo-ionized absorption table with turbulent velocity of 100 km s −1 and assuming the typ-2 http://pulsar.sternwarte.uni-erlangen.de/wilms/research/tbabs/ ical ionization of the warm absorber detected in other BLRGs of logξ≃2.5 erg s −1 cm and a velocity consistent with zero at the source rest-frame (e.g., Reeves et al 2009;Torresi et al 2010Torresi et al , 2012, we estimate an upper limit of the column density of a possible warm absorber of N H <2.5 × 10 20 cm −2 . The fact that we do not clearly detect a warm absorber in this source could partially be due to the intervening absorption from our own Galaxy and/or to the fact that the interstellar medium in this source could be hot, as observed in 3C 390.3 and 3C 120, and the low inclination estimated at ≃18 • from the radio jet (e.g., Torresi et al 2012;Tombesi et al 2016Tombesi et al , 2017.…”

Section: Data Analysis and Resultsmentioning

confidence: 72%

“…Here, we report on the analysis of a long 150 ks Chandra HETG observation of the broad-line radio galaxy (BLRG) 3C 111 (z = 0.0485), in combination with archived XMM-Newton RGS spectra. This is the third paper of this series, the previous two focused on 3C 390.3 and 3C 120, respectively (Tombesi et al 2016(Tombesi et al , 2017. The radio galaxy 3C 111 is an X-ray bright BLRG and it is classified as a Fanaroff-Riley type II (FRII) source with a double-lobe/single-jet morphology (Linfield & Perley 1984).…”

Section: Introductionmentioning

confidence: 99%

Excess Galactic Molecular Absorption Toward the Radio Galaxy 3C 111

Tombesi

Reynolds

Mushotzky

et al. 2017

ApJ

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We show the combined spectral analysis of Chandra high energy transmission grating (HETG) and XMM-Newton reflection grating spectrometer (RGS) observations of the broad-line radio galaxy 3C 111. The source is known to show excess neutral absorption with respect to the one estimated from 21 cm radio surveys of atomic H I in the Galaxy. However, previous works were not able to constrain the origin of such absorber as local to our Milky Way or intrinsic to the source (z = 0.0485). The high signal-to-noise grating spectra allow us to constrain the excess absorption as due to intervening gas in the Milky Way, and we estimate a time averaged total column density of N H = (7.4±0.1)×10 21 cm −2 , a factor of two higher than the tabulated H I value. We recommend to use the total average Galactic column density here estimated when studying 3C 111. The origin of the extra Galactic absorption of N H = 4.4 × 10 21 cm −2 is likely due to molecular gas associated with the Taurus molecular cloud complex toward 3C 111, which is our nearest star-forming region. We also detect a weak (EW=16±10 eV) and narrow (FWMH<5,500 km s −1 , consistent with optical Hα) Fe Kα emission line at E=6.4 keV likely from the torus in the central regions of 3C 111, and we place an upper limit on the column density of a possible intrinsic warm absorber of N H <2.5×10 20 cm −2 . These complexities make 3C 111 a very promising object for studying both the intrinsic properties of this active radio galaxy and the Galactic interstellar medium if used as a background source.

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The Complex Circumnuclear Environment of the Broad-Line Radio Galaxy 3c 390.3 Revealed by Chandra Hetg

Cited by 13 publications

References 76 publications

Feeding and Feedback in the Powerful Radio Galaxy 3C 120

Feeding and Feedback in the Powerful Radio Galaxy 3C 120

Ionized outflows from active galactic nuclei as the essential elements of feedback

Excess Galactic Molecular Absorption Toward the Radio Galaxy 3C 111

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