DISCOVERY OF ULTRA-FAST OUTFLOWS IN A SAMPLE OF BROAD-LINE RADIO GALAXIES OBSERVED WITH<i>SUZAKU</i>

Tombesi, Francesco; Sambruna, R. M.; Reeves, J. N.; Braito, V.; Ballo, L.; Gofford, J.; Cappi, M.; Mushotzky, R. F.

doi:10.1088/0004-637x/719/1/700

Cited by 177 publications

(203 citation statements)

References 69 publications

(150 reference statements)

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“…Unfortunately the resulting parameters values have large errors and provides us with only very limited information on the physical condition of the emitting gas. Nonetheless, the resulting values for the ionization parameter obtained in this framework are in the range log ξ ∼ 2.5−5, consistent with the median value of ∼4.8 erg s −1 cm found by Tombesi et al (2010), exploring the properties of ultra fast outflows in a sample of broad-line radio galaxies. Given the large change in radius going from pc to kpc scale, this requires a strong decrease in the gas density to maintain an approximately constant ionization parameter, that can be obtained with a gas density decreasing roughly proportionally to r −2 .…”

Section: Discussionsupporting

confidence: 85%

Extended soft X-ray emission in 3CR radio galaxies atz< 0.3: high excitation and broad line galaxies

Balmaverde

Capetti

Grandi

et al. 2012

A&A

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We analyze Chandra observations of diffuse soft X-ray emission associated with a complete sample of 3CR radio galaxies at z < 0.3. We focus on the properties of the spectroscopic sub-classes of high excitation galaxies (HEGs) and broad line objects (BLOs). Among the 33 HEGs we detect extended (or possibly extended) emission in about 40% of the sources; the fraction is even higher (8/10) when restricting the analysis to the objects with exposure times larger than 10 ks. In the 18 BLOs, extended emission is seen only in two objects; this lower detection rate can be ascribed to the presence of their bright X-ray nuclei that easily outshine any genuine diffuse emission. A very close correspondence between the soft X-ray and optical line morphology emerges. We also find that the ratio between [O III] and extended soft X-ray luminosity is confined within a factor of 2 around a median value of 5. Both results are similar to what is seen in Seyfert galaxies. We discuss different processes that could explain the soft X-ray emission and conclude that the photoionization of extended gas, coincident with the narrow line region, is the favored mechanism.

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Section: Discussionsupporting

confidence: 85%

Extended soft X-ray emission in 3CR radio galaxies atz< 0.3: high excitation and broad line galaxies

Balmaverde

Capetti

Grandi

et al. 2012

A&A

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“…A UFO with velocity v out ;0.15c was detected in 3C390.3 (Tombesi et al 2010bGofford et al 2013Gofford et al , 2015. The lower and upper limits on the distance, mass outflow rate, and mechanical power are d;0.002-0.02 pc,…”

Section: Warm Absorbermentioning

confidence: 94%

“…Increasing evidence for such ionized Fe K emission lines has been reported in the spectra of both radio-quiet and radio-loud AGNs (e.g., Bianchi et al 2005;Tombesi et al 2010aTombesi et al , 2010bLohfink et al 2013;Patrick et al 2012;Tombesi et al 2013b). The origin of such features is still unclear, possibly being associated with disk winds, extended photoionied gas, or disk reflection.…”

Section: Fe K Band Emissionmentioning

confidence: 99%

“…The detection of WAs was 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 , 2012. Moreover, UFOs have been reported in 3C111, 3C120, 3C390.3, 3C445, 4C +74.26, and Cygnus A (Tombesi et al 2010bBallo et al 2011;Braito et al 2011;Gofford et al 2013Gofford et al , 2015Reynolds et al 2015). A recent X-ray study of a sample of 26 radio galaxies reported that the frequency of UFOs is likely in the interval f; 50% ± 20% .…”

Section: Introductionmentioning

confidence: 96%

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

Tombesi

Reeves

Kallman

et al. 2016

ApJ

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We present the first high spectral resolution X-ray observation of the broad-line radio galaxy 3C390.3 obtained with the high-energy transmission grating spectrometer on board the Chandra X-ray Observatory. The spectrum shows complex emission and absorption features in both the soft X-rays and Fe K band. We detect emission and absorption lines in the energy range E=700-1000 eV associated with ionized Fe L transitions (Fe XVII-XX). An emission line at the energy of E;6.4 keV consistent with the Fe Kα is also observed. Our best-fit model requires at least three different components: (i) a hot emission component likely associated with the hot interstellar medium in this elliptical galaxy with temperature kT=0.5±0.1 keV; (ii) a warm absorber with ionization parameter logξ=2.3±0.5 erg s −1 cm, column density logN H =20.7±0.1 cm −2 , and outflow velocity v out <150 km s −1 ; and (iii) a lowly ionized reflection component in the Fe K band likely associated with the optical broad-line region or the outer accretion disk. These evidences suggest the possibility that we are looking directly down the ionization cone of this active galaxy and that the central X-ray source only photoionizes along the unobscured cone. This is overall consistent with the angle-dependent unified picture of active galactic nuclei.

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“…This may indicate that there is some kind of wind in the disk, probably caused by the radiation of the central source. Recently Tombesi et al (2010) performed a uniform and systematic search for the blueshifted Fe Kα absorption lines in the X-ray spectra of 3C 390.3 observed with Suzaku and detected absorption lines at energies higher than 7 keV. This implies that the origin of the Fe Kα is in the highly ionized outflowing gas with mildly relativistic velocities (in the velocity range from 0.04 to 0.15 light speed).…”

Section: Variability and The Blr Structure Of 3c 3903mentioning

confidence: 99%

Spectral optical monitoring of 3C 390.3 in 1995–2007

Popovic

Shapovalova

Ilić

et al. 2011

A&A

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Context. We present a study of the variability of the broad emission-line parameters of 3C390.3, an active galaxy with the doublepeaked emission-line profiles. We give a detailed analysis of the variation in the broad Hα and Hβ emission-line profiles, the ratios, and the Balmer decrement of different line segments. Aims. We explore the disk structure with an investigation of the variability of the broad-line profiles. This is assumed to emit the broad double-peaked Hβ and Hα emission lines in the spectrum of 3C390.3. Methods. We divided the observed spectra into two periods (before and after the outburst in 2002) and separately analyzed the variation in these two periods. First we analyzed the spectral emission-line profiles of the Hα and Hβ lines and measured the peak positions. Then, we divided the lines into several segments and measured the line-segment fluxes. The Balmer decrement variation for the entire Hα and Hβ fluxes and for the line segments was investigated and discussed. Additionally, we modeled the variations in the line parameters with an accretion disk model and compared our modeled line parameter variations with observed ones. Results. We compared the variability in the observed line parameters with the disk model predictions and found that the variation in line profiles and in the line segments corresponds to the emission of a disk-like broad-line region (BLR). But there is probably another additional emission component that contributes to the Hα and Hβ line center. We found that the variation in the line profiles is caused by the variation in the parameters of the disk-like BLR, first of all in the inner (outer) radius, which can well explain the line parameters variations in Period I. The Balmer decrement across the line profile has a bell-like shape and is affected not only by physical processes in the disk, but also by different emitting disk dimension of the Hα and Hβ line. Conclusions. The geometry of the BLR of 3C390.3 seems to be very complex, and inflows/outflows may be present, but evidently the broad-line region with its disk-like geometry is the dominant emitter.

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DISCOVERY OF ULTRA-FAST OUTFLOWS IN A SAMPLE OF BROAD-LINE RADIO GALAXIES OBSERVED WITHSUZAKU

Cited by 177 publications

References 69 publications

Extended soft X-ray emission in 3CR radio galaxies atz< 0.3: high excitation and broad line galaxies

Extended soft X-ray emission in 3CR radio galaxies atz< 0.3: high excitation and broad line galaxies

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

Spectral optical monitoring of 3C 390.3 in 1995–2007

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