Relativistic Outflow in CXOCDFS J033260.0-274748

Wang, J. X.; Wang, T. G.; Tozzi, P.; Giacconi, R.; Hasinger, G.; Kewley, Lisa J.; Mainieri, V.; Nonino, M.; Norman, C.; Streblyanska, A.; Szokoly, G.; Yaqoob, T.; Zirm, A.

doi:10.1086/496970

Cited by 7 publications

(6 citation statements)

References 24 publications

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“…Compared to the lensed high-redshift quasars with outflows HS 0810+2554 (z = 1.51; Chartas et al 2014) and H1413+117 (z = 2.56; Chartas et al 2007), the bolometric luminosity of PID352 is a factor of ∼3 and ∼(5−10) higher 6 . The relatively good constraints for the outflow parameters of PID352 are mostly due to the extensive observational X-ray campaign carried out in the CDF-S over more than a decade (in this regard, see also the claimed but never confirmed outflows reported by Wang et al 2005;Zheng & Wang 2008) and by the large collecting area of XMM-Newton.…”

Section: Radio Datamentioning

confidence: 99%

The XMM deep survey in the CDF-S

Vignali

Iwasawa

Comastri

et al. 2015

A&A

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In active galactic nuclei (AGN)-galaxy co-evolution models, AGN winds and outflows are often invoked to explain why super-massive black holes and galaxies stop growing efficiently at a certain phase of their lives. They are commonly referred to as the leading actors of feedback processes. Evidence of ultra-fast (v > ∼ 0.05c) outflows in the innermost regions of AGN has been collected in the past decade by sensitive X-ray observations for sizable samples of AGN, mostly at low redshift. Here we present ultra-deep XMM-Newton and Chandra spectral data of an obscured (N H ≈ 2 × 10 23 cm −2 ), intrinsically luminous (L 2−10 keV ≈ 4 × 10 44 erg s −1 ) quasar (named PID352) at z ≈ 1.6 (derived from the X-ray spectral analysis) in the Chandra Deep Field-South. The source is characterized by an iron emission and absorption line complex at observed energies of E ≈ 2−3 keV. While the emission line is interpreted as being due to neutral iron (consistent with the presence of cold absorption), the absorption feature is due to highly ionized iron transitions (FeXXV, FeXXVI) with an outflowing velocity of 0.14 +0.02 −0.06 c, as derived from photoionization models. The mass outflow rate -∼2 M yr −1 -is similar to the source accretion rate, and the derived mechanical energy rate is ∼9.5 × 10 44 erg s −1 , corresponding to 9% of the source bolometric luminosity. PID352 represents one of the few cases where indications of X-ray outflowing gas have been observed at high redshift thus far. This wind is powerful enough to provide feedback on the host galaxy.

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Section: Radio Datamentioning

confidence: 99%

The XMM deep survey in the CDF-S

Vignali

Iwasawa

Comastri

et al. 2015

A&A

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“…A series of works on the vertical structure of the slim disc indeed show that outflows are inevitably driven from the the disc surface provided the luminosity of the disc reaches the Eddington value (Gu & Lu 2007;Gu et al 2009;Jiao et al 2009;Gu 2012). Indeed, outflows have been observed in many luminous quasars (e.g., Pounds et al 2003;Wang et al 2005;Zhou et al 2006;Ganguly & Brotherton 2008;Wang et al 2008Wang et al , 2009Tombesi et al 2010Tombesi et al , 2011Tombesi et al , 2012.…”

Section: Introductionmentioning

confidence: 99%

Limits on luminosity and mass accretion rate of a radiation-pressure-dominated accretion disc

Cao

2015

Monthly Notices of the Royal Astronomical Society

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There is a maximum for the gravity of a black hole in the vertical direction in the accretion disc. Outflows may probably be driven from the disc if the radiation flux of the disc is greater than a critical value corresponding to the maximal vertical gravity. We find that outflows are driven by the radiation force from the disc if the dimensionless mass accretion rate at the outer radiusṁ out 1 (ṁ =Ṁ /Ṁ Edd ,Ṁ is the mass accretion rate,Ṁ Edd = L Edd /0.1c 2 , and L Edd is the Eddington luminosity). Assuming the outflow to be strong to carry away sufficient gas from the disc surface, we find that the radiation of the disc is limited by such outflows. The disc luminosity, L disc /L Edd ∝ lnṁ out , at large-ṁ out cases. The Eddington ratio of the disc is ∼ 3 forṁ out ∼ 100, which is significantly lower than that of a conventional slim disc without outflows (but it is comparable with that given in Kawaguchi 2003). This implies that the emission from some ultra-luminous X-ray sources with highly super Eddington luminosity should be Doppler beamed, or intermediate mass black holes are in these sources instead of stellar mass black holes. The spectra of the discs surrounding massive black holes with outflows are saturated in the high frequency end providedṁ out 2. We suggest that the saturated emission can be observed to estimate the masses of the black holes accreting at high rates, such as the narrow-line Seyfert galaxies, with the model calculations. The rate of the mass accreted by the black hole alwaysṀ in ≃Ṁ Edd even if the mass accretion rate at the outer radiusṀ out ≫Ṁ Edd , because most of the gas is removed into the outflows by the radiation force. If this is the case, the luminous quasars at high redshifts z 6 should have grown up through persistent accretion at a rate close to the Eddington rate.

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“…2 Note the blueshifted absorption feature in CDFS 11 is only marginally visible in the new 1 Ms spectrum, and we are unable to tell whether it varied based on current data. Except for providing marginally support to the reality of the unusual absorption feature in CDFS 11 with new 1 Ms spectrum, we are not discussing on its nature more than Wang et al (2005) did. In this paper we will focus on CDFS 46.…”

Section: The Data and X-ray Spectral Fittingmentioning

confidence: 89%

“…2 of Page et al 2005), and our independent analysis gives a confidence level of 99% in XMM PN spectrum. With the 1 Ms Chandra exposure on Chandra Deep Field South (CDF-S), Wang et al (2003;2005) reported the detection of strong blueshifted iron K line features with v ∼0. 65-0.84c, in CXO CDFS J033225.3-274219 (CDFS 46, z = 1.617, emission line, radio-loud) and CXO CDFS J033260.0-274748 (CDFS 11, z = 2.579, absorption line, radio-quiet) respectively.…”

Section: Introductionmentioning

confidence: 99%

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Relativistic Outflows in two quasars in the Chandra Deep Field South

Zheng,

Wang

2008

Preprint

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In this paper, we provide new 1 Ms Chandra ACIS spectra of two quasars in the Chandra Deep Field South (CDF-S), which were previously reported to show strong and extremely blueshifted X-ray emission/absorption line features in previous 1 Ms spectra, with outflowing bulk velocity v ∼0.65-0.84c. In the new 1 Ms spectra, the relativistic blueshifted line feature is solidly confirmed in CXO CDFS J033225.3-274219 (CDFS 46, z = 1.617), and marginally visible in CXO CDFS J033260.0-274748 (CDFS 11, z = 2.579), probably due to the increased Chandra ACIS background in the new 1 Ms exposure. The new data rule out the possibility (though very tiny already based on the old 1Ms data) that the two sources were selected to be unusual due to noise spikes in the spectra. The only likely interpretation is extremely blueshifted iron absorption/emission line or absorption edge due to relativistic outflow. We find that the rest frame emission line center in CDFS 46 marginally decreased from 16.2 keV to 15.2 keV after 7 years. The line shift can be due to either decreasing outflowing velocity or lower ionization level. Including the two quasars reported in this paper, we collect from literature a total of 7 quasars showing blueshifted emission or absorption line feature with v ≥ 0.4c in X-ray spectra, and discuss its connection to jet and/or BAL (broad absorption line) outflow.

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Relativistic Outflow in CXOCDFS J033260.0-274748

Cited by 7 publications

References 24 publications

The XMM deep survey in the CDF-S

The XMM deep survey in the CDF-S

Limits on luminosity and mass accretion rate of a radiation-pressure-dominated accretion disc

Relativistic Outflows in two quasars in the Chandra Deep Field South

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