FRINK Linked Data Fragments server

Matches in SemOpenAlex for { <https://semopenalex.org/work/W2143156612> ?p ?o ?g. }

• W2143156612 abstract "Context. Blue-shifted Fe K absorption lines have been detected in recent years between 7 and 10 keV in the X-ray spectra of several radio-quiet AGNs. The derived blue-shifted velocities of the lines can often reach mildly relativistic values, up to 0.2–0.4c. These findings are important because they suggest the presence of a previously unknown massive and highly ionized absorbing material outflowing from their nuclei, possibly connected with accretion disk winds/outflows.Aims. The scope of the present work is to statistically quantify the parameters and incidence of the blue-shifted Fe K absorption lines through a uniform analysis on a large sample of radio-quiet AGNs. This allows us to assess their global detection significance and to overcome any possible publication bias.Methods. We performed a blind search for narrow absorption features at energies greater than 6.4 keV in a sample of 42 radio-quiet AGNs observed with  XMM-Newton . A simple uniform model composed by an absorbed power-law plus Gaussian emission and absorption lines provided a good fit for all the data sets. We derived the absorption lines parameters and calculated their detailed detection significance making use of the classical F-test and extensive Monte Carlo simulations.Results. We detect 36 narrow absorption lines on a total of 101  XMM-Newton EPIC pn observations. The number of absorption lines at rest-frame energies higher than 7 keV is 22. Their global probability to be generated by random fluctuations is very low, less than 3 × 10-8 , and their detection have been independently confirmed by a spectral analysis of the MOS data, with associated random probability 10-7 . We identify the lines as Fe XXV and Fe XXVI K-shell resonant absorption. They are systematically blue-shifted, with a velocity distribution ranging from zero up to ~0.3c, with a peak and mean value at ~0.1c. We detect variability of the lines on both EW s and blue-shifted velocities among different  XMM-Newton observations even on time-scales as short as a few days, possibly suggesting somewhat compact absorbers. Moreover, we find no significant correlation between the cosmological red-shifts of the sources and the lines blue-shifted velocities, ruling out any systematic contamination by local absorption. If we define ultra-fast outflows (UFOs) those highly ionized absorbers with outflow velocities higher than 104  km s-1 , then the majority of the lines are consistent with being associated to UFOs and the fraction of objects with detected UFOs in the whole sample is at least ~35%. This fraction is similar for type 1 and type 2 sources. The global covering fraction of the absorbers is consequently estimated to be in the range C ∼ 0.4-0.6, thereby implying large opening angles.Conclusions. From our systematic X-ray spectral analysis on a large sample of radio-quiet AGNs we have been able to clearly assess the global veracity of the blue-shifted Fe K absorption lines at E > 7 keV and to overcome their publication bias. These lines indicate that UFOs are a rather common phenomenon observable in the central regions of these sources and they are probably the direct signature of AGN accretion disk winds/ejecta. The detailed photo-ionization modeling of these absorbers is presented in a companion paper." @default.
• W2143156612 created "2016-06-24" @default.
• W2143156612 creator A5034340850 @default.
• W2143156612 creator A5036806004 @default.
• W2143156612 creator A5047808605 @default.
• W2143156612 creator A5052940462 @default.
• W2143156612 creator A5076350341 @default.
• W2143156612 creator A5082880965 @default.
• W2143156612 creator A5085312138 @default.
• W2143156612 date "2010-10-01" @default.
• W2143156612 modified "2023-09-28" @default.
• W2143156612 title "Evidence for ultra-fast outflows in radio-quiet AGNs - I. Detection and statistical incidence of Fe K-shell absorption lines" @default.
• W2143156612 cites W1510875542 @default.
• W2143156612 cites W1978929779 @default.
• W2143156612 cites W1979649756 @default.
• W2143156612 cites W1987678168 @default.
• W2143156612 cites W1988414443 @default.
• W2143156612 cites W1999349187 @default.
• W2143156612 cites W2001519873 @default.
• W2143156612 cites W2002356930 @default.
• W2143156612 cites W2002358589 @default.
• W2143156612 cites W2012192418 @default.
• W2143156612 cites W2013776013 @default.
• W2143156612 cites W2015013267 @default.
• W2143156612 cites W2020539004 @default.
• W2143156612 cites W2022607433 @default.
• W2143156612 cites W2025552164 @default.
• W2143156612 cites W2031016170 @default.
• W2143156612 cites W2031680507 @default.
• W2143156612 cites W2032332325 @default.
• W2143156612 cites W2034901657 @default.
• W2143156612 cites W2037842846 @default.
• W2143156612 cites W2041554329 @default.
• W2143156612 cites W2043475284 @default.
• W2143156612 cites W2046618793 @default.
• W2143156612 cites W2052199532 @default.
• W2143156612 cites W2052692850 @default.
• W2143156612 cites W2059906292 @default.
• W2143156612 cites W2062976911 @default.
• W2143156612 cites W2073155743 @default.
• W2143156612 cites W2079040992 @default.
• W2143156612 cites W2079328014 @default.
• W2143156612 cites W2079474521 @default.
• W2143156612 cites W2081240894 @default.
• W2143156612 cites W2083299709 @default.
• W2143156612 cites W2083346911 @default.
• W2143156612 cites W2084098739 @default.
• W2143156612 cites W2099902204 @default.
• W2143156612 cites W2101045281 @default.
• W2143156612 cites W2103025225 @default.
• W2143156612 cites W2109118639 @default.
• W2143156612 cites W2111914795 @default.
• W2143156612 cites W2113226904 @default.
• W2143156612 cites W2113281869 @default.
• W2143156612 cites W2114804422 @default.
• W2143156612 cites W2115957581 @default.
• W2143156612 cites W2117800225 @default.
• W2143156612 cites W2121100147 @default.
• W2143156612 cites W2127318033 @default.
• W2143156612 cites W2131110256 @default.
• W2143156612 cites W2137513434 @default.
• W2143156612 cites W2139025630 @default.
• W2143156612 cites W2141467664 @default.
• W2143156612 cites W2146335537 @default.
• W2143156612 cites W2146359415 @default.
• W2143156612 cites W2152371761 @default.
• W2143156612 cites W2154359271 @default.
• W2143156612 cites W2158497581 @default.
• W2143156612 cites W2269481227 @default.
• W2143156612 cites W2903101379 @default.
• W2143156612 cites W2949188794 @default.
• W2143156612 cites W2950969827 @default.
• W2143156612 cites W3098281597 @default.
• W2143156612 cites W3098995908 @default.
• W2143156612 cites W3099996394 @default.
• W2143156612 cites W3101366175 @default.
• W2143156612 cites W3105361046 @default.
• W2143156612 cites W3105436689 @default.
• W2143156612 hasPublicationYear "2010" @default.
• W2143156612 type Work @default.
• W2143156612 sameAs 2143156612 @default.
• W2143156612 citedByCount "36" @default.
• W2143156612 countsByYear W21431566122012 @default.
• W2143156612 countsByYear W21431566122013 @default.
• W2143156612 countsByYear W21431566122014 @default.
• W2143156612 countsByYear W21431566122015 @default.
• W2143156612 countsByYear W21431566122016 @default.
• W2143156612 countsByYear W21431566122017 @default.
• W2143156612 countsByYear W21431566122018 @default.
• W2143156612 countsByYear W21431566122019 @default.
• W2143156612 countsByYear W21431566122020 @default.
• W2143156612 countsByYear W21431566122021 @default.
• W2143156612 crossrefType "journal-article" @default.
• W2143156612 hasAuthorship W2143156612A5034340850 @default.
• W2143156612 hasAuthorship W2143156612A5036806004 @default.
• W2143156612 hasAuthorship W2143156612A5047808605 @default.
• W2143156612 hasAuthorship W2143156612A5052940462 @default.
• W2143156612 hasAuthorship W2143156612A5076350341 @default.
• W2143156612 hasAuthorship W2143156612A5082880965 @default.
• W2143156612 hasAuthorship W2143156612A5085312138 @default.

• next