The Compact, Conical, Accretion-Disk Warm Absorber of the Seyfert 1 Galaxy NGC 4051 and Its Implications for IGM-Galaxy Feedback Processes
Using a 100 ks XMM-Newton exposure of NGC 4051, we show that the time evolution of the ionlzation state of the X-ray absorbers in response to the rapid and highly variable X-ray continuum constrains all the main physical and geometrical properties of an AGN "warm absorber" wind. The absorb...
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| Veröffentlicht in: | The Astrophysical journal 2007-04, Vol.659 (2), p.1022-1039 |
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| creator | Krongold, Yair Nicastro, Fabrizio Elvis, Martin Brickhouse, Nancy Binette, Luc Mathur, Smita Jiménez-Bailón, Elena |
| description | Using a 100 ks XMM-Newton exposure of NGC 4051, we show that the time evolution of the ionlzation state of the X-ray absorbers in response to the rapid and highly variable X-ray continuum constrains all the main physical and geometrical properties of an AGN "warm absorber" wind. The absorber consists of two different ionization components, with a difference of approximately 100 in ionization parameter and approximately 5 in column density. By tracking the response in the opacity of the gas to changes in the ionizing continuum, we were able to constrain the electron density of the system. We find n [unk] = (5.8-21.0) X 10 super(6) cm super(-3) for the high-ionization absorber and n [unk] > 8.1 x 10 super(7) cm super(-3) for the low-ionization absorber. These densities require that the high- and low-ionization absorbing components of NGC 4051 must be compact, at distances 0.5-1.0 It-days (2200R sub(s) 4400R sub(s)) and |
| doi_str_mv | 10.1086/512476 |
| format | Article |
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The absorber consists of two different ionization components, with a difference of approximately 100 in ionization parameter and approximately 5 in column density. By tracking the response in the opacity of the gas to changes in the ionizing continuum, we were able to constrain the electron density of the system. We find n [unk] = (5.8-21.0) X 10 super(6) cm super(-3) for the high-ionization absorber and n [unk] > 8.1 x 10 super(7) cm super(-3) for the low-ionization absorber. These densities require that the high- and low-ionization absorbing components of NGC 4051 must be compact, at distances 0.5-1.0 It-days (2200R sub(s) 4400R sub(s)) and <3.5 it-days (<15.800R sub(s)) from the continuum source, respectively. This rules out an origin in the dusty obscuring torus, as the dust sublimation radius is at least an order of magnitude larger ( similar to 12 It-days). An accretion-disk origin for the warm absorber wind is strongly suggested, and an association with the high-ionization, He II emitting, broad emission line region (radius <2 It-days) is possible. The two detected phases are consistent with pressure equilibrium, which suggests that the absorber consists of a two-phase medium. A radial flow in a spherical geometry is unlikely, and a conical wind geometry is preferred. The implied mass cutflow rate from this wind can be well constrained and is 2%-5% of the mass accretion rate. If the mass outflow rate scaling with accretion rate is representative of all quasars, our results imply that warm absorbers in powerful quasars are unlikely to produce important evolutionary effects on their larger environment, unless we are observing the winds before they get fully accelerated. 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The absorber consists of two different ionization components, with a difference of approximately 100 in ionization parameter and approximately 5 in column density. By tracking the response in the opacity of the gas to changes in the ionizing continuum, we were able to constrain the electron density of the system. We find n [unk] = (5.8-21.0) X 10 super(6) cm super(-3) for the high-ionization absorber and n [unk] > 8.1 x 10 super(7) cm super(-3) for the low-ionization absorber. These densities require that the high- and low-ionization absorbing components of NGC 4051 must be compact, at distances 0.5-1.0 It-days (2200R sub(s) 4400R sub(s)) and <3.5 it-days (<15.800R sub(s)) from the continuum source, respectively. This rules out an origin in the dusty obscuring torus, as the dust sublimation radius is at least an order of magnitude larger ( similar to 12 It-days). An accretion-disk origin for the warm absorber wind is strongly suggested, and an association with the high-ionization, He II emitting, broad emission line region (radius <2 It-days) is possible. The two detected phases are consistent with pressure equilibrium, which suggests that the absorber consists of a two-phase medium. A radial flow in a spherical geometry is unlikely, and a conical wind geometry is preferred. The implied mass cutflow rate from this wind can be well constrained and is 2%-5% of the mass accretion rate. If the mass outflow rate scaling with accretion rate is representative of all quasars, our results imply that warm absorbers in powerful quasars are unlikely to produce important evolutionary effects on their larger environment, unless we are observing the winds before they get fully accelerated. 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The absorber consists of two different ionization components, with a difference of approximately 100 in ionization parameter and approximately 5 in column density. By tracking the response in the opacity of the gas to changes in the ionizing continuum, we were able to constrain the electron density of the system. We find n [unk] = (5.8-21.0) X 10 super(6) cm super(-3) for the high-ionization absorber and n [unk] > 8.1 x 10 super(7) cm super(-3) for the low-ionization absorber. These densities require that the high- and low-ionization absorbing components of NGC 4051 must be compact, at distances 0.5-1.0 It-days (2200R sub(s) 4400R sub(s)) and <3.5 it-days (<15.800R sub(s)) from the continuum source, respectively. This rules out an origin in the dusty obscuring torus, as the dust sublimation radius is at least an order of magnitude larger ( similar to 12 It-days). An accretion-disk origin for the warm absorber wind is strongly suggested, and an association with the high-ionization, He II emitting, broad emission line region (radius <2 It-days) is possible. The two detected phases are consistent with pressure equilibrium, which suggests that the absorber consists of a two-phase medium. A radial flow in a spherical geometry is unlikely, and a conical wind geometry is preferred. The implied mass cutflow rate from this wind can be well constrained and is 2%-5% of the mass accretion rate. If the mass outflow rate scaling with accretion rate is representative of all quasars, our results imply that warm absorbers in powerful quasars are unlikely to produce important evolutionary effects on their larger environment, unless we are observing the winds before they get fully accelerated. 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| title | The Compact, Conical, Accretion-Disk Warm Absorber of the Seyfert 1 Galaxy NGC 4051 and Its Implications for IGM-Galaxy Feedback Processes |
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