Broad-band γ-ray and X-ray spectra of NGC 4151 and their implications for physical processes and geometry
We study ł-ray observations of NGC 4151 by the Gamma Ray Observatory (GRO)/OSSE contemporaneous with X-ray observations by ROSAT and Ginga in 1991 June and ASCA in 1993 May. The spectra are well modelled by thermal Comptonization and a dual neutral absorber. We also find, for the first time for NGC...
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| Vydáno v: | Monthly notices of the Royal Astronomical Society Ročník 283; číslo 1; s. 193 - 206 |
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| Hlavní autoři: | , , |
| Médium: | Journal Article |
| Jazyk: | angličtina |
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Oxford, UK
Blackwell Science Ltd
01.11.1996
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| Témata: | |
| ISSN: | 0035-8711, 1365-2966 |
| On-line přístup: | Získat plný text |
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| Abstract | We study ł-ray observations of NGC 4151 by the Gamma Ray Observatory (GRO)/OSSE contemporaneous with X-ray observations by ROSAT and Ginga in 1991 June and ASCA in 1993 May. The spectra are well modelled by thermal Comptonization and a dual neutral absorber. We also find, for the first time for NGC 4151, a Compton-reflection spectral component in the Ginga/OSSE data. When reflection is taken into account, the intrinsic X-ray energy spectral index is α ∼ 0.8 and the plasma temperature is ∼ 60 keV for both observations, conditions which imply an optical depth of ∼1. The X-ray spectral index is within the range, α≃0.95±0.15, observed from other Seyfert 1s. Also, the OSSE spectra of those and other observations of NGC 4151 are statistically indistinguishable from the average OSSE spectrum of radio-quiet Seyfert 1s. Thus, NGC 4151 observed in 1991 and 1993 has the intrinsic X-ray/γ-ray spectrum typical for Seyfert 1s, and the main property distinguishing it from other Seyfert 1s is a large absorbing column of ∼ 1023 cm−2. We find no evidence for a strong, broad and redshifted Fe Kα line component in the ASCA spectrum of 1993 May. Also, the Compton-reflection component in the Ginga/OSSE spectrum is a few times too small to account for the strength of the broad/redshifted line reported elsewhere to be found in this and other ASCA spectra of NGC 4151. On the other hand, we confirm previous studies in that archival X-ray data do imply strong intrinsic X-ray variability and hardness of the intrinsic spectrum in low X-ray states. An observed softening of the intrinsic X-ray spectrum with the increasing flux implies that variability in γ-rays is weaker than in X-rays, which agrees with the 100-keV flux changing only within a factor of 2 in archival OSSE and GRANAT/SIGMA observations. The relative hardness of the intrinsic X-ray spectrum rules out the homogeneous hot corona/cold disc model for this source. Instead, the hot plasma has to subtend a small solid angle as seen from the source of UV radiation. If the hot plasma is purely thermal, it consists of electrons rather than e+ pairs. On the other hand, the plasma can be pair-dominated if a small fraction of the power is non-thermal. |
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| AbstractList | We study gamma-ray observations of NGC 4151 by GRO/OSSE contemporaneous with X-ray observations by ROSAT and Ginga in 1991 June and ASCA in 1993 May. The spectra are well modeled by thermal Comptonization and a dual neutral absorber. We also find, for the first time for NGC 4151, a Compton-reflection spectral component in the Ginga/OSSE data. NGC 4151 observed in 1991 and 1993 has the intrinsic X-ray/gamma-ray spectrum typical for Seyfert 1s, and the main property distinguishing it from other Seyfert 1s is a large absorbing column of about 10 exp 23/sq cm. We find no evidence for a strong, broad, and redshifted Fe K-alpha line component in the ASCA spectrum of 1993 May. We confirm previous studies in that archival X-ray data imply strong intrinsic X-ray variability and hardness of the intrinsic spectrum in low X-ray states. The relative hardness of the intrinsic X-ray spectrum rules out the homogeneous hot corona/cold disk model for this source. Instead, the hot plasma has to subtend a small solid angle as seen from the source of UV radiation. If the hot plasma is purely thermal, it consists of electrons rather than e+/- pairs. On the other hand, the plasma can be pair-dominated if a small fraction of the power is nonthermal. (Author) We study ł-ray observations of NGC 4151 by the Gamma Ray Observatory (GRO)/OSSE contemporaneous with X-ray observations by ROSAT and Ginga in 1991 June and ASCA in 1993 May. The spectra are well modelled by thermal Comptonization and a dual neutral absorber. We also find, for the first time for NGC 4151, a Compton-reflection spectral component in the Ginga/OSSE data. When reflection is taken into account, the intrinsic X-ray energy spectral index is α ∼ 0.8 and the plasma temperature is ∼ 60 keV for both observations, conditions which imply an optical depth of ∼1. The X-ray spectral index is within the range, α≃0.95±0.15, observed from other Seyfert 1s. Also, the OSSE spectra of those and other observations of NGC 4151 are statistically indistinguishable from the average OSSE spectrum of radio-quiet Seyfert 1s. Thus, NGC 4151 observed in 1991 and 1993 has the intrinsic X-ray/γ-ray spectrum typical for Seyfert 1s, and the main property distinguishing it from other Seyfert 1s is a large absorbing column of ∼ 1023 cm−2. We find no evidence for a strong, broad and redshifted Fe Kα line component in the ASCA spectrum of 1993 May. Also, the Compton-reflection component in the Ginga/OSSE spectrum is a few times too small to account for the strength of the broad/redshifted line reported elsewhere to be found in this and other ASCA spectra of NGC 4151. On the other hand, we confirm previous studies in that archival X-ray data do imply strong intrinsic X-ray variability and hardness of the intrinsic spectrum in low X-ray states. An observed softening of the intrinsic X-ray spectrum with the increasing flux implies that variability in γ-rays is weaker than in X-rays, which agrees with the 100-keV flux changing only within a factor of 2 in archival OSSE and GRANAT/SIGMA observations. The relative hardness of the intrinsic X-ray spectrum rules out the homogeneous hot corona/cold disc model for this source. Instead, the hot plasma has to subtend a small solid angle as seen from the source of UV radiation. If the hot plasma is purely thermal, it consists of electrons rather than e+ pairs. On the other hand, the plasma can be pair-dominated if a small fraction of the power is non-thermal. |
| Author | Magdziarz, Paweł Zdziarski, Andrzej A. Johnson, W. Neil |
| Author_xml | – sequence: 1 givenname: Andrzej A. surname: Zdziarski fullname: Zdziarski, Andrzej A. organization: Copernicus Astronomical Center, Bartycka 18, 00-716 Warsaw, Poland – sequence: 2 givenname: W. Neil surname: Johnson fullname: Johnson, W. Neil organization: E. O. Hulburt Center for Space Research, Naval Research Lab, Washington, DC 20375, USA – sequence: 3 givenname: Paweł surname: Magdziarz fullname: Magdziarz, Paweł organization: Astronomical Observatory, Jagiellonian University, Orla 171, 30-244 Cracow, Poland |
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| Snippet | We study ł-ray observations of NGC 4151 by the Gamma Ray Observatory (GRO)/OSSE contemporaneous with X-ray observations by ROSAT and Ginga in 1991 June and... We study gamma-ray observations of NGC 4151 by GRO/OSSE contemporaneous with X-ray observations by ROSAT and Ginga in 1991 June and ASCA in 1993 May. The... |
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| SubjectTerms | galaxies: individual: NGC 4151 galaxies: Seyfert - gamma-rays: observations gamma-rays: theory X-rays: galaxies |
| Title | Broad-band γ-ray and X-ray spectra of NGC 4151 and their implications for physical processes and geometry |
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