Characterization of the emitting and absorbing media around the nucleus of the active galaxy UGC 11763 using XMM-Newton data

Cardaci, M. V.; Santos-Lleó, M.; Krongold, Y.; Hägele, G. F.; Díaz, Ángeles I.; Rodríguez-Pascual, P. M.

doi:10.1051/0004-6361/200911687

Cited by 17 publications

(16 citation statements)

References 79 publications

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“…Interestingly, none of these objects shows clear signs of partially ionized (warm) material in the vicinity of the central black hole and in the line of sight. Considering what was found for UGC 11763, the fifth object of our study, which was analysed in a previous paper (Cardaci et al 2009), it is interesting to note that the ionized material was detected in this galaxy, which was one of the two weakest objects. This means that the lack of detection in the other galaxies is due to intrinsically weaker or absent absorption in the line of sight and not to a lower signal-to-noise ratio in the data.…”

Section: Discussionsupporting

confidence: 63%

“…Nevertheless, the objects was classified as a NLS1 by Véron-Cetty & Véron (2006). As in the case of UGC 11763 (Cardaci et al 2009), Mrk 110 seems to be located in a transition zone between the Seyfert 1 and NLS1 classifications, showing some of the properties of each class.…”

Section: Introductionmentioning

confidence: 64%

“…The criteria we have used to include Gaussian profiles in the models is the same as described in Cardaci et al (2009). The lines are added constraining their energies to vary in a small range around their laboratory energies (E lab ) and taking the redshift of the source into account.…”

Section: Low-resolution Spectramentioning

confidence: 99%

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A comprehensive approach to analyzing theXMM-Newtondata of Seyfert 1 galaxies

Cardaci

Santos-Lleó

Hägele

et al. 2011

A&A

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Aims. We seek a comprehensive analysis of all the information provided by the XMM-Newton satellite of the four Seyfert 1 galaxies ESO 359-G19, HE 1143-1810, CTS A08.12, and Mrk 110, including the UV range, to characterize the different components that are emitting and absorbing radiation in the vicinity of the active nucleus. Methods. The continuum emission was studied through the EPIC spectra by taking advantage of the spectral range of these cameras. The high-resolution RGS spectra were analyzed to characterize the absorbing and emission line features that arise in the spectra of the sources. All these data, complemented by information in the UV, are analyzed jointly in order to achieve a consistent characterization of the observed features in each object. Results. The continuum emission of the sources can be characterized either by a combination of a power law and a black body for the weakest objects or by two power law components for the brightest ones. The continuum is not absorbed by neutral or ionized material in the line of sight to any of these sources. In all of them we have identified a narrow Fe-Kα line at 6.4 keV. In ESO 359-G19 we also find an Fexxvi line at about 7 keV. In the soft X-rays band, we identify only one Ovii line in the spectra of HE 1143-1810 and CTS A08.12, and two Ovii-Heα triplets and a narrow Oviii-Lyα emission line in Mrk 110. Conclusions. Not detecting warm material in the line of sight to the low state objects is due to intrinsically weaker or absent absorption in the line of sight and not to a low signal-to-noise ratio in the data. Besides this, the absence of clear emission lines cannot be fully attributed to dilution of those lines by a strong continuum.

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Section: Discussionsupporting

confidence: 63%

Section: Introductionmentioning

confidence: 64%

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A comprehensive approach to analyzing theXMM-Newtondata of Seyfert 1 galaxies

Cardaci

Santos-Lleó

Hägele

et al. 2011

A&A

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“…The presence of two different absorbing components with different temperatures but similar outflow velocity suggests that the absorber could arise from two phases of the same medium (e.g., Elvis et al 2000, Krongold et al 2003. This is further supported by the fact that multiple components of the ionized absorber are found in pressure balance (e.g., Krongold et al 2003;, Cardaci et al 2009, Andrade-Velazquez et al 2010, Zhang et al 2010. This result has proven valid against different methodologies and codes used in the analysis (Krongold et al 2013).…”

Section: Pressure Balance Between Lip and Hipmentioning

confidence: 92%

A TWO-PHASE LOW-VELOCITY OUTFLOW IN THE SEYFERT 1 GALAXY Ark 564

Gupta

Mathur

Krongold

et al. 2013

ApJ

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The Seyfert 1 galaxy Ark 564 was observed with Chandra high energy transmission gratings for 250 ks. We present the high resolution X-ray spectrum that shows several associated absorption lines. The photoionization model requires two warm absorbers with two different ionization states (logU = 0.39 ± 0.03 and logU = −0.99 ± 0.13), both with moderate outflow velocities (∼100 km s −1 ) and relatively low line of sight column densities (logN H = 20.94 and 20.11 cm −2 ). The high ionization phase produces absorption lines of O vii, O viii, Ne ix, Ne x, Mg xi, Fe xvii and Fe xviii while the low ionization phase produces lines at lower energies (O vi & O vii). The pressure-temperature equilibrium curve for the Ark 564 absorber does not have the typical "S" shape, even if the metallicity is super-solar; as a result the two warm-absorber phases do not appear to be in pressure balance. This suggests that the continuum incident on the absorbing gas is perhaps different from the observed continuum. We also estimated the mass outflow rate and the associated kinetic energy and find it to be at most 0.009% of the bolometric luminosity of Ark 564. Thus it is highly unlikely that these outflows provide significant feedback required by the galaxy formation models.1 The ionization parameter ξ = L ion /nr 2 , where L ion is the ionizing luminosity between 1 Ryd and 1000 Ryd (1 Ryd=13.6 eV), n is the number density of the material and r is the distance of the gas from the central source.

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“…There are several models that attempt to explain the distribution and physical conditions of the absorbing gas. One of them proposes that different WA phases can coexist in pressure equilibrium, a multiphase medium (Krongold et al 2003(Krongold et al , 2005bCardaci et al 2009). Another one suggests that the material, also in pressure equilibrium, is distributed with a radial stratification (Różańska et al 2006).…”

Section: Introductionmentioning

confidence: 99%

A Detailed Analysis of the High-Resolution X-Ray Spectra of NGC 3516: Variability of the Ionized Absorbers

Huerta

Krongold

Nicastro

et al. 2014

ApJ

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The 1.5 Seyfert galaxy NGC 3516 presents a strong time variability in X-rays. We re-analyzed the 9 observations performed on October 2006 by XMM-Newton and Chandra in the 0.3 to 10 keV energy band. An acceptable model was found to the XMM-Newton data fitting EPIC-PN and RGS spectra simultaneously; later, this model was successfully applied to the contemporary Chandra high resolution data. The model consists of a continuum emission component (power law + blackbody) absorbed by four ionized components (warm absorbers), and ten narrow emission lines. Three absorbing components are warm, producing features only in the soft X-ray band. The fourth ionization component produces FeXXV and FeXXVI in the hard-energy band. We study the time response of the absorbing components to the well detect changes in the X-ray luminosity of this source, and find that the two components with the lower ionization state show clear opacity changes consistent with gas close to photoionization equilibrium. These changes are supported by the models and by differences in the spectral features among the nine observations. On the other hand, the two components with higher ionization state do not seem to respond to continuum variations. The response time of the ionized absorbers allows us to constrain their electron density and location. We find that one component (with intermediate ionization) must be located within the obscuring torus, at a distance 2.7×10 17 cm from the central engine. This outflowing component is likely originated in the accretion disk. The three remaining components are at distances larger than 10 16−17 cm. Two of the absorbing components in the soft X-rays have similar outflow velocities and locations. These components may be in pressure equilibrium, forming a multi-phase medium, if the gas has metallicity larger than the solar one (Z 5Z ). We also search for variations in the covering factor of the ionized absorbers (although partial covering is not required in our models). We find no correlation between the change in covering factor and the flux of the source. This, in connection with the observed variability of the ionized absorbers, suggests that the changes in flux are not produced by this material. If the variations are indeed produced by obscuring clumps of gas, these must be located much closer in to the central source.

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Characterization of the emitting and absorbing media around the nucleus of the active galaxy UGC 11763 using XMM-Newton data

Cited by 17 publications

References 79 publications

A comprehensive approach to analyzing theXMM-Newtondata of Seyfert 1 galaxies

A comprehensive approach to analyzing theXMM-Newtondata of Seyfert 1 galaxies

A TWO-PHASE LOW-VELOCITY OUTFLOW IN THE SEYFERT 1 GALAXY Ark 564

A Detailed Analysis of the High-Resolution X-Ray Spectra of NGC 3516: Variability of the Ionized Absorbers

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