The<i>INTEGRAL</i>complete sample of type 1 AGN

Molina, M.; Bassani, L.; Malizia, A.; Stephen, J. B.; Bird, A. J.; Dean, A. J.; Panessa, F.; Rosa, A. De; Landi, R.

doi:10.1111/j.1365-2966.2009.15257.x

Cited by 85 publications

(114 citation statements)

References 70 publications

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“…But the authors of these works used a very small samples of Seyfert1s -six in (Petrucci et al 2001) and nine in (Perola et al 2002) and only four galaxies in (Piro 1999). Later this dependence has been studied using larger amount and better quality data (Dadina 2008;De Rosa et al 2012;Molina et al 2008;Molina et al 2009;Vasudevan et al 2013, Molina et al 2013. It is important to understand, either such correlation has a physical origin and or it is an interplay of errors.…”

Section: Cut-off Energy and The Photon Indexmentioning

confidence: 99%

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X-ray spectral parameters for a sample of 95 active galactic nuclei

Vasylenko

Жданов

Fedorova

2015

Astrophys Space Sci

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Section: Cut-off Energy and The Photon Indexmentioning

confidence: 99%

“…Ricci et al (2011) deal essentially with average hard X-ray spectra based only on the INTEGRAL data. Molina et al 2009 performed a detailed analysis with larger AGN sample, though for Seyfert1s only. Recent paper by Мolina et al 2013 deals with even larger sample based on the INTEGRAL/IBIS and Swift/BAT observations.…”

Section: Introductionmentioning

confidence: 99%

X-ray spectral parameters for a sample of 95 active galactic nuclei

Vasylenko

Жданов

Fedorova

2015

Astrophys Space Sci

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“…In Table 1 one sees that the source is stable on a long time scale at hard X-rays. It has been reported several times that, for Seyfert 1, their fluxes can be less variable at hard X-rays than at soft X-rays (Beckmann et al 2007;Molina et al 2009;Gliozzi et al 2003). A possible explanation for this is that the large number of the scatterings of the soft X-rays in the corona region can let the variability be washed out at hard X-rays.…”

Section: Discussion and Summarymentioning

confidence: 99%

“…A possible explanation for this could be that the spectrum is closer to the intrinsic one at hard X-rays than at soft X-rays due to the influence of the material local to AGN (Nandra et al 1999;Tueller et al 2008). The broad-band (1-100 keV) analysis of 36 Seyfert 1 AGNs, detected by INTEGRAL in the 20-40 keV band, presents a power law shape with an average photon index of 1.7 and a dispersion of 0.2 (Molina et al 2009). The photon index of 2.11±0.03 derived for IGR J19405-3016 in ∼1-100 keV is thus slightly more than the result of Molina et al (2009).…”

Section: Discussion and Summarymentioning

confidence: 99%

“…The broad-band (1-100 keV) analysis of 36 Seyfert 1 AGNs, detected by INTEGRAL in the 20-40 keV band, presents a power law shape with an average photon index of 1.7 and a dispersion of 0.2 (Molina et al 2009). The photon index of 2.11±0.03 derived for IGR J19405-3016 in ∼1-100 keV is thus slightly more than the result of Molina et al (2009). A similar discrepancy is found with the results of Beckmann et al (2009) regarding Seyfert 1 AGNs.…”

Section: Discussion and Summarymentioning

confidence: 99%

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INTEGRAL and Swift/XRT observations of IGR J19405-3016

Zhang

Chen

Torres

et al. 2009

A&A

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Aims. IGR J19405-3016 is reported in the 3rd IBIS catalog as one of its lowest significance sources (∼4.6σ under an exposure of about 371 ks). This leads to a caveat in multi-wavelength studies, although the source was identified in the optical as a Seyfert 1. The currently available INTEGRAL data on the source have increased to an exposure time of ∼1376 ks, which stimulates us to investigate the reality of this source again by using all the available data from INTEGRAL and Swift/XRT. Methods. We analyzed all available observations carried out by the International Gamma-Ray Astrophysics Laboratory (INTEGRAL) on IGR J19405-3016. The data were processed by using the latest version OSA 7.0. In addition, we analyzed all the available Swift/XRT data on this source. Results. We find that IGR J19405-3016 has a detection significance of ∼9.4σ in the 20-60 keV band during the observational period between March 2003 and March 2008. This confirms a real source detection reported previously. The source position and error location are therefore updated. The source is found to be constant over years at the hard X-rays. We analyzed the Swift/XRT observations on IGR J19405-3016 as well, and find that the spectrum can be fitted with a simple power law model. Over the three XRT observations, the source flux varied by up to 39% from the average, and the spectrum is generally soft. The combined XRT/ISGRI spectrum is well fitted with a simple power law model (photon index 2.11 ± 0.03) with a column density fixed at 8.73 × 10 20 atoms/cm 2 . Such a photon index is consistent with the mean value 1.98 (dispersion 0.27) obtained from Swift/BAT AGN samples at 14-195 keV. The spectral slope of IGR J19405-3016 is softer than the average spectral slope found elsewhere. A similar discrepancy is found with other results regarding Seyfert 1 AGNs. A possible explanation for this simple spectral description may be that the low level of the column density allows for the "true" spectrum to appear at soft X-rays as well.

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INTEGRAL: Science Highlights and Future Prospects

et al. 2011

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ESA's hard X-ray and soft gamma-ray observatory INTEGRAL is covering the 3 keV to 10 MeV energy band, with excellent sensitivity during long and uninterrupted observations of a large field of view (∼ 100 square degrees), with ms time resolution and keV energy resolution. It links the energy band of pointed soft X-ray missions such as XMMNewton with that of high-energy gamma-ray space missions such as Fermi and ground based TeV observatories. Key results obtained so far include the first sky map in the light of the 511 keV annihilation emission, the discovery of a new class of high mass X-ray binaries and detection of polarization in cosmic high energy radiation. For the foreseeable future, INTE-GRAL will remain the only observatory allowing the study of nucleosynthesis in our Galaxy, including the long overdue next nearby supernova, through high-resolution gamma-ray line spectroscopy. Science results to date and expected for the coming mission years span a wide range of high-energy astrophysics, including studies of the distribution of positrons in the Galaxy; reflection of gamma-rays off clouds in the interstellar medium near the Galactic Centre; studies of black holes and neutron stars particularly in high-mass systems; gamma-INTEGRAL: The International Gamma-Ray Astrophysics Laboratory, an ESA project with instruments and science data centre funded by ESA member states (especially the PI countries: 150 C. Winkler et al. ray polarization measurements for X-ray binaries and gamma-ray bursts, and sensitive detection capabilities for obscured active galaxies with more than 1000 expected to be found until 2014. This paper summarizes scientific highlights obtained since INTEGRAL's launch in 2002, and outlines prospects for the INTEGRAL mission.

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TheINTEGRALcomplete sample of type 1 AGN

Cited by 85 publications

References 70 publications

X-ray spectral parameters for a sample of 95 active galactic nuclei

X-ray spectral parameters for a sample of 95 active galactic nuclei

INTEGRAL and Swift/XRT observations of IGR J19405-3016

INTEGRAL: Science Highlights and Future Prospects

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