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

Vasylenko, A. A.; Жданов, В. І.; Fedorova, E.

doi:10.1007/s10509-015-2585-z

Cited by 14 publications

(16 citation statements)

References 77 publications

(159 reference statements)

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“…Àíàëèç â äèàïà çîíå 0.3...10 êýÂ ïî äàííûì XMM-New ton ïîêàçûâàåò áîëåå ïëîñêèé ñïåêòð ñ Ã = 1.55...1.65 [11,13,17], âîçìîaeíî, ïî ïðè÷èíå âëèÿíèÿ êîìïîíåíòà îòðàaeåíèÿ íà áîëåå âûñîêèõ ýíåðãèÿõ. Íàëè÷èå ýòîãî êîì ïîíåíòà áûëî óñòàíîâëåíî â ðàáîòàõ ñ èñïîëüçîâàíèåì â øèðîêîì äèàïàçîíå ýíåðãèé äàííûõ, XMM-New ton+IN TE GRAL/ISGRI [8,36], Suzaku [16] è BeppoSAX [7] (õîòÿ íàëè÷èå îòðàaeåíèÿ óñòàíîâëåíî â [7]…”

Section: îáðàáîòêà äàííûõ è êðèâàß áëåñêàunclassified

“…R ~ 1...3). Íåáîëüøèå îöåíêè ïàðàìåòðà îòðàaeåíèÿ R èç ðàáîò[8,16,36], à èìåííî R = 0.3 ± 0.1 L intr (2...10 êýÂ) = (1.14...1.23)×1036 Äae/ñ, L intr (10...40 êýÂ) = (1.56... 1.62)×1036 Äae/ñ, ÷òî ñîîòâåòñòâóåò ïîâûøåíèþ ÿðêîñòè èñòî÷íèêà. Äëÿ âû÷èñëåíèÿ áîëîìåòðè÷åñêîé ñâåòè ìîñòè âîñïîëüçóåìñÿ ôàêòîðîì ïîðÿäêà 10, âûâåäåííûì äëÿ äèàïàçîíà 2...10 êýÂ â ðàáîòå[19], ÷òî äà¸ò íàì L bol » 1.19×10 37 Äae/ñ.…”

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The obscured active nucleus of NGC 7172 as seen BY NuSTAR

Vasylenko¹

2018

Kinemat. fiz. nebesnyh tel (Online)

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Section: îáðàáîòêà äàííûõ è êðèâàß áëåñêàunclassified

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The obscured active nucleus of NGC 7172 as seen BY NuSTAR

Vasylenko¹

2018

Kinemat. fiz. nebesnyh tel (Online)

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“…One of the examples of using these sky maps in 2-5 and 5-10 keV range with a public database of X-ray observations by XMM-Newton is a search of the dark matter decay line (Boyarsky et al 2014, Savchenko & Iakubovskyi 2014. This web-based observatory contains also various catalogues of X-ray extragalaxy sources (active galaxy nuclei, galaxy clusters) compiled at the Main Astronomical Observatory of the National Academy of Sciences of Ukraine (MAO NASU) (see, for example, Chesnok et al 2009, Babyk et al 2014, Babyk & Vavilova 2014, Pulatova et al 2015, Vasylenko et al 2015. The VizieR web service (Strasbourg, France) contains more than 15400 published astronomical catalogues.…”

Section: Ukrvo and Virgo Astronomical Web-servicesmentioning

confidence: 99%

UkrVO Astroinformatics Software and Web-services

et al. 2016

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The aim of this paper is to introduce the software and astronomical web-services developed in frame of the Ukraine Virtual Observatory (UkrVO) and VIrtual Roentgen and Gamma Observatory (VIRGO) to the broad astronomical community. We report briefly on such web-services as the public databases "Sky Maps" of X-ray observations by XMM-Newton, the Earth Orbital Parameters for International Earth Rotation System, and the UkrVO Joint Digitized Archive of astroplates. We refer to such software as the "Multi-Column View", "Variable Stars Calculator", "FrameSmooth" for variable star's research and "Collection Light Technology" (CoLiTec) software for search and discovery of new Solar System bodies.

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“…Additionally, we consider for this aim the objects of INTEGRAL sample we worked out earlier in [10].…”

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confidence: 99%

“…After excluding blazars and bad datasets, the final sample consists of 79 AGNs, including 10 RL and 69 RQ AGNs. We also included in our consideration the INTEGRAL sample of 95 AGNs we treated earlier in [10].…”

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confidence: 99%

Peculiar AGNs from the INTEGRAL and RXTE data

Fedorova¹,

Vasylenko²,

Жданов³

2017

BTSNUA

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However, for a long time in past there were no detected the positive correlations between the characteristics of sunspots cycle (Wolf number or the total area of spots) and polar magnetic flux (which characterized the value of poloidal field B P ) at the end of the cycle. In the terms of dynamo theory it was supposedly evidenced of the absence of functional dependence poloidal fields B P at the end of cycles on the toroidal field B T in maximum of cycles. As it turned out later, this was due to the fact that the surface α-effect of Babcock-Leighton (which defined by tilt angles of the bipolar magnetic fields, turbulent diffusion and meridional circulation, and causes the regeneration of the poloidal field) is characterized by random fluctuations in time and space. The situation, however, changed drastically after the introducing of the parameter of magnetic strength spots of cycle, which is a product of the area of spots cycle and tilt angles of the bipolar magnetic groups. By combining assimilation of the area of spots, the distance between the weighted canters of opposite magnetic polarity and the tilt angles, the functional dependence of polar magnetic flux (which is an indicator of poloidal field B P ) on the assimilated parameter magnetic strength of sunspots (which describes the relative intensity of the toroidal field B T ) was restored. Within the framework of the αΩ-dynamo this indicates that the surface α-effect of Babcock-Leighton leads to the generation of the poloidal magnetic field at the end of the current cycle, and assimilated parameter of magnetic strength spots of cycle is an integral component for future forecasts of solar activity based on the dynamo models. УДК PECULIAR AGNS FROM THE INTEGRAL AND RXTE DATAWe analysed how the active galactic nucleus (AGN) X-ray primary continuum depends on AGN activity in radio, using the data of RXTE Spectral & Timing Database (Rossi X-ray Timing Explorer) and INTEGRAL (INTErnational Gamma-Ray Astrophysics Laboratory). Our aim is to test the relation between spectral shapes of these AGNs and the prediction of the "spinparadigm" model of the AGN "central engine". We have found that for the major part of radio-quiet (RQ) AGNs the value of highenergy exponential cut-off in primary spectrum appears to be significantly higher than 100 keV and thus follows the "spinparadigm" predictions. In the same time, near 25 % of radio-loud (RL) AGNs demonstrate the high-energy cut-off at the energies above 150 keV, contradicting the "spin paradigm". We have composed a sample of "peculiar" 69 RQ and 10 RL AGNs that seem to contradict to the "spin paradigm" for further individual studies of these objects.Key words: galaxies: Seyfert -X-rays: galaxies: active -galaxies Introduction. One of the most prominent physical differences between AGNs of various classes can be related with jet activity and RL/RQ dichotomy. There are several schemes explaining physical (non-geometrical) differences in the AGN structure, and one of the most well-known of them is often referred to as the ...

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

Cited by 14 publications

References 77 publications

The obscured active nucleus of NGC 7172 as seen BY NuSTAR

The obscured active nucleus of NGC 7172 as seen BY NuSTAR

UkrVO Astroinformatics Software and Web-services

Peculiar AGNs from the INTEGRAL and RXTE data

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