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dc.contributor.author | Burenin R. | |
dc.contributor.author | Mescheryakov A. | |
dc.contributor.author | Revnivtsev M. | |
dc.contributor.author | Sazonov S. | |
dc.contributor.author | Bikmaev I. | |
dc.contributor.author | Pavlinsky M. | |
dc.contributor.author | Sunyaev R. | |
dc.date.accessioned | 2018-09-18T20:15:30Z | |
dc.date.available | 2018-09-18T20:15:30Z | |
dc.date.issued | 2008 | |
dc.identifier.issn | 1063-7737 | |
dc.identifier.uri | https://dspace.kpfu.ru/xmlui/handle/net/138047 | |
dc.description.abstract | We present the results of our optical identifications of a set of X-ray sources from the INTEGRAL and SWIFT all-sky surveys. The optical data have been obtained with the 1.5-m Russian-Turkish Telescope (RTT-150). Nine X-ray sources have been identified with active galactic nuclei (AGNs). Two of them are located in the nearby spiral galaxies MCG-01-05-047 and NGC 973 seen almost edge-on. One source, IGR J16562-3301, is probably a BL Lac object (blazar). The remaining AGNs are observed as the starlike nuclei of spiral galaxies whose spectra exhibit broad emission lines. The relation between the hard X-ray (17-60 keV) luminosity and the [O III] 5007 line luminosity, log L x/L [O III] ≈ 2.1, holds good for most of the AGNs detected in hard X rays. However, the luminosities of some AGNs deviate from this relation. The fraction of such objects can reach ∼20%. In particular, the [O III] line flux is lower for two nearby edge-on spiral galaxies. This can be explained by the effect of absorption in the galactic disks. © 2008 Pleiades Publishing, Ltd. | |
dc.relation.ispartofseries | Astronomy Letters | |
dc.subject | Active galactic nuclei | |
dc.subject | Gamma-ray sources | |
dc.subject | Optical observations | |
dc.subject | X-ray sources | |
dc.title | New active galactic nuclei among the INTEGRAL and SWIFT X-ray sources | |
dc.type | Article | |
dc.relation.ispartofseries-issue | 6 | |
dc.relation.ispartofseries-volume | 34 | |
dc.collection | Публикации сотрудников КФУ | |
dc.relation.startpage | 367 | |
dc.source.id | SCOPUS10637737-2008-34-6-SID45349090161 |