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 |
|