X-ray spectral evolution of TeV BL Lacertae objects: eleven years of observations with BeppoSAX, XMM-Newton and Swift satellites
Context.Many of the extragalactic sources detected in γ rays at TeV energies are BL Lac objects. In particular, they belong to the subclass of “high frequency peaked BL Lacs” (HBLs), as their spectral energy distributions exhibit a first peak in the X-ray band. At a closer look, their X-ray spectra...
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Published in | Astronomy and astrophysics (Berlin) Vol. 478; no. 2; pp. 395 - 401 |
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Main Authors | , , , , |
Format | Journal Article |
Language | English |
Published |
Les Ulis
EDP Sciences
01.02.2008
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Subjects | |
Online Access | Get full text |
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Summary: | Context.Many of the extragalactic sources detected in γ rays at TeV energies are BL Lac objects. In particular, they belong to the subclass of “high frequency peaked BL Lacs” (HBLs), as their spectral energy distributions exhibit a first peak in the X-ray band. At a closer look, their X-ray spectra appear to be generally curved into a log-parabolic shape. In a previous investigation of Mrk 421, two correlations were found between the spectral parameters. One involves the height Sp increasing with the position Ep of the first peak; this was interpreted as a signature of synchrotron emission from relativistic electrons. The other involves the curvature parameter b decreasing as Ep increases; this points toward statistical/stochastic acceleration processes for the emitting electrons. Aims.We analyse X-ray spectra of several TeV HBLs to pinpoint their behaviours in the $E_{\rm p}-S_{\rm p}$ and $E_{\rm p}-b$ planes and to compare them with Mrk 421. Methods.We perfom X-ray spectral analyses of a sample of 15 BL Lacs. We report the whole set of observations obtained with the BeppoSAX, XMM-Newton and Swift satellites between 29/06/96 and 07/04/07. We focus on five sources (PKS 0548-322, 1H 1426+418, Mrk 501, 1ES 1959+650, PKS 2155-304) whose X-ray observations warrant detailed searching of correlations or trends. Results.Within our database, we find that four out of five sources, namely PKS 0548-322, 1H 1426+418, Mrk 501 and 1ES 1959+650, follow similar trends as Mrk 421 in the $E_{\rm p}-S_{\rm p}$ plane, while PKS 2155-304 differs. As for the $E_{\rm p}-b$ plane, all TeV HBLs follow a similar behaviour. Conclusions.The trends exhibited by Mrk 421 appear to be shared by several TeV HBLs, such as to warrant discussing predictions from the X-ray spectral evolution to that of TeV emissions. |
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Bibliography: | Appendix A is only available in electronic form at http://www.aanda.org ark:/67375/80W-0QFV8FZS-V publisher-ID:aa8639-07 other:2008A%26A...478..395M istex:811827F9F57DF050C3F362BC006D0A224AAE280D ObjectType-Article-2 SourceType-Scholarly Journals-1 ObjectType-Feature-1 content type line 23 |
ISSN: | 0004-6361 1432-0746 |
DOI: | 10.1051/0004-6361:20078639 |