Investigation of the energy dependence of the orbital light curve in LS 5039
Investigation of the energy dependence of the orbital light curve in LS 5039
复制标题
研究 LS 5039 轨道光变曲线的能量依赖性
DOI：
10.1093/mnras/stw2009
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发表时间：
2016-08
影响因子：
4.8
通讯作者：
Liu C. Z
中科院分区：
文献类型：
--
作者：
Kretschmar P;Kuulkers E;Collmar W;Liu C. Z
LS 5039 is so far the best studied $\gamma$-ray binary system at multi-wavelength energies. A time resolved study of its spectral energy distribution (SED) shows that above 1 keV its power output is changing along its binary orbit as well as being a function of energy. To disentangle the energy dependence of the power output as a function of orbital phase, we investigated in detail the orbital light curves as derived with different telescopes at different energy bands. We analysed the data from all existing \textit{INTEGRAL}/IBIS/ISGRI observations of the source and generated the most up-to-date orbital light curves at hard X-ray energies. In the $\gamma$-ray band, we carried out orbital phase-resolved analysis of \textit{Fermi}-LAT data between 30 MeV and 10 GeV in 5 different energy bands. We found that, at $\lesssim$100 MeV and $\gtrsim$1 TeV the peak of the $\gamma$-ray emission is near orbital phase 0.7, while between $\sim$100 MeV and $\sim$1 GeV it moves close to orbital phase 1.0 in an orbital anti-clockwise manner. This result suggests that the transition region in the SED at soft $\gamma$-rays (below a hundred MeV) is related to the orbital phase interval of 0.5--1.0 but not to the one of 0.0--0.5, when the compact object is "behind" its companion. Another interesting result is that between 3 and 20 GeV no orbital modulation is found, although \textit{Fermi}-LAT significantly ($\sim$18$\sigma$) detects LS 5039. This is consistent with the fact that at these energies, the contributions to the overall emission from the inferior conjunction phase region (INFC, orbital phase 0.45 to 0.9) and from the superior conjunction phase region (SUPC, orbital phase 0.9 to 0.45) are equal in strength. At TeV energies the power output is again dominant in the INFC region and the flux peak occurs at phase $\sim$0.7.
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DOI：
10.1088/0004-637x/753/2/127
发表时间：
2012-05
期刊：
The Astrophysical Journal
影响因子：
--
作者：
S. Kong;S. Kong;K. Cheng;Yue Huang
通讯作者：
S. Kong;S. Kong;K. Cheng;Yue Huang
影响因子：
6.5
作者：
F. Lebrun;J. Leray;P. Lavocat;J. Cretolle;M. Arques;C. Blondel;C. Bonnin;A. Bouère;C. Cara;T. Chaleil;F. Daly;F. Desages;H. Dzitko;B. Horeau;Philippe Laurent;O. Limousin;F. Mathy;V. Mauguen;F. Meignier;F. Molinié;E. Poindron;M. Rouger;A. Sauvageon;T. Tourette
通讯作者：
F. Lebrun;J. Leray;P. Lavocat;J. Cretolle;M. Arques;C. Blondel;C. Bonnin;A. Bouère;C. Cara;T. Chaleil;F. Daly;F. Desages;H. Dzitko;B. Horeau;Philippe Laurent;O. Limousin;F. Mathy;V. Mauguen;F. Meignier;F. Molinié;E. Poindron;M. Rouger;A. Sauvageon;T. Tourette
影响因子：
56.9
作者：
H. C. Aharonian;et al.
通讯作者：
H. C. Aharonian;et al.
影响因子：
6.5
作者：
P. Ubertini;F. Lebrun;G. Cocco;A. Bazzano;A. Bird;K. Broenstad;A. Goldwurm;G. Rosa;C. Labanti;P. Laurent;I. Mirabel;E. Quadrini;B. Ramsey;V. Reglero;L. Sabau;B. Sacco;R. Staubert;L. Vigroux;M. Weisskopf;A. Zdziarski
通讯作者：
P. Ubertini;F. Lebrun;G. Cocco;A. Bazzano;A. Bird;K. Broenstad;A. Goldwurm;G. Rosa;C. Labanti;P. Laurent;I. Mirabel;E. Quadrini;B. Ramsey;V. Reglero;L. Sabau;B. Sacco;R. Staubert;L. Vigroux;M. Weisskopf;A. Zdziarski
DOI：
10.1088/0004-637x/749/1/54
发表时间：
2012-02
期刊：
The Astrophysical Journal
影响因子：
--
作者：
D. Hadasch;D. Torres;T. Tanaka;R. Corbet;A. Hill;R. Dubois;G. Dubus;T. Glanzman;S. Corbel
通讯作者：
D. Hadasch;D. Torres;T. Tanaka;R. Corbet;A. Hill;R. Dubois;G. Dubus;T. Glanzman;S. Corbel