H.E.S.S. observations of the binary system PSR B1259-63/LS 2883 around the 2010/2011 periastron passage

• Autores: Abramowski, A.; Acero, F.; Aharonian, F.; Akhperjanian, A.G.; Anton, G.; Balenderan, S.; Balzer, A.; Barnacka, A.; Becherini, Y.; Becker Tjus, J.; Bernlöhr, K.; Birsin, E.; Biteau, J.; Boisson, C.; Bolmont, J.; Bordas, P.; Brucker, J.; Brun, F.; Brun, P.; Bulik, T.; Carrigan, S.; Casanova, S.; Cerruti, M.; Chadwick, P.M.; Chaves, R.C.G.; Cheesebrough, A.; Colafrancesco, S.; Cologna, G.; Conrad, J.; Couturier, C.; Medina, Maria Clementina
• Año de publicación: 2013
• Idioma: inglés
• Tipo de recurso: artículo
• Materia: X-Rays Binaries; Gamma-Rays; Pulsars; Psr B1259-63 (Pulsar); Be Stars; Ls 2883 (Estrella)
• Institución: Consejo Nacional de Investigaciones Científicas y Técnicas

Aim. In this paper we present very high energy (VHE; E>100 GeV) data from the \gamma-ray binary system PSR B1259-63/LS 2883 taken around its periastron passage (15th of December 2010) with the High Energy Stereoscopic System (H.E.S.S.) of Cherenkov Telescopes. We aim to search for a possible TeV counterpart of the GeV flare detected by the Fermi LAT. In addition, we aim to study the current periastron passage in the context of previous observations taken at similar orbital phases, testing the repetitive behavior of the source. Methods. Observations at VHE were conducted with H.E.S.S. from 9th to 16th of January 2011. The total dataset amounts to around 6 h of observing time. Results. The source is detected in the 2011 data at a significance level of 11.5\sigma\ revealing an averaged integral flux above 1 TeV of (1.01 \pm 0.18_{stat} \pm 0.20_{sys}) \times 10[elevado a la]{-12} cm[elevado a la]{-2}s[elevado a la]{-1}. The differential energy spectrum follows a power-law shape with a spectral index \Gamma = 2.92 \pm 0.30_{stat} \pm 0.20_{sys} and a flux normalisation at 1 TeV of N_{0} = 1.95 \pm 0.32_{stat} \pm 0.39_{sys}) \times 10[elevado a la]{-12} TeV[elevado a la]{-1} cm[elevado a la]{-2} s[elevado a la]{-1}. The measured lightcurve does not show any evidence for variability of the source on the daily scale. Conclusions. The measured integral flux and the spectral shape of the 2011 data are compatible with the results obtained around previous periastron passages. The absence of variability in the H.E.S.S. data indicates that the GeV flare observed by Fermi LAT in the time period covered also by H.E.S.S. observations originates in a different physical scenario than the TeV emission. Additionaly, new results compared to those obtained in the observations which were performed in 2004 at a similar orbital phase, further support the hypothesis of the repetitive behavior of the source
Fil: Abramowski, A.. Universitat Hamburg; Alemania
Fil: Acero, F.. Université Montpellier II; Francia
Fil: Aharonian, F.. National Academy of Sciences of the Republic of Armenia; Armenia. Dublin Institute for Advanced Studies; Irlanda. Max-Planck-Institut für Kernphysik; Alemania
Fil: Akhperjanian, A.G.. National Academy of Sciences of the Republic of Armenia; Armenia. Yerevan Physics Institute; Armenia
Fil: Anton, G.. Universitat Erlangen Nuremberg; Alemania
Fil: Balenderan, S.. Durham University; Reino Unido
Fil: Balzer, A.. Universitat Potsdam; Alemania. DESY; Alemania
Fil: Barnacka, A.. Nicolaus Copernicus Astronomical Center; Polonia. CEA Saclay; Francia
Fil: Becherini, Y.. Landessternwarte Heidelberg; . École Polytechnique; Francia
Fil: Becker Tjus, J.. Ruhr Universität Bochum; Alemania
Fil: Bernlöhr, K.. Max-planck-institut Für Kernphysik; . Humboldt-universität Zu Berlin;
Fil: Birsin, E.. Humboldt-Universität zu Berlin; Alemania
Fil: Biteau, J.. École Polytechnique; Francia
Fil: Boisson, C.. Centre National de la Recherche Scientifique. Observatoire de Paris. Laboratoire de L`univers Et Ses Theories; Francia
Fil: Bolmont, J.. Laboratoire de Physique Nucléaire Et de Hautes Energies;
Fil: Bordas, P.. Eberhard Karls Universität Tübingen;
Fil: Brucker, J.. Universitat Erlangen-Nuremberg; Alemania
Fil: Brun, F.. École Polytechnique; Francia
Fil: Brun, P.. Commissariat A L'energie Atomique. Institut de Recherche Des Lois Fondamentales de L'univers; Francia
Fil: Bulik, T.. Uniwersytet Warszawski; Argentina
Fil: Carrigan, S.. Max-planck-institut Für Kernphysik; Alemania
Fil: Casanova, S.. North-West University; Sudáfrica. University of the Witwatersrand; Sudáfrica
Fil: Cerruti, M.. Centre National de la Recherche Scientifique. Observatoire de Paris. Laboratoire de L`univers Et Ses Theories; Francia
Fil: Chadwick, P.M.. University of Durham; Reino Unido
Fil: Chaves, R.C.G.. Commissariat A L'energie Atomique. Institut de Recherche Des Lois Fondamentales de L'univers; Francia. Max-planck-institut Für Kernphysik; Alemania
Fil: Cheesebrough, A.. University of Durham; Reino Unido
Fil: Colafrancesco, S.. University of the Witwatersrand; Sudáfrica
Fil: Cologna, G.. Ruprecht Karls Universitat Heidelberg; Alemania
Fil: Conrad, J.. Stockholms Universitet; Suecia
Fil: Couturier, C.. Université Pierre et Marie Curie. Laboratoire de Physique Théorique et Hautes Energies; Francia
Fil: Medina, Maria Clementina. Provincia de Buenos Aires. Gobernación. Comisión de Investigaciones Científicas. Instituto Argentino de Radioastronomía. Consejo Nacional de Investigaciones Científicas y Técnicas. Centro Científico Tecnológico Conicet - La Plata. Instituto Argentino de Radioastronomía; Argentina