Context :

Aims : 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 on 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 \sim 6 h of observing time .
The data taken around the 2004 periastron passage were also re-analysed with the current analysis techniques in order to extend the energy spectrum above 3 TeV to fully compare observation results from 2004 and 2011 .

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 _ { \mathrm { stat } } \pm 0.20 _ { \mathrm { sys } } ) \times 10 ^ { -12 } cm ^ { -2 } s ^ { -1 } .
The differential energy spectrum follows a power-law shape with a spectral index \Gamma = 2.92 \pm 0.30 _ { \mathrm { stat } } \pm 0.20 _ { \mathrm { sys } } and a flux normalisation at 1 TeV of N _ { 0 } = ( 1.95 \pm 0.32 _ { \mathrm { stat } } \pm 0.39 _ { \mathrm { sys } } ) \times 10 ^ { -12 } % \textrm { TeV } ^ { -1 } \textrm { cm } ^ { -2 } \textrm { s } ^ { -1 } .
The measured lightcurve does not show any evidence for variability of the source on the daily scale .
The re-analysis of the 2004 data yields results compatible with the published ones .
The differential energy spectrum measured up to \sim 10 TeV is consistent with a power law with a spectral index \Gamma = 2.81 \pm 0.10 _ { \mathrm { stat } } \pm 0.20 _ { \mathrm { sys } } and a flux normalisation at 1 TeV of N _ { 0 } = ( 1.29 \pm 0.08 _ { \mathrm { stat } } \pm 0.26 _ { \mathrm { sys } } ) \times 10 ^ { -12 } % \textrm { TeV } ^ { -1 } \textrm { cm } ^ { -2 } \textrm { s } ^ { -1 } .

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 .