PSR B0540-69 is often called an extragalactic 'twin' of the Crab pulsar in
the Large Magellanic Cloud. The pulsar is embedded in a synchrotron nebula in
the center of SNR 0540-69.3. It was discovered with the Einstein satellite with
P~50 ms, spin-down age of ~1500 years and a spin-down luminosity of ~10^38
erg/s. It has since been detected with all major X-ray telescopes. At X-ray
energies up to ~40 keV the latest observations were reported from RXTE and from
INTEGRAL (only spectrum) in the context of a survey of the LMC. Optical pulsed
emission and faint radio emission have also been found from PSR B0540-69. The
INTEGRAL analysis presented here is based on observations of the LMC obtained
in Jan. 2003 and Jan. 2004 with a total exposure of ~1.5 Ms. In the mosaic maps
from the total exposure (JEM-X and IBIS/ISGRI) a source at the location of PSR
B0540-69 is clearly visible up to energies of ~200 keV. After barycentric
correction and determination of the pulsar phases, based on theephemeris
available from contemporaneous RXTE data, the lightcurves show the
characteristic shape of a broad pulse up into the 40-100 keV band. At higher
energies no significant pulsation is detectable. We derive the spectrum of the
total source from the ISGRI data. The photon spectrum can be fitted with a
power law of index 2.22, which is compatible with the result found by Goetz et
al., 2006.Comment: Proceedings of the 363. WE-Heraeus Seminar on: Neutron Stars and
Pulsars (Posters and contributed talks) Physikzentrum Bad Honnef, Germany,
May.14-19, 2006, eds. W.Becker, H.H.Huang, MPE Report 291, pp.44-5
