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We observed the young ($\sim 1700$ yrs) pulsar PSR B0540-69 in thenear-ultraviolet (UV) for the first time with the Space Telescope ImagingSpectrograph (STIS) aboard the {\em Hubble Space Telescope}. Imagingobservations with the NUV- and FUV-MAMA detectors in TIME-TAG mode allowed usto clearly detect the pulsar in two bands around 2350\AA\ and 1590\AA, withmagnitudes $m_{\rm NUV} =21.449 \pm 0.019$ and $m_{\rm FUV} =21.832 \pm 0.103$.We also detected the pulsar-wind nebula (PWN) in the NUV-MAMA image, with amorphology similar to that observed in the optical and near-infrared (IR). Theextinction-corrected NUV and FUV pulsar fluxes are compatible with a very steeppower law spectrum $F_{\nu} \propto \nu^{-\alpha}$ with spectral index$\alpha_{\rm UV} \sim 3$, non compatible with a Rayleigh Jeans spectrum,indicating a non-thermal origin of the emission. The comparison with theoptical/near-IR power-law spectrum (spectral index $\alpha_{\rm O,nIR} \sim0.7$), indicates an abrupt turn-off at wavelengths below 2500 \AA, not observedin other pulsars. We detected pulsations in both the NUV and FUV data at the 50ms pulsar period. In both cases, the pulse profile features two peaks closelyspaced in phase, as observed in the optical and X-ray light curves. The NUV/FUVpeaks are also aligned in phase with those observed in the radio (1.4 GHz),optical, X, and $\gamma$-ray light curves, like in the Crab pulsar, implying asimilar beaming geometry across all wavelengths. PSR B0540-69 is now the fifthisolated pulsar, together with Crab, Vela, PSR\, B0656+14, and the radio-quietGeminga, detected in the optical, near-UV, near-IR, X-rays and $\gamma$-rays,and seen to pulsate in at least four of these energy bands.

The first ultraviolet detection of the Large Magellanic Cloud pulsar PSR B0540-69 and its multi-wavelength properties