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- W2892442451 abstract "We observed the young ($sim 1700$ yrs) pulsar PSR B0540-69 in the near-ultraviolet (UV) for the first time with the Space Telescope Imaging Spectrograph (STIS) aboard the {em Hubble Space Telescope}. Imaging observations with the NUV- and FUV-MAMA detectors in TIME-TAG mode allowed us to clearly detect the pulsar in two bands around 2350AA and 1590AA, with magnitudes $m_{rm NUV} =21.449 pm 0.019$ and $m_{rm FUV} =21.832 pm 0.103$. We also detected the pulsar-wind nebula (PWN) in the NUV-MAMA image, with a morphology similar to that observed in the optical and near-infrared (IR). The extinction-corrected NUV and FUV pulsar fluxes are compatible with a very steep power 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 the optical/near-IR power-law spectrum (spectral index $alpha_{rm O,nIR} sim 0.7$), indicates an abrupt turn-off at wavelengths below 2500 AA, not observed in other pulsars. We detected pulsations in both the NUV and FUV data at the 50 ms pulsar period. In both cases, the pulse profile features two peaks closely spaced in phase, as observed in the optical and X-ray light curves. The NUV/FUV peaks 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 a similar beaming geometry across all wavelengths. PSR B0540-69 is now the fifth isolated pulsar, together with Crab, Vela, PSR, B0656+14, and the radio-quiet Geminga, 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." @default.
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- W2892442451 date "2018-09-28" @default.
- W2892442451 modified "2023-10-18" @default.
- W2892442451 title "The first ultraviolet detection of the Large Magellanic Cloud pulsar PSR B0540-69" @default.
- W2892442451 hasPublicationYear "2018" @default.
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