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We present detailed timing and spectral analyses of the transient X-raypulsar RX J0209.6$-$7427 in the Small Magellanic Cloud during its 2019 giantoutburst. With a better known distance than most galactic X-ray pulsars, itspeak luminosity is determined to be $(1.11\pm0.06)\times 10^{39}\, \rm erg\s^{-1}$; it is thus a {\it bonda fide} pulsating ultraluminous X-ray source(PULX). Owing to the broad energy band of \textit{Insight}-HXMT, its pulsedX-ray emission was detected from 1 keV up to the 130$-$180 keV band, which isthe highest energy emission detected from any PULXs outside the Milky Way. Thisallows us to conclude that its main pulsed X-ray emission is from the "fanbeam" of the accretion column, and its luminosity is thus intrinsic. We alsoestimate its magnetic field of (4.8$-$8.6)$\times10^{12}$ G or(1.7$-$2.2)$\times10^{13}$ G, from its spin evolution or transition in theaccretion column structure during the outburst; we suggest that the two valuesof the magnetic field strength correspond to the dipole and multipole magneticfields of the neutron star, similar to the recent discovery in the GalacticPULX Swift J0243.6+6124. Therefore, the nature of the neutron star and its ULXemission can be understood within the current theoretical frame of accretingneutron stars. This may have implications for understanding the nature of thosefarther away extragalactic PULXs.

Fan beamed X-ray emission from 1 keV to above 130 keV from the ultraluminous X-ray pulsar RX J0209.6-7427 in the Small Magellanic Cloud