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The variable X-ray source 1E 1547.0-5408 was identified by Gelfand & Gaensler(2007) as a likely magnetar in G327.24-0.13, an apparent supernova remnant. NoX-ray pulsations have been detected from it. Using the Parkes radio telescope,we discovered pulsations with period P = 2.069 s. Using the Australia TelescopeCompact Array, we localized these to 1E 1547.0-5408. We measure dP/dt =(2.318+-0.005)e-11, which for a magnetic dipole rotating in vacuo gives asurface field strength of 2.2e14 G, a characteristic age of 1.4 kyr, and aspin-down luminosity of 1.0e35 ergs/s. Together with its X-ray characteristics,these rotational parameters of 1E 1547.0-5408 prove that it is a magnetar, onlythe second known to emit radio waves. The distance is ~9 kpc, derived from thedispersion measure of 830 pc/cc. The pulse profile at a frequency of 1.4 GHz isextremely broad and asymmetric due to multipath propagation in the ISM, as aresult of which only approximately 75% of the total flux at 1.4 GHz is pulsed.At higher frequencies the profile is more symmetric and has FWHM = 0.12P.Unlike in normal radio pulsars, but in common with the other knownradio-emitting magnetar, XTE J1810-197, the spectrum over 1.4-6.6 GHz is flator rising, and we observe large, sudden changes in the pulse shape. In acontemporaneous Swift X-ray observation, 1E 1547.0-5408 was detected withrecord high flux, f_X(1-8 keV) ~ 5e-12 ergs/cm^2/s, 16 times the historicminimum. The pulsar was undetected in archival radio observations from 1998,implying a flux < 0.2 times the present level. Together with the transientbehavior of XTE J1810-197, these results suggest that radio emission istriggered by X-ray outbursts of usually quiescent magnetars.

1E 1547.0-5408: a radio-emitting magnetar with a rotation period of 2 seconds