The magnetar 1E 1547.0-5408 exhibited outbursts in October 2008 and January 2009 .
In this paper we present in great detail the evolution of the temporal and spectral characteristics of the persistent total and pulsed emission of 1E 1547.0-5408 between \sim 1 and 300 keV starting in October 3 , 2008 , and ending in January 2011 .
We analyzed data collected with the Rossi X-ray Timing Explorer , the International Gamma-Ray Astrophysics Laboratory and the Swift satellite .
We report the evolution of the pulse frequency , and the measurement at the time of the onset of the January 2009 outburst of an insignificant jump in frequency , but a major frequency derivative jump \Delta { \dot { \nu } } of + ( 1.30 \pm 0.14 ) \cdot 10 ^ { -11 } Hz/s ( \Delta \dot { \nu } / \dot { \nu } of -0.69 \pm 0.07 ) .
Before this \dot { \nu } glitch , a single broad pulse is detected , mainly for energies below \sim 10 keV .
Surprisingly , \sim 11 days after the glitch a new transient high-energy ( up to \sim 150 keV ) pulse appears with a Gaussian shape and width 0.23 , shifted in phase by \sim 0.31 compared to the low-energy pulse , which smoothly fades to undetectable levels in \sim 350 days .
We report the evolution of the pulsed emission spectra .
For energies 2.5–10 keV all pulsed spectra are very soft with photon indices \Gamma between -4.6 and -3.9 .
For \sim 10–150 keV , after the \dot { \nu } glitch , we report hard non-thermal pulsed spectra , similar to what has been reported for the persistent pulsed emission of some Anomalous X-ray Pulsars .
This pulsed hard X-ray emission reached maximal luminosity 70 \pm 30 days after the glitch epoch , followed by a gradual decrease by more than a factor 10 over \sim 300 days .
These characteristics differ from those of the total emission .
Both , the total soft X-ray ( 1–10 keV ) and hard X-ray ( 10–150 keV ) fluxes were maximal already two days after the 2009 January outburst , and decayed by a factor of \gtrsim 3 over \sim 400 days .
The total spectra can be described with a black-body ( kT values varying in the range 0.57–0.74 keV ) plus a single power-law model .
The photon index exhibited a hardening ( \sim -1.4 to \sim -0.9 ) with time , correlated with a decrease in flux in the 20–300 keV band .
We discuss these findings in the framework of the magnetar model .