5 2009 Fermi Symposium, Washington, D.C., Nov. 2-5 V. SUMMARY AND DISCUSSION FIG. 5: The photon spectrum of the time interval T 0 +122 to 169 s. The blackbody and power-law components are shown separately with dashed curves. The data are binned for display purpose only. A 3 σ upper limit is shown for the highest energy bin. B. Phase-Resolved Spectral Analysis trum as well (ΔC-stat = 42.9 and 15.3, corresponding to 6.2 σ and 3.5 σ improvements, respectively). The ra- tio of the blackbody flux to the total flux (8 − 150 keV) was found to be 34% in both intervals. The indices of the underlying power-law component, and the black- body temperature also remained constant, at ∼− 2 . 1 and ∼ 17 keV, respectively (within uncertainties; see also Table 1), while the power-law amplitude tracked the photon flux. We performed spin-phase-resolved spectral anal- ysis of the pulsed enhanced emission, as follows: we co-added the burst-free spectrum of each pulse (in T$_{0}$ +122 to 223 s, corresponding to second and third time-resolved spectra) using TTE data and ex- tracted a phase-maximum spectrum (between phases 0.75 − 1.25 in Figure 3) and a phase-minimum spec- trum (between phases 0.25 − 0.75). The spin phase for each photon was calculated using barycentered times, as was done for the timing analysis. We calculated the background spectrum, from the burst-free interval at T$_{0}$ to T$_{0}$ +60 s. The spectra of both the phase minimum and maxi- mum were adequately fitted with power law + black- body models, where we kept the power-law indices and the blackbody temperatures linked. The values of the linked parameters found in the fit were consistent (within 1 σ ) with those of the time-integrated spectra (see Table I). The contributions of the blackbody flux to the total flux were (52 ± 18)% and (35 ± 18)%, in the phase-maximum and phase-minimum spectra, re- spectively. This hints that the blackbody component was more significant in the phase-maximum spectrum than in the phase-minimum spectrum. We report here the discovery of coherent pulsa- tions in the persistent hard X-ray emission from SGR J1550–5418 in the Fermi /GBM data lasting ∼ 150 s. Coherent pulsations with a 55% RMS pulse fraction have never been detected in the persistent emission at these high energies from a magnetar as yet. These pulsations were detected only at the on- set of a major bursting episode and were not directly related to a major burst or flare from the source. Pre- viously, intermediate flares with pulsating tails were observed from SGR 1900+14 [22, 23] and very recently from SGR J1550–5418 ( ∼ 6 hours after T$_{0}$ )[8]. Ther- mal components were also found in the decaying tails of intermediate events from SGR 1900+14 with much lower blackbody temperatures of ∼ 2 keV [23]. The thermal component of the enhanced emission we re- port here is hotter (17 keV), exhibits a strong depen- dence of the pulse profile with energy with a very high RMS pulsed fraction (up to 55%), and is clearly not associated with a decaying event tail. Energetically, however, the fluence of this enhanced emission is com- parable to that of tail emission of the intermediate flares from SGR 1900+14. Our timing analysis showed that the detection of pulsations is most significant in the 120 − 210 s inter- val after trigger. We find that the spectrum requires a blackbody component along with a power law be- tween 122 − 223 s, which is consistent with the time interval of the most significant detection of pulsa- tions. Moreover, as determined by the energy depen- dent pulse profiles and RMS pulsed fractions, we find that the high-energy pulsations are most significant in the 50 − 74 keV range. Strikingly, the blackbody component of the enhanced persistent emission spec- trum peaks at around 51 keV (i.e., the Wien peak of 17 keV, see Figure 5). These two independent pieces of evidence lend strong support for a blackbody radi- ation component to account for the curvature in the spectrum of the enhanced emission. In our spin-phase-resolved spectral analysis, we find that the blackbody flux to the total emission is (52 ± 18)% and (35 ± 18)% in the phase-maximum and phase-minimum spectra, respectively. This also suggests that a major contribution to the observed pulsations is from the blackbody component. If we assume a surface hot-spot during this pulsating in- terval, then the best-fit blackbody corresponds to an effective radiating area (as projected on the plane of the sky, far from the star) of S ∞ = πD $^{2}$F/ ( σT $^{4}$) ≈ eConf C091122