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We report on INTEGRAL, Swift and XMM-Newton observations of IGR J17511-3057performed during the outburst that occurred between March 23 and April 25,2015. The source reached a peak flux of 0.7(2)E-9 erg/cm$^2$/s and decayed toquiescence in approximately a month. The X-ray spectrum was dominated by apower-law with photon index between 1.6 and 1.8, which we interpreted asthermal Comptonization in an electron cloud with temperature > 20 keV . A broad({\sigma} ~ 1 keV) emission line was detected at an energy (E =6.9$^{+0.2}_{-0.3}$ keV) compatible with the K{\alpha} transition of ionizedFe, suggesting an origin in the inner regions of the accretion disk. Theoutburst flux and spectral properties shown during this outburst wereremarkably similar to those observed during the previous accretion eventdetected from the source in 2009. Coherent pulsations at the pulsar spin periodwere detected in the XMM-Newton and INTEGRAL data, at a frequency compatiblewith the value observed in 2009. Assuming that the source spun up during the2015 outburst at the same rate observed during the previous outburst, we derivea conservative upper limit on the spin down rate during quiescence of 3.5E-15Hz/s. Interpreting this value in terms of electromagnetic spin down yields anupper limit of 3.6E26 G/cm$^3$ to the pulsar magnetic dipole (assuming amagnetic inclination angle of 30{\deg}). We also report on the detection offive type-I X-ray bursts (three in the XMM-Newton data, two in the INTEGRALdata), none of which indicated photospheric radius expansion.

The 2015 outburst of the accreting millisecond pulsar IGR J17511-3057 as seen by INTEGRAL, Swift and XMM-Newton