Discovery of a 2.8 s Pulsar in a 2 Day Orbit High-mass X-Ray Binary Powering the Ultraluminous X-Ray Source ULX-7 in M51
Salvaterra, R.; Haberl, F.; Tiengo, A.; Harrison, F. A.; Stella, L.; Wolter, A.; Belfiore, A.; Marelli, M.; Pinto, C.; Esposito, P.; De Luca, A.; Israel, G. L.; Dall'Osso, S.; Bernardini, F.; Bachetti, M.; Casella, P.; Papitto, A.; Turolla, R.; Earnshaw, H. P.; Roberts, T. P.; Rodríguez Castillo, G. A.; Pintore, F.; Brightman, M.; Walton, D. J.; Fürst, F.; D'Agostino, D.; Middleton, M.; Zampieri, L.; Mapelli, M.
Italy, United Arab Emirates, United States, Spain, Germany, Austria, United Kingdom, Netherlands
Abstract
We discovered 2.8 s pulsations in the X-ray emission of the ultraluminous X-ray source (ULX) M51 ULX-7 within the UNSEeN project, which was designed to hunt for new pulsating ULXs (PULXs) with XMM-Newton. The pulse shape is sinusoidal, and large variations of its amplitude were observed even within single exposures (pulsed fraction from less than 5% to 20%). Source M51 ULX-7 is variable, generally observed at an X-ray luminosity between 1039 and 1040 erg s-1, located in the outskirts of the spiral galaxy M51a at a distance of 8.6 Mpc. According to our analysis, the X-ray pulsar orbits in a 2 day binary with a projected semimajor axis ${a}_{{\rm{X}}}\sin I\,\simeq $ 28 lt-s. For a neutron star (NS) of 1.4 M⊙, this implies a lower limit on the companion mass of 8 M⊙, placing the system hosting M51 ULX-7 in the high-mass X-ray binary class. The barycentric pulse period decreased by ≃0.4 ms in the 31 days spanned by our 2018 May-June observations, corresponding to a spin-up rate $\dot{P}\simeq -1.5\times {10}^{-10}\,{\rm{s}}\ {{\rm{s}}}^{-1}$ . In an archival 2005 XMM-Newton exposure, we measured a spin period of ∼3.3 s, indicating a secular spin-up of ${\dot{P}}_{\sec }\simeq -{10}^{-9}\,{\rm{s}}\ {{\rm{s}}}^{-1}$ , a value in the range of other known PULXs. Our findings suggest that the system consists of a massive donor, possibly an OB giant or supergiant, and a moderately magnetic (dipole field component in the range 1012 G $\lesssim {B}_{\mathrm{dip}}\lesssim {10}^{13}$ G) accreting NS with weakly beamed emission ( $1/12\lesssim b\lesssim 1/4$ ).