Journal
MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY
Volume 466, Issue 1, Pages L48-L52Publisher
OXFORD UNIV PRESS
DOI: 10.1093/mnrasl/slw218
Keywords
galaxies: individual: NGC 7793; X-rays: binaries : X-rays: individual:CXOU J235750.9-323726 (XMMU J235751.1-323725; NGC 7793 P13).
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Funding
- EU's Seventh Framework Programme [607452]
- NWO Vidi award [A.2320.0076]
- ASI - INAF [NuSTAR I/037/12/0]
- EU Marie Sklodowska Curie Individual Fellowship [660657-TMSPH2020-MSCA-IF-2014]
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NGC 7793 P13 is a variable (luminosity range similar to 100) ultraluminous X-ray source proposed to host a stellar-mass black hole of less than 15M circle dot in a binary system with orbital period of 64 d and a 18-23 M-circle dot B9Ia companion. Within the EXTraS ( Exploring the X-ray Transient and variable Sky) project, we discovered pulsations at a period of similar to 0.42 s in two XMM-Newton observations of NGC 7793 P13, during which the source was detected at LX similar to 2.1 x 1039 and 5 x 1039 erg s(-1) (0.3- 10 keV band). These findings unambiguously demonstrate that the compact object in NGC 7793 P13 is a neutron star accreting at super-Eddington rates. While standard accretion models face difficulties accounting for the pulsar X-ray luminosity, the presence of a multipolar magnetic field with B similar to few x 10(13) G close to the base of the accretion column appears to be in agreement with the properties of the system.
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