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Discovery of a 2.8 s pulsar in a 2 d orbit High-Mass X-ray Binary powering the Ultraluminous X-ray source ULX-7 in M51

Rodríguez Castillo, G. A. and Israel, G. L. and Belfiore, A. and Bernardini, F. and Esposito, P. and Pintore, F. and De Luca, A. and Papitto, A. and Stella, L. and Tiengo, A. and Zampieri, L. and Bachetti, M. and Brightman, M. and Casella, P. and D'Agostino, D. and Dall'Osso, S. and Earnshaw, H. P. and Fürst, F. and Haberl, F. and Harrison, F. A. and Mapelli, M. and Marelli, M. and Middleton, M. and Pinto, C. and Roberts, T. P. and Salvaterra, R. and Turolla, R. and Walton, D. J. and Wolter, A. (2019) Discovery of a 2.8 s pulsar in a 2 d orbit High-Mass X-ray Binary powering the Ultraluminous X-ray source ULX-7 in M51. . (Unpublished) http://resolver.caltech.edu/CaltechAUTHORS:20190619-080458696

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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%). M51 ULX-7 is a variable source, generally observed at an X-ray luminosity between 10^(39) and 10^(40) 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-d binary with a projected semi-major axis a X sin I ≃ 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 d spanned by our May -- June 2018 observations, corresponding to a spin-up rate P˙≃ −1.5×10^(−10)s s^(−1). In an archival 2005 XMM-Newton exposure, we measured a spin period of ∼3.3 s, indicating a secular spin-up of P˙_(sec) ≃ −10^(−9) s s^(−1), a value in the range of other known PULXs. Our findings suggest that the system consists of an OB giant and a moderately magnetic (dipole field component in the range 10^(12) G ≲ B_(dip) ≲ 10^(13)G) accreting NS with weakly beamed emission (1/12 ≲ b ≲ 1/4).


Item Type:Report or Paper (Discussion Paper)
Related URLs:
URLURL TypeDescription
http://arxiv.org/abs/1906.04791arXivDiscussion Paper
ORCID:
AuthorORCID
Esposito, P.0000-0003-4849-5092
Tiengo, A.0000-0002-6038-1090
Bachetti, M.0000-0002-4576-9337
Brightman, M.0000-0002-8147-2602
Earnshaw, H. P.0000-0001-5857-5622
Fürst, F.0000-0003-0388-0560
Harrison, F. A.0000-0003-2992-8024
Middleton, M.0000-0002-8183-2970
Pinto, C.0000-0003-2532-7379
Roberts, T. P.0000-0001-8252-6337
Walton, D. J.0000-0001-5819-3552
Additional Information:We thank Dr. Norbert Schartel for granting DPS XMM–Newton time. The scientific results reported in this article are based on observations obtained with XMM–Newton, an ESA science mission with instruments and contributions directly funded by ESA Member States and NASA. GR acknowledges the support of high performance computing resources awarded by CINECA (MARCONI and GALILEO), under the ISCRA initiative and the INAF-CIENCA MoU; and also the computing centres of INAF – Osservatorio Astronomico di Trieste and Osservatorio Astrofisico di Catania, under the coordination of the CHIPP project, for the availability of computing resources and support. This work has also made use of observations made with the NASA/ESA Hubble Space Telescope, and obtained from the Hubble Legacy Archive, which is a collaboration between the Space Telescope Science Institute (STScI/NASA), the Space Telescope European Coordinating Facility (ST-ECF/ESA) and the Canadian Astronomy Data Centre (CADC/NRC/CSA). This work has also made use of data from the ESA mission Gaia, processed by the Gaia Data Processing and Analysis Consortium (DPAC). We acknowledge funding in the framework of the project ULTraS ASI–INAF contract N. 2017-14-H.0, and project ASI–INAF contract I/037/12/0. FB is funded by the European Unions Horizon 2020 research and innovation programme under the Marie Skłodowska Curie grant agreement no. 664931. This research was supported by high performance computing resources at New York University Abu Dhabi. HPE acknowledges support under NASA contract NNG08FD60C. TPR acknowledges support from STFC as part of the consolidated grant ST/K000861/1. Facility: XMM–Newton (EPIC), HST (ACS) Software: SAS ( v.17.0; Gabriel et al. 2004), FTOOLS (v6.21; Blackburn 1995), XSPEC (v12.9.1; Arnaud 1996)
Group:Space Radiation Laboratory
Funders:
Funding AgencyGrant Number
ESA Member StatesUNSPECIFIED
Agenzia Spaziale Italiana (ASI)2017-14-H.0
Agenzia Spaziale Italiana (ASI)I/037/12/0
Marie Curie Fellowship664931
NASANNG08FD60C
Science and Technology Facilities Council (STFC)ST/K000861/1
Subject Keywords:accretion, accretion disks — galaxies: individual: M51a — pulsars: individual (M51 ULX-7, aka CXOM51 J133001.0+47134)— stars: neutron— X-rays: binaries
Record Number:CaltechAUTHORS:20190619-080458696
Persistent URL:http://resolver.caltech.edu/CaltechAUTHORS:20190619-080458696
Usage Policy:No commercial reproduction, distribution, display or performance rights in this work are provided.
ID Code:96512
Collection:CaltechAUTHORS
Deposited By: Tony Diaz
Deposited On:19 Jun 2019 18:37
Last Modified:19 Jun 2019 18:37

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