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

Castillo, G. A. Rodríguez; Israel, G. L.; Belfiore, A.; Bernardini, F.; Esposito, P.; Pintore, F.; De Luca, A.; Papitto, A.; Stella, L.; Tiengo, A.; Zampieri, L.; Bachetti, M.; Brightman, M.; Casella, P.; D'Agostino, D.; Dall'Osso, S.; Earnshaw, H. P.; Fürst, F.; Haberl, F.; Harrison, F. A.; Mapelli, M.; Marelli, M.; Middleton, M.; Pinto, C.; Roberts, T. P.; Salvaterra, R.; Turolla, R.; Walton, D. J.; Wolter, A.

doi:10.48550/arxiv.1906.04791

Cited by 29 publications

(58 citation statements)

References 68 publications

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“…Understanding the nature of ULXs became more and more challenging after the discovery of the first pulsating ULX (Bachetti et al 2014), which unequivocally showed that ULXs can also be accreting neutron stars. This discovery has been confirmed by the identification of other five pulsar ULXs (Israel et al 2017a,b;Carpano et al 2018;Rodríguez Castillo et al 2019;Sathyaprakash et al 2019) whose emission properties can only been explained in terms of super-Eddington accretion (Mushtukov et al 2017). ULXs appear to be the sources where super-Eddington accretion reveals itself in a variety of phenomenological modes.…”

Section: Introductionmentioning

confidence: 83%

“…10 we show the different components which contribute to the overall emission spectrum: the optical band is dominated by the outer accretion disc, which is very bright because of the very high mass transfer rate. 2018; Sathyaprakash et al 2019;Rodríguez Castillo et al 2019). Detecting pulsations likely requires a specific viewing angle and/or special physical conditions.…”

Section: Ngc 5907 Ulx2mentioning

confidence: 99%

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Modelling optical emission of Ultra-luminous X-ray Sources accreting above the Eddington limit

Ambrosi

Zampieri

2018

Monthly Notices of the Royal Astronomical Society

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We study the evolution of binary systems of Ultra-luminous X-ray sources and compute their optical emission assuming accretion onto a black hole via a non standard, advection-dominated slim disc with an outflow. We consider systems with black holes of 20M and 100M , and donor masses between 8M and 25M . Super-critical accretion has considerable effects on the optical emission. The irradiating flux in presence of an outflow remains considerably stronger than that produced by a standard disc. However, at very high accretion rates the contribution of X-ray irradiation becomes progressively less important in comparison with the intrinsic flux emitted from the disc. After Main Sequence the evolutionary tracks of the optical counterpart on the colourmagnitude diagram are markely different from those computed for Eddington-limited accretion. Systems with stellar-mass black holes and 12 − 20M donors accreting supercritically are characterized by blue colors (F450W -F555W −0.2 : +0.1) and high luminosity (M V −4 : −6.5). Systems with more massive black holes accreting supercritically from evolved donors of similar mass have comparable colours but can reach M V −8. We apply our model to NGC 1313 X-2 and NGC 4559 X-7. Both sources are well represented by a system accreting above Eddington from a massive evolved donor. For NGC 1313 X-2 the agreement is for a ∼ 20M black hole, while NGC4559 X-7 requires a significantly more massive black hole.

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Section: Introductionmentioning

confidence: 83%

Section: Ngc 5907 Ulx2mentioning

confidence: 99%

Modelling optical emission of Ultra-luminous X-ray Sources accreting above the Eddington limit

Ambrosi

Zampieri

2018

Monthly Notices of the Royal Astronomical Society

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“…Motivated by the recent discovery of pulsating ULXs (Bachetti et al 2014;Fürst et al 2016;Israel et al 2017b,a;Carpano et al 2018;Rodríguez Castillo et al 2019;Sathyaprakash et al 2019) and their proposed interpretation in terms of accreting magnetars (see Tong & Wang 2019), we have reconsidered the problem of columnated accretion onto a highly magnetized NS. The main aim was to find model configurations capable of producing a high, super-Eddington luminosity while not in the propeller regime (for the values of the spin period typical of PULXs, 𝑃 ∼ 1s).…”

Section: Discussionmentioning

confidence: 99%

“…For the first time, firm evidence was presented that a ULX could host an accreting, neutron star (NS). Since then, further discoveries of PULXs have been made (Fürst et al 2016;Israel et al 2017b,a;Rodríguez Castillo et al 2019;Sathyaprakash et al 2019). At present, there is no evidence that PULXs differ from non-pulsating ULX basing on their spectral ★ E-mail: nabil.brice.17@ucl.ac.uk properties alone, which hints at the possibility that there are may be many more NS-powered ULXs than previously thought (e.g.…”

Section: Introductionmentioning

confidence: 99%

Super-Eddington Emission from Accreting, Highly Magnetised Neutron Stars with a Multipolar Magnetic Field

Brice,

Zane,

Turolla

et al. 2021

Preprint

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Pulsating ultra-luminous X-ray sources (PULXs) are characterised by an extremely large luminosity (> 10 40 erg s −1 ). While there is a general consensus that they host an accreting, magnetized neutron star (NS), the problem of how to produce luminosities > 100 times the Eddington limit, 𝐿 𝐸 , of a solar mass object is still debated. A promising explanation relies on the reduction of the opacities in the presence of a strong magnetic field, which allows for the local flux to be much larger than the Eddington flux. However, avoiding the onset of the propeller effect may be a serious problem. Here, we reconsider the problem of column accretion onto a highly magnetized NS, extending previously published calculations by relaxing the assumption of a pure dipolar field and allowing for more complex magnetic field topologies. We find that the maximum luminosity is determined primarily by the magnetic field strength near the NS surface. We also investigate other factors determining the accretion column geometry and the emergent luminosity, such as the assumptions on the parameters governing the accretion flow at the disk-magnetosphere boundary. We conclude that a strongly magnetized NS with a dipole component of ∼ 10 13 G, octupole component of ∼ 10 14 G and spin period ∼ 1s can produce a luminosity of ∼ 10 41 erg s −1 while avoiding the propeller regime. We apply our model to two PULXs, NGC 5907 ULX-1 and NGC 7793 P13, and discuss how their luminosity and spin period rate can be explained in terms of different configurations, either with or without multipolar magnetic components.

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“…The recent detection of coherent pulsations in several ULXs in-★ E-mail: walston@sciops.esa.int dicates they are powered by neutron stars (NS) accreting at very high Eddington rates, with luminosities up to ∼ 500𝐿 Edd (Bachetti et al 2014;Israel et al 2017a,b;Carpano et al 2018;Sathyaprakash et al 2019. Rodriguez Castillo et al 2019.…”

Section: Introductionmentioning

confidence: 99%

Quasi-periodic dipping in the ultraluminous X-ray source, NGC 247 ULX-1

Alston,

Pinto,

Barret

et al. 2021

Preprint

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Most ultraluminous X-ray sources (ULXs) are believed to be stellar mass black holes or neutron stars accreting beyond the Eddington limit. Determining the nature of the compact object and the accretion mode from broadband spectroscopy is currently a challenge, but the observed timing properties provide insight into the compact object and details of the geometry and accretion processes. Here we report a timing analysis for an 800 ks XMM-Newton campaign on the supersoft ultraluminous X-ray source, NGC 247 ULX-1. Deep and frequent dips occur in the X-ray light curve, with the amplitude increasing with increasing energy band. Power spectra and coherence analysis reveals the dipping preferentially occurs on ∼ 5 ks and ∼ 10 ks timescales, indicating the mechanism is located at ∼ 10 4 𝑅 𝐺 from the compact object. The dips can be caused by either the occultation of the central X-ray source by an optically thick structure, such as warping of the accretion disc, or from obscuration by a wind launched from the accretion disc, or both. This behaviour supports the idea that supersoft ULXs are viewed close to edge-on to the accretion disc.

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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

Cited by 29 publications

References 68 publications

Modelling optical emission of Ultra-luminous X-ray Sources accreting above the Eddington limit

Modelling optical emission of Ultra-luminous X-ray Sources accreting above the Eddington limit

Super-Eddington Emission from Accreting, Highly Magnetised Neutron Stars with a Multipolar Magnetic Field

Quasi-periodic dipping in the ultraluminous X-ray source, NGC 247 ULX-1

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