Sizing up the population of gamma-ray binaries

Dubus, G.; Guillard, Nicolas; Petrucci, Pierre-Olivier; Martin, Pierrick

doi:10.1051/0004-6361/201731084

Cited by 43 publications

(45 citation statements)

References 52 publications

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“…Gamma-ray binaries, which are characterised by non-thermal emission peaking above 1 MeV, are compact objects in orbit with a massive companion. These systems are usually thought to be a short-lived phase in the evolution of HMXBs, preceding the phase when the accretion commences on to the compact object (Tauris & van den Heuvel 2006;Dubus et al 2017). The only gamma-ray binary in the LMC known to date is DEM L241 (LMC P3, Corbet et al 2016) which is also a XRB-SNR system as discussed earlier.…”

Section: The Youngest Known Hmxb Caught At the Onset Of Accretion?mentioning

confidence: 99%

Discovery of a very young high-mass X-ray binary associated with the supernova remnant MCSNR J0513-6724 in the LMC

Maitra

Haberl

Filipović

et al. 2019

Monthly Notices of the Royal Astronomical Society

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We report the discovery of a very young high-mass X-ray binary (HMXB) system associated with the supernova remnant (SNR) MCSNR J0513-6724 in the Large Magellanic Cloud (LMC), using XMM-Newton X-ray observations. The HMXB is located at the geometrical centre of extended soft X-ray emission, which we confirm as an SNR. The HMXB spectrum is consistent with an absorbed power law with spectral index ∼1.6 and a luminosity of 7×10 33 erg s −1 (0.2-12 keV). Tentative X-ray pulsations are observed with a periodicity of 4.4 s and the OGLE I-band light curve of the optical counterpart from more than 17.5 years reveals a period of 2.2324±0.0003 d, which we interpret as the orbital period of the binary system. The X-ray spectrum of the SNR is consistent with non-equilibrium shock models as expected for young/less evolved SNRs. From the derived ionisation time scale we estimate the age of the SNR to be <6 kyr. The association of the HMXB with the SNR makes it the youngest HMXB, in the earliest evolutionary stage known to date. A HMXB as young as this can switch on as an accreting pulsar only when the spin period has reached a critical value. Under this assumption, we obtain an upper limit to the magnetic field of <5×10 11 G. This implies several interesting possibilities including magnetic field burial, possibly by an episode of post-supernova hyper-critical accretion. Since these fields are expected to diffuse out on a timescale of 10 3 − 10 4 years, the discovery of a very young HMXB can provide us the unique opportunity to observe the evolution of the observable magnetic field for the first time in X-ray binaries.

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Section: The Youngest Known Hmxb Caught At the Onset Of Accretion?mentioning

confidence: 99%

Discovery of a very young high-mass X-ray binary associated with the supernova remnant MCSNR J0513-6724 in the LMC

Maitra

Haberl

Filipović

et al. 2019

Monthly Notices of the Royal Astronomical Society

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“…Early works predicted an overall population of ∼ 30 γ-ray binaries in the Milky Way (Meurs & van den Heuvel 1989). However, in a more recent study performed by Dubus et al (2017), the population of Galactic γ-ray binaries was estimated to be 101 +89 −52 . The main factor of uncertainty in this model is the TeV unassociated sources whose GeV component might be faint (i.e.…”

Section: A New Gev-faint γ-Ray Binarymentioning

confidence: 97%

“…systems similar to HESS J0632+057). According to Dubus et al (2017), such systems have a extremely low probability to be detected in Fermi-LAT or H.E.S.S.-like surveys (∼ 0.8%), but the detection of HESS J0632+057 as a faint GeV source (Li et al 2017) placed an upper limit to the number of similar systems as 231.…”

Section: A New Gev-faint γ-Ray Binarymentioning

confidence: 99%

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X-ray andγ-ray orbital variability from theγ-ray binary HESS J1832−093

Martí-Devesa

Reimer

2020

A&A

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Context. Gamma-ray binaries are systems composed of a massive star and a compact object whose interaction leads to particle acceleration up to relativistic energies. In the last fifteen years, a few binaries have been discovered to emit at high energies, but their number is still scarce. The TeV source HESS J1832−093 has been proposed as a binary candidate, although its nature is unclear. Neither a GeV counterpart nor a period was found for it. Aims. The purpose of this work is to search for a γ-ray source at GeV energies to understand the origin of the TeV signal. For an unambiguous identification of its binary nature, finding an orbital modulation is crucial. Methods. We have analysed data spanning more than 10 years from the Fermi Large Area Telescope (Fermi-LAT), together with Swift archival observations taken between 2015 and 2018, using both the X-Ray Telescope (XRT) and UltraViolet and Optical Telescope (UVOT). We searched for periodicities in both X-ray and γ-ray bands using a Lomb-Scargle periodogram. Results. We find a periodic modulation of ∼ 86 days in the X-ray source XMMU J183245−0921539, together with indications of γ-ray modulation with a compatible period in 4FGL J1832.9−0913. Neither an optical nor an UV counterpart is found at the X-ray source location. The overall spectral energy distribution strongly resembles the known γ-ray binary HESS J0632+057.Conclusions. Both the spectrum and the discovery of an orbital period allow the identification of the TeV source HESS J1832−093 as a new member of the γ-ray binary class.

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“…Beyond detailed studies of the known binaries, CTA is foreseen to discover new sources, enlarging the population. Dubus et al (2017) has estimated that four new gamma-ray binaries can be expected in the first two years of the CTA Galactic Plane survey.…”

Section: Introductionmentioning

confidence: 99%

Overview of non-transientγ-ray binaries and prospects for the Cherenkov Telescope Array

Chernyakova

Malyshev

Paizis

et al. 2019

A&A

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Aims. Despite recent progress in the field, there are still many open questions regarding γ-ray binaries. In this paper we provide an overview of non-transient γ-ray binaries and discuss how observations with the Cherenkov Telescope Array (CTA) will contribute to their study. Methods. We simulate the spectral behaviour of the non-transient γ-ray binaries using archival observations as a reference. With this we test the CTA capability to measure the sources' spectral parameters and detect variability on various time scales. Results. We review the known properties of γ-ray binaries and the theoretical models that have been used to describe their spectral and timing characteristics. We show that CTA is capable of studying these sources on time scales comparable to their characteristic variability time scales. For most of the binaries, the unprecedented sensitivity of CTA will allow the spectral evolution to be studied on a time scale as short as 30 min. This will enable a direct comparison of the TeV and lower energy (radio to GeV) properties of these sources from simultaneous observations. We also review the source-specific questions that can be addressed with such high-accuracy CTA measurements.

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Sizing up the population of gamma-ray binaries

Cited by 43 publications

References 52 publications

Discovery of a very young high-mass X-ray binary associated with the supernova remnant MCSNR J0513-6724 in the LMC

Discovery of a very young high-mass X-ray binary associated with the supernova remnant MCSNR J0513-6724 in the LMC

X-ray andγ-ray orbital variability from theγ-ray binary HESS J1832−093

Overview of non-transientγ-ray binaries and prospects for the Cherenkov Telescope Array

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