Discovery of the Galactic High-mass Gamma-Ray Binary 4FGL J1405.1−6119

Corbet, R. H. D.; Chomiuk, Laura; Coe, M. J.; Coley, Joel B.; Dubus, G.; Edwards, P. G.; Martin, Pierrick; McBride, V. A.; Stevens, J.; Strader, Jay; Townsend, L. J.

doi:10.3847/1538-4357/ab3e32

Cited by 43 publications

(37 citation statements)

References 68 publications

(91 reference statements)

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“…Up to date, there are nine confirmed high-mass gamma-ray binaries for which emission above 100 MeV has been detected: LS I +61 303 (Tavani et al 1998), LS 5039 (Paredes et al 2000), PSR B1259-63 (Aharonian et al 2005), HESS J0632+057 (Aharonian et al 2007;Hinton et al 2009), 1FGL J1018. 6-5856 (Fermi LAT Collaboration et al 2012), HESS J1832-093 (HESS Collaboration et al 2015;Eger et al 2016), LMC P3 (Corbet et al 2016), PSR J2032+4127 (Abeysekara et al 2018), and 4FGL J1405-6119 (Corbet et al 2019). There are other candidate systems with a pulsar orbiting a massive star that exhibit non-thermal radio emission, but for which gamma rays have yet to be detected (see Dubus et al 2017, and references therein).…”

Section: Introductionmentioning

confidence: 99%

A dynamical and radiation semi-analytical model of pulsar-star colliding winds along the orbit: Application to LS 5039

Molina

Bosch‐Ramon

2020

A&A

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Context. Gamma-ray binaries are systems that emit nonthermal radiation peaking at energies above 1 MeV. One proposed scenario to explain their emission consists of a pulsar orbiting a massive star, with particle acceleration taking place in shocks produced by the interaction of the stellar and pulsar winds. Aims. We develop a semi-analytical model of the nonthermal emission of the colliding-wind structure, which includes the dynamical effects of orbital motion. We apply the model to a general case and to LS 5039. Methods. The model consists of a one-dimensional emitter, the geometry of which is affected by Coriolis forces owing to orbital motion. Two particle accelerators are considered: one at the two-wind standoff location and the other one at the turnover produced by the Coriolis force. Synchrotron and inverse Compton emission is studied taking into account Doppler boosting and absorption processes associated to the massive star. Results. If both accelerators are provided with the same energy budget, most of the radiation comes from the region of the Coriolis turnover and beyond, up to a few orbital separations from the binary system. Significant orbital changes of the nonthermal emission are predicted in all energy bands. The model allows us to reproduce some of the LS 5039 emission features, but not all of them. In particular, the MeV radiation is probably too high to be explained by our model alone, the GeV flux is recovered but not its modulation, and the radio emission beyond the Coriolis turnover is too low. The predicted system inclination is consistent with the presence of a pulsar in the binary. Conclusions. The model is quite successful in reproducing the overall nonthermal behavior of LS 5039. Some improvements are suggested to better explain the phenomenology observed in this source, such as accounting for particle reacceleration beyond the Coriolis turnover, unshocked pulsar wind emission, and the three-dimensional extension of the emitter.

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Section: Introductionmentioning

confidence: 99%

A dynamical and radiation semi-analytical model of pulsar-star colliding winds along the orbit: Application to LS 5039

Molina

Bosch‐Ramon

2020

A&A

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“…The resemblance between HESS J1832−093 and HESS J0632+057 might be an indication of a population of γ-ray binaries which have been elusive to detection due to observational biases. The detection threshold in systematic searches for periodicity performed by Corbet et al (2019) is consistent with the non-identification of HESS J1832−093 due to its lack of detection above 10 GeV. Given the low probability of serendipitous detections of new binaries, new observational approaches are required.…”

Section: A New Gev-faint γ-Ray Binarymentioning

confidence: 70%

“…Almost all the systems known are located in the Galactic Plane -PSR B1259-63 (Aharonian et al 2005), LS 5039 (Aharonian et al 2006), LS I +61 303 (Albert et al 2006), HESS J0632+057 (Aharonian et al 2007), 1FGL J1018. 6-5856 (Fermi LAT Collaboration et al 2012), PSR J2032+4127 (Abeysekara et al 2018) and 4FGL J1405.1-6119 (Corbet et al 2019) -with the notable exception of LMC P3 in the Large Magellanic Cloud (Corbet et al 2016).…”

Section: Introductionmentioning

confidence: 99%

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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“…We used data covering the interval from MJD 54682 to 58745 with a time resolution of 500 s. The technique of probabilityweighted aperture photometry was used for this purpose. This is the same technique that led to the most recent discoveries of the GBs LMC P3 (Corbet et al 2016) and 4FGL J1405.1-6119 (Corbet et al 2019). The resulting power spectrum is shown in Fig.…”

Section: Looking For the Orbital Period Signature In Fermi Datamentioning

confidence: 94%

A blazar as the likely counterpart to 4FGL J0647.7−4418 instead of a gamma-ray binary

Martı́

Sánchez-Ayaso

Luque-Escamilla

et al. 2020

Monthly Notices of the Royal Astronomical Society

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The persistent gamma-ray source 4FGL J0647.7−4418 is tentatively associated in the latest Fermi catalogue with the sub-dwarf O-type X-ray binary HD 49798. However, an AGN candidate is also mentioned as an alternative identification in updated versions of the catalogue accompanying paper. If the first association were correct, this would add HD 49798 to the handful of currently known gamma-ray binaries and, therefore, represent a significant breakthrough not only because of a new member addition, but also because of the apparent white dwarf companion in this system. Despite these perspectives, here we show that the stellar association is likely wrong and that the proposed AGN object, well inside the Fermi 95% confidence ellipse, is a more conceivable counterpart candidate to the Fermi source due to its strong blazar similarities.

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Discovery of the Galactic High-mass Gamma-Ray Binary 4FGL J1405.1−6119

Cited by 43 publications

References 68 publications

A dynamical and radiation semi-analytical model of pulsar-star colliding winds along the orbit: Application to LS 5039

A dynamical and radiation semi-analytical model of pulsar-star colliding winds along the orbit: Application to LS 5039

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

A blazar as the likely counterpart to 4FGL J0647.7−4418 instead of a gamma-ray binary

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