A comprehensive study of high-energy gamma-ray and radio emission from Cyg X-3

Zdziarski, A. A.; Malyshev, D.; Dubus, G.; Pooley, G. G.; Johnson, T. J.; Frankowski, A.; Marco, Barbara De; Chernyakova, M.; Rao, A. R.

doi:10.1093/mnras/sty1618

Cited by 54 publications

(59 citation statements)

References 69 publications

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“…Such systems would include Cygnus X-3 (e.g. Corbel et al 2012;Zdziarski et al 2018) and Cygnus X-1 (e.g. Bodaghee et al 2013;Zanin et al 2016;Zdziarski et al 2017).…”

Section: Introductionmentioning

confidence: 99%

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

Corbet

Chomiuk

Coe

et al. 2019

ApJ

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We report the identification from multi-wavelength observations of the Fermi Large Area Telescope (LAT) source 4FGL J1405.1-6119 (= 3FGL J1405.4-6119) as a high-mass gamma-ray binary. Observations with the LAT show that gamma-ray emission from the system is modulated at a period of 13.7135 ± 0.0019 days, with the presence of two maxima per orbit with different spectral properties. X-ray observations using the Neil Gehrels Swift Observatory X-ray Telescope (XRT) show that X-ray emission is also modulated at this period, but with a single maximum that is closer to the secondary lower-energy gamma-ray maximum. A radio source, coincident with the X-ray source is also found from Australia Telescope Compact Array (ATCA) observations, and the radio emission is modulated on the gamma-ray period with similar phasing to the X-ray emission. A large degree of interstellar obscuration severely hampers optical observations, but a near-infrared counterpart is found. Nearinfrared spectroscopy indicates an O6 III spectral classification. This is the third gamma-ray binary to be discovered with the Fermi LAT from periodic modulation of the gamma-ray emission, the other two sources also have early O star, rather than Be star, counterparts. We consider at what distances we can detect such modulated gamma-ray emission with the LAT, and examine constraints on the gamma-ray binary population of the Milky Way.

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“…Such systems would include Cygnus X-3 (e.g. Corbel et al 2012;Zdziarski et al 2018) and Cygnus X-1 (e.g. Bodaghee et al 2013;Zanin et al 2016;Zdziarski et al 2017).…”

Section: Introductionmentioning

confidence: 99%

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

Corbet

Chomiuk

Coe

et al. 2019

ApJ

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“…In addition, the hard state is defined to correspond to the range of the radio flux of 30-300 mJy, while no constraint on it is imposed in the soft/intermediate state. Adapted from Zdziarski et al (2018), see that paper for details of the data and the used method.…”

Section: Introductionmentioning

confidence: 99%

“…In addition, former is restricted to the range of the radio flux of 30-300 mJy. Adapted fromZdziarski et al (2018). varying trajectories, see Figs. 4 and 5 ofSzostek et al (2008).…”

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confidence: 99%

Jets in the soft state in Cyg X-3 caused by advection of the donor magnetic field and unification with low-mass X-ray binaries

Cao

Zdziarski

2019

Monthly Notices of the Royal Astronomical Society

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The high-mass accreting binary Cyg X-3 is distinctly different from low-mass X-ray binaries (LMXBs) in having powerful radio and γ-ray emitting jets in its soft spectral state. However, the transition from the hard state to the soft one is first associated with quenching of the hardstate radio emission, as in LMXBs. The powerful soft-state jets in Cyg X-3 form, on average, ∼50 d later. We interpret the initial jet quenching as due to the hard-state vertical magnetic field quickly diffusing away in the thin disc extending to the innermost stable circular orbit in the soft state, or, if that field is produced in situ, also cessation of its generation. The subsequent formation of the powerful jets occurs due to advection of the magnetic field from the donor. We find this happens only above certain threshold accretion rate associated with appearance of magnetically driven outflows. The ∼50 d lag is of the order of the viscous timescale in the outer disc, while the field advection is much faster. This process does not happen in LMXBs due to the magnetic fluxes available from their donors being lower than that for the wind accretion from the Wolf-Rayet donor of Cyg X-3. In our model, the vertical magnetic field in the hard state, required to form the jets both in Cyg X-3 and LMXBs, is formed in situ rather than advected from the donor. Our results provide a unified scenario of the soft and hard states in both Cyg X-3 and LMXBs.

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“…Tavani et al 2009a;Sabatini et al 2010;Bodaghee et al 2013;Malyshev et al 2013). Cyg X-1 is detected up to about 10 GeV in the hard state (Zanin et al 2016;Zdziarski et al 2017), and Cyg X-3 is detected up to about 10 GeV during flares that mostly occur when the source is in the soft state (Zdziarski et al 2018). In 2006 MAGIC telescope has also reported marginal detection of TeV flare from Cyg X-1 at a 3.2 σ confidence level coinciding with an X-ray flare seen by RXTE, Swift, and INTEGRAL (Albert et al 2007).…”

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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A comprehensive study of high-energy gamma-ray and radio emission from Cyg X-3

Cited by 54 publications

References 69 publications

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

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

Jets in the soft state in Cyg X-3 caused by advection of the donor magnetic field and unification with low-mass X-ray binaries

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

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