The bright unidentifiedγ-ray source 1FGL J1227.9−4852: can it be associated with a low-mass X-ray binary?

Hill, A. B.; Szostek, A.; Corbel, S.; Camilo, F.; Corbet, R. H. D.; Dubois, R.; Dubus, G.; Edwards, P. G.; Ferrara, E. C.; Kerr, M.; Koerding, E.; Kozieł, D.; Stawarz, Ł.

doi:10.1111/j.1365-2966.2011.18692.x

Cited by 71 publications

(91 citation statements)

References 41 publications

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“…This variability reinforced the prediction, first made by Hill et al (2011), that the system could harbour an active radio MSP, sharing similar properties with J1023. Follow-up observations in the radio finally succeeded in detecting pulsations at a period of 1.69 ms (Roy et al 2014).…”

Section: Xss J12270-4859mentioning

confidence: 48%

“…Subsequent independent multi-wavelength studies (Pretorius 2009;Saitou et al 2009;de Martino et al 2010de Martino et al , 2013Hill et al 2011; casted doubts on this classification, suggesting instead an identification as a LMXB showing unusual dipping and flaring behaviour on timescales of few hundreds of seconds. XSS J12270−4859 was subsequently recognised to be spatially coincident with a moderately bright gamma-ray source that was detected by Fermi-LAT emitting up to 10 GeV (de Martino et al 2010;Hill et al 2011), and is now known as 3FGL J1227.9−4854.…”

Section: Xss J12270-4859mentioning

confidence: 99%

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Different twins in the millisecond pulsar recycling scenario: Optical polarimetry of PSR J1023+0038 and XSS J12270-4859

Baglio

D’Avanzo

Campana

et al. 2016

A&A

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We present the first optical polarimetric study of the two transitional pulsars PSR J1023+0038 and XSS J12270-4859. This work is focused on the search for intrinsically linearly polarised optical emission from the two systems. To this aim, we carried out multiband optical (BVRi) and near-infrared (NIR; JHK) photo-polarimetric observations of the two systems using the ESO New Technology Telescope (NTT) at La Silla (Chile), equipped with the EFOSC2 and the SOFI instruments. The system XSS J12270-4859 was observed during its radio-pulsar state; we did not detect a significant degree of polarisation in any of the bands, with 3σ upper limits, for example, of 1.4% in the R-band. We built the NIR−optical averaged spectral energy distribution (SED) of the system, which could be described well by an irradiated black body with radius R * = 0.33 ± 0.03 R and albedo η = 0.32 ± 0.05, without the need for further components. Thus, we excluded the visible presence of an extended accretion disc and/or of relativistic jets. The case was different for PSR J1023+0038, which was in its accretion phase during our campaign. We measured a linear polarisation of 1.09 ± 0.27% and 0.90 ± 0.17% in the V and R bands, respectively. The phase-resolved polarimetric curve of the source in the R band reveals a hint of a sinusoidal modulation at the source 4.75 h orbital period, peaked at the same orbital phase as the light curve. The measured optical polarisation of PSR J1023+0038 could, in principle, be interpreted as electron scattering with free electrons, which can be found in the accretion disc of the system or even in the hot corona that sorrounds the disc itself, or as synchrotron emission from a jet of relativistic particles or an outflow. However, the NIR-optical SED of the system built from our dataset did not suggest the presence of a jet. We conclude that the optical linear polarisation observed for PSR J1023+0038 is possibly due to Thomson scattering with electrons in the disc, as is also suggested from the possible modulation of the R-band linear polarisation at the system orbital period.

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Section: Xss J12270-4859mentioning

confidence: 48%

Section: Xss J12270-4859mentioning

confidence: 99%

Different twins in the millisecond pulsar recycling scenario: Optical polarimetry of PSR J1023+0038 and XSS J12270-4859

Baglio

D’Avanzo

Campana

et al. 2016

A&A

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“…This object has also been detected at hard X-ray energies by INTEGRAL/IBIS and Swift/BAT, it has then be classified as a CV of the magnetic type (Masetti et al 2006) and subsequently it was associated with a Fermi source (1FGL J1227.9−4852/2FGL J1227.7−4853) listed in the first and second catalogues (Abdo et al 2010(Abdo et al , 2012; only recently, it was described as a peculiar type of X-ray binary (De Martino et al 2010Hill et al 2011). Furthermore, XSS J12270−4859 is not the first time that a CV has been associated with a GeV emitter.…”

Section: Connection To the Gev/tev Emissionmentioning

confidence: 99%

The counterpart/s of IGR J20159+3713/SWIFT J2015.9+3715: dissecting a complex region with emission from keV to TeV

Bassani¹,

Landi²,

Malizia³

et al. 2014

A&A

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We report on the identification of a new soft gamma-ray source, namely IGR J20159+3713/SWIFT J2015.9+3715, first detected by INTEGRAL/IBIS and then confirmed by Swift/BAT. The source, which has an observed 20-100 keV flux in the range (0.7−1.4)×10 −11 erg cm −2 s −1 , encloses a Fermi variable source (2FGL J2015.6+3709) and is spatially close to a TeV emitter (VER J2016+372). Thanks to X-ray follow-up observations performed with the X-ray telescope on board Swift, we have been able to identify the new IBIS/BAT detection with the combined emission of the blazar B2013+370 and the cataclysmic variable RX J2015.6+3711. Both objects show variability in X-rays, with the CV being the most variable of the two. At high energies (above 20 keV) the emission is likely dominated by B2013+370, but the contribution from RX J2015.6+3711 is not negligible. The blazar emits up to GeV frequencies where it is seen by Fermi, while the cataclysmic variable has a bremsstrahlung temperature which is too low to provide any contribution at these high energies. These findings also indicate that the INTEGRAL/Swift source is not associated with the TeV emission, which is most likely due to the supernova remnant (SNR)/pulsar wind nebula (PWN) CTB 87.

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“…The number of members of the class of gamma-ray binaries is growing, being at present around ten, including unconfirmed candidates (e.g. Albert et al 2006Albert et al , 2007Aharonian et al 2005a,b;Abdo et al 2009aAbdo et al ,b,c, 2010aAbdo et al ,b, 2011Tavani et al 2009a,b;Sabatini et al 2010;Williams et al 2010;Tam et al 2010;Hill et al 2011;Falcone et al 2011;Corbet et al 2011).…”

Section: Introductionmentioning

confidence: 99%

Large-scale flow dynamics and radiation in pulsarγ-ray binaries

Bosch‐Ramon

Barkov

2011

A&A

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Context. Several gamma-ray binaries show extended X-ray emission that may be associated to interactions of an outflow with the medium. Some of these systems are, or may be, high-mass binaries harboring young nonaccreting pulsars, in which the stellar and the pulsar winds collide, generating a powerful outflow that should terminate at some point in the ambient medium. Aims. This work studies the evolution and termination, as well as the related radiation, of the shocked-wind flow generated in highmass binaries hosting powerful pulsars. Methods. A characterization, based on previous numerical work, is given for the stellar/pulsar wind interaction. Then, an analytical study of the further evolution of the shocked flow and its dynamical impact on the surrounding medium is carried out. Finally, the expected nonthermal emission from the flow termination shock, likely the dominant emitting region, is calculated. Results. The shocked wind structure, initially strongly asymmetric, becomes a quasi-spherical, supersonically expanding bubble, with its energy coming from the pulsar and mass from the stellar wind. This bubble eventually interacts with the environment on ∼pc scales, producing a reverse and, sometimes, a forward shock. Nonthermal leptonic radiation can be efficient in the reverse shock. Radio emission is expected to be faint, whereas X-rays can easily reach detectable fluxes. Under very low magnetic fields and large nonthermal luminosities, gamma rays may also be significant. Conclusions. The complexity of the stellar/pulsar wind interaction is likely to be smoothed out outside the binary system, where the wind-mixed flow accelerates and eventually terminates in a strong reverse shock. This shock may be behind the extended Xrays observed in some binary systems. For very powerful pulsars, part of the unshocked pulsar wind may directly interact with the large-scale environment.

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The bright unidentifiedγ-ray source 1FGL J1227.9−4852: can it be associated with a low-mass X-ray binary?

Cited by 71 publications

References 41 publications

Different twins in the millisecond pulsar recycling scenario: Optical polarimetry of PSR J1023+0038 and XSS J12270-4859

Different twins in the millisecond pulsar recycling scenario: Optical polarimetry of PSR J1023+0038 and XSS J12270-4859

The counterpart/s of IGR J20159+3713/SWIFT J2015.9+3715: dissecting a complex region with emission from keV to TeV

Large-scale flow dynamics and radiation in pulsarγ-ray binaries

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