The γ-ray binary LS 5039: mass and orbit constraints from MOST observations★

Sarty, Gordon E.; Szalai, T.; Kiss, L. L.; Matthews, J. M.; Wu, Kinwah; Kuschnig, R.; Guenther, D. B.; Moffat, A. F. J.; Ruciński, S. M.; Sasselov, Dimitar; Weiß, W. W.; Huziak, Richard; Johnston, Helen M.; Phillips, A.; Ashley, M. C. B.

doi:10.1111/j.1365-2966.2010.17757.x

Cited by 55 publications

(79 citation statements)

References 54 publications

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“…This does not strongly constrain the system parameters as the expected tidal distortion of the O star due to a 1.4M ⊙ companion would be small. We note that for the gamma-ray binary LS 5039 which has a 3.9 day period any photometric variability is below 2 millimagnitudes (Sarty et al 2011). Thus the lack of detection of photometric variability for CXOU J053600.0-673507, which has a longer period and a giant rather than main-sequence primary, is not surprising.…”

Section: Ogle Photometric Resultsmentioning

confidence: 95%

A Luminous Gamma-Ray Binary in the Large Magellanic Cloud

Corbet

Chomiuk

Coe

et al. 2016

ApJ

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Gamma-ray binaries consist of a neutron star or a black hole interacting with a normal star to produce gamma-ray emission that dominates the radiative output of the system. Only a handful of such systems have been previously discovered, all within our Galaxy. Here we report the discovery with the Fermi Large Area Telescope (LAT) of a luminous gamma-ray binary in the Large Magellanic Cloud from a search for periodic modulation in all sources in the third Fermi LAT catalog. This is the first such system to be found outside the Milky Way. The system has an orbital period of 10.3 days and is associated with a massive O5III star located in the supernova remnant DEM L241, previously identified as the candidate high-mass X-ray binary (HMXB) CXOU J053600.0-673507. X-ray and radio emission are also modulated on the 10.3 day period, but are in anti-phase with the gamma-ray modulation. Optical radial velocity measurements suggest that the system contains a neutron star. The source is significantly more luminous than similar sources in the Milky Way at radio, optical, X-ray and gamma-ray wavelengths. The detection of this extra-galactic system, but no new Galactic systems raises the possibility that the predicted number of gamma-ray binaries in our Galaxy have been overestimated, and that HMXBs may be born containing relatively slowly rotating neutron stars.

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Section: Ogle Photometric Resultsmentioning

confidence: 95%

A Luminous Gamma-Ray Binary in the Large Magellanic Cloud

Corbet

Chomiuk

Coe

et al. 2016

ApJ

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“…The Cn nature is still unclear; its mass is estimated to be M = 3.7 M , but this value is highly dependent on the poorly known inclination of the orbit (for discussions on the nature of the Cn, see Casares et al 2005;and Bosch-Ramon & Khangulyan 2009;Dubus 2013 and references therein) 1 . The orbit of LS 5039 is mildly eccentric, e = 0.24−0.35 (Casares et al 2005;Aragona et al 2009;Sarty et al 2011), with a semi-major axis a ≈ 3.5 R * . We adopt the value of a as the binary spatial scale here.…”

Section: An Application To Ls 5039mentioning

confidence: 99%

Gamma-ray binaries beyond one-zone models: an application to LS 5039

Palacio

Bosch‐Ramon

Romero

2015

A&A

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Context. Several binary systems hosting massive stars present gamma-ray emission. In most of these systems, despite detailed observational information being available, the nature and the structure of the emitter are still poorly known. Aims. We investigate the validity of the so-called one-zone approximation for the high-energy emitter in binary systems hosting a massive star. In particular, the case of LS 5039 is considered. Methods. Assuming a point-like emitter at rest, the presence of a nearby massive star, and the observed MeV and GeV fluxes as a reference, a non-thermal leptonic model is systematically applied for different locations, magnetic fields, and non-radiative losses. This allows us to identify both the emitter configurations that are most compatible with observations and inconsistencies between model predictions and the available data. Results. In the case of LS 5039, the best parameter combination is fast non-radiative cooling and a low magnetic field. However, discrepancies appear when comparing the model results at the MeV and GeV energy ranges with the observed fluxes. Predictions fail when the orbital motion is included in the analysis, because emitters and energy budgets that are too large are required. Values of X-ray and TeV fluxes that are too high are predicted in such a case, along half of the orbit. Conclusions. We show that the radiation in LS 5039 does not come from only one electron population, and the emitter is likely extended and inhomogeneous with a low magnetic field. We suggest that the emitter moves at relativistic velocities with Doppler boosting playing a significant role.

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“…This degenerate companion has a mass greater than ∼1.5 M , which depends on the binary system inclination, which is an unknown parameter (Casares et al 2005). The orbit of the system has a period of 3.9 days and an eccentricity around 0.35 (Casares et al 2005;Aragona et al 2009;Sarty et al 2011). The distance to the source has recently been updated to 2.9 ± 0.8 kpc (Casares et al, in prep.).…”

Section: The Gamma-ray Binary Ls 5039mentioning

confidence: 99%

“…The orbital parameters of LS 5039 such as the eccentricity, masses, and orbit inclination are not well constrained or are still under discussion (Casares et al 2005;Aragona et al 2009;Sarty et al 2011). The proper motion and the space velocity of the source were first determined in Ribó et al (2002).…”

Section: The Gamma-ray Binary Ls 5039mentioning

confidence: 99%

On the origin of LS 5039 and PSR J1825−1446

Moldón

Ribó

Paredes

et al. 2012

A&A

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Context. The gamma-ray binary LS 5039 and the isolated pulsar PSR J1825−1446 were proposed to have been formed in the supernova remnant (SNR) G016.8−01.1. Aims. We aim to obtain the Galactic trajectory of LS 5039 and PSR J1825−1446 to find their origin in the Galaxy, and in particular to check their association with SNR G016.8−01.1 to restrict their age. Methods. By means of radio and optical observations we obtained the proper motion and the space velocity of the sources. Results. The proper motion of PSR J1825−1446 corresponds to a transverse space velocity of 690 km s −1 at a distance of 5 kpc. Its Galactic velocity at different distances is not compatible with the expected Galactic rotation. The velocity and characteristic age of PSR J1825−1446 make it incompatible with SNR G016.8−01.1. There are no clear OB associations or SNRs crossing the past trajectory of PSR J1825−1446. We estimate the age of the pulsar to be 80-245 kyr, which is compatible with its characteristic age. The proper motion of LS 5039 is μ α cos δ = 7.09 and μ δ = −8.82 mas yr −1 . The association of LS 5039 with SNR G016.8−01.1 is unlikely, although we cannot discard it. The system would have had to be formed in the association Ser OB2 (at 2.0 kpc) if the age of the system is 1.0-1.2 Myr, or in the association Sct OB3 (distance 1.5-2 kpc) for an age of 0.1-0.2 Myr. If the system were not formed close to Ser OB2, the pseudo-synchronization of the orbit would be unlikely. Conclusions. PSR J1825−1446 is a high-velocity isolated pulsar ejected from the Galaxy. The distance to LS 5039, which needs to be constrained by future astrometric missions such as Gaia, is a key parameter for restricting its origin and age.

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The γ-ray binary LS 5039: mass and orbit constraints from MOST observations★

Cited by 55 publications

References 54 publications

A Luminous Gamma-Ray Binary in the Large Magellanic Cloud

A Luminous Gamma-Ray Binary in the Large Magellanic Cloud

Gamma-ray binaries beyond one-zone models: an application to LS 5039

On the origin of LS 5039 and PSR J1825−1446

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