<i>FERMI</i>
                    /LAT OBSERVATIONS OF LS 5039

Abdo, A. A.; Ackermann, M.; Ajello, M.; Atwood, W. B.; Axelsson, M.; Baldini, Luca; Ballet, J.; Barbiellini, G.; Bastieri, D.; Baughman, B. M.; Bechtol, K.; Bellazzini, R.; Berenji, B.; Blandford, R. D.; Bloom, E. D.; Bonamente, E.; Borgland, A. W.; Bregeon, J.; Brez, A.; Brigida, M.; Bruel, Pascal; Burnett, T. H.; Buson, S.; Caliandro, G. A.; Cameron, R. A.; Caraveo, P. A.; Casandjian, J. M.; Cavazzuti, E.; Cecchi, C.; Çelik, Ö.; Chaty, S.; Chekhtman, A.; Cheung, C. C.; Chiang, J.; Ciprini, S.; Claus, R.; Cohen-Tanugi, J.; Cominsky, L.; Conrad, J.; Corbel, S.; Corbet, R. H. D.; Cutini, S.; Dermer, C. D.; Angelis, A. De; Palma, F. de; Digel, S. W.; Silva, E. do Couto e; Drell, P. S.; Dubois, R.; Dubus, G.; Dumora, D.; Farnier, C.; Favuzzi, C.; Fegan, S. J.; Focke, W. B.; Fortin, P.; Frailis, M.; Fukazawa, Y.; Funk, S.; Fusco, P.; Gargano, F.; Gasparrini, D.; Gehrels, N.; Germani, S.; Giebels, B.; Giglietto, N.; Giordano, Fabrizio; Glanzman, T.; Godfrey, G.; Grenier, I. A.; Grondin, M.‐H.; Grove, J. E.; Guillemot, L.; Guiriec, S.; Hanabata, Y.; Harding, A. K.; Hayashida, M.; Hays, E.; Hill, A. B.; Horan, D.; Hughes, R. E.; Jackson, M. S.; Jóhannesson, G.; Johnson, A. S.; Johnson, T. J.; Johnson, W. N.; Kamae, T.; Katagiri, H.; Kataoka, J.; Kawai, N.; Kerr, M.; Knödlseder, J.; Kocian, M.; Kuehn, F.; Kuss, M.; Landé, J.; Larsson, Stefan; Latronico, L.; Lemoine‐Goumard, M.; Longo, F.; Loparco, F.; Lott, B.; Lovellette, M. N.; Lubrano, P.; Madejski, G. M.; Makeev, A.; Marelli, M.; Mazziotta, M. N.; McEnery, J. E.; Meurer, C.; Michelson, P. F.; Mitthumsiri, W.; Mizuno, T.; Моисеев, А. А.; Monte, C.; Monzani, M. E.; Morselli, A.; Moskalenko, I. V.; Murgia, S.; Nolan, P. L.; Norris, J. P.; Nuss, E.; Ohsugi, T.; Omodei, N.; Orlando, E.; Ormes, J. F.; Ozaki, Masanori; Paneque, D.; Panetta, J.; Parent, D.; Pelassa, V.; Pepé, M.; Pesce-Rollins, M.; Piron, F.; Porter, T. A.; Rainò, S.; Rando, R.; Ray, Paul S.; Razzano, M.; Rea, N.; Reimer, A.; Reimer, O.; Reposeur, T.; Ritz, S.; Rochester, Lynn; Rodriguez, A. Y.; Romani, Roger W.; Roth, M.; Ryde, F.; Sadrozinski, H. F-W.; Sánchez, David; Sander, A.; Parkinson, P. M. Saz; Scargle, Jeffrey D.; Sgrò, C.; Sierpowska-Bartosik, A.; Siskind, E. J.; Smith, David A.; Smith, P. D.; Spandre, G.; Spinelli, P.; Strickman, M. S.; Suson, D. J.; Tajima, H.; Takahashi, H.; Takahashi, Tadayuki; Tanaka, T.; Tanaka, Yasuyuki; Thayer, J. B.; Thompson, D. J.; Tibaldo, L.; Torres, D. F.; Tosti, G.; Tramacere, A.; Uchiyama, Y.; Usher, T.; Vasileiou, V.; Venter, C.; Vilchez, N.; Vitale, V.; Waite, A. P.; Wallace, E.; Wang, P.; Winer, B. L.; Wood, K. S.; Ylinen, T.; Ziegler, M.

doi:10.1088/0004-637x/706/1/l56

Cited by 300 publications

(455 citation statements)

References 36 publications

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“…The orbital period obtained by C05 is shorter than that obtained by M04. It is however consistent with the modulations observed in the X-rays (Bosch-Ramon et al 2005;Takahashi et al 2009) and γ -rays at GeV (Abdo et al 2009) and TeV (Aharonian et al 2006) energies. Aragona et al (2009) (hereafter A09) revisited radial velocity (RV) measurements from optical spectra, confirming the 3.9-d orbital period.…”

supporting

confidence: 88%

“…Observationally, Ribó et al (2008) found that changes in the mas morphology of the radio images were difficult to reconcile with the micro-quasar (black hole binary) scenario in which the radio emission originates from expanding plasmons. The situation is further complicated by the fact that the temporal and spectral behaviour of the X-ray emission (Bosch-Ramon et al 2007;Kishishita et al 2009;Takahashi et al 2009;Bosch-Ramon 2010) and properties of the TeV emission (Bosch-Ramon, Abdo et al 2009) indicate that the high-energy radiation might originate from regions far outside the binary orbit of LS 5039.…”

mentioning

confidence: 99%

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

Sarty

Szalai

Kiss

et al. 2010

Monthly Notices of the Royal Astronomical Society

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The results of a coordinated space‐based photometric and ground‐based spectroscopic observing campaign on the enigmatic γ‐ray binary LS 5039 are reported. 16 d of observations from the MOST satellite have been combined with high‐resolution optical echelle spectroscopy from the 2.3‐m ANU Telescope in Siding Spring, Australia. These observat ions were used to measure the orbital parameters of the binary and to study the properties of stellar wind from the O primary. We found that any broad‐band optical photometric variability at the orbital period is below the 2 mmag level, supporting the scenario that the orbital eccentricity of the system is near the 0.24 ± 0.08 value implied by our spectroscopy, which is lower than values previously obtained by other workers. The low amplitude optical variability also implies the component masses are at the higher end of estimates based on the primary's O6.5V((f)) spectral type with a primary mass of ∼26 M⊙ and a mass for the compact star of at least 1.8 M⊙. The mass‐loss rate from the O primary was determined to be 3.7 to 4.8 × 10−7 M⊙ yr−1.

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supporting

confidence: 88%

mentioning

confidence: 99%

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

Sarty

Szalai

Kiss

et al. 2010

Monthly Notices of the Royal Astronomical Society

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“…To date, three high-mass X-ray binaries (HMXBs) have been detected by Fermi-LAT: LS I +61 • 303 (Abdo et al 2009b), LS 5039 (Abdo et al 2009c) and Cyg X-3 (Abdo et al 2009f). All of these systems contain >10 M donor stars.…”

Section: Introductionmentioning

confidence: 99%

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

Hill¹,

Szostek

Corbel

et al. 2011

Monthly Notices of the Royal Astronomical Society

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We present an analysis of high energy (HE; 0.1–300 GeV) γ‐ray observations of 1FGL J1227.9−4852 with the Fermi Gamma‐ray Space Telescope, follow‐up radio observations with the Australia Telescope Compact Array, Giant Metrewave Radio Telescope and Parkes radio telescopes of the same field and follow‐up optical observations with the ESO VLT. We also examine archival XMM–Newton and INTEGRAL X‐ray observations of the region around this source. The γ‐ray spectrum of 1FGL J1227.9−4852 is best fitted with an exponentially cut‐off power law, reminiscent of the population of pulsars observed by Fermi. A previously unknown, compact radio source within the 99.7 per cent error circle of 1FGL J1227.9−4852 is discovered and has a morphology consistent either with an AGN core/jet structure or with two roughly symmetric lobes of a distant radio galaxy. A single bright X‐ray source XSS J12270−4859, a low‐mass X‐ray binary, also lies within the 1FGL J1227.9−4852 error circle and we report the first detection of radio emission from this source. The potential association of 1FGL J1227.9−4852 with each of these counterparts is discussed. Based upon the available data we find the association of the γ‐ray source to the compact double radio source unlikely and suggest that XSS J12270−4859 is a more likely counterpart to the new HE source. We propose that XSS J12270−4859 may be a millisecond binary pulsar and draw comparisons with PSR J1023+0038.

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“…They are likely to be generated by a hadronic process, i.e. inelastic collisions between CR protons accelerated in SNRs and ambient protons (Abdo et al 2009(Abdo et al , 2010aGiuliani et al 2010;Tavani et al 2010). TeV γray emissions have also been discovered from some of these clouds (Aharonian et al 2008).…”

Section: Introductionmentioning

confidence: 99%

Alfvén wave amplification and self-containment of cosmic rays escaping from a supernova remnant

Fujita

Takahara

Ohira³

et al. 2011

Monthly Notices of the Royal Astronomical Society

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We study the escape of cosmic ray (CR) protons accelerated in a supernova remnant (SNR) by numerically solving a diffusion–convection equation for regions from the vicinity of the shock front to those far away from the front. We consider the amplifications of Alfvén waves generated by the escaping CR particles and their effects on CR escape into the interstellar medium (ISM). We find that the amplification of the waves significantly delays the escape of the particles even in regions far away from the shock front (on the scale of an SNR). This means that the energy spectrum of CR particles determined through γ‐ray observations of molecular clouds around SNRs is seriously affected by the particle scattering by the waves.

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FERMI /LAT OBSERVATIONS OF LS 5039

Cited by 300 publications

References 36 publications

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

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

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

Alfvén wave amplification and self-containment of cosmic rays escaping from a supernova remnant

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