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  Search for radio pulsations in LS I +61 303

Cañellas, A., Joshi, B. C., Paredes, J. M., Ishwara-Chandra, C. H., Moldón, J., Zabalza, V., et al. (2012). Search for radio pulsations in LS I +61 303. Astronomy and Astrophysics, 543: A122. doi:10.1051/0004-6361/201117619.

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1206.0543.pdf (Publisher version), 228KB
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http://dx.doi.org/10.1051/0004-6361/201117619 (Publisher version)
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 Creators:
Cañellas, A., Author
Joshi, B. C., Author
Paredes, J. M., Author
Ishwara-Chandra, C. H., Author
Moldón, J., Author
Zabalza, Victor1, 2, Author           
Martí, J., Author
Ribó, M., Author
Affiliations:
1Division Prof. Dr. Werner Hofmann, MPI for Nuclear Physics, Max Planck Society, ou_904550              
2Departament d’Astronomia i MeteorologiaInstitut de Ciències del Cosmos (ICC), Universitat de Barcelona (IEEC-UB), Martí i Franquès 1, 08028 Barcelona Spain , ou_persistent22              

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Free keywords: Astrophysics, High Energy Astrophysical Phenomena, astro-ph.HE
 Abstract: Context. LS I +61 303 is a member of the select group of gamma-ray binaries: galactic binary systems that contain a massive star and a compact object, show a changing milliarcsecond morphology and a similar broad spectral energy distribution (SED) that peaks at MeV-TeV energies and is modulated by the orbital motion. The nature of the compact object is unclear in LS I +61 303, LS 5039 and HESS J0632+057, whereas PSR B1259-63 harbours a 47.74 ms radio pulsar. Aims. A scenario in which a young pulsar wind interacts with the stellar wind has been proposed to explain the very high energy (VHE, E > 100 GeV) gamma-ray emission detected from LS I +61 303, although no pulses have been reported from this system at any wavelength. We aim to find evidence of the pulsar nature of the compact object. Methods. We performed phased array observations with the Giant Metrewave Radio Telescope (GMRT) at 1280 MHz centred at phase 0.54. Simultaneous data from the multi-bit phased array (PA) back-end with a sampling time of tsamp = 128 microsec and from the polarimeter (PMT) back-end with tsamp = 256 microsec where taken. Results. No pulses have been found in the data set, with a minimum detectable mean flux density of \sim 0.38 mJy at 8-sigma level for the pulsed emission from a putative pulsar with period P >2 ms and duty cycle D = 10% in the direction of LS I +61 303. Conclusions. The detection of posible radio pulsations will require deep and sensitive observations at frequencies \sim0.5-5 GHz and orbital phases 0.6-0.7. However, it may be unfeasible to detect pulses if the putative pulsar is not beamed at the Earth or if there is a strong absorption within the binary system.

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 Dates: 2012-07-09
 Publication Status: Published online
 Pages: 8 pages. 5 figures. Accepted for publication in Astronomy and Astrophysics
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 Table of Contents: -
 Rev. Type: -
 Identifiers: arXiv: 1206.0543
DOI: 10.1051/0004-6361/201117619
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Title: Astronomy and Astrophysics
  Other : Astron. Astrophys.
Source Genre: Journal
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Publ. Info: Berlin : Springer-Verlag
Pages: 8 Volume / Issue: 543 Sequence Number: A122 Start / End Page: - Identifier: ISSN: 0004-6361
CoNE: https://pure.mpg.de/cone/journals/resource/954922828219_1