EDP Sciences
Free Access
Volume 497, Number 2, April II 2009
Page(s) 445 - 450
Section Stellar structure and evolution
DOI https://doi.org/10.1051/0004-6361/200810677
Published online 24 February 2009
A&A 497, 445-450 (2009)
DOI: 10.1051/0004-6361/200810677

Searching for pulsed emission from XTE J0929–314 at high radio frequencies

M. N. Iacolina1, M. Burgay2, L. Burderi1, A. Possenti2, and T. Di Salvo3

1  Università di Cagliari, Dipartimento di Fisica, SP Monserrato-Sestu km 0.7, 09042 Monserrato (CA), Italy
    e-mail: iacolina@ca.astro.it
2  INAF-Osservatorio Astronomico di Cagliari, Loc. Poggio dei Pini, Strada 54, 09012 Capoterra (CA), Italy
3  Università di Palermo, Dipartimento di Scienze Fisiche ed Astronomiche, via Archirafi 36, 90123 Palermo, Italy

Received 25 July 2008 / Accepted 15 January 2009

Aims. The aim of this work is to search for radio signals in the quiescent phase of accreting millisecond X-ray pulsars, in this way giving an ultimate proof of the recycling model, thereby unambiguously establishing that accreting millisecond X-ray pulsars are the progenitors of radio millisecond pulsars.
Methods. To overcome the possible free-free absorption caused by matter surrounding accreting millisecond X-ray pulsars in their quiescence phase, we performed the observations at high frequencies. Making use of particularly precise orbital and spin parameters obtained from X-ray observations, we carried out a deep search for radio-pulsed emission from the accreting millisecond X-ray pulsar XTE J0929–314 in three steps, correcting for the effect of the dispersion due to the interstellar medium, eliminating the orbital motions effects, and finally folding the time series.
Results. No radio pulsation is present in the analyzed data down to a limit of 68 $\mu$Jy at 6.4 GHz and 26 $\mu$Jy at 8.5 GHz.
Conclusions. We discuss several mechanisms that could prevent the detection, concluding that beaming factor and intrinsic low luminosity are the most likely explanations.

Key words: pulsars: general -- methods: data analysis -- methods: observational -- X-rays: binaries -- stars: neutron

© ESO 2009

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