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

Iacolina, M. N.; Burgay, M.; Burderi, L.; Possenti, A.; Salvo, T. Di

doi:10.1051/0004-6361/200810677

Cited by 16 publications

(17 citation statements)

References 31 publications

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“…We note that no radio pulsations were detected from XTE J0929−314 during quiescence. Beaming factor and intrinsic low radio luminosity were suggested as the most likely explanations for this non-detection (Iacolina et al 2009). XTE J1751−305 and XTE J1807−294 lie both on the Galactic plane and are therefore heavily absorbed (we estimated A V ∼ 5.2 mag and A V ∼ 2.4 mag, respectively).…”

Section: Discussionmentioning

confidence: 96%

The optical counterparts of accreting millisecond X-ray pulsars during quiescence

D’Avanzo

Campana²,

Casares

et al. 2009

A&A

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Context. Eight accreting millisecond X-ray pulsars (AMXPs) are known to date. Although these systems are well studied at high energies, very little information is available for their optical/NIR counterparts. Up to now, only two of them, SAX J1808.4−3658 and IGR J00291+5934, have a secure multi-band detection of their optical counterparts in quiescence. Aims. All these systems are transient low-mass X-ray binaries. Optical and NIR observations carried out during quiescence give a unique opportunity to constrain the nature of the donor star and to investigate the origin of the observed quiescent luminosity at long wavelengths. In addition, optical observations can be fundamental as they ultimately allow us to estimate the compact object mass through mass function measurements. Methods. Using data obtained with the ESO-Very Large Telescope, we performed a deep optical and NIR photometric study of the fields of XTE J1814−338 and of the ultracompact systems XTE J0929−314 and XTE J1807−294 during quiescence in order to look for the presence of a variable counterpart. If suitable candidates were found, we also carried out optical spectroscopy. Results. We present here the first multi-band (VR) detection of the optical counterpart of XTE J1814−338 in quiescence together with its optical spectrum. The optical light curve shows variability in both bands consistent with a sinusoidal modulation at the known 4.3 h orbital period and presents a puzzling decrease of the V-band flux around superior conjunction that may be interpreted as a partial eclipse. The marginal detection of the very faint counterpart of XTE J0929−314 and deep upper limits for the optical/NIR counterpart of XTE J1807−294 are also reported. We also briefly discuss the results reported in the literature for the optical/NIR counterpart of XTE J1751−305. Conclusions. Our findings are consistent with AMXPs being systems containing an old, weakly magnetized neutron star, reactivated as a millisecond radio pulsar during quiescence which irradiates the low-mass companion star. The absence of type I X-ray bursts and of hydrogen and helium lines in outburst spectra of ultracompact (P orb < 1 h) AMXPs suggests that the companion stars are likely evolved dwarf stars.

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Section: Discussionmentioning

confidence: 96%

The optical counterparts of accreting millisecond X-ray pulsars during quiescence

D’Avanzo

Campana²,

Casares

et al. 2009

A&A

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“…To check the plausibility of the adopted spin period interval, for XTE J1814−338, we derived the spin period derivative,Ṗ dip , through an estimate of the surface magnetic field, considering the magnetic torque acting on the neutron star, as discussed by Iacolina et al (2009). The value obtained isṖ dip = 6 × 10 −20 , which is lower thanṖ X and then safely contained in our interval of spin period trial values.…”

Section: Introductionmentioning

confidence: 94%

“…Results for XTE J0929−314 were presented in Iacolina et al (2009). Here we used the same equation to estimate τ ff for the other three sources, and we obtained the values listed in Table 1.…”

Section: Introductionmentioning

confidence: 99%

“…The data analysis methodology was chosen on the basis of the precise knowledge of the spin and orbital parameters from X-ray observation. It is the same as was adopted for the source XTE J0929−314 presented by Iacolina et al (2009), where it is described in detail. The original ephemerides were published by Markwardt et al (2002) for XTE J1751−305, by Markwardt & Swank (2003) for XTE J1814−338 and by Chakrabarty & Morgan (1998) for SAX J1808.4−3658, and subsequently refined by Papitto et al (2007Papitto et al ( , 2008 for XTE J1751−305 and XTE J1814−338, and by Hartman et al (2009) (but also by Burderi et al 2009;Di Salvo et al 2008;and Hartman et al 2008) for SAX J1808.4−3658.…”

Section: Introductionmentioning

confidence: 99%

“…The spin period range explored has to be chosen by considering the nominal value of the spin period at the epoch of the radio observations, as explained by Iacolina et al (2009).…”

Section: Introductionmentioning

confidence: 99%

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Search for pulsations at high radio frequencies from accreting millisecond X-ray pulsars in quiescence

Iacolina

Burgay

Burderi

et al. 2010

A&A

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Context. It is commonly believed that millisecond radio pulsars have been spun up by transfer of matter and angular momentum from a low-mass companion during an X-ray active mass transfer phase. A subclass of low-mass X-ray binaries is that of the accreting millisecond X-ray pulsars, transient systems that show periods of X-ray quiescence during which radio emission could switch on. Aims. The aim of this work is to search for millisecond pulsations from three accreting millisecond X-ray pulsars, XTE J1751−305, XTE J1814−338, and SAX J1808.4−3658, observed during their quiescent X-ray phases at high radio frequencies (5 ÷ 8 GHz) in order to overcome the problem of the free-free absorption due to the matter engulfing the system. A positive result would provide definite proof of the recycling model, providing the direct link between the progenitors and their evolutionary products. Methods. The data analysis methodology has been chosen on the basis of the precise knowledge of orbital and spin parameters from X-ray observations. It is subdivided in three steps: we corrected the time series for the effects of (I) the dispersion due to interstellar medium and (II) of the orbital motions, and finally (III) folded modulo the spin period to increase the signal-to-noise ratio. Results. No radio signal with spin and orbital characteristics matching those of the X-ray sources has been found in our search, down to very low flux density upper limits. Conclusions. We analysed several mechanisms that could have prevented the detection of the signal, concluding that the low luminosity of the sources and the geometric factor are the most likely reasons for this negative result.

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Accretion Powered X-ray Millisecond Pulsars

Salvo

Sanna

2021

Astrophysics and Space Science Library

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

Cited by 16 publications

References 31 publications

The optical counterparts of accreting millisecond X-ray pulsars during quiescence

The optical counterparts of accreting millisecond X-ray pulsars during quiescence

Search for pulsations at high radio frequencies from accreting millisecond X-ray pulsars in quiescence

Accretion Powered X-ray Millisecond Pulsars

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