The X‐Ray Position and Optical Counterpart of the Accretion‐powered Millisecond Pulsar XTE J1814−338

Krauss, M. I.; Wang, Zhongxiang; Dullighan, A.; Juett, Adrienne M.; Kaplan, David L.; Chakrabarty, Deepto; Kerkwijk, M. H. van; Steeghs, D.; Jonker, P. G.; Markwardt, C.

doi:10.1086/430595

Cited by 42 publications

(74 citation statements)

References 31 publications

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“…3 (0.3 error). This position is coincident with the one of the optical counterpart of XTE J1814−338 detected by Krauss et al (2005) during the 2003 outburst. The object has V ∼ 23.3 and R ∼ 22.5.…”

Section: Optical Counterpart During Quiescencesupporting

confidence: 74%

“…Based on the harmonic properties of the burst oscillations, Bhattacharyya et al (2005) were able to derive 90% confidence intervals of 26 • < i < 50 • for the inclination of XTE J1814−338. A similar constraint was derived by Krauss et al (2005) from the absence of X-ray eclipses or dips and assuming an absolute magnitude of the system during quiescence of M V < 13.2. With these constraints on the system inclination the companion mass should be in the range (0.2 ≤ M 2 ≤ 0.5) M .…”

Section: Origin Of the Quiescent Optical Emissionmentioning

confidence: 56%

“…An R ∼ 18.3 candidate optical counterpart was identified within the small Chandra error box during the outburst and was no longer visible during quiescence down to a limiting magnitude R > 23.3 (3σ c.l. ; Krauss et al 2005). Optical spectroscopy of the candidate carried out during the outburst revealed prominent hydrogen and helium emission lines, supporting its association with XTE J1814−338 (Steeghs 2003).…”

Section: Observations and Data Reductionmentioning

confidence: 62%

“…Assuming the Eddington limit for the brightest of those bursts Strohmayer et al (2003) obtained a source distance of 8.0 ± 1.6 kpc. X-ray observations carried out with the Chandra satellite during outburst led to a precise source position and showed a featureless X-ray spectrum which is best fit by an absorbed power law plus blackbody model, where the equivalent hydrogen column density (N H ) is comparable to the Galactic value (Krauss et al 2005). An R ∼ 18.3 candidate optical counterpart was identified within the small Chandra error box during the outburst and was no longer visible during quiescence down to a limiting magnitude R > 23.3 (3σ c.l.…”

Section: Observations and Data Reductionmentioning

confidence: 99%

“…Optical and NIR observations performed in the past by different groups only led to deep upper limits for the counterparts of XTE J1751−305 (Jonker et al 2003) and XTE J1814−338 (Krauss et al 2005) or to the detection of very faint candidates, if any (Monelli et al 2005 for XTE J0929−314). No observations of XTE J1807−294 during quiescence have been reported to date, while HETE J1900.1-2455 is still in outburst and SWIFT J1756.9-2508 has been discovered very recently (June 2007).…”

Section: Introductionmentioning

confidence: 99%

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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: Optical Counterpart During Quiescencesupporting

confidence: 74%

Section: Origin Of the Quiescent Optical Emissionmentioning

confidence: 56%

Section: Observations and Data Reductionmentioning

confidence: 62%

Section: Observations and Data Reductionmentioning

confidence: 99%

Section: Introductionmentioning

confidence: 99%

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