Discovery of the millisecond pulsar PSR J2043+1711 in a Fermi source   with the Nancay Radio Telescope
  We report the discovery of the millisecond pulsar PSR J2043+1711 in a search of a Fermi Large Area Telescope (LAT) source with no known associations, with the Nancay Radio Telescope. The new pulsar, confirmed with the Green Bank Telescope, has a spin period of 2.38 ms, is relatively nearby (d <~ 2 kpc), and is in a 1.48 day orbit around a low mass companion, probably a He-type white dwarf. Pulsed gamma-ray emission was detected in the data recorded by the Fermi LAT. The gamma-ray light curve and spectral properties are typical of other gamma-ray millisecond pulsars seen with Fermi. X-ray observations of the pulsar with Suzaku and the Swift/XRT yielded no detection. At 1.4 GHz we observe strong flux density variations because of interstellar diffractive scintillation, however a sharp peak can be observed at this frequency during bright scintillation states. At 327 MHz the pulsar is detected with a much higher signal-to-noise ratio and its flux density is far more steady. However, at that frequency the Arecibo instrumentation cannot yet fully resolve the pulse profile. Despite that, our pulse time-of-arrival measurements have a post-fit residual rms of 2 \mus. This and the expected stability of this system has made PSR J2043+1711 one of the first new Fermi-selected millisecond pulsars to be added to pulsar gravitational wave timing arrays. It has also allowed a significant measurement of relativistic delays in the times of arrival of the pulses due to the curvature of space-time near the companion, but not yet with enough precision to derive useful masses for the pulsar and the companion. A mass for the pulsar between 1.7 and 2.0 solar masses can be derived if a standard millisecond pulsar formation model is assumed. In this article we also present a comprehensive summary of pulsar searches in Fermi LAT sources with the Nancay Radio Telescope to date. 
L. Guillemot, P. C. C. Freire, I. Cognard, T. J. Johnson, Y.   Takahashi, J. Kataoka, G. Desvignes, F. Camilo, E. C. Ferrara...
astro-ph.HE astro-ph.GA