Discovery of the millisecond pulsar PSR J2043+1711 in a Fermi source with the Nançay Radio Telescope

L. Guillemot, P. C C Freire, I. Cognard, T. J. Johnson, Y. Takahashi, Jun Kataoka, G. Desvignes, F. Camilo, E. C. Ferrara, A. K. Harding, G. H. Janssen, M. Keith, M. Kerr, M. Kramer, D. Parent, S. M. Ransom, P. S. Ray, P. M. Saz Parkinson, D. A. Smith, B. W. StappersG. Theureau

    Research output: Contribution to journalArticle

    34 Citations (Scopus)

    Abstract

    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 Nançay Radio Telescope. The new pulsar, confirmed with the Green Bank Telescope, has a spin period of 2.38ms, is relatively nearby (kpc) and is in a 1.48-d orbit around a low-mass companion, probably an He-type white dwarf. Using an ephemeris based on Arecibo, Nançay and Westerbork timing measurements, 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 X-ray Telescope yielded no detection. At 1.4GHz, 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 327MHz, 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 2s. This and the expected stability of this system have 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. Nevertheless, a mass for the pulsar between 1.7 and 2.0M can be derived if a standard millisecond pulsar formation model is assumed. In this paper, we also present a comprehensive summary of pulsar searches in Fermi LAT sources with the Nançay Radio Telescope to date.

    Original languageEnglish
    Pages (from-to)1294-1305
    Number of pages12
    JournalMonthly Notices of the Royal Astronomical Society
    Volume422
    Issue number2
    DOIs
    Publication statusPublished - 2012 May

    Fingerprint

    radio telescopes
    pulsars
    radio
    telescopes
    signal-to-noise ratio
    curvature
    instrumentation
    gamma rays
    scintillation
    arrivals
    flux density
    pulses
    time measurement
    gravitational waves
    light curve
    signal to noise ratios
    x rays
    orbits

    Keywords

    • Gamma-rays: general
    • Pulsars: general
    • Pulsars: individual: PSR J2043+1711

    ASJC Scopus subject areas

    • Space and Planetary Science
    • Astronomy and Astrophysics

    Cite this

    Discovery of the millisecond pulsar PSR J2043+1711 in a Fermi source with the Nançay Radio Telescope. / Guillemot, L.; Freire, P. C C; Cognard, I.; Johnson, T. J.; Takahashi, Y.; Kataoka, Jun; Desvignes, G.; Camilo, F.; Ferrara, E. C.; Harding, A. K.; Janssen, G. H.; Keith, M.; Kerr, M.; Kramer, M.; Parent, D.; Ransom, S. M.; Ray, P. S.; Saz Parkinson, P. M.; Smith, D. A.; Stappers, B. W.; Theureau, G.

    In: Monthly Notices of the Royal Astronomical Society, Vol. 422, No. 2, 05.2012, p. 1294-1305.

    Research output: Contribution to journalArticle

    Guillemot, L, Freire, PCC, Cognard, I, Johnson, TJ, Takahashi, Y, Kataoka, J, Desvignes, G, Camilo, F, Ferrara, EC, Harding, AK, Janssen, GH, Keith, M, Kerr, M, Kramer, M, Parent, D, Ransom, SM, Ray, PS, Saz Parkinson, PM, Smith, DA, Stappers, BW & Theureau, G 2012, 'Discovery of the millisecond pulsar PSR J2043+1711 in a Fermi source with the Nançay Radio Telescope', Monthly Notices of the Royal Astronomical Society, vol. 422, no. 2, pp. 1294-1305. https://doi.org/10.1111/j.1365-2966.2012.20694.x
    Guillemot, L. ; Freire, P. C C ; Cognard, I. ; Johnson, T. J. ; Takahashi, Y. ; Kataoka, Jun ; Desvignes, G. ; Camilo, F. ; Ferrara, E. C. ; Harding, A. K. ; Janssen, G. H. ; Keith, M. ; Kerr, M. ; Kramer, M. ; Parent, D. ; Ransom, S. M. ; Ray, P. S. ; Saz Parkinson, P. M. ; Smith, D. A. ; Stappers, B. W. ; Theureau, G. / Discovery of the millisecond pulsar PSR J2043+1711 in a Fermi source with the Nançay Radio Telescope. In: Monthly Notices of the Royal Astronomical Society. 2012 ; Vol. 422, No. 2. pp. 1294-1305.
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    AU - Freire, P. C C

    AU - Cognard, I.

    AU - Johnson, T. J.

    AU - Takahashi, Y.

    AU - Kataoka, Jun

    AU - Desvignes, G.

    AU - Camilo, F.

    AU - Ferrara, E. C.

    AU - Harding, A. K.

    AU - Janssen, G. H.

    AU - Keith, M.

    AU - Kerr, M.

    AU - Kramer, M.

    AU - Parent, D.

    AU - Ransom, S. M.

    AU - Ray, P. S.

    AU - Saz Parkinson, P. M.

    AU - Smith, D. A.

    AU - Stappers, B. W.

    AU - Theureau, G.

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    N2 - 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 Nançay Radio Telescope. The new pulsar, confirmed with the Green Bank Telescope, has a spin period of 2.38ms, is relatively nearby (kpc) and is in a 1.48-d orbit around a low-mass companion, probably an He-type white dwarf. Using an ephemeris based on Arecibo, Nançay and Westerbork timing measurements, 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 X-ray Telescope yielded no detection. At 1.4GHz, 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 327MHz, 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 2s. This and the expected stability of this system have 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. Nevertheless, a mass for the pulsar between 1.7 and 2.0M ⊙ can be derived if a standard millisecond pulsar formation model is assumed. In this paper, we also present a comprehensive summary of pulsar searches in Fermi LAT sources with the Nançay Radio Telescope to date.

    AB - 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 Nançay Radio Telescope. The new pulsar, confirmed with the Green Bank Telescope, has a spin period of 2.38ms, is relatively nearby (kpc) and is in a 1.48-d orbit around a low-mass companion, probably an He-type white dwarf. Using an ephemeris based on Arecibo, Nançay and Westerbork timing measurements, 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 X-ray Telescope yielded no detection. At 1.4GHz, 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 327MHz, 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 2s. This and the expected stability of this system have 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. Nevertheless, a mass for the pulsar between 1.7 and 2.0M ⊙ can be derived if a standard millisecond pulsar formation model is assumed. In this paper, we also present a comprehensive summary of pulsar searches in Fermi LAT sources with the Nançay Radio Telescope to date.

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