Radio detection of lat psrs j1741-2054 and j2032+4127

No longer just gamma-ray pulsars

F. Camilo, P. S. Ray, S. M. Ransom, M. Burgay, T. J. Johnson, M. Kerr, E. V. Gotthelf, J. P. Halpern, J. Reynolds, R. W. Romani, P. Demorest, S. Johnston, W. Van Straten, P. M.Saz Parkinson, M. Ziegler, M. Dormody, D. J. Thompson, D. A. Smith, A. K. Harding, A. A. Abdo & 7 others F. Crawford, P. C.C. Freire, M. Keith, M. Kramer, Mallory Roberts, P. Weltevrede, K. S. Wood

    Research output: Contribution to journalArticle

    Abstract

    Sixteen pulsars have been discovered so far in blind searches of photons collected with the Large Area Telescope on the Fermi Gamma-ray Space Telescope. We here report the discovery of radio pulsations from two of them. PSR J1741-2054, with period P = 413 ms, was detected in archival Parkes telescope data and subsequently has been detected at the Green Bank Telescope (GBT). Its received flux varies greatly due to interstellar scintillation and it has a very small dispersion measure of DM = 4.7 pc cm-3, implying a distance of 0.4 kpc and possibly the smallest luminosity of any known radio pulsar. At this distance, for isotropic emission, its gamma-ray luminosity above 0.1 GeV corresponds to 28% of the spin-down luminosity of erg s-1. The gamma-ray profile occupies 1/3 of pulse phase and has three closely spaced peaks with the first peak lagging the radio pulse by δ = 0.29 P. We have also identified a soft Swift source that is the likely X-ray counterpart. In many respects PSRJ1741-2054 resembles the Geminga pulsar. The second source, PSR J2032+4127, was detected at the GBT. It has P = 143 ms, and its DM = 115 pc cm-3 suggests a distance of 3.6 kpc, but we consider it likely that it is located within the Cyg OB2 stellar association at half that distance. The radio emission is nearly 100% linearly polarized, and the main radio peak precedes by δ = 0.15 P the first of two narrow gamma-ray peaks that are separated by Δ = 0.50 P. The second peak has a harder spectrum than the first one, following a trend observed in young gamma-ray pulsars. Faint, diffuse X-ray emission in a Chandra image is possibly its pulsar wind nebula. The wind of PSR J2032+4127 is responsible for the formerly unidentified HEGRA source TeV J2032+4130. PSR J2032+4127 is coincident in projection with MT91 213, a Be star in Cyg OB2, although apparently not a binary companion of it.

    Original languageEnglish (US)
    Pages (from-to)1-13
    Number of pages13
    JournalAstrophysical Journal
    Volume705
    Issue number1
    DOIs
    StatePublished - Jan 1 2009

    Fingerprint

    pulsars
    gamma rays
    radio
    telescopes
    luminosity
    Fermi Gamma-ray Space Telescope
    radio emission
    nebulae
    pulses
    erg
    scintillation
    x rays
    projection
    detection
    trends
    stars
    photons
    profiles

    Keywords

    • Gamma rays: observations
    • Open clusters and associations:individual (Cyg OB2)
    • X-rays: individual (Swift J174157.6-205411)

    ASJC Scopus subject areas

    • Astronomy and Astrophysics
    • Space and Planetary Science

    Cite this

    Camilo, F., Ray, P. S., Ransom, S. M., Burgay, M., Johnson, T. J., Kerr, M., ... Wood, K. S. (2009). Radio detection of lat psrs j1741-2054 and j2032+4127: No longer just gamma-ray pulsars. Astrophysical Journal, 705(1), 1-13. https://doi.org/10.1088/0004-637X/705/1/1

    Radio detection of lat psrs j1741-2054 and j2032+4127 : No longer just gamma-ray pulsars. / Camilo, F.; Ray, P. S.; Ransom, S. M.; Burgay, M.; Johnson, T. J.; Kerr, M.; Gotthelf, E. V.; Halpern, J. P.; Reynolds, J.; Romani, R. W.; Demorest, P.; Johnston, S.; Van Straten, W.; Parkinson, P. M.Saz; Ziegler, M.; Dormody, M.; Thompson, D. J.; Smith, D. A.; Harding, A. K.; Abdo, A. A.; Crawford, F.; Freire, P. C.C.; Keith, M.; Kramer, M.; Roberts, Mallory; Weltevrede, P.; Wood, K. S.

    In: Astrophysical Journal, Vol. 705, No. 1, 01.01.2009, p. 1-13.

    Research output: Contribution to journalArticle

    Camilo, F, Ray, PS, Ransom, SM, Burgay, M, Johnson, TJ, Kerr, M, Gotthelf, EV, Halpern, JP, Reynolds, J, Romani, RW, Demorest, P, Johnston, S, Van Straten, W, Parkinson, PMS, Ziegler, M, Dormody, M, Thompson, DJ, Smith, DA, Harding, AK, Abdo, AA, Crawford, F, Freire, PCC, Keith, M, Kramer, M, Roberts, M, Weltevrede, P & Wood, KS 2009, 'Radio detection of lat psrs j1741-2054 and j2032+4127: No longer just gamma-ray pulsars', Astrophysical Journal, vol. 705, no. 1, pp. 1-13. https://doi.org/10.1088/0004-637X/705/1/1
    Camilo, F. ; Ray, P. S. ; Ransom, S. M. ; Burgay, M. ; Johnson, T. J. ; Kerr, M. ; Gotthelf, E. V. ; Halpern, J. P. ; Reynolds, J. ; Romani, R. W. ; Demorest, P. ; Johnston, S. ; Van Straten, W. ; Parkinson, P. M.Saz ; Ziegler, M. ; Dormody, M. ; Thompson, D. J. ; Smith, D. A. ; Harding, A. K. ; Abdo, A. A. ; Crawford, F. ; Freire, P. C.C. ; Keith, M. ; Kramer, M. ; Roberts, Mallory ; Weltevrede, P. ; Wood, K. S. / Radio detection of lat psrs j1741-2054 and j2032+4127 : No longer just gamma-ray pulsars. In: Astrophysical Journal. 2009 ; Vol. 705, No. 1. pp. 1-13.
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    abstract = "Sixteen pulsars have been discovered so far in blind searches of photons collected with the Large Area Telescope on the Fermi Gamma-ray Space Telescope. We here report the discovery of radio pulsations from two of them. PSR J1741-2054, with period P = 413 ms, was detected in archival Parkes telescope data and subsequently has been detected at the Green Bank Telescope (GBT). Its received flux varies greatly due to interstellar scintillation and it has a very small dispersion measure of DM = 4.7 pc cm-3, implying a distance of 0.4 kpc and possibly the smallest luminosity of any known radio pulsar. At this distance, for isotropic emission, its gamma-ray luminosity above 0.1 GeV corresponds to 28{\%} of the spin-down luminosity of erg s-1. The gamma-ray profile occupies 1/3 of pulse phase and has three closely spaced peaks with the first peak lagging the radio pulse by δ = 0.29 P. We have also identified a soft Swift source that is the likely X-ray counterpart. In many respects PSRJ1741-2054 resembles the Geminga pulsar. The second source, PSR J2032+4127, was detected at the GBT. It has P = 143 ms, and its DM = 115 pc cm-3 suggests a distance of 3.6 kpc, but we consider it likely that it is located within the Cyg OB2 stellar association at half that distance. The radio emission is nearly 100{\%} linearly polarized, and the main radio peak precedes by δ = 0.15 P the first of two narrow gamma-ray peaks that are separated by Δ = 0.50 P. The second peak has a harder spectrum than the first one, following a trend observed in young gamma-ray pulsars. Faint, diffuse X-ray emission in a Chandra image is possibly its pulsar wind nebula. The wind of PSR J2032+4127 is responsible for the formerly unidentified HEGRA source TeV J2032+4130. PSR J2032+4127 is coincident in projection with MT91 213, a Be star in Cyg OB2, although apparently not a binary companion of it.",
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    T2 - No longer just gamma-ray pulsars

    AU - Camilo, F.

    AU - Ray, P. S.

    AU - Ransom, S. M.

    AU - Burgay, M.

    AU - Johnson, T. J.

    AU - Kerr, M.

    AU - Gotthelf, E. V.

    AU - Halpern, J. P.

    AU - Reynolds, J.

    AU - Romani, R. W.

    AU - Demorest, P.

    AU - Johnston, S.

    AU - Van Straten, W.

    AU - Parkinson, P. M.Saz

    AU - Ziegler, M.

    AU - Dormody, M.

    AU - Thompson, D. J.

    AU - Smith, D. A.

    AU - Harding, A. K.

    AU - Abdo, A. A.

    AU - Crawford, F.

    AU - Freire, P. C.C.

    AU - Keith, M.

    AU - Kramer, M.

    AU - Roberts, Mallory

    AU - Weltevrede, P.

    AU - Wood, K. S.

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    N2 - Sixteen pulsars have been discovered so far in blind searches of photons collected with the Large Area Telescope on the Fermi Gamma-ray Space Telescope. We here report the discovery of radio pulsations from two of them. PSR J1741-2054, with period P = 413 ms, was detected in archival Parkes telescope data and subsequently has been detected at the Green Bank Telescope (GBT). Its received flux varies greatly due to interstellar scintillation and it has a very small dispersion measure of DM = 4.7 pc cm-3, implying a distance of 0.4 kpc and possibly the smallest luminosity of any known radio pulsar. At this distance, for isotropic emission, its gamma-ray luminosity above 0.1 GeV corresponds to 28% of the spin-down luminosity of erg s-1. The gamma-ray profile occupies 1/3 of pulse phase and has three closely spaced peaks with the first peak lagging the radio pulse by δ = 0.29 P. We have also identified a soft Swift source that is the likely X-ray counterpart. In many respects PSRJ1741-2054 resembles the Geminga pulsar. The second source, PSR J2032+4127, was detected at the GBT. It has P = 143 ms, and its DM = 115 pc cm-3 suggests a distance of 3.6 kpc, but we consider it likely that it is located within the Cyg OB2 stellar association at half that distance. The radio emission is nearly 100% linearly polarized, and the main radio peak precedes by δ = 0.15 P the first of two narrow gamma-ray peaks that are separated by Δ = 0.50 P. The second peak has a harder spectrum than the first one, following a trend observed in young gamma-ray pulsars. Faint, diffuse X-ray emission in a Chandra image is possibly its pulsar wind nebula. The wind of PSR J2032+4127 is responsible for the formerly unidentified HEGRA source TeV J2032+4130. PSR J2032+4127 is coincident in projection with MT91 213, a Be star in Cyg OB2, although apparently not a binary companion of it.

    AB - Sixteen pulsars have been discovered so far in blind searches of photons collected with the Large Area Telescope on the Fermi Gamma-ray Space Telescope. We here report the discovery of radio pulsations from two of them. PSR J1741-2054, with period P = 413 ms, was detected in archival Parkes telescope data and subsequently has been detected at the Green Bank Telescope (GBT). Its received flux varies greatly due to interstellar scintillation and it has a very small dispersion measure of DM = 4.7 pc cm-3, implying a distance of 0.4 kpc and possibly the smallest luminosity of any known radio pulsar. At this distance, for isotropic emission, its gamma-ray luminosity above 0.1 GeV corresponds to 28% of the spin-down luminosity of erg s-1. The gamma-ray profile occupies 1/3 of pulse phase and has three closely spaced peaks with the first peak lagging the radio pulse by δ = 0.29 P. We have also identified a soft Swift source that is the likely X-ray counterpart. In many respects PSRJ1741-2054 resembles the Geminga pulsar. The second source, PSR J2032+4127, was detected at the GBT. It has P = 143 ms, and its DM = 115 pc cm-3 suggests a distance of 3.6 kpc, but we consider it likely that it is located within the Cyg OB2 stellar association at half that distance. The radio emission is nearly 100% linearly polarized, and the main radio peak precedes by δ = 0.15 P the first of two narrow gamma-ray peaks that are separated by Δ = 0.50 P. The second peak has a harder spectrum than the first one, following a trend observed in young gamma-ray pulsars. Faint, diffuse X-ray emission in a Chandra image is possibly its pulsar wind nebula. The wind of PSR J2032+4127 is responsible for the formerly unidentified HEGRA source TeV J2032+4130. PSR J2032+4127 is coincident in projection with MT91 213, a Be star in Cyg OB2, although apparently not a binary companion of it.

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    KW - Open clusters and associations:individual (Cyg OB2)

    KW - X-rays: individual (Swift J174157.6-205411)

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