XMM-Newton and SUZAKU detection of an X-ray emitting shell around the pulsar wind nebula G54.1+0.3

F. Bocchino, R. Bandiera, Joseph (Yosi) Gelfand

    Research output: Contribution to journalArticle

    Abstract

    Context. X-ray observations have proven to be very effective in detecting previously unknown supernova remnant shells around pulsar wind nebulae (PWNe), and in these cases the characteristics of the shell provide information about the evolutionary stage of the embedded PWN. However, it is not clear why some PWNe are "naked". Aims. We perform an X-ray observational campaign targeting the PWN G54.1+0.3, the "close cousin" of the Crab Nebula, to try to detect the associated SNR shell. Methods. We analyze XMM-Newton and Suzaku observations of G54.1+0.3 to model the contribution of a dust scattering halo. Results. We detecte an intrinsic faint diffuse X-ray emission surrounding the PWN out to ∼ 6' (∼10 pc) from the pulsar, characterized by a hard spectrum, which can be modeled with either a power law (γ = 2.9) or a thermal plasma model (kT = 2.0 keV.) Conclusions. Assuming the shell to be thermal, we derive an explosion energy E = 0.5-1.6×1051 erg, a pre-shock ISM density of 0.2 cm-3, and an age of ∼2000 yr. Using these results in the MHD model of PWN-SNR evolution, we obtain excellent agreement between the predicted and observed location of the shell and PWN shock.

    Original languageEnglish (US)
    Article numberA71
    JournalAstronomy and Astrophysics
    Volume520
    Issue number10
    DOIs
    StatePublished - Jan 1 2010

    Fingerprint

    XMM-Newton telescope
    nebulae
    pulsars
    newton
    shell
    shock
    Crab nebula
    x rays
    thermal plasmas
    supernova remnants
    explosions
    halos
    dust
    erg
    targeting
    explosion
    crab
    scattering
    power law
    detection

    Keywords

    • dust, extinction
    • ISM: supernova remnants

    ASJC Scopus subject areas

    • Astronomy and Astrophysics
    • Space and Planetary Science

    Cite this

    XMM-Newton and SUZAKU detection of an X-ray emitting shell around the pulsar wind nebula G54.1+0.3. / Bocchino, F.; Bandiera, R.; Gelfand, Joseph (Yosi).

    In: Astronomy and Astrophysics, Vol. 520, No. 10, A71, 01.01.2010.

    Research output: Contribution to journalArticle

    Bocchino, F. ; Bandiera, R. ; Gelfand, Joseph (Yosi). / XMM-Newton and SUZAKU detection of an X-ray emitting shell around the pulsar wind nebula G54.1+0.3. In: Astronomy and Astrophysics. 2010 ; Vol. 520, No. 10.
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    abstract = "Context. X-ray observations have proven to be very effective in detecting previously unknown supernova remnant shells around pulsar wind nebulae (PWNe), and in these cases the characteristics of the shell provide information about the evolutionary stage of the embedded PWN. However, it is not clear why some PWNe are {"}naked{"}. Aims. We perform an X-ray observational campaign targeting the PWN G54.1+0.3, the {"}close cousin{"} of the Crab Nebula, to try to detect the associated SNR shell. Methods. We analyze XMM-Newton and Suzaku observations of G54.1+0.3 to model the contribution of a dust scattering halo. Results. We detecte an intrinsic faint diffuse X-ray emission surrounding the PWN out to ∼ 6' (∼10 pc) from the pulsar, characterized by a hard spectrum, which can be modeled with either a power law (γ = 2.9) or a thermal plasma model (kT = 2.0 keV.) Conclusions. Assuming the shell to be thermal, we derive an explosion energy E = 0.5-1.6×1051 erg, a pre-shock ISM density of 0.2 cm-3, and an age of ∼2000 yr. Using these results in the MHD model of PWN-SNR evolution, we obtain excellent agreement between the predicted and observed location of the shell and PWN shock.",
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    N2 - Context. X-ray observations have proven to be very effective in detecting previously unknown supernova remnant shells around pulsar wind nebulae (PWNe), and in these cases the characteristics of the shell provide information about the evolutionary stage of the embedded PWN. However, it is not clear why some PWNe are "naked". Aims. We perform an X-ray observational campaign targeting the PWN G54.1+0.3, the "close cousin" of the Crab Nebula, to try to detect the associated SNR shell. Methods. We analyze XMM-Newton and Suzaku observations of G54.1+0.3 to model the contribution of a dust scattering halo. Results. We detecte an intrinsic faint diffuse X-ray emission surrounding the PWN out to ∼ 6' (∼10 pc) from the pulsar, characterized by a hard spectrum, which can be modeled with either a power law (γ = 2.9) or a thermal plasma model (kT = 2.0 keV.) Conclusions. Assuming the shell to be thermal, we derive an explosion energy E = 0.5-1.6×1051 erg, a pre-shock ISM density of 0.2 cm-3, and an age of ∼2000 yr. Using these results in the MHD model of PWN-SNR evolution, we obtain excellent agreement between the predicted and observed location of the shell and PWN shock.

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