Suzaku X-ray observations of the fermi bubbles: Northernmost cap and southeast claw discovered with MAXI-SSC

M. Tahara, Jun Kataoka, Y. Takeuchi, T. Totani, Y. Sofue, J. S. Hiraga, H. Tsunemi, Y. Inoue, M. Kimura, C. C. Cheung, S. Nakashima

    研究成果: Article

    12 引用 (Scopus)

    抄録

    We report on Suzaku observations of large-scale X-ray structures possibly related to the Fermi Bubbles obtained in 2013 with a total duration of ≃80 ks. The observed regions were (1) the northern cap (N-cap; l ∼ 0°, 45° < b< 55°) seen in the mid-band (1.7-4.0 keV) map recently provided by Monitor of All-sky X-ray Image Solid-state Slit Camera (MAXI-SSC) and (2) the southeast claw (SE-claw; l ∼ 10°, -20° < b < -10°) seen in the ROSAT all-sky map and MAXI-SSC low-band (0.7-1.7 keV) map. In each region, we detected diffuse X-ray emission, which is represented by a three-component plasma model consisting of an unabsorbed thermal component (kT ≃ 0.1 keV) from the Local Hot Bubble, absorbed kT = 0.30 ± 0.05 keV emission representing the Galactic halo (GH), and a power-law component due to the isotropic cosmic X-ray background radiation. The emission measure of the GH component in the SE-claw shows an excess by a factor of ≃2.5 over the surrounding emission at 2° away. We also found a broad excess in the 1.7-4.0 keV count rates across the N-cap after compiling other archival data from Suzaku and Swift. The spectral stacking analysis of the N-cap data indicates the presence of another thermal component with kT = 0.70-0.11 +0.22keV. The temperature kT ≃ 0.3 keV of the GH is higher than the ubiquitous value of kT ≃ 0.2 keV near the Fermi bubbles, and can be even higher (∼0.7 keV). We discuss our findings in the context of the bubble-halo interaction.

    元の言語English
    記事番号91
    ジャーナルAstrophysical Journal
    802
    発行部数2
    DOI
    出版物ステータスPublished - 2015 4 1

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    caps
    slits
    sky
    monitors
    bubble
    bubbles
    cameras
    galactic halos
    solid state
    x rays
    background radiation
    stacking
    halos
    power law
    plasma
    temperature
    interactions

    ASJC Scopus subject areas

    • Space and Planetary Science
    • Astronomy and Astrophysics

    これを引用

    Suzaku X-ray observations of the fermi bubbles : Northernmost cap and southeast claw discovered with MAXI-SSC. / Tahara, M.; Kataoka, Jun; Takeuchi, Y.; Totani, T.; Sofue, Y.; Hiraga, J. S.; Tsunemi, H.; Inoue, Y.; Kimura, M.; Cheung, C. C.; Nakashima, S.

    :: Astrophysical Journal, 巻 802, 番号 2, 91, 01.04.2015.

    研究成果: Article

    Tahara, M, Kataoka, J, Takeuchi, Y, Totani, T, Sofue, Y, Hiraga, JS, Tsunemi, H, Inoue, Y, Kimura, M, Cheung, CC & Nakashima, S 2015, 'Suzaku X-ray observations of the fermi bubbles: Northernmost cap and southeast claw discovered with MAXI-SSC', Astrophysical Journal, 巻. 802, 番号 2, 91. https://doi.org/10.1088/0004-637X/802/2/91
    Tahara, M. ; Kataoka, Jun ; Takeuchi, Y. ; Totani, T. ; Sofue, Y. ; Hiraga, J. S. ; Tsunemi, H. ; Inoue, Y. ; Kimura, M. ; Cheung, C. C. ; Nakashima, S. / Suzaku X-ray observations of the fermi bubbles : Northernmost cap and southeast claw discovered with MAXI-SSC. :: Astrophysical Journal. 2015 ; 巻 802, 番号 2.
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    abstract = "We report on Suzaku observations of large-scale X-ray structures possibly related to the Fermi Bubbles obtained in 2013 with a total duration of ≃80 ks. The observed regions were (1) the northern cap (N-cap; l ∼ 0°, 45° < b< 55°) seen in the mid-band (1.7-4.0 keV) map recently provided by Monitor of All-sky X-ray Image Solid-state Slit Camera (MAXI-SSC) and (2) the southeast claw (SE-claw; l ∼ 10°, -20° < b < -10°) seen in the ROSAT all-sky map and MAXI-SSC low-band (0.7-1.7 keV) map. In each region, we detected diffuse X-ray emission, which is represented by a three-component plasma model consisting of an unabsorbed thermal component (kT ≃ 0.1 keV) from the Local Hot Bubble, absorbed kT = 0.30 ± 0.05 keV emission representing the Galactic halo (GH), and a power-law component due to the isotropic cosmic X-ray background radiation. The emission measure of the GH component in the SE-claw shows an excess by a factor of ≃2.5 over the surrounding emission at 2° away. We also found a broad excess in the 1.7-4.0 keV count rates across the N-cap after compiling other archival data from Suzaku and Swift. The spectral stacking analysis of the N-cap data indicates the presence of another thermal component with kT = 0.70-0.11 +0.22keV. The temperature kT ≃ 0.3 keV of the GH is higher than the ubiquitous value of kT ≃ 0.2 keV near the Fermi bubbles, and can be even higher (∼0.7 keV). We discuss our findings in the context of the bubble-halo interaction.",
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    T1 - Suzaku X-ray observations of the fermi bubbles

    T2 - Northernmost cap and southeast claw discovered with MAXI-SSC

    AU - Tahara, M.

    AU - Kataoka, Jun

    AU - Takeuchi, Y.

    AU - Totani, T.

    AU - Sofue, Y.

    AU - Hiraga, J. S.

    AU - Tsunemi, H.

    AU - Inoue, Y.

    AU - Kimura, M.

    AU - Cheung, C. C.

    AU - Nakashima, S.

    PY - 2015/4/1

    Y1 - 2015/4/1

    N2 - We report on Suzaku observations of large-scale X-ray structures possibly related to the Fermi Bubbles obtained in 2013 with a total duration of ≃80 ks. The observed regions were (1) the northern cap (N-cap; l ∼ 0°, 45° < b< 55°) seen in the mid-band (1.7-4.0 keV) map recently provided by Monitor of All-sky X-ray Image Solid-state Slit Camera (MAXI-SSC) and (2) the southeast claw (SE-claw; l ∼ 10°, -20° < b < -10°) seen in the ROSAT all-sky map and MAXI-SSC low-band (0.7-1.7 keV) map. In each region, we detected diffuse X-ray emission, which is represented by a three-component plasma model consisting of an unabsorbed thermal component (kT ≃ 0.1 keV) from the Local Hot Bubble, absorbed kT = 0.30 ± 0.05 keV emission representing the Galactic halo (GH), and a power-law component due to the isotropic cosmic X-ray background radiation. The emission measure of the GH component in the SE-claw shows an excess by a factor of ≃2.5 over the surrounding emission at 2° away. We also found a broad excess in the 1.7-4.0 keV count rates across the N-cap after compiling other archival data from Suzaku and Swift. The spectral stacking analysis of the N-cap data indicates the presence of another thermal component with kT = 0.70-0.11 +0.22keV. The temperature kT ≃ 0.3 keV of the GH is higher than the ubiquitous value of kT ≃ 0.2 keV near the Fermi bubbles, and can be even higher (∼0.7 keV). We discuss our findings in the context of the bubble-halo interaction.

    AB - We report on Suzaku observations of large-scale X-ray structures possibly related to the Fermi Bubbles obtained in 2013 with a total duration of ≃80 ks. The observed regions were (1) the northern cap (N-cap; l ∼ 0°, 45° < b< 55°) seen in the mid-band (1.7-4.0 keV) map recently provided by Monitor of All-sky X-ray Image Solid-state Slit Camera (MAXI-SSC) and (2) the southeast claw (SE-claw; l ∼ 10°, -20° < b < -10°) seen in the ROSAT all-sky map and MAXI-SSC low-band (0.7-1.7 keV) map. In each region, we detected diffuse X-ray emission, which is represented by a three-component plasma model consisting of an unabsorbed thermal component (kT ≃ 0.1 keV) from the Local Hot Bubble, absorbed kT = 0.30 ± 0.05 keV emission representing the Galactic halo (GH), and a power-law component due to the isotropic cosmic X-ray background radiation. The emission measure of the GH component in the SE-claw shows an excess by a factor of ≃2.5 over the surrounding emission at 2° away. We also found a broad excess in the 1.7-4.0 keV count rates across the N-cap after compiling other archival data from Suzaku and Swift. The spectral stacking analysis of the N-cap data indicates the presence of another thermal component with kT = 0.70-0.11 +0.22keV. The temperature kT ≃ 0.3 keV of the GH is higher than the ubiquitous value of kT ≃ 0.2 keV near the Fermi bubbles, and can be even higher (∼0.7 keV). We discuss our findings in the context of the bubble-halo interaction.

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    KW - X-rays: ISM

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