Hitomi observations of the LMC SNR N 132 D: Highly redshifted X-ray emission from iron ejecta

Hitomi Collaboration

    Research output: Contribution to journalArticle

    Abstract

    We present Hitomi observations of N 132 D, a young, X-ray bright, O-rich core-collapse supernova remnant in the Large Magellanic Cloud (LMC). Despite a very short observation of only 3.7 ks, the Soft X-ray Spectrometer (SXS) easily detects the line complexes of highly ionized S K and Fe K with 16-17 counts in each. The Fe feature is measured for the first time at high spectral resolution. Based on the plausible assumption that the Fe K emission is dominated by He-like ions, we find that the material responsible for this Fe emission is highly redshifted at ∼ 800 km s−1 compared to the local LMC interstellar medium (ISM), with a 90% credible interval of 50-1500 km s−1 if a weakly informative prior is placed on possible line broadening. This indicates (1) that the Fe emission arises from the supernova ejecta, and (2) that these ejecta are highly asymmetric, since no blueshifted component is found. The S K velocity is consistent with the local LMC ISM, and is likely from swept-up ISM material. These results are consistent with spatial mapping that shows the He-like Fe concentrated in the interior of the remnant and the S tracing the outer shell. The results also show that even with a very small number of counts, direct velocity measurements from Doppler-shifted lines detected in extended objects like supernova remnants are now possible. Thanks to the very low SXS background of ∼ 1 event per spectral resolution element per 100 ks, such results are obtainable during short pointed or slew observations with similar instruments. This highlights the power of high-spectral-resolution imaging observations, and demonstrates the new window that has been opened with Hitomi and will be greatly widened with future missions such as the X-ray Astronomy Recovery Mission (XARM) and Athena.

    Original languageEnglish
    Article numberpsx151
    JournalPublications of the Astronomical Society of Japan
    Volume70
    Issue number2
    DOIs
    Publication statusPublished - 2018 Mar 1

    Fingerprint

    Magellanic clouds
    ejecta
    spectral resolution
    iron
    supernova remnants
    x rays
    spectrometer
    spectrometers
    high resolution
    astronomy
    tracing
    velocity measurement
    supernovae
    recovery
    shell
    intervals
    ion
    ions
    material

    Keywords

    • Instrumentation: spectrographs
    • ISM: individual objects (N 132 D)
    • ISM: supernova remnants
    • Methods: observational
    • X-rays: individual (N 132 D)

    ASJC Scopus subject areas

    • Astronomy and Astrophysics
    • Space and Planetary Science

    Cite this

    Hitomi observations of the LMC SNR N 132 D : Highly redshifted X-ray emission from iron ejecta. / Hitomi Collaboration.

    In: Publications of the Astronomical Society of Japan, Vol. 70, No. 2, psx151, 01.03.2018.

    Research output: Contribution to journalArticle

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    title = "Hitomi observations of the LMC SNR N 132 D: Highly redshifted X-ray emission from iron ejecta",
    abstract = "We present Hitomi observations of N 132 D, a young, X-ray bright, O-rich core-collapse supernova remnant in the Large Magellanic Cloud (LMC). Despite a very short observation of only 3.7 ks, the Soft X-ray Spectrometer (SXS) easily detects the line complexes of highly ionized S K and Fe K with 16-17 counts in each. The Fe feature is measured for the first time at high spectral resolution. Based on the plausible assumption that the Fe K emission is dominated by He-like ions, we find that the material responsible for this Fe emission is highly redshifted at ∼ 800 km s−1 compared to the local LMC interstellar medium (ISM), with a 90{\%} credible interval of 50-1500 km s−1 if a weakly informative prior is placed on possible line broadening. This indicates (1) that the Fe emission arises from the supernova ejecta, and (2) that these ejecta are highly asymmetric, since no blueshifted component is found. The S K velocity is consistent with the local LMC ISM, and is likely from swept-up ISM material. These results are consistent with spatial mapping that shows the He-like Fe concentrated in the interior of the remnant and the S tracing the outer shell. The results also show that even with a very small number of counts, direct velocity measurements from Doppler-shifted lines detected in extended objects like supernova remnants are now possible. Thanks to the very low SXS background of ∼ 1 event per spectral resolution element per 100 ks, such results are obtainable during short pointed or slew observations with similar instruments. This highlights the power of high-spectral-resolution imaging observations, and demonstrates the new window that has been opened with Hitomi and will be greatly widened with future missions such as the X-ray Astronomy Recovery Mission (XARM) and Athena.",
    keywords = "Instrumentation: spectrographs, ISM: individual objects (N 132 D), ISM: supernova remnants, Methods: observational, X-rays: individual (N 132 D)",
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    TY - JOUR

    T1 - Hitomi observations of the LMC SNR N 132 D

    T2 - Highly redshifted X-ray emission from iron ejecta

    AU - Hitomi Collaboration

    AU - Aharonian, Felix

    AU - Akamatsu, Hiroki

    AU - Akimoto, Fumie

    AU - Allen, Steven W.

    AU - Angelini, Lorella

    AU - Audard, Marc

    AU - Awaki, Hisamitsu

    AU - Axelsson, Magnus

    AU - Bamba, Aya

    AU - Bautz, Marshall W.

    AU - Blandford, Roger

    AU - Brenneman, Laura W.

    AU - Brown, Gregory V.

    AU - Bulbul, Esra

    AU - Cackett, Edward M.

    AU - Chernyakova, Maria

    AU - Chiao, Meng P.

    AU - Coppi, Paolo S.

    AU - Costantini, Elisa

    AU - De Plaa, Jelle

    AU - De Vries, Cor P.

    AU - Den Herder, Jan Willem

    AU - Done, Chris

    AU - Dotani, Tadayasu

    AU - Ebisawa, Ken

    AU - Eckart, Megan E.

    AU - Enoto, Teruaki

    AU - Ezoe, Yuichiro

    AU - Fabian, Andrew C.

    AU - Ferrigno, Carlo

    AU - Foster, Adam R.

    AU - Fujimoto, Ryuichi

    AU - Fukazawa, Yasushi

    AU - Furuzawa, Akihiro

    AU - Galeazzi, Massimiliano

    AU - Gallo, Luigi C.

    AU - Gandhi, Poshak

    AU - Giustini, Margherita

    AU - Goldwurm, Andrea

    AU - Gu, Liyi

    AU - Guainazzi, Matteo

    AU - Haba, Yoshito

    AU - Hagino, Kouichi

    AU - Hamaguchi, Kenji

    AU - Harrus, Ilana M.

    AU - Hatsukade, Isamu

    AU - Hayashi, Katsuhiro

    AU - Hayashi, Takayuki

    AU - Hayashida, Kiyoshi

    AU - Kataoka, Jun

    PY - 2018/3/1

    Y1 - 2018/3/1

    N2 - We present Hitomi observations of N 132 D, a young, X-ray bright, O-rich core-collapse supernova remnant in the Large Magellanic Cloud (LMC). Despite a very short observation of only 3.7 ks, the Soft X-ray Spectrometer (SXS) easily detects the line complexes of highly ionized S K and Fe K with 16-17 counts in each. The Fe feature is measured for the first time at high spectral resolution. Based on the plausible assumption that the Fe K emission is dominated by He-like ions, we find that the material responsible for this Fe emission is highly redshifted at ∼ 800 km s−1 compared to the local LMC interstellar medium (ISM), with a 90% credible interval of 50-1500 km s−1 if a weakly informative prior is placed on possible line broadening. This indicates (1) that the Fe emission arises from the supernova ejecta, and (2) that these ejecta are highly asymmetric, since no blueshifted component is found. The S K velocity is consistent with the local LMC ISM, and is likely from swept-up ISM material. These results are consistent with spatial mapping that shows the He-like Fe concentrated in the interior of the remnant and the S tracing the outer shell. The results also show that even with a very small number of counts, direct velocity measurements from Doppler-shifted lines detected in extended objects like supernova remnants are now possible. Thanks to the very low SXS background of ∼ 1 event per spectral resolution element per 100 ks, such results are obtainable during short pointed or slew observations with similar instruments. This highlights the power of high-spectral-resolution imaging observations, and demonstrates the new window that has been opened with Hitomi and will be greatly widened with future missions such as the X-ray Astronomy Recovery Mission (XARM) and Athena.

    AB - We present Hitomi observations of N 132 D, a young, X-ray bright, O-rich core-collapse supernova remnant in the Large Magellanic Cloud (LMC). Despite a very short observation of only 3.7 ks, the Soft X-ray Spectrometer (SXS) easily detects the line complexes of highly ionized S K and Fe K with 16-17 counts in each. The Fe feature is measured for the first time at high spectral resolution. Based on the plausible assumption that the Fe K emission is dominated by He-like ions, we find that the material responsible for this Fe emission is highly redshifted at ∼ 800 km s−1 compared to the local LMC interstellar medium (ISM), with a 90% credible interval of 50-1500 km s−1 if a weakly informative prior is placed on possible line broadening. This indicates (1) that the Fe emission arises from the supernova ejecta, and (2) that these ejecta are highly asymmetric, since no blueshifted component is found. The S K velocity is consistent with the local LMC ISM, and is likely from swept-up ISM material. These results are consistent with spatial mapping that shows the He-like Fe concentrated in the interior of the remnant and the S tracing the outer shell. The results also show that even with a very small number of counts, direct velocity measurements from Doppler-shifted lines detected in extended objects like supernova remnants are now possible. Thanks to the very low SXS background of ∼ 1 event per spectral resolution element per 100 ks, such results are obtainable during short pointed or slew observations with similar instruments. This highlights the power of high-spectral-resolution imaging observations, and demonstrates the new window that has been opened with Hitomi and will be greatly widened with future missions such as the X-ray Astronomy Recovery Mission (XARM) and Athena.

    KW - Instrumentation: spectrographs

    KW - ISM: individual objects (N 132 D)

    KW - ISM: supernova remnants

    KW - Methods: observational

    KW - X-rays: individual (N 132 D)

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