Expansion velocity of ejecta in tycho's supernova remnant measured by doppler broadened X-RAY line emission

Asami Hayato, Hiroya Yamaguchi, Toru Tamagawa, Satoru Katsuda, Una Hwang, John P. Hughes, Midori Ozawa, Aya Bamba, Kenzo Kinugasa, Yukikatsu Terada, Akihiro Furuzawa, Hideyo Unieda, Kazuo Makishima

Research output: Contribution to journalArticle

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Abstract

We showthat the expansion of ejecta in Tycho's supernova remnant (SNR) is consistent with a spherically symmetric shell, based on Suzaku measurements of the Doppler broadened X-ray emission lines. All of the strong Kα line emissions show broader widths at the center than at the rim, while the centroid energies are constant across the remnant (except for Ca). This is the pattern expected for Doppler broadening due to expansion of the SNR ejecta in a spherical shell. To determine the expansion velocities of the ejecta, we applied a model for each emission-line feature having two Gaussian components separately representing red- and blueshifted gas, and inferred the Doppler velocity difference between these two components directly from the fitted centroid energy difference. Taking into account the effect of projecting a three-dimensional shell to the plane of the detector, we derived average spherical expansion velocities independently for the Kα emission of Si, S, Ar, and Fe, and Kβ of Si. We found that the expansion velocities of Si, S, and Ar ejecta of 4700 ± 100 km s-1 are distinctly higher than that obtained from Fe Kα emission, 4000 ±300 km s-1, which is consistent with segregation of the Fe in the inner ejecta. Combining the observed ejecta velocities with the ejecta proper-motion measurements by Chandra, we derived a distance to Tycho's SNR of 4 ± 1 kpc.

Original languageEnglish
Pages (from-to)894-903
Number of pages10
JournalAstrophysical Journal
Volume725
Issue number1
DOIs
Publication statusPublished - 10-12-2010

Fingerprint

supernova remnants
ejecta
expansion
x rays
shell
centroids
K lines
spherical shells
proper motion
rims
energy
detectors
gases
gas

All Science Journal Classification (ASJC) codes

  • Astronomy and Astrophysics
  • Space and Planetary Science

Cite this

Hayato, A., Yamaguchi, H., Tamagawa, T., Katsuda, S., Hwang, U., Hughes, J. P., ... Makishima, K. (2010). Expansion velocity of ejecta in tycho's supernova remnant measured by doppler broadened X-RAY line emission. Astrophysical Journal, 725(1), 894-903. https://doi.org/10.1088/0004-637X/725/1/894
Hayato, Asami ; Yamaguchi, Hiroya ; Tamagawa, Toru ; Katsuda, Satoru ; Hwang, Una ; Hughes, John P. ; Ozawa, Midori ; Bamba, Aya ; Kinugasa, Kenzo ; Terada, Yukikatsu ; Furuzawa, Akihiro ; Unieda, Hideyo ; Makishima, Kazuo. / Expansion velocity of ejecta in tycho's supernova remnant measured by doppler broadened X-RAY line emission. In: Astrophysical Journal. 2010 ; Vol. 725, No. 1. pp. 894-903.
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abstract = "We showthat the expansion of ejecta in Tycho's supernova remnant (SNR) is consistent with a spherically symmetric shell, based on Suzaku measurements of the Doppler broadened X-ray emission lines. All of the strong Kα line emissions show broader widths at the center than at the rim, while the centroid energies are constant across the remnant (except for Ca). This is the pattern expected for Doppler broadening due to expansion of the SNR ejecta in a spherical shell. To determine the expansion velocities of the ejecta, we applied a model for each emission-line feature having two Gaussian components separately representing red- and blueshifted gas, and inferred the Doppler velocity difference between these two components directly from the fitted centroid energy difference. Taking into account the effect of projecting a three-dimensional shell to the plane of the detector, we derived average spherical expansion velocities independently for the Kα emission of Si, S, Ar, and Fe, and Kβ of Si. We found that the expansion velocities of Si, S, and Ar ejecta of 4700 ± 100 km s-1 are distinctly higher than that obtained from Fe Kα emission, 4000 ±300 km s-1, which is consistent with segregation of the Fe in the inner ejecta. Combining the observed ejecta velocities with the ejecta proper-motion measurements by Chandra, we derived a distance to Tycho's SNR of 4 ± 1 kpc.",
author = "Asami Hayato and Hiroya Yamaguchi and Toru Tamagawa and Satoru Katsuda and Una Hwang and Hughes, {John P.} and Midori Ozawa and Aya Bamba and Kenzo Kinugasa and Yukikatsu Terada and Akihiro Furuzawa and Hideyo Unieda and Kazuo Makishima",
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Hayato, A, Yamaguchi, H, Tamagawa, T, Katsuda, S, Hwang, U, Hughes, JP, Ozawa, M, Bamba, A, Kinugasa, K, Terada, Y, Furuzawa, A, Unieda, H & Makishima, K 2010, 'Expansion velocity of ejecta in tycho's supernova remnant measured by doppler broadened X-RAY line emission', Astrophysical Journal, vol. 725, no. 1, pp. 894-903. https://doi.org/10.1088/0004-637X/725/1/894

Expansion velocity of ejecta in tycho's supernova remnant measured by doppler broadened X-RAY line emission. / Hayato, Asami; Yamaguchi, Hiroya; Tamagawa, Toru; Katsuda, Satoru; Hwang, Una; Hughes, John P.; Ozawa, Midori; Bamba, Aya; Kinugasa, Kenzo; Terada, Yukikatsu; Furuzawa, Akihiro; Unieda, Hideyo; Makishima, Kazuo.

In: Astrophysical Journal, Vol. 725, No. 1, 10.12.2010, p. 894-903.

Research output: Contribution to journalArticle

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T1 - Expansion velocity of ejecta in tycho's supernova remnant measured by doppler broadened X-RAY line emission

AU - Hayato, Asami

AU - Yamaguchi, Hiroya

AU - Tamagawa, Toru

AU - Katsuda, Satoru

AU - Hwang, Una

AU - Hughes, John P.

AU - Ozawa, Midori

AU - Bamba, Aya

AU - Kinugasa, Kenzo

AU - Terada, Yukikatsu

AU - Furuzawa, Akihiro

AU - Unieda, Hideyo

AU - Makishima, Kazuo

PY - 2010/12/10

Y1 - 2010/12/10

N2 - We showthat the expansion of ejecta in Tycho's supernova remnant (SNR) is consistent with a spherically symmetric shell, based on Suzaku measurements of the Doppler broadened X-ray emission lines. All of the strong Kα line emissions show broader widths at the center than at the rim, while the centroid energies are constant across the remnant (except for Ca). This is the pattern expected for Doppler broadening due to expansion of the SNR ejecta in a spherical shell. To determine the expansion velocities of the ejecta, we applied a model for each emission-line feature having two Gaussian components separately representing red- and blueshifted gas, and inferred the Doppler velocity difference between these two components directly from the fitted centroid energy difference. Taking into account the effect of projecting a three-dimensional shell to the plane of the detector, we derived average spherical expansion velocities independently for the Kα emission of Si, S, Ar, and Fe, and Kβ of Si. We found that the expansion velocities of Si, S, and Ar ejecta of 4700 ± 100 km s-1 are distinctly higher than that obtained from Fe Kα emission, 4000 ±300 km s-1, which is consistent with segregation of the Fe in the inner ejecta. Combining the observed ejecta velocities with the ejecta proper-motion measurements by Chandra, we derived a distance to Tycho's SNR of 4 ± 1 kpc.

AB - We showthat the expansion of ejecta in Tycho's supernova remnant (SNR) is consistent with a spherically symmetric shell, based on Suzaku measurements of the Doppler broadened X-ray emission lines. All of the strong Kα line emissions show broader widths at the center than at the rim, while the centroid energies are constant across the remnant (except for Ca). This is the pattern expected for Doppler broadening due to expansion of the SNR ejecta in a spherical shell. To determine the expansion velocities of the ejecta, we applied a model for each emission-line feature having two Gaussian components separately representing red- and blueshifted gas, and inferred the Doppler velocity difference between these two components directly from the fitted centroid energy difference. Taking into account the effect of projecting a three-dimensional shell to the plane of the detector, we derived average spherical expansion velocities independently for the Kα emission of Si, S, Ar, and Fe, and Kβ of Si. We found that the expansion velocities of Si, S, and Ar ejecta of 4700 ± 100 km s-1 are distinctly higher than that obtained from Fe Kα emission, 4000 ±300 km s-1, which is consistent with segregation of the Fe in the inner ejecta. Combining the observed ejecta velocities with the ejecta proper-motion measurements by Chandra, we derived a distance to Tycho's SNR of 4 ± 1 kpc.

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