Suzaku observations of tycho's supernova remnant

Toru Tamagawa; Asami Hayato; Satoshi Nakamura; Yukikatsu Terada; Aya Bamba; Junko S. HLraga; John P. Hughes; Una Hwang; Jun Kataoka; Kenzo Kinugasa; Hideyo Kunieda; Takaaki Tanaka; Hiroshi Tsunemi; Masaru Ueno; Stephen S. Holt; Motohide Kokubun; Emi Mlyata; Andrew Szymkowiak; Tadayuki Takahashi; Keisuke Tamura; Daisuke Ueno; Kazuo Makishima

doi:10.1093/pasj/61.sp1.s167

Suzaku observations of tycho's supernova remnant

Toru Tamagawa^*, Asami Hayato, Satoshi Nakamura, Yukikatsu Terada, Aya Bamba, Junko S. HLraga, John P. Hughes, Una Hwang, Jun Kataoka, Kenzo Kinugasa, Hideyo Kunieda, Takaaki Tanaka, Hiroshi Tsunemi, Masaru Ueno, Stephen S. Holt, Motohide Kokubun, Emi Mlyata, Andrew Szymkowiak, Tadayuki Takahashi, Keisuke TamuraDaisuke Ueno, Kazuo Makishima

^*Corresponding author for this work

Research output: Contribution to journal › Article › peer-review

43 Citations (Scopus)

Abstract

Tycho's supernova remnant was observed by the XIS and HXD instruments onboard the Suzaku satellite on 2006 June 26-29 for 92 ks. The spectrum up to 30 keV was well fitted with a two-component model, consisting of a power-law with a photon index of 2.7 and a thermal bremsstrahlung model with a temperature of 4.7 keV. The former component can alternatively be modeled as synchrotron emission from a population of relativistic electrons with an estimated roll-off energy of around 1 keV. In the XIS spectra, in addition to the prominent Fe Ka line (6.445 keV), we observed for the first time significant Ka line emission from trace species Cr and Mn at energies of 5.48 keV and 5.95 keV, respectively. Faint K/5 lines from Ca (4.56keV) and Fe (7.11 keV) were also seen. The ionization states of Cr and Mn, based on their line centroids, are estimated to be similar to that of Fe Ka (Fexv orxvi).

Original language	English
Pages (from-to)	S167-S174
Journal	Publications of the Astronomical Society of Japan
Volume	61
Issue number	SUPPL. 1
DOIs	https://doi.org/10.1093/pasj/61.sp1.s167
Publication status	Published - 2009
Externally published	Yes

Keywords

Acceleration of particles - ISM
Individual (Tycho)
Supernova remnants - X-rays

ASJC Scopus subject areas

Astronomy and Astrophysics
Space and Planetary Science

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10.1093/pasj/61.sp1.s167

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Tamagawa, T., Hayato, A., Nakamura, S., Terada, Y., Bamba, A., HLraga, J. S., Hughes, J. P., Hwang, U., Kataoka, J., Kinugasa, K., Kunieda, H., Tanaka, T., Tsunemi, H., Ueno, M., Holt, S. S., Kokubun, M., Mlyata, E., Szymkowiak, A., Takahashi, T., ... Makishima, K. (2009). Suzaku observations of tycho's supernova remnant. Publications of the Astronomical Society of Japan, 61(SUPPL. 1), S167-S174. https://doi.org/10.1093/pasj/61.sp1.s167

Tamagawa, T, Hayato, A, Nakamura, S, Terada, Y, Bamba, A, HLraga, JS, Hughes, JP, Hwang, U, Kataoka, J, Kinugasa, K, Kunieda, H, Tanaka, T, Tsunemi, H, Ueno, M, Holt, SS, Kokubun, M, Mlyata, E, Szymkowiak, A, Takahashi, T, Tamura, K, Ueno, D & Makishima, K 2009, 'Suzaku observations of tycho's supernova remnant', Publications of the Astronomical Society of Japan, vol. 61, no. SUPPL. 1, pp. S167-S174. https://doi.org/10.1093/pasj/61.sp1.s167

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title = "Suzaku observations of tycho's supernova remnant",

abstract = "Tycho's supernova remnant was observed by the XIS and HXD instruments onboard the Suzaku satellite on 2006 June 26-29 for 92 ks. The spectrum up to 30 keV was well fitted with a two-component model, consisting of a power-law with a photon index of 2.7 and a thermal bremsstrahlung model with a temperature of 4.7 keV. The former component can alternatively be modeled as synchrotron emission from a population of relativistic electrons with an estimated roll-off energy of around 1 keV. In the XIS spectra, in addition to the prominent Fe Ka line (6.445 keV), we observed for the first time significant Ka line emission from trace species Cr and Mn at energies of 5.48 keV and 5.95 keV, respectively. Faint K/5 lines from Ca (4.56keV) and Fe (7.11 keV) were also seen. The ionization states of Cr and Mn, based on their line centroids, are estimated to be similar to that of Fe Ka (Fexv orxvi).",

keywords = "Acceleration of particles - ISM, Individual (Tycho), Supernova remnants - X-rays",

author = "Toru Tamagawa and Asami Hayato and Satoshi Nakamura and Yukikatsu Terada and Aya Bamba and HLraga, {Junko S.} and Hughes, {John P.} and Una Hwang and Jun Kataoka and Kenzo Kinugasa and Hideyo Kunieda and Takaaki Tanaka and Hiroshi Tsunemi and Masaru Ueno and Holt, {Stephen S.} and Motohide Kokubun and Emi Mlyata and Andrew Szymkowiak and Tadayuki Takahashi and Keisuke Tamura and Daisuke Ueno and Kazuo Makishima",

year = "2009",

doi = "10.1093/pasj/61.sp1.s167",

language = "English",

volume = "61",

pages = "S167--S174",

journal = "Publication of the Astronomical Society of Japan",

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publisher = "Astronomical Society of Japan",

number = "SUPPL. 1",

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T1 - Suzaku observations of tycho's supernova remnant

AU - Tamagawa, Toru

AU - Hayato, Asami

AU - Nakamura, Satoshi

AU - Terada, Yukikatsu

AU - Bamba, Aya

AU - HLraga, Junko S.

AU - Hughes, John P.

AU - Hwang, Una

AU - Kataoka, Jun

AU - Kinugasa, Kenzo

AU - Kunieda, Hideyo

AU - Tanaka, Takaaki

AU - Tsunemi, Hiroshi

AU - Ueno, Masaru

AU - Holt, Stephen S.

AU - Kokubun, Motohide

AU - Mlyata, Emi

AU - Szymkowiak, Andrew

AU - Takahashi, Tadayuki

AU - Tamura, Keisuke

AU - Ueno, Daisuke

AU - Makishima, Kazuo

PY - 2009

Y1 - 2009

N2 - Tycho's supernova remnant was observed by the XIS and HXD instruments onboard the Suzaku satellite on 2006 June 26-29 for 92 ks. The spectrum up to 30 keV was well fitted with a two-component model, consisting of a power-law with a photon index of 2.7 and a thermal bremsstrahlung model with a temperature of 4.7 keV. The former component can alternatively be modeled as synchrotron emission from a population of relativistic electrons with an estimated roll-off energy of around 1 keV. In the XIS spectra, in addition to the prominent Fe Ka line (6.445 keV), we observed for the first time significant Ka line emission from trace species Cr and Mn at energies of 5.48 keV and 5.95 keV, respectively. Faint K/5 lines from Ca (4.56keV) and Fe (7.11 keV) were also seen. The ionization states of Cr and Mn, based on their line centroids, are estimated to be similar to that of Fe Ka (Fexv orxvi).

AB - Tycho's supernova remnant was observed by the XIS and HXD instruments onboard the Suzaku satellite on 2006 June 26-29 for 92 ks. The spectrum up to 30 keV was well fitted with a two-component model, consisting of a power-law with a photon index of 2.7 and a thermal bremsstrahlung model with a temperature of 4.7 keV. The former component can alternatively be modeled as synchrotron emission from a population of relativistic electrons with an estimated roll-off energy of around 1 keV. In the XIS spectra, in addition to the prominent Fe Ka line (6.445 keV), we observed for the first time significant Ka line emission from trace species Cr and Mn at energies of 5.48 keV and 5.95 keV, respectively. Faint K/5 lines from Ca (4.56keV) and Fe (7.11 keV) were also seen. The ionization states of Cr and Mn, based on their line centroids, are estimated to be similar to that of Fe Ka (Fexv orxvi).

KW - Acceleration of particles - ISM

KW - Individual (Tycho)

KW - Supernova remnants - X-rays

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VL - 61

SP - S167-S174

JO - Publication of the Astronomical Society of Japan

JF - Publication of the Astronomical Society of Japan

IS - SUPPL. 1

ER -

Suzaku observations of tycho's supernova remnant

Abstract

Keywords

ASJC Scopus subject areas

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