Suzaku observation of AXP 1E 1841-045 in SNR Kes 73

M. Morii; S. Kitamoto; N. Shibazaki; D. Takei; N. Kawai; M. Arimoto; M. Ueno; Y. Terada; T. Kohmura; S. Yamauchi

doi:10.1063/1.2900159

Suzaku observation of AXP 1E 1841-045 in SNR Kes 73

M. Morii^*, S. Kitamoto, N. Shibazaki, D. Takei, N. Kawai, M. Arimoto, M. Ueno, Y. Terada, T. Kohmura, S. Yamauchi

^*Corresponding author for this work

Research output: Chapter in Book/Report/Conference proceeding › Conference contribution

2 Citations (Scopus)

Abstract

Anomalous X-ray pulsars (AXPs) are thought to be magnetars, which are neutron stars with ultra strong magnetic field of 10¹⁴-10 ¹⁵G. Their energy spectra below ∼10keV are modeled well by two components consisting of a blackbody (BB) (∼0.4keV) and rather steep power-law (POW) function (photon index ∼2-4). Kuiper et al. (2004) discovered hard X-ray component above ∼10keV from some AXPs. Here, we present the Suzaku observation of the AXP 1E 1841-045 at the center of supernova remnant Kes 73. By this observation, we could analyze the spectrum from 0.4 to 50 keV at the same time. Then, we could test whether the spectral model above was valid or not in this wide energy range. We found that there were residual in the spectral fits when fit by the model of BB + POW. Fits were improved by adding another BB or POW component. But the meaning of each component became ambiguous in the phase-resolved spectroscopy. Alternatively we found that NPEX model fit well for both phase-averaged spectrum and phase-resolved spectra. In this case, the photon indices were constant during all phase, and spectral variation seemed to be very clear. This fact suggests somewhat fundamental meaning for the emission from magnetars.

Original language	English
Title of host publication	40 Years Of Pulsars: Millisecond Pulsars, Magnetars and More
Pages	268-270
Number of pages	3
Volume	983
DOIs	https://doi.org/10.1063/1.2900159
Publication status	Published - 2008
Externally published	Yes
Event	40 Years Of Pulsars: Millisecond Pulsars, Magnetars and More - Montreal, QC Duration: 2007 Aug 12 → 2007 Aug 17

Other

Other	40 Years Of Pulsars: Millisecond Pulsars, Magnetars and More
City	Montreal, QC
Period	07/8/12 → 07/8/17

Keywords

Stars: pulsars: individual (IE 1841-045)
X-rays: individual (IE 1841-045)

ASJC Scopus subject areas

Physics and Astronomy(all)

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10.1063/1.2900159

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Morii, M, Kitamoto, S, Shibazaki, N, Takei, D, Kawai, N, Arimoto, M, Ueno, M, Terada, Y, Kohmura, T & Yamauchi, S 2008, Suzaku observation of AXP 1E 1841-045 in SNR Kes 73. in 40 Years Of Pulsars: Millisecond Pulsars, Magnetars and More. vol. 983, pp. 268-270, 40 Years Of Pulsars: Millisecond Pulsars, Magnetars and More, Montreal, QC, 07/8/12. https://doi.org/10.1063/1.2900159

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title = "Suzaku observation of AXP 1E 1841-045 in SNR Kes 73",

abstract = "Anomalous X-ray pulsars (AXPs) are thought to be magnetars, which are neutron stars with ultra strong magnetic field of 1014-10 15G. Their energy spectra below ∼10keV are modeled well by two components consisting of a blackbody (BB) (∼0.4keV) and rather steep power-law (POW) function (photon index ∼2-4). Kuiper et al. (2004) discovered hard X-ray component above ∼10keV from some AXPs. Here, we present the Suzaku observation of the AXP 1E 1841-045 at the center of supernova remnant Kes 73. By this observation, we could analyze the spectrum from 0.4 to 50 keV at the same time. Then, we could test whether the spectral model above was valid or not in this wide energy range. We found that there were residual in the spectral fits when fit by the model of BB + POW. Fits were improved by adding another BB or POW component. But the meaning of each component became ambiguous in the phase-resolved spectroscopy. Alternatively we found that NPEX model fit well for both phase-averaged spectrum and phase-resolved spectra. In this case, the photon indices were constant during all phase, and spectral variation seemed to be very clear. This fact suggests somewhat fundamental meaning for the emission from magnetars.",

keywords = "Stars: pulsars: individual (IE 1841-045), X-rays: individual (IE 1841-045)",

author = "M. Morii and S. Kitamoto and N. Shibazaki and D. Takei and N. Kawai and M. Arimoto and M. Ueno and Y. Terada and T. Kohmura and S. Yamauchi",

year = "2008",

doi = "10.1063/1.2900159",

language = "English",

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volume = "983",

pages = "268--270",

booktitle = "40 Years Of Pulsars: Millisecond Pulsars, Magnetars and More",

note = "40 Years Of Pulsars: Millisecond Pulsars, Magnetars and More ; Conference date: 12-08-2007 Through 17-08-2007",

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T1 - Suzaku observation of AXP 1E 1841-045 in SNR Kes 73

AU - Morii, M.

AU - Kitamoto, S.

AU - Shibazaki, N.

AU - Takei, D.

AU - Kawai, N.

AU - Arimoto, M.

AU - Ueno, M.

AU - Terada, Y.

AU - Kohmura, T.

AU - Yamauchi, S.

PY - 2008

Y1 - 2008

N2 - Anomalous X-ray pulsars (AXPs) are thought to be magnetars, which are neutron stars with ultra strong magnetic field of 1014-10 15G. Their energy spectra below ∼10keV are modeled well by two components consisting of a blackbody (BB) (∼0.4keV) and rather steep power-law (POW) function (photon index ∼2-4). Kuiper et al. (2004) discovered hard X-ray component above ∼10keV from some AXPs. Here, we present the Suzaku observation of the AXP 1E 1841-045 at the center of supernova remnant Kes 73. By this observation, we could analyze the spectrum from 0.4 to 50 keV at the same time. Then, we could test whether the spectral model above was valid or not in this wide energy range. We found that there were residual in the spectral fits when fit by the model of BB + POW. Fits were improved by adding another BB or POW component. But the meaning of each component became ambiguous in the phase-resolved spectroscopy. Alternatively we found that NPEX model fit well for both phase-averaged spectrum and phase-resolved spectra. In this case, the photon indices were constant during all phase, and spectral variation seemed to be very clear. This fact suggests somewhat fundamental meaning for the emission from magnetars.

AB - Anomalous X-ray pulsars (AXPs) are thought to be magnetars, which are neutron stars with ultra strong magnetic field of 1014-10 15G. Their energy spectra below ∼10keV are modeled well by two components consisting of a blackbody (BB) (∼0.4keV) and rather steep power-law (POW) function (photon index ∼2-4). Kuiper et al. (2004) discovered hard X-ray component above ∼10keV from some AXPs. Here, we present the Suzaku observation of the AXP 1E 1841-045 at the center of supernova remnant Kes 73. By this observation, we could analyze the spectrum from 0.4 to 50 keV at the same time. Then, we could test whether the spectral model above was valid or not in this wide energy range. We found that there were residual in the spectral fits when fit by the model of BB + POW. Fits were improved by adding another BB or POW component. But the meaning of each component became ambiguous in the phase-resolved spectroscopy. Alternatively we found that NPEX model fit well for both phase-averaged spectrum and phase-resolved spectra. In this case, the photon indices were constant during all phase, and spectral variation seemed to be very clear. This fact suggests somewhat fundamental meaning for the emission from magnetars.

KW - Stars: pulsars: individual (IE 1841-045)

KW - X-rays: individual (IE 1841-045)

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BT - 40 Years Of Pulsars: Millisecond Pulsars, Magnetars and More

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Y2 - 12 August 2007 through 17 August 2007

ER -

Suzaku observation of AXP 1E 1841-045 in SNR Kes 73

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