TY - JOUR
T1 - A Suzaku observation of the low-ionization fe-line emission from RCW 86
AU - Ueno, Masaru
AU - Sato, Rie
AU - Kataoka, Jun
AU - Bamba, Aya
AU - Harrus, Ilana
AU - Hiraga, Junko
AU - Hughes, John P.
AU - Kilbourne, Caroline A.
AU - Koyama, Katsuji
AU - Kokubun, Motohide
AU - Nakajima, Hiroshi
AU - Ozaki, Masanobu
AU - Petre, Robert
AU - Takahashi, Tadayuki
AU - Tanaka, Takaaki
AU - Tomida, Hiroshi
AU - Yamaguchi, Hiroya
PY - 2007
Y1 - 2007
N2 - The newly operational X-ray satellite Suzaku observed the southwestern quadrant of the supernova remnant RCW 86 in 2006 February to study the nature of the 6.4 keV emission line first detected with the Advanced Satellite for Cosmology and Astronomy (ASCA). The new data confirm the existence of the line, localizing it for the first time; most of the line emission is adjacent and interior to the forward shock, and not at the locus of the continuum hard emission. We also report the first detection of a 7.1 keV line, which we interpret as Kβ emission from low-ionization iron. The Fe K line features are consistent with a non-equilibrium plasma of Fe-rich ejecta with n e t ≲ 109cm-3 s and kTe - 5keV. This combination of low net and high kTe suggests collisionless electron heating in an SNR shock. The Fe Kα line shows evidence for intrinsic broadening, with a width of 47 (34-59) eV (99% error region). The difference in the spatial distributions of the hard continuum above 3 keV and the Fe K line emission supports a synchrotron origin for the hard continuum.
AB - The newly operational X-ray satellite Suzaku observed the southwestern quadrant of the supernova remnant RCW 86 in 2006 February to study the nature of the 6.4 keV emission line first detected with the Advanced Satellite for Cosmology and Astronomy (ASCA). The new data confirm the existence of the line, localizing it for the first time; most of the line emission is adjacent and interior to the forward shock, and not at the locus of the continuum hard emission. We also report the first detection of a 7.1 keV line, which we interpret as Kβ emission from low-ionization iron. The Fe K line features are consistent with a non-equilibrium plasma of Fe-rich ejecta with n e t ≲ 109cm-3 s and kTe - 5keV. This combination of low net and high kTe suggests collisionless electron heating in an SNR shock. The Fe Kα line shows evidence for intrinsic broadening, with a width of 47 (34-59) eV (99% error region). The difference in the spatial distributions of the hard continuum above 3 keV and the Fe K line emission supports a synchrotron origin for the hard continuum.
KW - ISM: individual (RCW 86)
KW - ISM: supernova remnants
KW - Shock waves
KW - X-rays: ISM
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U2 - 10.1093/pasj/59.sp1.s171
DO - 10.1093/pasj/59.sp1.s171
M3 - Article
AN - SCOPUS:34047153266
SN - 0004-6264
VL - 59
SP - S171-S176
JO - Publication of the Astronomical Society of Japan
JF - Publication of the Astronomical Society of Japan
IS - 1 SPEC. ISS.
ER -