521 research outputs found
Chandra Observations of the Northeastern Rim of the Cygnus Loop
We present results from spatially resolved spectral analyses of the
northeastern (NE) rim of the Cygnus Loop supernova remnant (SNR) based on two
Chandra observations. One pointing includes northern outermost
abundance-enhanced regions discovered by recent Suzaku observations, while the
other pointing is located on regions with "normal" abundances in the NE rim of
the Cygnus Loop. The superior spatial resolving power of Chandra allows us to
reveal that the abundance-enhanced region is concentrated in an about
200"-thickness region behind the shock front. We confirm absolute metal
abundances (i.e., relative to H) as well as abundance ratios between metals are
consistent with those of the solar values within a factor of about 2. Also, we
find that the emission measure in the region gradually decreases toward the
shock front. These features are in contrast with those of the ejecta fragments
around the Vela SNR, which leads us to believe that the abundance enhancements
are not likely due to metal-rich ejecta. We suggest that the origin of the
plasma in this region is the interstellar medium (ISM). In the "normal"
abundance regions, we confirm that abundances are depleted to the solar values
by a factor of about 5 that is not expected in the ISM around the Cygnus Loop.
Introduction of non-thermal emission in our model fitting can not naturally
resolve the abundance-depletion problem. The origin of the depletion still
remains as an open question.Comment: 18 pages, 6 figure
First Detection of Ar-K Line Emission from the Cygnus Loop
We observed the Cygnus Loop with XMM-Newton (9 pointings) and Suzaku (32
pointings) between 2002 and 2008. The total effective exposure time is 670.2
ks. By using all of the available data, we intended to improve a
signal-to-noise ratio of the spectrum. Accordingly, the accumulated spectra
obtained by the XIS and the EPIC show some line features around 3 keV that are
attributed to the S He and Ar He lines, respectively. Since the
Cygnus Loop is an evolved (10,000 yr) supernova remnant whose temperature
is relatively low (1 keV) compared with other young remnants, its spectrum
is generally faint above 3.0 keV, no emission lines, such as the Ar-K line have
ever been detected. The detection of the Ar-K line is the first time and we
found that its abundance is significantly higher than that of the solar value;
9.0 and 8.4 (in units of solar), estimated from
the XIS and the EPIC spectra, respectively. We conclude that the Ar-K line
originated from the ejecta of the Cygnus Loop. Follow-up X-ray observations to
tightly constrain the abundances of Ar-rich ejecta will be useful to accurately
estimate the progenitor's mass.Comment: 12 pages, 9 figures, accepted for publication in PAS
Suzaku Spectroscopy of Vela Shrapnel B
We present the X-ray observation of Vela shrapnel B with the XIS on board the
Suzaku satellite. The shrapnel is one of several ejecta fragment-like features
protruding beyond the primary blast wave shock front of the Vela supernova
remnant. The spectrum of shrapnel B is well-represented by a single-temperature
thin-thermal plasma in a non-equilibrium ionization state. The elemental
abundances of O, Ne, and Mg are found to be significantly higher than the solar
values, supporting that shrapnel B originates from supernova ejecta. The
abundances of O, Ne, and Mg relative to Fe are enhanced above their solar
values, while that of Si relative to Fe are at their solar values. This
abundance pattern is similar to that in shrapnel D, except that the
enhancements of the lighter elements are less prominent, suggesting more
extensive mixing with the interstellar medium (ISM) in shrapnel B. The
contribution of the ISM is considered to be larger at the trailing region,
because the absolute abundances of some elements there are depleted relative to
those at the shrapnel's head.Comment: accepted for publication in ApJ, 7 pages, 5 figure
Spatially Resolved X-ray Spectroscopy of Vela Shrapnel A
We present the detailed X-ray spectroscopy of Vela shrapnel A with the
XMM-Newton satellite. Vela shrapnel A is one of several protrusions identified
as bullets from Vela supernova explosion. The XMM-Newton image shows that
shrapnel A consists of a bright knot and a faint trailing wake. We extracted
spectra from various regions, finding a prominent Si Ly emission line
in all the spectra. All the spectra are well represented by the non-equilibrium
ionization (NEI) model. The abundances are estimated to be O0.3,
Ne0.9, Mg0.8, Si3, Fe0.8 times their solar values. The
non-solar abundance ratio between O and Si indicates that shrapnel A originates
from a deep layer of a progenitor star. We found that the relative abundances
between heavy elements are almost uniform in shrapnel A, which suggests that
the ejecta from supernova explosion are well mixed with swept-up interstellar
medium.Comment: 11 pages, 10 figures, ApJ 10 May 2006, v642 2 issu
First Detection of X-Ray Line Emission from Type IIn Supernova 1978K with XMM-Newton's RGS
We report on robust measurements of elemental abundances of the Type IIn
supernova SN 1978K, based on the high-resolution X-ray spectrum obtained with
the Reflection Grating Spectrometer (RGS) onboard XMM-Newton. The RGS clearly
resolves a number of emission lines, including N Ly, O Ly, O
Ly, Fe XVII, Fe XVIII, Ne He and Ne Ly for the first
time from SN 1978K. The X-ray spectrum can be represented by an absorbed,
two-temperature thermal emission model, with temperatures of keV
and keV. The elemental abundances are obtained to be N
, O , Ne , Fe
times the solar values. The low metal abundances except
for N show that the X-ray emitting plasma originates from the circumstellar
medium blown by the progenitor star. The abundances of N and O are far from
CNO-equilibrium abundances expected for the surface composition of a luminous
blue variable, and resemble the H-rich envelope of less-massive stars with
masses of 10-25 M. Together with other peculiar properties of SN 1978K,
i.e., a low expansion velocity of 500-1000 km s and SN IIn-like optical
spectra, we propose that SN 1978K is a result of either an electron-capture SN
from a super asymptotic giant branch star, or a weak Fe core-collapse explosion
of a relatively low-mass (10 M) or high-mass (20-25
M) red supergiant star. However, these scenarios can not naturally
explain the high mass-loss rate of the order of over 1000 yr before the explosion, which is
inferred by this work as well as many other earlier studies. Further
theoretical studies are required to explain the high mass-loss rates at the
final evolutionary stages of massive stars.Comment: 10 pages, 6 figures, accepted for publication in PAS
The Slow X-Ray Expansion of the Northwestern Rim of the Supernova Remnant RX J0852.0-4622
The detection of radioactive decay line of 44Ti provides a unique evidence
that the gamma-ray source is a young (< 1,000 yr) supernova remnant because of
its short lifetime of about 90 yr. Only two Galactic remnants, Cassiopeia A and
RX J0852.0-4622, are hitherto reported to be the 44Ti line emitter, although
the detection from the latter has been debated. Here we report on an expansion
measurement of the northwestern rim of RX J0852.0-4622 obtained with X-ray
observations separated by 6.5 yr. The expansion rate is derived to be
0.023+/-0.006% that is about five times lower than those of young historical
remnants. Such a slow expansion suggests that RX J0852.0-4622 is not a young
remnant as has been expected. We estimate the age of 1,700-4,300 yr of this
remnant depending on its evolutionary stage. Assuming a high shock speed of
about 3000 km/sec, which is suggested by the detection of non-thermal X-ray
radiation, the distance of about 750 pc to this remnant is also derived.Comment: 12 pages, 3 figures, Accepted for publication in the Astrophysical
Journal Letter
Performance of the Charge Injection Capability of Suzaku XIS
A charge injection technique is applied to the X-ray CCD camera, XIS (X-ray
Imaging Spectrometer) onboard Suzaku. The charge transfer inefficiency (CTI) in
each CCD column (vertical transfer channel) is measured by the injection of
charge packets into a transfer channel and subsequent readout. This paper
reports the performances of the charge injection capability based on the ground
experiments using a radiation damaged device, and in-orbit measurements of the
XIS. The ground experiments show that charges are stably injected with the
dispersion of 91eV in FWHM in a specific column for the charges equivalent to
the X-ray energy of 5.1keV. This dispersion width is significantly smaller than
that of the X-ray events of 113eV (FWHM) at approximately the same energy. The
amount of charge loss during transfer in a specific column, which is measured
with the charge injection capability, is consistent with that measured with the
calibration source. These results indicate that the charge injection technique
can accurately measure column-dependent charge losses rather than the
calibration sources. The column-to-column CTI correction to the calibration
source spectra significantly reduces the line widths compared to those with a
column-averaged CTI correction (from 193eV to 173eV in FWHM on an average at
the time of one year after the launch). In addition, this method significantly
reduces the low energy tail in the line profile of the calibration source
spectrum.Comment: Paper contains 18 figures and 15 tables. Accepted for publication in
PAS
Abundance Inhomogeneity in the Northeastern Rim of the Cygnus Loop Revealed by Suzaku Observatory
We present the results of a spatially resolved spectral analysis from four
Suzaku observations covering the northeastern rim of the Cygnus Loop. A
two-kT_e non-ionization equilibrium (NEI) model fairly well represents our
data, which confirms the NEI condition of the plasma there. The metal
abundances are depleted relative to the solar values almost everywhere in our
field of view. We find abundance inhomogeneities across the field: the
northernmost region (Region A) has enhanced absolute abundances compared with
other regions. In addition, the relative abundances of Mg/O and Fe/O in Region
A are lower than the solar values, while those in the other regions are twice
higher than the solar values. As far as we are concerned, neither a
circumstellar medium, fragments of ejecta, nor abundance inhomogeneities of the
local interstellar medium around the Cygnus Loop can explain the relatively
enhanced abundance in Region A. This point is left as an open question for
future work.Comment: 13 pages, 6 figure
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