290 research outputs found
Metal Rich Plasma at the Center Portion of the Cygnus Loop
We observed the center portion of the Cygnus Loop supernova remnant with the
ASCA observatory. The X-ray spectrum of the center portion was significantly
different from that obtained at the North-East (NE) limb. The emission lines
from Si and S were quite strong while those of O and the continuum emission
were similar to those obtained at the NE limb. Based on the spectral analysis,
Si and S emission lines originated from a high-kTe and low ionization plasma
whereas O and most of the continuum emission arose from a low-kTe and high
ionization plasma. We suppose that Si and S emitting gas are present at the
interior of the Loop while O lines and continuum emission mainly arise from the
shell region. Therefore, we subtracted the spectrum of the NE limb from that of
the center. Obtained abundances of Si, S, and Fe were 4 1, 6 2, and
times higher than those of the cosmic abundances,
respectively, and are 40 times richer than those obtained at the NE limb.
These facts strongly support that some of the crude ejecta must be left at the
center portion of the Cygnus Loop. The low abundance of Fe relative to Si and S
suggests a type II SN with a massive progenitor star as the origin of the
Cygnus Loop.Comment: Accepted for Publications of the Astronomical Society of Japan, 40
pages, 12 Postscript figures, uses PASJ95.sty, PASJadd.sty, and psbox.st
The Earliest Optical Observations of GRB 030329
We present the earliest optical imaging observations of GRB 030329 related to
SN 2003dh. The burst was detected by the HETE-2 satellite at 2003 March 29,
11:37:14.67 UT. Our wide-field monitoring started 97 minutes before the trigger
and the burst position was continuously observed. We found no precursor or
contemporaneous flare brighter than () in 32 s (64 s) timescale
between 10:00 and 13:00 UT. Follow-up time series photometries started at
12:51:39 UT (75 s after position notice through the GCN) and continued for more
than 5 hours. The afterglow was at min after burst.
Its fading between 1.2 and 6.3 hours is well characterized by a single
power-law of the form in -band. No significant flux variation was
detected and upper limits are derived as % in
minutes to hours timescales and % in seconds to
minutes timescales. Such a featureless lightcurve is explained by the smooth
distribution of circumburst medium. Another explanation is that the optical
band was above the synchrotron cooling frequency where emergent flux is
insensitive to the ambient density contrasts. Extrapolation of the afterglow
lightcurve to the burst epoch excludes the presence of an additional flare
component at minutes as seen in GRB 990123 and GRB 021211.Comment: ApJL, in pres
High spatial resolution hard X-ray microscope using X-ray refractive lens and phase contrast imaging experiments
A high spatial resolution X-ray microscope was constructed using an X-ray refractive lens as an objective. The spatial resolution was tested using 18 keV X-ray. A 0.4 mm line and 0.4 mm space tantalum test pattern was successfully resolved. Using the similar setup with the addition of a phase plate, a Zernike type phase-contrast microscopy experiment was carried out for the phase retrieval of the samples. Two-dimensional phase-contrast images were successfully taken for the ïŹrst time in the hard X-ray region. Images of a gold mesh sample were analyzed and the validity of this method was indicated. An improvement of the lens, however, is required for the precise phase retrieval of the samples. # 2001 Elsevier Science B.V. All rights reserved
Wide band X-ray Imager (WXI) and Soft Gamma-ray Detector (SGD) for the NeXT Mission
The NeXT mission has been proposed to study high-energy non-thermal phenomena
in the universe. The high-energy response of the super mirror will enable us to
perform the first sensitive imaging observations up to 80 keV. The focal plane
detector, which combines a fully depleted X-ray CCD and a pixellated CdTe
detector, will provide spectra and images in the wide energy range from 0.5 keV
to 80 keV. In the soft gamma-ray band up to ~1 MeV, a narrow field-of-view
Compton gamma-ray telescope utilizing several tens of layers of thin Si or CdTe
detector will provide precise spectra with much higher sensitivity than present
instruments. The continuum sensitivity will reach several times 10^(-8)
photons/s/keV/cm^(2) in the hard X-ray region and a few times10^(-7)
photons/s/keV/cm^(2) in the soft gamma-ray region.Comment: 12 pages, 13 figures, to be published in the SPIE proceedings 5488,
typo corrected in sec.
Development of achromatic full-field hard X-ray microscopy and its application to X-ray absorption near edge structure spectromicroscopy
S. Matsuyama, Y. Emi, H. Kino, Y. Kohmura, M. Yabashi, T. Ishikawa, and K. Yamauchi "Development of achromatic full-field hard x-ray microscopy and its application to x-ray absorption near edge structure spectromicroscopy", Proc. SPIE 9207, Advances in X-Ray/EUV Optics and Components IX, 92070Q (5 September 2014); https://doi.org/10.1117/12.2060783
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