29 research outputs found
ASCA Observation of the Crab-Like Supernova Remnant 3C58
We present here the X-ray observation of a Crab-like supernova remnant (SNR)
3C58 with ASCA. We find that the integrated energy spectrum over the nebula is
consistent with previous results, showing a power-law spectrum with the photon
index modified by interstellar absorption of about
. Inclusion of a blackbody component which is
attributable to the central compact source significantly improves the spectral
fit. Stringent upper limits for any line emitting thin hot plasma are
established. We find for the first time that the nebular spectrum is harder in
the central part of the SNR, becoming softer toward the periphery, while the
absorption column is uniform across the nebula. Correspondingly, the nebular
size decreases with increasing photon energy which is a steeper function of
radius than that of the Crab nebula. The results are compared with synchrotron
energy loss models and the nature of the putative pulsar is discussed. Timing
analysis was performed to search for pulsed X-ray emission from the central
compact source. No significant pulsations are observed, and we present the
upper limit for the pulsed fraction.Comment: 27 pages, 7 figures, to appear in PAS
Discovery of Non Thermal X-Rays from the Northwest Shell of the New SNR RX J1713.7-3946: The Second SN1006 ?
We report ASCA results of a featureless X-ray spectrum from RX J1713.7-3946,
a new shell-like SNR discovered with the ROSAT all sky survey. The northwest
part of RX J1713.7-3946 was in the field of the ASCA Galactic Plane Survey
Project and was found to exhibit a shell-like structure. The spectrum, however
shows neither line emission nor any signature of a thermal origin. Instead, a
power-law model with a photon index of 2.4-2.5 gives reasonable fit to the
spectrum, suggesting a non-thermal origin. Together with the similarity to
SN1006, we propose that RX J1713.7-3946 is the second example, after SN1006, of
a synchrotron X-ray radiation from a shell of SNRs. Since the synchrotron
X-rays suggest existence of extremely high energy charged particles in the SNR
shell, our discovery should have strong impact on the origin of the cosmic
X-rays.Comment: 4 pages, 3 postscript figure
Probable association of T Tauri stars with the L1014 dense core
Using the Wide Field Grism Spectrograph 2 (WFGS2), we have carried out
slit-less spectroscopy, g'r'i' photometry, and slit spectroscopy on the L1014
dense core. We detected three Halpha emission line stars. We interpret one as
weak-line T Tauri star (WTTS) and the others as classical T Tauri stars (CTTS).
Since their g'-i' colors and/or classified spectral types are consistent with
those of T Tauri stars and two of them show less extinction than the cloud,
these three stars are likely to be T Tauri stars associated with L1014.
Adopting an age range for T Tauri stars, 1-10 Myr, the color-magnitude diagram
suggests a distance of ~400-900 pc, rather than the previously assumed
distance, 200 pc. This could strongly affect on the mass estimate of L1014-IRS,
which is thought to be either a very young protostar or proto-brown dwarf.Comment: 5 pages, 5 figures, to be published in Vol.58, No.5, October 25, 200
Early Spectral Evolution of the Rapidly Expanding Type Ia SN 2006X
We present optical spectroscopic and photometric observations of Type Ia
supernova (SN) 2006X from --10 to +91 days after the -band maximum. This SN
exhibits one of the highest expansion velocity ever published for SNe Ia. At
premaximum phases, the spectra show strong and broad features of
intermediate-mass elements such as Si, S, Ca, and Mg, while the O{\sc
i}7773 line is weak. The extremely high velocities of Si{\sc ii} and
S{\sc ii} lines and the weak O{\sc i} line suggest that an intense
nucleosynthesis might take place in the outer layers, favoring a delayed
detonation model. Interestingly, Si{\sc ii}5972 feature is quite
shallow, resulting in an unusually low depth ratio of Si{\sc ii}5972
to 6355, (Si{\sc ii}). The low (Si{\sc ii}) is usually
interpreted as a high photospheric temperature. However, the weak Si{\sc
iii}4560 line suggests a low temperature, in contradiction to the low
(Si{\sc ii}). This could imply that the Si{\sc ii}5972 line
might be contaminated by underlying emission. We propose that (Si{\sc
ii}) may not be a good temperature indicator for rapidly expanding SNe Ia at
premaximum phases.Comment: 20 pages, 7 figures, (Received 2008 August 17; Accepted 2009 April
13
Suzaku and Optical Spectroscopic Observations of SS 433 in the 2006 April Multiwavelength Campaign
We report results of the 2006 April multi-wavelengths campaign of SS 433,
focusing on X-ray data observed with Suzaku at two orbital phases (in- and
out-of- eclipse) and simultaneous optical spectroscopic observations. By
analyzing the Fe25 K_alpha lines originating from the jets, we detect rapid
variability of the Doppler shifts, dz/dt ~ 0.019/0.33 day^-1, which is larger
than those expected from the precession and/or nodding motion. This phenomenon
probably corresponding to "jitter" motions observed for the first time in
X-rays, for which significant variability both in the jet angle and intrinsic
speed is required. From the time lag of optical Doppler curves from those of
X-rays, we estimate the distance of the optical jets from the base to be ~(3-4)
\times 10^14 cm. Based on the radiatively cooling jet model, we determine the
innermost temperature of the jets to be T_0 = 13 +/- 2 keV and 16 +/- 3 keV
(the average of the blue and red jets) for the out-of-eclipse and in-eclipse
phase, respectively, from the line intensity ratio of Fe25 K_alpha and Fe26
K_alpha. While the broad band continuum spectra over the 5--40 keV band in
eclipse is consistent with a multi-temperature bremsstrahlung emission expected
from the jets, and its reflection component from cold matter, the
out-of-eclipse spectrum is harder than the jet emission with the base
temperature determined above, implying the presence of an additional hard
component.Comment: 12 pages, 15 figures, accepted for publication in PAS
Discovery of a new pulsating X-ray source with a 1549.1-s period, AX J183220-0840
A new pulsating X-ray source, AX J183220-0840, with a 1549.1-s period was
discovered at R.A.= 18h32m20s and Dec.=-8d40'30'' (J2000,
uncertainty=0.6degree) during an ASCA observation on the Galactic plane. The
source was observed two times, in 1997 and in 1999. A phase-averaged X-ray flux
of 1.1E-11 ergs cm-2 s-1 and pulsation period of 1549.1+/-0.4 s were
consistently obtained from these two observations. The X-ray spectrum was
represented by a flat absorbed power-law with a photon-index of =~0.8 and an
absorption column density of =~1.3E22 cm-2. Also, a signature of iron K-shell
line emission with a centroid of 6.7 keV and an equivalent width of
approximately 450 eV was detected. From the pulsation period and the iron-line
feature, AX J183220-0840 is likely to be a magnetic white dwarf binary with a
complexly absorbed thermal spectrum with a temperature of about 10 keV.Comment: 13 pages, 4 figures, accepted for publication in ApJ Letter
Expansion Velocity of Ejecta in Tycho's Supernova Remnant Measured by Doppler Broadened X-ray Line Emission
We show that the expansion of ejecta in Tycho's supernova remnant (SNR) is
consistent with a spherically symmetric shell, based on Suzaku measurements of
the Doppler broadened X-ray emission lines. All the strong K_alpha line
emission show broader widths at the center than at the rim, while the centroid
energies are constant across the remnant (except for Ca). This is the pattern
expected for Doppler broadening due to expansion of the SNR ejecta in a
spherical shell. To determine the expansion velocities of the ejecta, we
applied a model for each emission line feature having two Gaussian components
separately representing red- and blue-shifted gas, and inferred the Doppler
velocity difference between these two components directly from the fitted
centroid energy difference. Taking into account the effect of projecting a
three-dimensional shell to the plane of the detector, we derived average
spherical expansion velocities independently for the K_alpha emission of Si, S,
Ar, and Fe, and K_beta of Si. We found that the expansion velocities of Si, S,
and Ar ejecta of 4700+/-100 km/s are distinctly higher than that obtained from
Fe K_alpha emission, 4000+/-300 km/s, which is consistent with segregation of
the Fe in the inner ejecta. Combining the observed ejecta velocities with the
ejecta proper-motion measurements by Chandra, we derived a distance to the
Tycho's SNR of 4+/-1 kpc.Comment: Accepted to Apj, 25 pages, 7 figures, 5 table
Spectroscopic Observations of the WZ Sge-Type Dwarf Nova GW Librae during the 2007 Superoutburst
We carried out an international spectroscopic observation campaign of the
dwarf nova GW Librae (GW Lib) during the 2007 superoutburst. Our observation
period covered the rising phase of the superoutburst, maximum, slowly decaying
phase (plateau), and long fading tail after the rapid decline from the plateau.
The spectral features dramatically changed during the observations. In the
rising phase, only absorption lines of H, H, and H were
present. Around the maximum, the spectrum showed singly-peaked emission lines
of H, He I 5876, He I 6678, He II 4686, and C III/N III as well as
absorption lines of Balmer components and He I. These emission lines
significantly weakened in the latter part of the plateau phase. In the fading
tail, all the Balmer lines and He I 6678 were in emission, as observed in
quiescence. We find that the center of the H emission component was
mostly stable over the whole orbital phase, being consistent with the low
inclination of the system. Comparing with the observational results of WZ Sge
during the 2001 superoutburst, the same type of stars as GW Lib seen with a
high inclination angle, we interpret that the change of the H profile
before the fading tail phase is attributed to a photoionized region formed at
the outer edge of the accretion disk, irradiated from the white dwarf and inner
disk.Comment: 10 pages, 9 figures, accepted for publication in PAS
The Type Ic Hypernova SN 2002ap
Photometric and spectroscopic data of the energetic Type Ic supernova (SN)
2002ap are presented, and the properties of the SN are investigated through
models of its spectral evolution and its light curve. The SN is
spectroscopically similar to the "hypernova" SN 1997ef. However, its kinetic
energy [ erg] and the mass ejected (2.5-5
) are smaller, resulting in a faster-evolving light curve. The SN
synthesized of Ni, and its peak luminosity was
similar to that of normal SNe. Brightness alone should not be used to define a
hypernova, whose defining character, namely very broad spectral features, is
the result of a high kinetic energy. The likely main-sequence mass of the
progenitor star was 20-25 , which is also lower than that of both
hypernovae SNe 1997ef and 1998bw. SN 2002ap appears to lie at the low-energy
and low-mass end of the hypernova sequence as it is known so far. Observations
of the nebular spectrum, which is expected to dominate by summer 2002, are
necessary to confirm these values.Comment: 10 pages, 4 figures, accepted for publication in ApJL, 30 April 2002
(minor changes to match the accepted version, with figures being colored