3 research outputs found
ASCA Observation of the Nearest Gravitational Lensing Cluster Candidate -- A 3408
We observed the nearest gravitational lensing cluster candidate, A 3408
(), with ASCA. The projected mass profile of A 3408 was
determined from the ICM temperature and the -model parameters obtained
with ASCA, assuming that the hot gas is spherically symmetric and in
hydrostatic equilibrium. The projected mass within an arc radius, , of 110 kpc is M(r_{\rm arc})=1.2^{+0.8}_{-0.4} \times10^{13} \MO. This
is 18 -- 45% of the mass previously derived from a lensing analysis by
Campusano et al. (1998, AAA 069.160.189) without any X-ray information.
The primary cause of this discrepancy is in their assumption that the center
of the cluster potential coincides with the position of the brightest cluster
galaxy (BCG), while we reveal the BCG position to be 60 outside of the
X-ray center. We further calculated a model for the source galaxy position and
the gravitational potential that can reproduce both the X-ray data and the arc
image. In this model, the magnification factor of the lens for the source
galaxy was evaluated to be 0.070.03 mag; i.e., the source
galaxy is slightly magnified by the lens cluster A 3408.Comment: 13 pages, 6 figures, to appear in PASJ vol. 5
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