312 research outputs found
An X-Ray Detection Possibility of Star-Formation-Bursting Proto-Elliptical Galaxies
A possibility to detect X-rays from star-formation burst activities in
proto-elliptical galaxies is considered. The X-ray flux of an emission due to
inverse Compton scattering of the cosmic microwave background (CMB) by high
energy electrons accelerated in SNRs is shown to increase as z increases far
beyond unity, since the local CMB flux largely increases in association with a
z-increase. The flux is estimated for the case of a very high rate of type II
supernovae at an initial star formation burst of a proto-elliptical galaxy and
is found to be detectable with a future large X-ray telescope such as intended
in the XEUS mission.Comment: 4 pages, 1 figure, will appear in PAS
Metallicity of the Fossil Group NGC 1550 Observed with Suzaku
We studied the temperature and metal abundance distributions of the
intra-cluster medium (ICM) in a group of galaxies NGC 1550 observed with
Suzaku. The NGC 1550 is classified as a fossil group, which have few bright
member galaxies except for the central galaxy. Thus, such a type of galaxy is
important to investigate how the metals are enriched to the ICM. With the
Suzaku XIS instruments, we directly measured not only Si, S, and Fe lines but
also O and Mg lines and obtained those abundances to an outer region of ~0.5
r_180 for the first time, and confirmed that the metals in the ICM of such a
fossil group are indeed extending to a large radius. We found steeper gradients
for Mg, Si, S, and Fe abundances, while O showed almost flat abundance
distribution. Abundance ratios of alpha-elements to Fe were similar to those of
the other groups and poor clusters. We calculated the number ratio of type II
to type Ia supernovae for the ICM enrichment to be 2.9 +- 0.5 within 0.1 r_180,
and the value was consistent with those for the other groups and poor clusters
observed with Suzaku. We also calculated metal mass-to-light ratios (MLRs) for
Fe, O and Mg with B-band and K-band luminosities of the member galaxies of NGC
1550. The derived MLRs were comparable to those of NGC 5044 group in the r<0.1
r_180 region, while those of NGC 1550 are slightly higher than those of NGC
5044 in the outer region.Comment: 11 pages, 7 figures, accepted for publication in PAS
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