66 research outputs found
High Resolution X-ray Spectroscopy of G292.0+1.8/MSH 11-54
We present a preliminary analysis of XMM-Newton observations of the
oxygen-rich supernova remnant G292.0+1.8 (MSH 11-54). Although the spatial
extent of the remnant is 8 arcmin the bright central bar is narrow (1'-2')
resulting in RGS spectra of a high spectral quality. This allows us to
spectroscopically identify a cool, Te = 0.3 keV, and underionized component,
resolve details of the Fe-L complex, and resolve the forbidden and resonant
lines of the O VII triplet. We are also able to constrain the kinematics of the
remnant using Ne IX as observed in the second order spectrum, and O VIII in the
first order spectrum. We do not find evidence for O VII line shifts or Doppler
broadening (sigma_v < 731 km/s), but line broadening of the Ne X Ly-alpha line
seems to be present, corresponding to sigma_v ~ 1500 km/s.Comment: To appear in Proc. of the BeppoSAX Symposium: "The Restless
High-Energy Universe", E.P.J. van den Heuvel, J.J.M. in 't Zand, and R.A.M.J.
Wijers (Eds
High- and low energy nonthermal X-ray emission from the cluster of galaxies A 2199
We report the detection of both soft and hard excess X-ray emission in the
cluster of galaxies A 2199, based upon spatially resolved spectroscopy with
data from the BeppoSAX, EUVE and ROSAT missions. The excess emission is visible
at radii larger than 300 kpc and increases in strength relative to the
isothermal component. The total 0.1-100 keV luminosity of this component is 15
% of the cluster luminosity, but it dominates the cluster luminosity at high
and low energies. We argue that the most plausible interpretation of the excess
emission is an inverse Compton interaction between the cosmic microwave
background and relativistic electrons in the cluster. The observed spatial
distribution of the non-thermal component implies that there is a large halo of
cosmic ray electrons between 0.5-1.5 Mpc surrounding the cluster core. The
prominent existence of this component has cosmological implications, as it is
significantly changing our picture of a clusters's particle acceleration
history, dynamics between the thermal and relativistic media, and total mass
budgets.Comment: Accepted for publication in Astrophysical Journal, Letter
- …