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Title:
An X-ray and optical study of the supernova remnant W44
Authors:
Rho, Jeonghee; Petre, R.; Schlegel, Eric M.; Hester, J. Jeff
Affiliation:
AA(NASA. Goddard Space Flight Center, Greenbelt, MD, US), AB(NASA. Goddard Space Flight Center, Greenbelt, MD, US), AC(Arizona State Univ., Tempe, AZ), AD(Arizona State Univ., Tempe, AZ)
Publication:
The Astrophysical Journal, vol. 430, no. 2, pt. 1, p. 757-773 (ApJ Homepage)
Publication Date:
08/1994
Category:
Astrophysics
Origin:
STI
NASA/STI Keywords:
ABUNDANCE, COSMIC X RAYS, EMISSION SPECTRA, INTERSTELLAR MATTER, MOLECULAR CLOUDS, RADIO EMISSION, SHOCK WAVES, SUPERNOVA REMNANTS, ASTRONOMICAL MODELS, PLASMA DENSITY, PLASMA EQUILIBRIUM, SOLAR LIMB, SPECTRUM ANALYSIS, STELLAR TEMPERATURE, X RAY SPECTRA
DOI:
10.1086/174446
Bibliographic Code:
1994ApJ...430..757R

Abstract

We report the results of a 8000 s observation of the supernova remnant W44 using the ROSAT Position Sensitive Proportional Counter (PSPC). The image shows the same centrally peaked morphology observed by the Einstein IPC and contrasts with the shell-like radio morphology. The eastern limb shows a lack of X-ray emission within the radio shell, probably due to the interaction between the Supernova Remnants (SNR) and a molecular cloud. No counterpart to the pulsar 1853 + 01 in W44 has been detected, with LX less than 1.3 x 1032 ergs/s in the 0.2 to 2.4 keV band. The spectral analysis of the central part of W44, combining EXOSAT ME and Einstein SSS data, shows that the shocked plasma has not reached ionization equilibrium. The best nonequilibrium fit to PSPC, ME, and SSS spectra gives Eta = 1051 ergs cm-6, Ts = 107 K with Te = Ti, suggesting conditions are approaching ionization equilibrium. There is no evidence of enhanced abundances of Mg, Si, S, or Fe. The variation of temperature and column density was obtained region by region using the PSPC and Einstein IPC. The temperature is largely uniform over the remnant, but strong column density variations are found to be consistent with molecular clouds in the line of sight. An evaporation model with a two-phase interstellar medium structure of clumps and interclump gas (White & Long 1991) can explain the X-ray centrally peaked morphology of W44. The clumps remaining behind a SN shock provide a reservoir of material, and evaporat e to increase the density of X-ray emitting gas in the interior of a SNR. The uniform temperature distribution of W44 strongly supports the predictions of this model. In addition, mosaiced H alpha and (S II) images of W44, taken using the prime focus universal extragalactic instrument (PFUEI) camera on the Palomar 60 sec telescope, reveal the first discovery of optical filaments (both H alpha and (S II)) in the northwestern and southeastern portion of the remnant, within the X-ray emitting region. The optical filaments and the X-ray image showing locally brighter emission and clumps along the filaments suggest both are produced by the interaction between the supernova shock front and regions of enhanced ambient density.

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