We present an analysis of data from both the Röntgen Satellite ( ROSAT ) , and the Advanced Satellite for Cosmology and Astrophysics ( ASCA ) of the supernova remnant ( SNR ) G18.95 - 1.1 .
We find that the X-ray emission from G18.95 - 1.1 is predominantly thermal , heavily absorbed with a column density around 10 ^ { 22 } atoms cm ^ { -2 } and can be best described by an NEI ( nonequilibrium ionization ) model with a temperature around 0.9 keV , and an ionization timescale of 1.1 \times 10 ^ { 10 } cm ^ { -3 } s ^ { -1 } .
We find only marginal evidence for non-solar abundances .
Comparisons between 21 cm HI absorption data and derived parameters from our spectral analysis strongly suggest a relatively near-by remnant ( a distance of about 2 kpc ) .

Above 4 keV , we identify a small region of emission located at the tip of the central , flat spectrum bar-like feature in the radio image .
We examine two possibilities for this emission region : a temperature variation within the remnant or a pulsar wind nebula ( PWN ) .
The current data do not allow us to distinguish between these possible explanations .
In the scenario where this high-energy emission region corresponds to a PWN , our analysis suggests a rotational loss rate for the unseen pulsar of about 7 \times 10 ^ { 35 } erg s ^ { -1 } and a ratio L _ { r } / L _ { x } about 3.6 for the entire PWN , slightly above the maximum ratio ( 3.4 for Vela ) measured in known PWN .