  We present X-ray, infrared and radio observations of the field centered on
X-ray source 1E 1547.0-5408 in the Galactic Plane. A new Chandra observation of
this source shows it is unresolved at arc-second resolution, and a new XMM
observation shows that its X-ray spectrum is best described by an absorbed
power-law and blackbody model. A comparison of the X-ray flux observed from
this source between 1980 and 2006 reveals that its absorbed 0.5-10 keV X-ray
flux decreased from ~2x10^-12 ergs cm-2 s-1 to ~3x10^-13 ergs cm-2 during this
period. The most recent XMM observation allows us to put a 5 sigma confidence
upper limit of 14% for the 0.5-10 keV peak-to-peak pulsed fraction. A
near-infrared observation of this field shows a source with magnitude Ks =
15.9+/-0.2 near the position of 1E 1547.0-5408, but the implied X-ray to
infrared flux ratio indicates the infrared emission is from an unrelated field
source, allowing us to limit the IR magnitude of 1E 1547.0-5408 to >17.5.
Archival radio observations reveal that 1E 1547.0-5408 sits at the center of a
faint, small (4' diameter) radio shell, G327.24-0.13, which is possibly a
previously unidentified supernova remnant. The X-ray properties of 1E
1547.0-5408 suggest that this source is a magnetar - a young neutron star whose
X-ray emission is powered by the decay of its extremely strong magnetic field.
The spatial coincidence between this source and G327.24-0.13 suggests that 1E
1547.0-5408 is associated with a young supernova remnant, supporting a neutron
star interpretation. Additional observations are needed to confirm the nature
of both 1E 1547.0-5408 and G327.24-0.13, and to determine if these sources are
associated. If so, this pair will be an important addition to the small number
of known associations between magnetars and supernova remnants.
