  We present a detailed analysis of XMM archival data of two Ultraluminous
X-ray Sources (ULXs) in the nearby spiral galaxy NGC 1313: NGC 1313 X-1 and
X-2. The spectral continuum of these sources was modeled with a soft thermal
component plus a power-law. If the soft component originates from an accretion
disk, the inferred mass of the compact remnant is > 100 M_sun, making it an
Intermediate Mass Black Hole (IMBH). A detailed analysis of the residuals of
the XMM EPIC-pn spectrum shows some evidence for the presence of an Oxygen
emission line in NGC 1313 X-1. The simultaneous presence of an excess in
emission, although at a much reduced significance level, at different energies
in the X-ray spectra of NGC 1313 X-1 and X-2 is suggestive of typical emission
lines from young supernova remnants. An optical counterpart for NGC 1313 X-2
was also identified. On an ESO 3.6 m image, the Chandra error box embraces a R
\~ 23 mag stellar-like object and excludes a previously proposed optical
counterpart.
