  We present an XMM-Newton observation of the massive edge-on Sb galaxy NGC
2613. We discover that this galaxy contains a deeply embedded active nucleus
with a 0.3-10 keV luminosity of 3.3x10^40 erg/s and a line-of-sight absorption
column of 1.2x10^23 cm^-2. Within the 25 mag/arcsec^2 optical B-band isophote
of the galaxy, we detect an additional 4 sources with an accumulated luminosity
of 4.3x10^39 erg/s. The bulk of the unresolved X-ray emission spatially follows
the near-infrared (NIR) K-band surface brightness distribution; the luminosity
ratio L_X/L_K ~ 8x10^-4 is consistent with that inferred from galactic discrete
sources. This X-ray-NIR association and the compatibility of the X-ray spectral
fit with the expected spectrum of a population of discrete sources suggest that
low-mass X-ray binaries (LMXBs) are the most likely emitters of the unresolved
emission in the disk region. The remaining unresolved emission is primarily due
to extraplanar hot gas. The luminosity of this gas is at least a factor of 10
less than that predicted by recent simulations of intergalactic gas accretion
by such a massive galaxy with a circular rotation speed V_c ~ 304 km/s^2 (Toft
et al. 2002). Instead, we find that the extraplanar hot gas most likely
represents discrete extensions away from the disk, including two
``bubble-like'' features on either side of the nucleus. These extensions appear
to correlate with radio continuum emission and, energetically, can be easily
explained by outflows from the galactic disk.
