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 3.3 \times 10 ^ { 40 } { ~ { } ergs~ { } s ^ { -1 } } and a line-of-sight absorption column of 1.2 \times 10 ^ { 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 4.3 \times 10 ^ { 39 } { ~ { } ergs~ { } s ^ { -1 } } .
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 } \sim 8 \times 10 ^ { -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 } \sim 304 { ~ { } km~ { } s ^ { -1 } } ( 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 .