deletions | additions       diff --git a/subsection_Faint_Images_of_the__.tex b/subsection_Faint_Images_of_the__.tex  index 4d966eb..1ba5d93 100644  --- a/subsection_Faint_Images_of_the__.tex  +++ b/subsection_Faint_Images_of_the__.tex 
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FIRST’s high angular resolution and faint flux density threshold (the rms is 0.15 mJy) come at a price. Some of the flux from extended sources is resolved out. This leads to a systematic underestimation of extended source flux density and a survey threshold that is a function of source size  Moreover ,the Moreover, the  higher angular resolution achieved by a more extended antenna configuration comes at a price of lower brightness temperature sensitivity. Brightness temperature ($T_{b}$) is a measure of the source brightness (or specific intensity - referring to frequency) irrespective of the radiation mechanism. specific intensity: $I_{v} = \frac{dE}{dAd \Omega dt dv}$ W.$m^{-2}$.$sr^{-1}$.$Hz^{-1}$ 
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$I_{v} = B_{v}(T_{b})$  where Where  $B_{v}(T)$ is the Planck distribution brightness. The associated sensitivity is then proportional to the ratio of the system sensitivity and the solid angle subtended by the receiver's diffraction pattern. Given that the sensitivity limit of FIRST and our knowledge of radio source populations, we know this survey is dominated by the FR-I and FR-II sources described earlier. That is, radio jets that results from collimated electrons spiraling around magnetic field lines at relativistic speeds following acceleration by a centered SMBH.