accepted manuscript

lkreidberg · Oct 6, 2015 · 98765ff · 98765ff
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 where $f$ is the true anomaly.  The true anomaly is calculated with the algorithm provided by Murray \& Correia in Chapter 1 of \cite{seager10}. For circular orbits, we adopt the convention $f = \pi/2$.
 
-\texttt{batman} provides utilities to calculate the time of periastron, time of inferior conjunction, and the secondary eclipse time from the other transit parameters, using the method described in \S 3.1 of \cite{eastman13}.  Note however that ``batman`` does not correct for the effects of light travel time.
+\texttt{batman} provides utilities to calculate the time of periastron, time of inferior conjunction, and the secondary eclipse time from the other transit parameters, using the method described in \S 3.1 of \cite{eastman13}.  Note however that \texttt{batman} does not correct for the effects of light travel time.
 
 An additional utility is light curve supersampling, which allows the user to calculate the average value of the light curve over a specified number of evenly spaced points during an exposure.