deletions | additions       diff --git a/Abstract.tex b/Abstract.tex  index 6ead686..2bbb3fe 100644  --- a/Abstract.tex  +++ b/Abstract.tex 
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nicknamed ``Spock''. Both transient episodes were faster and fainter  than any of the broad class of supernova-like transients. They both  rose to a peak absolute optical/ultraviolet luminosity of $M\sim-14$  mag ($10^{41}$ ergs/sec) erg s$^{-1}$)  in only $\sim$3 $\lessim$5  rest-frame days, and then faded away below detectability in roughly the same amount of time. These events appeared in two adjacent arcs of a strongly lensed galaxy that is multiply-imaged into at least 3 distinct images by the gravitational potential of the galaxy cluster \MACS0416 (z=0.396).  Using four five  independent lens models of this cluster, we find it is entirely plausible that the two events are {\it spatially} coincident  on the source plane, but very unlikely that they were also {\it  temporally} coincident. We evaluate several physical models for compare  these events, events to existing  categories of astrophysical transients  and find that none of them can  readily account for all characteristics of  the least disfavored explanation is that  we have observed two distinct outbursts \spock events. The  light curves could be plausibly explained as optical/UV emission from  a neutron star merger (a kilonova), a white dwarf He shell explosion  (a .Ia supernova), eruptive episodes  from a single extraordinary  recurrent luminous blue variable  (LBV), or H explosions from an extremely luminous  nova. Among these,  the nova model is the least disfavored, as it allows for a rapid  recurrence period with little or no intervening variability.  This model would imply that the \spock system has the fastest known recurrence timescale of any nova (3 to 5 months).  Furthermore, if our estimate for the gravitational lensing  magnification is correct, then months) and that  \spock is about 2 orders of magnitude more luminous than an average nova. This then suggests that the \spock system's primary star is a white dwarf very close to the Chandrasekhar mass limit, and that it is drawing mass from the secondary star at an extremely efficient rate ($>10^{-7}$ \Msun yr$^{-1}$), making it a plausible potential  Type Ia Supernova progenitor candidate. We conclude with suggestions forlens  modeling efforts  and observational tests that could help to clarify the nature of this unusual transient. \end{abstract}