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this expectation of an unchanging color (Methods  \ref{sec:ColorCurves}).  Although the phenomenology of each \spock event is compatible with a  microlensing explanation, when applying this The lensing  scenario that has been most consistently applied  to the MACS0416  field it is still difficult to explain {\it two} events with similar  decay timescales at such distinct locations on the sky. This this  host galaxy \todo{add references}  is primarily because that  a caustic-crossing transient event must appear at  the location of the lensing single  critical curve.   It is possible for such  microlensing transients curve  passes roughly mid-way between the two observed \spock locations.  Each event then belongs  to appear offset from one of two images (11.1 and 11.2) that  comprise  the central spine long arc  of the critical curve, and host galaxy. For  this may in fact be observed in single critical  curve scenario,  the case angular separation  of {\it Icarus}  due $1\farcs8$ between the  \spock events corresponds  to a ``blurring'' physical separation of many tens  of parsecs in the source plane. A star could not traverse that distance  in the $\sim$120 rest-frame days that separate  the two \spock events.  Thus, even with a critical  curve caused smeared out  by the intracluster stars   It is possible to ubstantial clumping of mass along the line effects  ofsight through the lensing cluster (from  the The consensus from our  six lens models is that there is only ICL, it would be impossible for  a single critical curve passing  roughly mid-way between star crossing a single  caustic in  the two observed \spock locations.    The source plane to be responsible for both transients.  Some  lens models could, can,  however, be modified so that instead of just two host images (11.1 and 11.2 in Figure~\ref{fig:Discovery}), the lensed galaxy arc is made up of three or more images of the host, with multiple critical curves subtending the arc where the \spock events  appeared. By tuning the assumed masses of cluster galaxies near the  \spock host, those multiple critical curves can be made to cross very  close to the positions of the two \spock transient events. This In the  {\it Kawamata} and {\it Diego} lens models, this  alternative lensing scenario is disfavored by the fact requires  that the host  galaxy arc is quite smooth. If it were composed masses  ofmore than two  images one would expect to see gaps or bright knots where  the multiple  images two nearest cluster galaxies  are imperfectly joined. Setting aside increased by $30-60\%$. With  this qualitative  incompatibility, even with multiple critical curves near the \spock  events it would still be impossible to have a single star in the  source plane be responsible for adjustment,  both transients. The angular  separation of models can  reproduce  the two \spock events corresponds to a physical  separation observed morphology  ofmany tens of parsecs in  the source plane, and HFF14Spo host galaxy as  a star  could not traverse that distance in smooth, unbroken arc. These model realizations imply magnifications  on  the $\sim$120 rest-frame days that  separate the two order of $\mu\sim1000$ for both  \spock events. Thus, even if multiple critical  curves pass very near transients. If this  lensing scenario is correct, then similar microlensing transients  would be expected to appear at different locations along  the \spock events, a stellar host  galaxy arc, instigated by new  caustic crossing could account for at best only one of episodes from different  stars in  the \spock events, not both. host galaxy.  \subsection{Ruling Out Common Astrophysical Transients}  Since Instead of relying on  lensing effects  aloneis insufficient  to explain the rise and  fall of the  \spock events, we must might instead  invoke some astrophysical transient source in the host galaxy. There are several categories of astrophysical transients that cannot accommodate the light curve characteristics of the \spock transients. We may first dismiss any of the category of {\it periodic} sources (e.g. Cepheids, RR Lyrae, or Mira variables) that exhibit regular changes in flux due to pulsations of the stellar photosphere. These variable stars do not exhibit sharp, isolated transient episodes that could match the \spock light curve shapes. We can also rule out active galactic nuclei (AGN), in which brief transient episodes (a few days in duration) may be observed from X-ray to infrared wavelengths \citep[e.g.][]{Gaskell:2003}, principally due to the quiescence of the \spock sources between the two observed episodes and the absence of any of the broad emission lines that are often (though not always) observed in AGN. Stellar flares provide another very common source for optical transient events, but the total energy released by even the most extreme stellar flare falls far short of the observed energy release from the \spock transients \citep{Balona:2012,Karoff:2016} . Many types of stellar explosions can generate isolated  transient events, and a useful starting point for classification of  diff --git a/spock_localbuild.pdf b/spock_localbuild.pdf  index 2eed736..167cb15 100644  Binary files a/spock_localbuild.pdf and b/spock_localbuild.pdf differ