deletions | additions       diff --git a/Abstract.tex b/Abstract.tex  index 43e5548..5afc69e 100644  --- a/Abstract.tex  +++ b/Abstract.tex 
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transients---collectively nicknamed ``Spock''---were faster and  fainter than any supernova, but significantly more luminous than a  classical nova: they reached peak luminosities of $\sim10^{41}$ erg  s$^{-1}$ (M$_{AB}<-14$) in $\lesssim$5 rest-frame days, then faded below detectability in roughly the same time span. Lens models of the foreground cluster suggest that it is entirely plausible that the two  events are {\it spatially} coincident at the source plane, but very  unlikely that they were also {\it temporally} coincident. We find 
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High-cadence monitoring of the field could help to distinguish between  these hypotheses by detecting new transient episodes at or near the  \spock locations. Improvements to the lens models are also needed to  clarify the position of the critical curves. curves, which impacts  magnification estimates and the viability of the microlensing  hypothesis.  \end{abstract}      diff --git a/Acknowledgments.tex b/Acknowledgments.tex  index 436f7a1..d74b2c2 100644  --- a/Acknowledgments.tex  +++ b/Acknowledgments.tex 
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KAKENHI Grant Number 26800093 and 15H05892.  J.R. acknowledges support from the ERC starting grant  336736-CALENDS.  G.C. and  S.H.S. thanks the Max Planck Society for support through the Max Planck Research Group.  T.T. and the GLASS team were funded by NASA through HST grant  HST-GO-13459 from STScI.  diff --git a/Authors.tex b/Authors.tex  index 8fe96ba..3192294 100644  --- a/Authors.tex  +++ b/Authors.tex 
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\newcommand{\TokyoAstro}{Department of Astronomy, Graduate School of Science, The University of Tokyo, 7-3-1 Hongo, Bunkyo-ku, Tokyo 113-0033, Japan}  %\newcommand{\TokyoAstron}{Department of Astronomy, University of Tokyo, Tokyo 113-0033, Japan}  \newcommand{\DARK}{Dark Cosmology Centre, Niels Bohr Institute, University of Copenhagen, Juliane Maries Vej 30, DK-2100 Copenhagen, Denmark}   \newcommand{\Milan}{Dipartimento di Fisica, Universit\`a degli Studi di Milano, via Celoria 16, I-20133 Milano, Italy}  \newcommand{\INFN}{INFN, Sezione di Bologna, Viale Berti Pichat 6/2, I-40127 Bologna, Italy}  \newcommand{\EHU}{Fisika Teorikoa, Zientzia eta Teknologia Fakultatea, Euskal Herriko Unibertsitatea UPV/EHU}  \newcommand{\Basque}{IKERBASQUE, Basque Foundation for Science, Alameda Urquijo, 36-5 48008 Bilbao, Spain} 
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\author{G.~B.~Caminha\altaffilmark{\affilref{Ferrara}}}  \affilreftxt{Ferrara}{\Ferrara}  \author{G.~Chirivi\altaffilmark{\affilref{MPIA}}} \author{G.~Chiriv{\`i}\altaffilmark{\affilref{MPIA}}}  \affilreftxt{MPIA}{\MPIA}  \author{J.~M.~Diego\altaffilmark{\affilref{IFCA}}} 
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\affilreftxt{AMNH}{\AMNH}  \affilreftxt{CfA}{\CfA}  \author{C.~Grillo\altaffilmark{\affilref{DARK}}} \author{C.~Grillo\altaffilmark{\affilref{Milan},\affilref{DARK}}}  \affilreftxt{Milan}{\Milan}  \affilreftxt{DARK}{\DARK}  \author{S.~Hemmati\altaffilmark{\affilref{CalTech}}} 
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\author{L.-G.~Strolger\altaffilmark{\affilref{STScI}}}  \affilreftxt{STScI}{\STScI}  \author{S.-H.~Suyu\altaffilmark{\affilref{MPIA},\affilref{ASIAA},\affilref{Garching}}} \author{S.~H.~Suyu\altaffilmark{\affilref{MPIA},\affilref{ASIAA},\affilref{Garching}}}  \affilreftxt{MPIA}{\MPIA}  \affilreftxt{ASIAA}{\ASIAA}  \affilreftxt{Garching}{\Garching} 
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\affilreftxt{Minnesota}{\Minnesota}  \author{A.~Zitrin\altaffilmark{\affilref{CalTech},\affilref{BenGurion},\affilref{HubbleFellow}}} \author{A.~Zitrin\altaffilmark{\affilref{CalTech},\affilref{BenGurion}}}  \affilreftxt{CalTech}{\CalTech}  \affilreftxt{BenGurion}{\BenGurion}  diff --git a/LensingModels.tex b/LensingModels.tex  index f098614..009e5d6 100644  --- a/LensingModels.tex  +++ b/LensingModels.tex 
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Because of the proximity of the critical curves in all models, the  predicted time delays and magnification factors are significantly  different if calculated at the model-predicted positions instead of  the observed positions. For example, in the GLEE model series (GLEE-A (GLEE  and GLEE-B) GLEE-var)  when switching from the observed to model-predicted positions the arrival order of the NW and SE images flips, the  expected time delay drops from tens of days to $<$1 day, and the  magnifications decrease change  by 40-60\%. 30-60\%.  However, the expected magnifications and time delays between the events still fall within  the broad ranges summarized in Table~\ref{tab:LensModelPredictions}  and shown in Figure~\ref{fig:LensModelContours}. Regardless of  whether the model predictions are extracted at the observed or  predicted positions of the \spock events, none of the lens models can  accommodate the observed 220-day 234-day  time difference as purely a gravitational lensing time delay. 
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and includes only 98 galaxies identified as cluster members. In this  variation the nearby cluster member galaxy is not included, so the  \spocktwo event is not intersected by a critical curve. However, the  \spockone event is approximately coincident witha  the primary critical curve of the \macs0416 cluster. When the critical curve is  close to either \spock location, the magnifications predicted by the  CATS model are driven up to $\mu>100$. However, the time delays  remain small, on the order of tens of days, and incompatible with the  observed 220-day 234-day  gap. The WSLAP-var model evaluates whether the cluster redshift  significantly impacts the positioning of the critical curve. In this 
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the critical curve to intersect either or both of the \spock  locations.  The GLEE-var model is a multi-plane lens model (Chiriv{\`i} et al.~in  prep.)  that incorporates 13 galaxies with spectroscopic redshifts that place them either in the foreground or background of the \macs0416 cluster. Figure~\ref{fig:LineOfSightLenses} marks these 13 galaxies and highlights two of them that appear in the foreground of the \spock host galaxy and are close to the lines of sight to the \spock  transients. Both the foreground $z=0.0557$ galaxy and the  reconstructed position of the $z=0.9397$ galaxy have a projected  separation of $<$4\arcsec from the \spocktwo transient position.  Including these galaxies in the GLEE lensing model has a minor impact  on changes  the magnifications at the location of HFF14Spo-NW (HFF14Spo-SE) to  $\sim-70$ ($\sim250$)  and the  time delays, and delay between the two locations to  $\sim50$ days. The line-of-sight galaxies  also results result  in a shift of the position of the critical curve--as can be seen by comparing the  GLEE-A GLEE  and GLEE-B GLEE-var  models in Figure~\ref{fig:SpockCriticalCurves}. For the  GLEE model, incorporating these line-of-sight effects does not  substantially change the predicted magnifications or time delays, and Nonetheless,  the predicted time delays are still incompatible with the observed gap of 220 234  days between events. The GLAFIC-var model examines whether it is plausible for a critical  curve to intersect both \spock locations---contrary to the baseline  diff --git a/Observations.tex b/Observations.tex  index d7185bf..a9fe71f 100644  --- a/Observations.tex  +++ b/Observations.tex 
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\citep{Grillo:2015,Balestra:2016}. These massively multi-object  observations could potentially have provided confirmation of the  redshift of the \spock host galaxy with separate spectral line  identifications in each of the three host galaxy images. On For  the \macs0416 field this the CLASH-VLT  program collected 1 hr hour  of useful exposure time in good seeing conditions with the Low Resolution Blue grism. Unfortunately, the wavelength range of this grism (3600-6700 \AA) does not include any strong emission lines for a source at z=1.0054, and the signal-to-noise (S/N) was not sufficient to provide any clear line identifications for the three images of the \spock host galaxy. The VLT Multi Unit Spectroscopic Explorer  \citep[MUSE;][]{Henault:2003,Bacon:2012} observed the NE portion of  diff --git a/Results.tex b/Results.tex  index d57b46e..8a1791e 100644  --- a/Results.tex  +++ b/Results.tex 
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magnification) for sources at $z=1$. The location of the critical  curve varies significantly among the models, and is sensitive to many  parameters that are poorly constrained. We have explored model  variations (Methods \ref{sec:LensModelVariations}) that adjust the cluster redshift and the masses of cluster member galaxies, and that account for the impact of lensing perturbations from galaxies along the line of sight. Most Within a given model,  variations that move a critical curve closer to the position of \spockone\ would drive the magnification of that event much higher (toward $\mu_{\rm NW}\sim200$). This generally also has the effect of moving the critical curve farther from \spocktwo, which would necessarily drive its magnification downward (toward $\mu_{\rm SE}\sim10$). Our model variations also show that it is possible to make reasonable adjustments to the lens model parameters in order to ensure that a critical curve intersects both of the \spock locations. Such lensing configurations can qualitatively reproduce the observed morphology of the \spock host galaxy, but they are disfavored by a purely quantitative assessment of the positional strong-lensing constraints. Figure~\ref{fig:LightCurves} shows that the observed peak brightnesses  for the two events agree to within $\sim30\%$, which means that if 
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E_{\rm rad} = \zeta \t2 \Lpk,  \end{equation}  \noindent where $\zeta$ is a dimensionless  factor of order unity that depends on the precise shape of the light curve.\footnote{Note that  \citet{Smith:2011b} used $t_{1.5}$ instead of $t_2$, which amounts  to a different light curve shape term, $\zeta$.} Adopting  \Lpk$\sim10^{41}$ erg s$^{-1}$ and \t2$\sim$2 days \t2$\sim$1 day  (as shown in Figure~\ref{fig:PeakLuminosityDeclineTime}), we find that the total  radiated energy is $E_{\rm rad}\sim10^{46}$ erg. A realistic range  for this estimate would span $10^{44} 
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in some way ``bottled up'' by the stellar envelope, before being  released in a rapid mass ejection. By assuming that the build-up  timescale is comparable to the rest-frame time between the two  observed events, we estimate a quiescent luminosity of $L_{\rm qui}\sim10^{39.5} erg s^{-1}$ qui}\sim10^{39.5}$~erg~s$^{-1}$  ($M_V\sim-10$). This value is fully consistent with the expected range for LBV progenitor stars (e.g.,  \etacar has $M_V\sim-12$ and the faintest known LBV progenitors such  as SN 2010dn have $M_V\sim-6$).  diff --git a/figures/LineOfSightLenses/caption.tex b/figures/LineOfSightLenses/caption.tex  index 8a3ce3c..c3e3972 100644  --- a/figures/LineOfSightLenses/caption.tex  +++ b/figures/LineOfSightLenses/caption.tex 
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cluster redshift (magenta circles) and four galaxies in the cluster  foreground (light blue circles). The inset panel at right zooms in on  the \spock host galaxy (enclosed by the orange ellipse in each panel).  Cluster member galaxies with spectroscopic redshifts that were  included in the GLEE models are marked with black diamonds.  The magenta circle marks a spiral galaxy at $z=0.9397$, which is also strongly lensed by the \macs0416 cluster into three highly distorted  images (System 12 in \citet{Caminha:2017}). This image of the System  12 galaxy is further strongly lensed into arcs around a cluster member  galaxy, which is marked by the black diamond near the center of the  magenta circle.  The galaxy in the foreground of the cluster at $z=0.0557$ is encircled in light blue. Crosses mark the reconstructed source positions (from the GLEE model) for the $z=0.9397$ galaxy and the \spock host. diff --git a/figures/LineOfSightLenses/macs0416_lineofsight_lensing.png b/figures/LineOfSightLenses/macs0416_lineofsight_lensing.png  index c56d129..608fedc 100644  Binary files a/figures/LineOfSightLenses/macs0416_lineofsight_lensing.png and b/figures/LineOfSightLenses/macs0416_lineofsight_lensing.png differ diff --git a/figures/LineOfSightLenses/macs0416_lineofsight_lensing_original.png b/figures/LineOfSightLenses/macs0416_lineofsight_lensing_original.png  deleted file mode 100644  index b5ed595..0000000  Binary files a/figures/LineOfSightLenses/macs0416_lineofsight_lensing_original.png and /dev/null differ diff --git a/figures/detection_image/detection_image.png b/figures/detection_image/detection_image.png  index 1a612e8..da22531 100644  Binary files a/figures/detection_image/detection_image.png and b/figures/detection_image/detection_image.png differ diff --git a/figures/detection_image/detection_image_original.png b/figures/detection_image/detection_image_original.png  deleted file mode 100644  index 6464728..0000000  Binary files a/figures/detection_image/detection_image_original.png and /dev/null differ diff --git a/figures/spock_critical_curves/caption.tex b/figures/spock_critical_curves/caption.tex  index 1465c0d..3bb6e30 100644  --- a/figures/spock_critical_curves/caption.tex  +++ b/figures/spock_critical_curves/caption.tex 
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the two \spock sources. Panel (a) shows the HST Frontier Fields  composite near-infrared image of the full \macs0416 field. The  magnification map from the \citet{Caminha:2017} model is overlaid with  orange and black contours. The white box marks the region that  is shown in panel (b) with a closer view of the \spock host galaxy. Panels b Panel (c)  shows a trace of the lensing critical curve from the GRALE model, and panels d-i (d)-(i)  show magnification maps for the six other primary models, all for a source at the \spock redshift. The magnification maps are plotted with log scaling, such that white is $\mu=1$ and black is $\mu=10^3$. Panels j-m show the same magnification maps, extracted from the lens model variations described in \ref{sec:LensModelVariations}. diff --git a/layout.md b/layout.md  index 7af3af2..a9e04d9 100644  --- a/layout.md  +++ b/layout.md 
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figures/composite_lens_model_contours/composite_lens_model_contours.png  figures/spock_critical_curves/spock_critical_curves.png  figures/LineOfSightLenses/macs0416_lineofsight_lensing.png  figures/spock_predictions/spock_predictions.png  figures/LineOfSightLenses/macs0416_lineofsight_lensing.png  LensingModels.tex  Xray.tex  diff --git a/spock_localbuild.pdf b/spock_localbuild.pdf  index bc16744..9bc94af 100644  Binary files a/spock_localbuild.pdf and b/spock_localbuild.pdf differ