deletions | additions       diff --git a/HostGalaxy.tex b/HostGalaxy.tex  index 0578af9..757af07 100644  --- a/HostGalaxy.tex  +++ b/HostGalaxy.tex 
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together, these color and age gradients suggest that the two  transients are not coincident with the center of their host galaxy.  \input{muse_linefits}  In addition to the \HST imaging data, we also have spatially resolved  spectroscopy from the MUSE integral field data. The only significant  spectral line feature for the \spock host is the \ionline{O}{[ii]} \forbidden{O}{ii}  ($\lambda\lambda$ 3727, 3729) doublet, observed at 7474 and 7478  \AA. Figure~\ref{fig:MUSEOIISequence} shows the observed  \ionline{O}{[ii]} \forbidden{O}{ii}  lines at 10 positions along the length of the arc, which comprises images 11.1 and 11.2.At each position the lines were  extracted using apertures with a radius of 0\farcs6, so adjacent  extractions are not independent, but extractions at the two \spock  locations have no overlap.  Each extraction has been normalized to show a peak line flux at unity, so that the line profiles and the doublet line ratios may be more easily compared. At  each position the lines were extracted using apertures with a radius  of 0\farcs6, so adjacent extractions are not independent, although the  two extractions centered on the \spockone and -SE positions have no  overlap.  From each extracted 1-D spectrum the integrated line flux, observed  wavelength of line center ($\lambda_{\rm center}$), and full width at  half maximum (FWHM) were found by fitting a Gaussian profile to each  component of the doublet.  Properties derived from these line fits are reported in Table~\ref{tab:MuseLineFits}. The \ionline{O}{[ii]} \forbidden{O}{ii}  lines do not exhibit any discernible gradient across the host galaxy images in terms of the wavelength of line centers, full width at half maximum, or the intensity ratio of the two components of the doublet. Thus, the \ionline{O}{[ii]} \forbidden{O}{ii}  measurements from MUSE cannot be used to distinguish either \spock location from the other, or to definitively  answer whether either position is coincident with the center of the  host galaxy. We conclude that it is plausible but not certain that  the two \spock events arose from the same physical location in the  host galaxy.  \input{muse_linefits}  diff --git a/LensingModels.tex b/LensingModels.tex  index ca07836..75ad810 100644  --- a/LensingModels.tex  +++ b/LensingModels.tex 
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light-traces-mass assumption and parameterizes cluster and galaxy components  using pseudo-isothermal elliptical mass distribution (PIEMD) density profiles  \citep{Eliasdottir:2007, Limousin:2007}.  \item{\it GLAFIC:} The model of \citet{Kawamata:2016}, built using the {\tt GLAFIC}\footnote{\url{http://www.slac.stanford.edu/~oguri/glafic/}}  software \citep{Oguri:2010b} with strong-lensing constraints. This  model assumes simply parametrized mass distributions, and model  diff --git a/Observations.tex b/Observations.tex  index 58bf36e..d7185bf 100644  --- a/Observations.tex  +++ b/Observations.tex 
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transient source itself (as we will see below, it had already faded  back to its quiescent state by that time). However, it did provide an  unambiguous redshift for the host galaxy of $z=1.0054\pm0.0002$ from  \Ha\ and the \ionline{O}{[ii]} \forbidden{O}{ii}  doublet in data from the NIR and VIS arms, respectively. These line identifications are consistent with  two measures of the photometric redshift of the host: $z=1.00\pm0.02$  from the BPZ algorithm \citep{Benitez:2000}, and $z=0.92\pm0.05$ from 
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December, 2014 for 2 hours of integration time (ESO program  094.A-0115, PI: J.\,Richard). These observations also confirmed the  redshift of the host galaxy with clear detection of the  \ionline{O}{[ii]} \forbidden{O}{ii}  doublet. Importantly, since MUSE is an integral field spectrograph, these observations also provided a confirmation of  the redshift of the third image of the host galaxy, 11.3, with a  matching \ionline{O}{[ii]} \forbidden{O}{ii}  line at the same wavelength (\citealt{Caminha:2017}, Richard et al. in prep).  A final source of spectroscopic information relevant to \spock is the  diff --git a/Results.tex b/Results.tex  index 600bea7..5c4d8f0 100644  --- a/Results.tex  +++ b/Results.tex 
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consistent with each other, and if both events are representative of a  single system (or a homogeneous class) then the most likely peak  luminosity and decline time (the region with the most overlap) would  be $L_{\rm pk}\sim10^{41}$ ergs/s erg s$^{-1}$  and $t_2\sim1$ day. As shown in Figure~\ref{fig:PeakLuminosityDeclineTime}, the relatively  low peak luminosities and the very rapid rise and fall of both \spock  diff --git a/Summary.tex b/Summary.tex  index 51f2fe0..fc48b36 100644  --- a/Summary.tex  +++ b/Summary.tex 
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of $\pm60$ days or less in the observer frame.}  \item{\label{obs:timescale} Each event lasted for $<$15 rest-frame days\label{itm:FastLC}}  \item{\label{obs:luminosity} After correcting for lensing magnification of $\mu\sim30$, both  events reach a peak luminosity of $\sim10^{41}$ ergs erg  s$^{-1}$ \textcolor{red}{(NEED TO REFINE THIS NUMBER)}}  \item{\label{obs:xray} \textcolor{red}{ADD IN X-RAY AND GAMMA RAY CONSTRAINTS}}  \end{enumerate}  diff --git a/Xray.tex b/Xray.tex  index f440ff3..bc1ffa1 100644  --- a/Xray.tex  +++ b/Xray.tex 
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The \MACS0416 field was observed by the SWIFT X-Ray Telescope (XRT) and  UltraViolet/Optical Telescope (UVOT) in April 2013. No source was  detected near the locations of the \spock events (N. Gehrels, private  communication). The field was also observed by the Chandra X-ray x-ray  space telescope with the ACIS-I instrument for three separate  programs. On June 7, 2009 it was observed for GO program 10800770  (PI: H.\,Ebeling). It was revisited for GTO program 15800052 (PI:  diff --git a/header.tex b/header.tex  index fb75291..ffb39e5 100644  --- a/header.tex  +++ b/header.tex 
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\def\Rv{\mbox{$R_V$}\xspace}  \def\Ha{\mbox{H$\alpha$}\xspace}  \newcommand\ionline[2]{#1{\scshape{#2}}}  \newcommand\forbidden[2]{[#1{\scshape{#2}}]}  \newcommand{\isotope}[2]{${}^{#1}$#2}  % Supernovae :   diff --git a/muse_linefits.tex b/muse_linefits.tex  index 0bebfe7..35296e3 100644  --- a/muse_linefits.tex  +++ b/muse_linefits.tex 
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\begin{deluxetable*}{rllc ccc ccc c}  \tablewidth{\linewidth}  \tablecolumns{12}  \tablecaption{Measurements of the \ionline{O}{[ii]} \forbidden{O}{ii}  $\lambda\lambda$3626,3629 lines from \spock host galaxy images 11.1 and 11.2\tablenotemark{a}} 11.2}%\tablenotemark{a}}  \tablehead{ \colhead{Aperture} & \colhead{R.A.} & \colhead{Dec.} & \colhead{distance to} & \multicolumn{3}{c}{\ionline{O}{[ii]} \multicolumn{3}{c}{\forbidden{O}{ii}  $\lambda$3726} & \multicolumn{3}{c}{\ionline{O}{[ii]} \multicolumn{3}{c}{\forbidden{O}{ii}  $\lambda$3729} & \colhead{Line}\\ \colhead{ID} & \colhead{J2000} & \colhead{J2000} & \colhead{\spocktwo} & \colhead{Flux} & \colhead{$\lambda_{\rm center}$} & \colhead{FWHM} &  \colhead{Flux} & \colhead{$\lambda_{\rm center}$} & \colhead{FWHM} & \colhead{Ratio}\\  & \colhead{(degrees)} & \colhead{(degrees)} & \colhead{(Arcsec)} & \colhead{(erg\,s$^{-1}$\,cm$^{-2}$)} & \colhead{(\AA)} & \colhead{(\AA)} & 
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8 & 64.038352 & -24.069752 & 2.92 & 4.70e-18 & 7472.54 & 3.54 & 6.22e-18 & 7478.16 & 2.95 & 1.32\\  9 & 64.038229 & -24.069648 & 3.50 & 3.26e-18 & 7472.83 & 2.80 & 5.79e-18 & 7478.16 & 2.84 & 1.77\\  10 & 64.038076 & -24.069532 & 4.19 & 2.44e-18 & 7473.01 & 2.57 & 3.22e-18 & 7478.10 & 2.73 & 1.32\\  Spo-1 NW  & 64.038565 & -24.069939 & 1.90 & 4.30e-18 & 7472.55 & 3.13 & 5.49e-18 & 7478.01 & 2.89 & 1.28\\ Spo-2 SE  & 64.038998 & -24.070241 & 0.00 & 4.37e-18 & 7472.46 & 4.00 & 6.10e-18 & 7478.22 & 3.79 & 1.40\\ \enddata  \tablenote{Properties of the of the \ionline{O}{[ii]} lines were  derived from 1-D spectra extracted from the MUSE data cube at 10  locations spaced 0\farcs6 apart along the length of the arc that  comprises images 11.1 and 11.2 of the \spock host galaxy. Each  extraction used an aperture of 0\farcs6 radius, centered on the  mid-line of the host galaxy arc. The integrated line flux, observed  wavelength of line center ($\lambda_{\rm center}$), and full width  at half maximum (FWHM) were found by fitting a Gaussian profile to  each component of the doublet.} %\tablenote{}  \label{tab:MuseLineFits}  \end{deluxetable*}  %# ID RA DEC Delta_spock2 OII]3726 OII]3729 OII]3729/OII]3726  %# Arcsec Flux(erg/s/cm^2) Center(Angstrom) Amplitude(erg/s/cm^2) FWHM(Angstrom) Flux(erg/s/cm^2) Center(Angstrom) Amplitude(erg/s/cm^2) FWHM(Angstrom)   %# ID RA DEC d_spock2 flux3726 wave3726 amplitude3726 fwhm3726 flux3729 wave37269 amplitude3729 fwhm3729 fluxratio3729to3726  diff --git a/spock_localbuild.pdf b/spock_localbuild.pdf  index 6126f08..1be013d 100644  Binary files a/spock_localbuild.pdf and b/spock_localbuild.pdf differ