deletions | additions       diff --git a/HostGalaxy.tex b/HostGalaxy.tex  index 757af07..94bca42 100644  --- a/HostGalaxy.tex  +++ b/HostGalaxy.tex 
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\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 \forbidden{O}{ii}  ($\lambda\lambda$ 3727, 3726,  3729) doublet, observed at 7474 and 7478 \AA. Figure~\ref{fig:MUSEOIISequence} shows the observed  \forbidden{O}{ii} lines at 10 positions along the length of the arc,  which comprises images 11.1 and 11.2. 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 To examine this feature in detail, one-dimensional spectra  were extracted using apertures with from the three-dimensional MUSE data cube at  a radius series  of 0\farcs6, so adjacent extractions are not independent, although the  two extractions centered on locations along  the \spockone and -SE positions have no  overlap. \spock host galaxy arc.  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 Figure~\ref{fig:MUSEOIISequence} depicts  the doublet. Properties derived from apertures used for  these line fits are  reported in Table~\ref{tab:MuseLineFits}. The extractions, shows the observed  \forbidden{O}{ii} linesdo not exhibit any discernible gradient across the host galaxy images  in terms of the wavelength of line centers, full width  athalf  maximum, or  the intensity ratio of the two components of the doublet.  Thus, \spock-NW and SE positions, and compares  the \forbidden{O}{ii} measurements from MUSE cannot be used line  profiles  to distinguish either \spock location from other positions along  the other, or to definitively  answer whether either position is coincident with the center length  of the host galaxy. We conclude that it is plausible but galaxy arc.  At each position the lines were extracted using apertures with a  radius of 0\farcs6, so adjacent extractions are  not certain that independent,  although  the two \spock events arose from extractions centered on  the same physical location in the  host galaxy. \spockone and -SE  positions have no overlap.  A difference in the shape of the \forbidden{O}{ii} lines or the  doublet line ratio could provide evidence for a different environment  at the two \spock locaions, which would suggest that the two events  emerged from independent sources. For a visual test for spectral  deviations, we first constructed a mean spectrum by averaging the 1-D  spectra from five non-overlapping apertures (apertures 1, 3, 5, 7,  9). To account for differences in magnification and host galaxy  intensity across the arc, each input spectrum was normalized at the  wavelength 7477.7 $\AA$, which corresponds to the center of the  $\lambda$3729 component of the \forbidden{O}{ii} emission line. This  mean spectrum was then subtracted from the 1-D spectrum of each  aperture, producing a set of ``residual spectra,'' shown in  Figure~\ref{fig:MUSEOIISequence} in the lower left panel. These  spectra show no indication of a systematic trend in the wavelength  position, shape or line ratio across the arc. Similarly, a comparison  of the spectra from the \spock-NW and SE locations (right panels of  Figure~\ref{fig:MUSEOIISequence}) reveals no significant difference in  the \forbidden{O}{ii} line shapes.  This qualitative comparison is born out by a more quantitative  assessment, reported in Table~\ref{tab:MuseLineFits}. We fit a  Gaussian profile to each component of the \forbidden{O}{ii} doublet,  separately in each extracted 1-D spectrum. From these fits we measured  the integrated line flux, observed wavelength of line center  ($\lambda_{\rm center}$), full width at half maximum (FWHM), and the  intensity ratio of the two components of the doublet. These  quantities--all reported in Table~\ref{tab:MuseLineFits}--do not  exhibit any discernible gradient across the host galaxy. Thus, the  \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 (as would be required, for example, if these transients were  from an AGN). We conclude that it is entirely plausible but not  certain that the two \spock events arose from the same physical  location in the host galaxy.  diff --git a/figures/muse_oii_sequence/caption.tex b/figures/muse_oii_sequence/caption.tex  index a649490..7251a1c 100644  --- a/figures/muse_oii_sequence/caption.tex  +++ b/figures/muse_oii_sequence/caption.tex 
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\label{fig:MUSEOIISequence}  The [OII] line, observed with MUSE, at a series Measurements  often locations along  the \forbidden{O}{ii} $\lambda\lambda$3726,3729 doublet, observed  with MUSE after both  \spock host galaxy arc. \todo{add in values events had faded. The upper left panel  shows the 12 apertures with radius 0.6\arcsec that were used  for the [OII] doublet  line ratio} \todo{Add extractions reported  in panels showing [OII] lines Table~\ref{tab:MuseLineFits}. Odd-numbered  apertures are plotted with solid lines, while even-numbered apertures  are shown as unlabeled dashed circles. The apertures centered on  the \spock-NW and SE locations are highlighted in orange and magenta,  respectively. The 1-D spectra extracted  from 11.3 these \spock locations  are shown in the upper right and lower right panels, centered around  the observed wavelength of the \forbidden{O}{ii} doublet,  and normalized to reach a value of unity at the peak of the $\lambda$3729  line. Dashed vertical lines mark  the spock locations.} \todo{add vacuum wavelengths of the  doublet, redshifted to $z=1.0054$. The width of the shaded region  indicates the $1\sigma$ uncertainty  in the measured flux. Below each  spectrum,  a residual plot shows the flux that remains after  subtracting off a mean spectrum constructed from the normalized  spectra of the odd-numbered apertures. The lower left  panel showing shows the  same residual spectra constructed for  the extraction  apertures.} odd-numbered apertures,  demonstrating that the \forbidden{O}{ii} line profile does not exhibit  any significant gradients across the length of the host galaxy arc.  diff --git a/figures/muse_oii_sequence/muse_oii_sequence.pdf b/figures/muse_oii_sequence/muse_oii_sequence.pdf  deleted file mode 100644  index 5285339..0000000  Binary files a/figures/muse_oii_sequence/muse_oii_sequence.pdf and /dev/null differ diff --git a/figures/muse_oii_sequence/muse_oii_sequence.png b/figures/muse_oii_sequence/muse_oii_sequence.png  index a2f3c7f..be6fa8d 100644  Binary files a/figures/muse_oii_sequence/muse_oii_sequence.png and b/figures/muse_oii_sequence/muse_oii_sequence.png differ