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diff --git a/docs/_build/html/2411.19126.md b/docs/_build/html/2411.19126.md
@@ -24,7 +24,7 @@ $\newcommand$</div>
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-[![arXiv](https://img.shields.io/badge/arXiv-2411.19126-b31b1b.svg)](https://arxiv.org/abs/2411.19126)<mark>Appeared on: 2024-12-02</mark> -  _16 pages, 19 figures, accepted for publication in A&A_
+[![arXiv](https://img.shields.io/badge/arXiv-2411.19126-b31b1b.svg)](https://arxiv.org/abs/2411.19126)<mark>Appeared on: 2024-12-03</mark> -  _16 pages, 19 figures, accepted for publication in A&A_
 
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diff --git a/docs/_build/html/2411.19489.md b/docs/_build/html/2411.19489.md
@@ -26,7 +26,7 @@ $\newcommand{\thebibliography}{\DeclareRobustCommand{\VAN}[3]{##3}\VANthebibliog
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-[![arXiv](https://img.shields.io/badge/arXiv-2411.19489-b31b1b.svg)](https://arxiv.org/abs/2411.19489)<mark>Appeared on: 2024-12-02</mark> -  _23 pages, 14 figures_
+[![arXiv](https://img.shields.io/badge/arXiv-2411.19489-b31b1b.svg)](https://arxiv.org/abs/2411.19489)<mark>Appeared on: 2024-12-03</mark> -  _23 pages, 14 figures_
 
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diff --git a/docs/_build/html/2411.19686.md b/docs/_build/html/2411.19686.md
@@ -64,7 +64,7 @@ $\newcommand{\lamobs}{\lambda_{\rm obs}}$</div>
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-[![arXiv](https://img.shields.io/badge/arXiv-2411.19686-b31b1b.svg)](https://arxiv.org/abs/2411.19686)<mark>Appeared on: 2024-12-02</mark> -  _submitted to A&A on July 30, 2024_
+[![arXiv](https://img.shields.io/badge/arXiv-2411.19686-b31b1b.svg)](https://arxiv.org/abs/2411.19686)<mark>Appeared on: 2024-12-03</mark> -  _submitted to A&A on July 30, 2024_
 
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diff --git a/docs/_build/html/2411.19916.md b/docs/_build/html/2411.19916.md
@@ -51,7 +51,7 @@ $\newcommand{\urlprefix}{URL }$</div>
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-[![arXiv](https://img.shields.io/badge/arXiv-2411.19916-b31b1b.svg)](https://arxiv.org/abs/2411.19916)<mark>Appeared on: 2024-12-02</mark> -  _40 pages, 7 figures, 2 tables_
+[![arXiv](https://img.shields.io/badge/arXiv-2411.19916-b31b1b.svg)](https://arxiv.org/abs/2411.19916)<mark>Appeared on: 2024-12-03</mark> -  _40 pages, 7 figures, 2 tables_
 
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@@ -61,7 +61,7 @@ E. T. Chickles, et al. -- incl., <mark>K. El-Badry</mark>
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-**Abstract:** Type Ia supernovae, critical for studying cosmic expansion \citemain{1998AJ....116.1009R} $^,$ \citemain{1998ApJ...507...46S} , arise from thermonuclear explosions of white dwarfs \citemain{1960ApJ...132..565H} , but their precise progenitor pathways remain unclear. Growing evidence supports the "double-degenerate" scenario, where two white dwarfs interact \citemain{1984ApJS...54..335I} $^,$ \citemain{1984ApJ...277..355W} . The absence of other companion types capable of explaining the observed Ia rate \citemain{1984ApJ...277..355W} , along with observations of hyper-velocity white dwarfs interpreted as surviving companions of such systems \citemain{2018ApJ...865...15S} $^,$ \citemain{2023OJAp....6E..28E} provide compelling evidence in favor of this scenario. Upcoming millihertz gravitational wave observatories like the Laser Interferometer Space Antenna (LISA) \citemain{2017arXiv170200786A} are expected to detect thousands of double-degenerate systems, though the most compact known candidate Ia progenitors produce only marginally detectable gravitational wave signals. Here, we report observations of ATLAS J1138-5139, a binary white dwarf system with an orbital period of just 28 minutes. Our analysis reveals a 1 solar mass carbon-oxygen white dwarf accreting from a helium-core white dwarf. Given its mass, the accreting carbon-oxygen white dwarf is poised to trigger a typical-luminosity Type Ia supernova within a few million years, or to evolve into a stably mass-transferring AM CVn system. ATLAS J1138-5139 provides a rare opportunity to calibrate binary evolution models by directly comparing observed orbital parameters and mass transfer rates closer to merger than any previously identified candidate Type Ia progenitor. Its compact orbit ensures detectability by LISA, demonstrating the potential of millihertz gravitational wave observatories to reveal a population of Type Ia progenitors on a Galactic scale, paving the way for multi-messenger studies offering insights into the origins of these cosmologically significant explosions.
+**Abstract:** Type Ia supernovae, critical for studying cosmic expansion \citemain{1998AJ....116.1009R} $^,$ \citemain{1998ApJ...507...46S} , arise from thermonuclear explosions of white dwarfs \citemain{1960ApJ...132..565H} , but their precise progenitor pathways remain unclear. Growing evidence supports the "double-degenerate" scenario, where two white dwarfs interact \citemain{1984ApJS...54..335I} $^,$ \citemain{1984ApJ...277..355W} . The absence of other companion types capable of explaining the observed Ia rate \citemain{1984ApJ...277..355W} , along with observations of hyper-velocity white dwarfs interpreted as surviving companions of such systems \citemain{2018ApJ...865...15S} $^,$ \citemain{2023OJAp....6E..28E} provide compelling evidence in favor of this scenario. Upcoming millihertz gravitational wave observatories like the Laser Interferometer Space Antenna (LISA) \citemain{2017arXiv170200786A} are expected to detect thousands of double-degenerate systems, though the most compact known candidate Ia progenitors produce only marginally detectable gravitational wave signals. Here, we report observations of ATLAS J1138-5139, a binary white dwarf system with an orbital period of just 28 minutes. Our analysis reveals a 1 solar mass carbon-oxygen white dwarf accreting from a helium-core white dwarf. Given its mass, the accreting carbon-oxygen white dwarf is poised to trigger a typical-luminosity Type Ia supernova within a few million years, or to evolve into a stably mass-transferring AM CVn system. sudo apt install texlive-font-utilsATLAS J1138-5139 provides a rare opportunity to calibrate binary evolution models by directly comparing observed orbital parameters and mass transfer rates closer to merger than any previously identified candidate Type Ia progenitor. Its compact orbit ensures detectability by LISA, demonstrating the potential of millihertz gravitational wave observatories to reveal a population of Type Ia progenitors on a Galactic scale, paving the way for multi-messenger studies offering insights into the origins of these cosmologically significant explosions.
 
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@@ -81,8 +81,8 @@ E. T. Chickles, et al. -- incl., <mark>K. El-Badry</mark>
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-<img src="tmp_2411.19916/./Figures/Fig_Lcurve.png" alt="Fig6" width="100%"/>
+<img src="tmp_2411.19916/./Figures/lightcurve_model.png" alt="Fig6" width="100%"/>
 
-**Figure 6. -** ULTRACAM light curve from March 8, 2023 (green points), overlaid with the best-fit \texttt{LCURVE} model (solid line). The model includes contributions from an accretion disk a hot spot, which were needed to achieve an acceptable fit to the lightcurve. (*fig:LCURVE*)
+**Figure 6. -** Three color ULTRACAM light curve from March 20, 2023, overlaid with the best-fit toy \texttt{LCURVE} model (solid black lines). The model includes contributions from an accretion disk and a hot spot where the accretion stream intersects the outer disk, which were needed to achieve an acceptable fit to the lightcurve. The best fit model gives a near edge-on inclination (88.6 degrees), though we chose not to include this model as part of our joint fit, due to the large number of model-dependent free parameters involved, as compared to our more simple and robust approach. (*fig:LCURVE*)
 
 </div><div id="qrcode"><img src=https://api.qrserver.com/v1/create-qr-code/?size=100x100&data="https://arxiv.org/abs/2411.19916"></div>
diff --git a/docs/_build/html/2411.19945.md b/docs/_build/html/2411.19945.md
@@ -24,7 +24,7 @@ $\newcommand{\arraystretch}{1.5}$</div>
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-[![arXiv](https://img.shields.io/badge/arXiv-2411.19945-b31b1b.svg)](https://arxiv.org/abs/2411.19945)<mark>Appeared on: 2024-12-02</mark> -  _16 pages, 12 figures, accepted for publication in A&A_
+[![arXiv](https://img.shields.io/badge/arXiv-2411.19945-b31b1b.svg)](https://arxiv.org/abs/2411.19945)<mark>Appeared on: 2024-12-03</mark> -  _16 pages, 12 figures, accepted for publication in A&A_
 
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