adsabs/AstroCLIMB huggingface dataset:
Paper: A Radio Technosignature Search of TRAPPIST-1 with the Allen Telescope Array
Authors: Nick Tusay, Sofia Z. Sheikh, Evan L. Sneed, Wael Farah, Alexander W. Pollak, Luigi F. Cruz, Andrew Siemion, David R. DeBoer, Jason T. Wright
Figure caption: An example of some one-off “blip” results. The red framed central panel is the 10 minutes integration from the observations taken on 2022 November 5 in which the signal was found, showing reasonable attenuation but lacking the drifting narrowband morphology and persistence in time expected from a true signal in this kind of search. It appears to mimic other confirmed RFI in morphology, though at a distinct and isolated frequency. The observing time progresses from the bottom to the top of each panel. The bottom and top rows show adjacent integrations at the same frequency.
Paper: A Radio Technosignature Search of TRAPPIST-1 with the Allen Telescope Array
Authors: Nick Tusay, Sofia Z. Sheikh, Evan L. Sneed, Wael Farah, Alexander W. Pollak, Luigi F. Cruz, Andrew Siemion, David R. DeBoer, Jason T. Wright
Figure caption: SNR ratio vs. DOT score for each day of the TRAPPIST-1 observations. Each observation was analyzed independently to account for temporal variability in the RFI environment. The red dashed line represents a conservative cutoff defined by an empirical power law designed to isolate the bulk of the RFI. RFI is expected to have high DOT scores and low SNR ratios, while true signals are expected to trend toward lower DOT scores and higher SNR ratios. All signals above the cutoff are plotted as individual black points, while signals captured below the cutoff are represented as a heatmap, with the color bar showing the base 10 exponent of the number of signals represented in a given region.
Paper: A Radio Technosignature Search of TRAPPIST-1 with the Allen Telescope Array
Authors: Nick Tusay, Sofia Z. Sheikh, Evan L. Sneed, Wael Farah, Alexander W. Pollak, Luigi F. Cruz, Andrew Siemion, David R. DeBoer, Jason T. Wright
Figure caption: An example of unique and unexpected RFI in the primary panel framed in red. The observing time progresses from the bottom to the top of each panel. The other rows show adjacent integrations at the same frequency. The apparently alternating pings in the primary frame explain the low correlation score and spark curiosity. However, the low SNR ratio, small drift rate, and bright features in later integrations all suggest that the source of the signal is likely not localized to the TRAPPIST-1 system.
Paper: A Radio Technosignature Search of TRAPPIST-1 with the Allen Telescope Array
Authors: Nick Tusay, Sofia Z. Sheikh, Evan L. Sneed, Wael Farah, Alexander W. Pollak, Luigi F. Cruz, Andrew Siemion, David R. DeBoer, Jason T. Wright
Figure caption: Original plot of a signal over the expected frequency span based on drift rate in the top row, and the same signal zoomed out in frequency in the bottom row. The true morphology of this broadband signal can be seen over a wider bandwidth and is reflected in the increase in correlation (DOT) score. This demonstrates how small slices of broadband signals are often misinterpreted by current de-Doppler algorithms as narrowband signals.
Paper: Analyzing the Onset of Cometary Activity by the Jupiter-family Comet 2023 RN3 
Authors: Matthew M. Dobson, Megan E. Schwamb, Alan Fitzsimmons, Michael S. P. Kelley, Carrie E. Holt, Joseph Murtagh, Henry H. Hsieh, Larry Denneau, Nicolas Erasmus, A. N. Heinze, Luke J. Shingles, Robert J. Siverd, Ken W. Smith, John L. Tonry, Henry Weiland, David. R. Young, Tim Lister, Edward Gomez, Joey Chatelain, Sarah Greenstreet
Figure caption: Orbital evolution calculations of the 2023 RN3 nominal orbit and 100 clones. Top panel: semimajor axis a vs. date. The red dashed line indicates the starting epoch of the orbital integrations. The y-axis range of the top panel has been chosen to clearly show the small jumps in a near the current epoch. Middle and bottom panels: as for the top panel, but showing eccentricity e and perihelion distance q.
Paper: Analyzing the Onset of Cometary Activity by the Jupiter-family Comet 2023 RN3 
Authors: Matthew M. Dobson, Megan E. Schwamb, Alan Fitzsimmons, Michael S. P. Kelley, Carrie E. Holt, Joseph Murtagh, Henry H. Hsieh, Larry Denneau, Nicolas Erasmus, A. N. Heinze, Luke J. Shingles, Robert J. Siverd, Ken W. Smith, John L. Tonry, Henry Weiland, David. R. Young, Tim Lister, Edward Gomez, Joey Chatelain, Sarah Greenstreet
Figure caption: Top: LOOK g-filter reduced magnitudes (green circles) vs. time with third-order interpolated splines fitted to synthetic data overplotted (green). Middle: LOOK r filter reduced magnitudes (red circles) vs. time with third-order interpolated splines fitted to synthetic data overplotted (turquoise). Bottom: g − r color index value calculated from the predicted magnitudes in each filter from the synthetic magnitudes plotted across time. Red circles denote nominal color index values with green lines highlighting the range that includes the central 68.3% of synthetic values.
Paper: Analyzing the Onset of Cometary Activity by the Jupiter-family Comet 2023 RN3 
Authors: Matthew M. Dobson, Megan E. Schwamb, Alan Fitzsimmons, Michael S. P. Kelley, Carrie E. Holt, Joseph Murtagh, Henry H. Hsieh, Larry Denneau, Nicolas Erasmus, A. N. Heinze, Luke J. Shingles, Robert J. Siverd, Ken W. Smith, John L. Tonry, Henry Weiland, David. R. Young, Tim Lister, Edward Gomez, Joey Chatelain, Sarah Greenstreet
Figure caption: Top: ZTF g-filter reduced magnitudes (green circles) vs. time with third-order interpolated splines fitted to synthetic data overplotted (green). Middle: ZTF r filter reduced magnitudes (red circles) vs. time with third-order interpolated splines fitted to synthetic data overplotted (turquoise). Bottom: g − r color index value calculated from the predicted magnitudes in each filter from the synthetic magnitudes plotted across time. Red circles denote nominal color index values with green lines highlighting the range that includes the central 68.3% of synthetic values.
Paper: Analyzing the Onset of Cometary Activity by the Jupiter-family Comet 2023 RN3 
Authors: Matthew M. Dobson, Megan E. Schwamb, Alan Fitzsimmons, Michael S. P. Kelley, Carrie E. Holt, Joseph Murtagh, Henry H. Hsieh, Larry Denneau, Nicolas Erasmus, A. N. Heinze, Luke J. Shingles, Robert J. Siverd, Ken W. Smith, John L. Tonry, Henry Weiland, David. R. Young, Tim Lister, Edward Gomez, Joey Chatelain, Sarah Greenstreet
Figure caption:  A(0°)f ρ values of 2023 RN3 across time. A(0°)f ρ values have been corrected for color and phase effects.
Paper: The Roasting Marshmallows Program with IGRINS on Gemini South. II. WASP-121 b has Superstellar C/O and Refractory-to-volatile Ratios
Authors: Peter C. B. Smith, Jorge A. Sanchez, Michael R. Line, Emily Rauscher, Megan Weiner Mansfield, Eliza M.-R. Kempton, Arjun Savel, Joost P. Wardenier, Lorenzo Pino, Jacob L. Bean, Hayley Beltz, Vatsal Panwar, Matteo Brogi, Isaac Malsky, Jonathan Fortney, Jean-Michel Désert, Stefan Pelletier, Vivien Parmentier, Sai Krishna Teja Kanumalla, Luis Welbanks, Michael Meyer, John Monnier
Figure caption: Marginalized posterior distributions for each of the elemental enrichments included in the chemically consistent retrieval model with both volatile and refractory species. When constrained, the posterior median and 1σ confidence intervals are listed. For posteriors against the prior boundaries, 3σ and 5σ upper or lower limits are listed. These quantities were retrieved as log10[(x/H)/(x/H)solar] and have been converted here to log10[(x/H)/(x/H)stellar], assuming the values and associated uncertainties for WASP-121 from A. S. Polanski et al. (2022). Because WASP-121 has a slightly supersolar metallicity, the upper prior bound on [x/H]solar at +3 is slightly lower than 3 when converted to [x/H]stellar for any given element. These effective upper prior bounds are indicated by the vertical dotted lines, and the effective lower bounds are less than −3 and beyond the plot. The quantities in the top row are, from left to right, the total atmospheric metal enrichment, the volatile enrichment, and the total refractory enrichment. These are derived from the individual elemental enrichment posterior distributions as described in Section 6. For reference, the elemental enrichment relative to the solar value is also listed.
Paper: The Roasting Marshmallows Program with IGRINS on Gemini South. II. WASP-121 b has Superstellar C/O and Refractory-to-volatile Ratios
Authors: Peter C. B. Smith, Jorge A. Sanchez, Michael R. Line, Emily Rauscher, Megan Weiner Mansfield, Eliza M.-R. Kempton, Arjun Savel, Joost P. Wardenier, Lorenzo Pino, Jacob L. Bean, Hayley Beltz, Vatsal Panwar, Matteo Brogi, Isaac Malsky, Jonathan Fortney, Jean-Michel Désert, Stefan Pelletier, Vivien Parmentier, Sai Krishna Teja Kanumalla, Luis Welbanks, Michael Meyer, John Monnier
Figure caption: Cross-correlation detection maps calculated using the methods and models described in Section 3. The “All Gases” map in the top left is the result of cross-correlating the solar composition 1D-RCTE model spectrum including all sources of opacity listed in that same section. Every other panel displays the residuals between the “All Gases” map and the resultant CCF map from cross-correlating a model with all sources of opacity except the gas listed in the upper left of each individual panel. The dashed white lines indicate the expected K P and dV sys of the true planet signal, and the quoted S/N values are the maximum value found within a 20 km s−1 × 20 km s−1 box centered at the expected K P and dV sys.
Paper: The Roasting Marshmallows Program with IGRINS on Gemini South. II. WASP-121 b has Superstellar C/O and Refractory-to-volatile Ratios
Authors: Peter C. B. Smith, Jorge A. Sanchez, Michael R. Line, Emily Rauscher, Megan Weiner Mansfield, Eliza M.-R. Kempton, Arjun Savel, Joost P. Wardenier, Lorenzo Pino, Jacob L. Bean, Hayley Beltz, Vatsal Panwar, Matteo Brogi, Isaac Malsky, Jonathan Fortney, Jean-Michel Désert, Stefan Pelletier, Vivien Parmentier, Sai Krishna Teja Kanumalla, Luis Welbanks, Michael Meyer, John Monnier
Figure caption: 2D posterior distributions for our inferences of WASP-121 b’s radial velocity semi-amplitude, K P, and a systematic velocity offset, dV sys, using four different 1D-RCTE models. The colored posterior distributions use models that include only continuum opacity sources and the opacity of that one particular gas using the P-T and abundance profile as output by the solar composition 1D-RCTE model, while the black posterior distribution is from using the 1D-RCTE model including all gases mentioned in Section 3. There is a clear discrepancy in K P and dV sys between H2O, CO, and OH. H2O appears to have a larger K P compared to the other gases, while OH appears to have net relative blueshift by about 1.5 km s−1 compared to the other gases. The contours show 1σ, 2σ, and 3σ confidence intervals.
Paper: The Roasting Marshmallows Program with IGRINS on Gemini South. II. WASP-121 b has Superstellar C/O and Refractory-to-volatile Ratios
Authors: Peter C. B. Smith, Jorge A. Sanchez, Michael R. Line, Emily Rauscher, Megan Weiner Mansfield, Eliza M.-R. Kempton, Arjun Savel, Joost P. Wardenier, Lorenzo Pino, Jacob L. Bean, Hayley Beltz, Vatsal Panwar, Matteo Brogi, Isaac Malsky, Jonathan Fortney, Jean-Michel Désert, Stefan Pelletier, Vivien Parmentier, Sai Krishna Teja Kanumalla, Luis Welbanks, Michael Meyer, John Monnier
Figure caption: Our measured absolute abundances (top panel) and relative abundances (to Fe; bottom panel) in black compared to those measured by C. Maguire et al. (2023) over the course of three transits (dark blue). Also shown are the solar (M. Asplund et al. 2009) and stellar (A. S. Polanski et al. 2022) photospheric values for these quantities (the turquoise and green horizontal lines, respectively). While there is some scatter among the absolute abundances, the relative abundance ratios are mostly consistent across these two studies, with the exception of Ca. As discussed in Section 5.3, this may be an artifact of the different chemistry prescriptions used in each study, or this may be evidence of partial Ca condensation on the planet’s terminator. The arrows represent 3σ upper or lower limits.
Paper: The Roasting Marshmallows Program with IGRINS on Gemini South. II. WASP-121 b has Superstellar C/O and Refractory-to-volatile Ratios
Authors: Peter C. B. Smith, Jorge A. Sanchez, Michael R. Line, Emily Rauscher, Megan Weiner Mansfield, Eliza M.-R. Kempton, Arjun Savel, Joost P. Wardenier, Lorenzo Pino, Jacob L. Bean, Hayley Beltz, Vatsal Panwar, Matteo Brogi, Isaac Malsky, Jonathan Fortney, Jean-Michel Désert, Stefan Pelletier, Vivien Parmentier, Sai Krishna Teja Kanumalla, Luis Welbanks, Michael Meyer, John Monnier
Figure caption: Left: the median retrieved P-T profile using the model as described in Section 5.1 (orange line) as well as the 1σ confidence interval about this median profile (orange shaded region). For comparison, we also plot the output P-T profile from a 1D-RCTE model at the retrieved best-fit metallicity and C/O ratio (black dashed line). Also shown is the τ = 2/3 spectrum of the retrieved best-fit model, which approximates the location of the photosphere (light gray). Top right: the derived posterior distribution for the C/O ratio from that same model. For comparison, the stellar value (0.23) is shown as the dotted black line. Bottom right: the derived posterior distribution for the R/V ratio in relation to the stellar value.
Paper: The Roasting Marshmallows Program with IGRINS on Gemini South. II. WASP-121 b has Superstellar C/O and Refractory-to-volatile Ratios
Authors: Peter C. B. Smith, Jorge A. Sanchez, Michael R. Line, Emily Rauscher, Megan Weiner Mansfield, Eliza M.-R. Kempton, Arjun Savel, Joost P. Wardenier, Lorenzo Pino, Jacob L. Bean, Hayley Beltz, Vatsal Panwar, Matteo Brogi, Isaac Malsky, Jonathan Fortney, Jean-Michel Désert, Stefan Pelletier, Vivien Parmentier, Sai Krishna Teja Kanumalla, Luis Welbanks, Michael Meyer, John Monnier
Figure caption: Measured velocities for each gas and the full atmospheric model in the planet rest frame as measured using the “All Gases” model. The H2O signal has a notably larger K P compared to the other gases (manifesting here as a greater slant to the left). A possible explanation is that the CO and OH signals are mostly originating from WASP-121 b’s hotspot region and are effectively blue- and redshifted as the planet rotates, resulting in an effectively lower K P (greater slant to the right). H2O may not experience this effect because it is largely dissociated in the hotspot.
Paper: The Roasting Marshmallows Program with IGRINS on Gemini South. II. WASP-121 b has Superstellar C/O and Refractory-to-volatile Ratios
Authors: Peter C. B. Smith, Jorge A. Sanchez, Michael R. Line, Emily Rauscher, Megan Weiner Mansfield, Eliza M.-R. Kempton, Arjun Savel, Joost P. Wardenier, Lorenzo Pino, Jacob L. Bean, Hayley Beltz, Vatsal Panwar, Matteo Brogi, Isaac Malsky, Jonathan Fortney, Jean-Michel Désert, Stefan Pelletier, Vivien Parmentier, Sai Krishna Teja Kanumalla, Luis Welbanks, Michael Meyer, John Monnier
Figure caption: Cross-correlation “trail” as described in Section 3. The solar composition 1D-RCTE model spectrum was cross-correlated with the post-SVD data at each frame in both observational sequences along a grid of possible line-of-sight radial velocities in the system barycentric frame. The dotted white lines indicate the planet signal’s expected path in velocity-time space, offset by ±20 km s−1 for clarity. The hatched region indicates the secondary eclipse, during which the planet is occulted by the star and data were not taken.
Paper: The Roasting Marshmallows Program with IGRINS on Gemini South. II. WASP-121 b has Superstellar C/O and Refractory-to-volatile Ratios
Authors: Peter C. B. Smith, Jorge A. Sanchez, Michael R. Line, Emily Rauscher, Megan Weiner Mansfield, Eliza M.-R. Kempton, Arjun Savel, Joost P. Wardenier, Lorenzo Pino, Jacob L. Bean, Hayley Beltz, Vatsal Panwar, Matteo Brogi, Isaac Malsky, Jonathan Fortney, Jean-Michel Désert, Stefan Pelletier, Vivien Parmentier, Sai Krishna Teja Kanumalla, Luis Welbanks, Michael Meyer, John Monnier
Figure caption: Similar to Figure 4, but using the log-likelihood function from M. Brogi & M. R. Line (2019) instead of cross-correlation coefficients.
Paper: The Roasting Marshmallows Program with IGRINS on Gemini South. II. WASP-121 b has Superstellar C/O and Refractory-to-volatile Ratios
Authors: Peter C. B. Smith, Jorge A. Sanchez, Michael R. Line, Emily Rauscher, Megan Weiner Mansfield, Eliza M.-R. Kempton, Arjun Savel, Joost P. Wardenier, Lorenzo Pino, Jacob L. Bean, Hayley Beltz, Vatsal Panwar, Matteo Brogi, Isaac Malsky, Jonathan Fortney, Jean-Michel Désert, Stefan Pelletier, Vivien Parmentier, Sai Krishna Teja Kanumalla, Luis Welbanks, Michael Meyer, John Monnier
Figure caption: Abundance ratios of refractory species both in total and individually to oxygen (top) and carbon (bottom) in terms of the stellar ratios. The arrows indicate the upper limits at 3σ.
Paper: Deepest Limits on Scattered Light Emission from the Epsilon Eridani Inner Debris Disk with HST/STIS
Authors: Sai Krishanth P. M., Ewan S. Douglas, Ramya M. Anche, Justin Hom, Kerri L. Cahoy, John H. Debes, Hannah Jang-Condell, Isabel Rebollido, Bin B. Ren, 彬 任, Christopher C. Stark, Robert Thompson, Yinzi Xin
Figure caption: Left panel: NMF result using 90% closest frames of δ Eri as reference and 30 NMF components. Right panel: signal-to-noise ratio (SNR) map of the reduced image, calculated by dividing the median of used frames by the standard deviation of the used frames.
Paper: Deepest Limits on Scattered Light Emission from the Epsilon Eridani Inner Debris Disk with HST/STIS
Authors: Sai Krishanth P. M., Ewan S. Douglas, Ramya M. Anche, Justin Hom, Kerri L. Cahoy, John H. Debes, Hannah Jang-Condell, Isabel Rebollido, Bin B. Ren, 彬 任, Christopher C. Stark, Robert Thompson, Yinzi Xin
Figure caption: Contrast vs. separation sensitivity curves showing the KLIP reduction optimized for disks (in dashed blue), KLIP reduction optimized for planets (in dotted magenta), NMF reduction (in solid purple), and the photon limit (in thick solid gray). We note that the KLIP subtraction optimized for planets has the best contrast under 1″, but the NMF curve has the best contrast overall.
Paper: Deepest Limits on Scattered Light Emission from the Epsilon Eridani Inner Debris Disk with HST/STIS
Authors: Sai Krishanth P. M., Ewan S. Douglas, Ramya M. Anche, Justin Hom, Kerri L. Cahoy, John H. Debes, Hannah Jang-Condell, Isabel Rebollido, Bin B. Ren, 彬 任, Christopher C. Stark, Robert Thompson, Yinzi Xin
Figure caption: Left panel: disk-optimized KLIP reduction. The combination of a single annulus and a low number of KL modes is ideal to avoid oversubtraction and preserve the disk signal. Right panel: KLIP reduction optimized for detection of substellar companions. This combination of a large number of annuli gives us the most contrast while 10 KL modes give us a good balance of contrast and throughput.
Paper: Deepest Limits on Scattered Light Emission from the Epsilon Eridani Inner Debris Disk with HST/STIS
Authors: Sai Krishanth P. M., Ewan S. Douglas, Ramya M. Anche, Justin Hom, Kerri L. Cahoy, John H. Debes, Hannah Jang-Condell, Isabel Rebollido, Bin B. Ren, 彬 任, Christopher C. Stark, Robert Thompson, Yinzi Xin
Figure caption: Median combined images for each visit. The mean of the median of each roll for the first and last visit shows relatively similar structure and brightness between the two visits. No images were dropped before the median combining shown in this illustration.
Paper: Deepest Limits on Scattered Light Emission from the Epsilon Eridani Inner Debris Disk with HST/STIS
Authors: Sai Krishanth P. M., Ewan S. Douglas, Ramya M. Anche, Justin Hom, Kerri L. Cahoy, John H. Debes, Hannah Jang-Condell, Isabel Rebollido, Bin B. Ren, 彬 任, Christopher C. Stark, Robert Thompson, Yinzi Xin
Figure caption: Classical RDI subtraction as described in 3.2.3.
Paper: Deepest Limits on Scattered Light Emission from the Epsilon Eridani Inner Debris Disk with HST/STIS
Authors: Sai Krishanth P. M., Ewan S. Douglas, Ramya M. Anche, Justin Hom, Kerri L. Cahoy, John H. Debes, Hannah Jang-Condell, Isabel Rebollido, Bin B. Ren, 彬 任, Christopher C. Stark, Robert Thompson, Yinzi Xin
Figure caption: Contrast vs. separation sensitivity curves showing our classical RDI (in dotted green), classical RDI reduction from S. G. Wolff et al. (2023; in dotted–dashed orange), NMF reduction (in solid purple), and the photon limit (in thick solid gray). We note that the NMF curve has better contrast out to 3″, after which both classical RDI reductions perform better. Our reductions also extend to a smaller radial separation because of the occulter location we used in our observations.
Paper: Deepest Limits on Scattered Light Emission from the Epsilon Eridani Inner Debris Disk with HST/STIS
Authors: Sai Krishanth P. M., Ewan S. Douglas, Ramya M. Anche, Justin Hom, Kerri L. Cahoy, John H. Debes, Hannah Jang-Condell, Isabel Rebollido, Bin B. Ren, 彬 任, Christopher C. Stark, Robert Thompson, Yinzi Xin
Figure caption: The simulated disk models of ϵ Eri through the Roman Coronagraph Instrument. We use the LBTI HOSTS measurements from S. Ertel et al. (2020) for the smooth disk model and disk properties from D. Backman et al. (2009), and S. G. Wolff et al. (2023) for the two ring models. The disks are processed through the HLC and SPC mode of the Roman Coronagraph instrument using realistic noise and speckle background levels from OS9 (for HLC) and OS11 (for SPC) for a 26.67 hr exposure. The IWA and OWA for the coronagraphs are marked in red for each of the input disk models. The Roman Coronagraph will achieve deeper contrast at smaller separations with both modes than we have achieved with STIS.
Paper: Deepest Limits on Scattered Light Emission from the Epsilon Eridani Inner Debris Disk with HST/STIS
Authors: Sai Krishanth P. M., Ewan S. Douglas, Ramya M. Anche, Justin Hom, Kerri L. Cahoy, John H. Debes, Hannah Jang-Condell, Isabel Rebollido, Bin B. Ren, 彬 任, Christopher C. Stark, Robert Thompson, Yinzi Xin
Figure caption: Contrast curves from three different postprocessing approaches plotted against predicted planetary masses (using the Sonora Bobcat planetary evolution models; M. S. Marley et al. 2021) in units of M Jup. We use 5σ contrast instead of MAD contrast for this plot to maintain consistency with published exoplanet literature. This plot assumes purely emissive light contrast and does not take reflected light from the planet into effect.
Paper: Deepest Limits on Scattered Light Emission from the Epsilon Eridani Inner Debris Disk with HST/STIS
Authors: Sai Krishanth P. M., Ewan S. Douglas, Ramya M. Anche, Justin Hom, Kerri L. Cahoy, John H. Debes, Hannah Jang-Condell, Isabel Rebollido, Bin B. Ren, 彬 任, Christopher C. Stark, Robert Thompson, Yinzi Xin
Figure caption: Flux profile of the ϵ Eri system using NMF in red. The shaded blue region represents the 1σ uncertainty in the measurement. Consistent with our derived SNR map, our result is indicative of a nondetection.
Paper: Exomoons and Exorings with the Habitable Worlds Observatory. I. On the Detection of Earth–Moon Analog Shadows and Eclipses
Authors: Mary Anne Limbach, Jacob Lustig-Yaeger, Andrew Vanderburg, Johanna M. Vos, René Heller, Tyler D. Robinson
Figure caption:  Top: Flux from the Earth (blue line), the Moon (red), and a moon with R = 2 R Moon (red dashed line) plus blended SEDs of the Earth and moons (dotted lines) as measured by the NASA EPOXI mission. Middle: The Moon-to-Earth Flux ratio (blue line), which demonstrates that the Moon is significantly fainter than the Earth in the UV/visible, but reaches 64% of the apparent brightness of the Earth in the NIR. For the case of equal albedos, the Moon would be 7.4% the brightness of the Earth (gray dashed line). Bottom: Depth of mutual events created by the Earth and Moon. The transit and shadow depth varies greatly depending on phase, but is relatively stable with wavelength. Occultation and eclipse events remain a constant depth with phase, but vary in depth by more than an order of magnitude with wavelength.