adsabs/AstroCLIMB huggingface dataset:
Paper: A Refined Photometric Constraint for Exoplanet Direct Imaging Yield Estimation and Observation Scheduling
Authors: Corey Spohn, Dmitry Savransky, Christopher C. Stark
Figure caption: Demonstrating successful inversion of the Roman CGI’s ETC using the minimization routine on HIP 57, HIP 169 A, and HIP 263. Each dot represents a step the minimization routine took, with the first step in dark purple and the last in bright yellow. Each row represents a specific star. The left column shows the minimization steps compared to the minimization objective function, Equation (11), and the Δmag bounds given to the minimization routine. The middle column shows the corresponding integration times for the steps taken by the minimization routine, the Δmag bounds, and the input tint that the minimization routine is attempting to converge to. The right column shows the Δmag step sizes and their corresponding change in tint.
Paper: A Refined Photometric Constraint for Exoplanet Direct Imaging Yield Estimation and Observation Scheduling
Authors: Corey Spohn, Dmitry Savransky, Christopher C. Stark
Figure caption: Comparison of the Roman ETC and the analytic polynomial-based approach to determine the dimmest planet flux that meets the required SNR for a given integration time. The observing mode used is the narrow-field imager (see Section 4). The top of the plot shows the Roman ETC evaluated for six stars at different planet Δmag values and a horizontal line that represents the reference integration time of 30 days. The Δmag value corresponding to an integration time of 30 days represents Δmag0, or the dimmest planet that can reach the required SNR. The bottom plot shows the polynomial from Equation (16) for the same six stars.
Paper: A Refined Photometric Constraint for Exoplanet Direct Imaging Yield Estimation and Observation Scheduling
Authors: Corey Spohn, Dmitry Savransky, Christopher C. Stark
Figure caption: Showing the Roman CGI’s ETC integration time response to varying Δmag. Astrophysical inputs here are the same as in Figure 1.
Paper: SQuIGG﹩\overrightarrow{L}﹩E: Buried Star Formation Cannot Explain the Rapidly Fading CO(2–1) Luminosity in Massive, z ∼ 0.7 Post-starburst Galaxies
Authors: David J. Setton, Justin S. Spilker, Rachel Bezanson, Katherine A. Suess, Jenny E. Greene, Andy D. Goulding, Elia Cenci, Vincenzo R. D'Onofrio, Robert Feldmann, Mariska Kriek, Anika Kumar, Yuanze Luo, Desika Narayanan, Margaret E. Verrico, Pengpei Zhu
Figure caption: Resolved Kennicutt–Schmidt relation for the CO-detected SQuIGG﹩\overrightarrow{L}﹩E  galaxies under four sets of assumptions: τBC Tied, αCO = 4.0 (top left), τBC Tied, αCO = 0.8 (bottom left), τBC Free, αCO = 4.0 (top right), and τBC Free, αCO = 0.8 (bottom right). In galaxies where the median SFR is less than 0.1 M⊙ yr−1, we instead show the 3σ upper limit. As background contours, we show all detected galaxies with ﹩\mathrm{log}({M}_{\star }/{M}_{\odot })\gt 10.8﹩ from the COLDGASS Survey (z ∼ 0, A. Saintonge et al. 2011) and PHIBSS/PHIBSS2 (z = 0.5–2.5, L. J. Tacconi et al. 2018; J. Freundlich et al. 2019), assuming αCO = 4.0. In blue, we show lines of constant depletion time for the molecular gas, with the target depletion time of ∼150 Myr highlighted as a thick line. In the bottom right panel, we show vectors that indicate the typical shift that comes from changing one of these assumptions: 0.7 dex in ﹩{M}_{{{\rm{H}}}_{2}}﹩ (from changing to a starburst αCO assumption) and 0.5 dex in SFR. Even under the assumption that all the youngest (t < 10 Myr) stars in every SQuIGG﹩\overrightarrow{L}﹩E  are behind optically thick dust cannot place the galaxies in a part of the SFR vs. ﹩{M}_{{{\rm{H}}}_{2}}﹩ space that results in depletion times that align with the trend in Figure 11. Similarly, a modification to αCO can raise the depletion times significantly, but at the low inferred SFRs, the majority of the galaxies still fall below the target depletion timescale of 150 Myr. Even the combination of these effects is not enough to resolve the tension with the observed depletion times.
Paper: SQuIGG﹩\overrightarrow{L}﹩E: Buried Star Formation Cannot Explain the Rapidly Fading CO(2–1) Luminosity in Massive, z ∼ 0.7 Post-starburst Galaxies
Authors: David J. Setton, Justin S. Spilker, Rachel Bezanson, Katherine A. Suess, Jenny E. Greene, Andy D. Goulding, Elia Cenci, Vincenzo R. D'Onofrio, Robert Feldmann, Mariska Kriek, Anika Kumar, Yuanze Luo, Desika Narayanan, Margaret E. Verrico, Pengpei Zhu
Figure caption: Comparison between the time since quenching (tq) measured in K. A. Suess et al. (2022a) and the post-starburst time (tPSB) we measure in this work, for the τBC Tied prior (left) and τBC Free prior (right). For both sets of the fits, these quantities scatter around the 1:1 line with minimal scatter.
Paper: SQuIGG﹩\overrightarrow{L}﹩E: Buried Star Formation Cannot Explain the Rapidly Fading CO(2–1) Luminosity in Massive, z ∼ 0.7 Post-starburst Galaxies
Authors: David J. Setton, Justin S. Spilker, Rachel Bezanson, Katherine A. Suess, Jenny E. Greene, Andy D. Goulding, Elia Cenci, Vincenzo R. D'Onofrio, Robert Feldmann, Mariska Kriek, Anika Kumar, Yuanze Luo, Desika Narayanan, Margaret E. Verrico, Pengpei Zhu
Figure caption: Gas fraction vs. age, using our alternate metrics of age defined in Appendix B. While the specific age we measure differs depending on the timescale adopted, the qualitative behavior of the youngest galaxies being CO-detected remains, and the decay timescale we measure is robust within a factor of 2 with our fiducial tPSB metric.
Paper: HST-COS Transit Spectroscopy of KELT-20b: First Detection of Excess Far-ultraviolet Absorption from an Ultrahot Jupiter
Authors: Patrick R. Behr, Kevin France, Luca Fossati, Tommi Koskinen, Patricio E. Cubillos, Arika Egan, P. Wilson Cauley
Figure caption: Out-of-transit 2D spectrum of KELT-20 before data reduction. Both axes are in units of detector pixels. Data are binned to 6 pixels in the dispersion direction and unbinned in the cross-dispersion direction. Denoted in the image are the strong Al II (λ1671) and C I (λ1657) absorption features, as well as detector locations that suffer from gain sag and background hot spots (see Section 2.1). The two background extraction regions are shown with horizontal red lines. The spectrum extraction region is shown with horizontal blue lines.
Paper: HST-COS Transit Spectroscopy of KELT-20b: First Detection of Excess Far-ultraviolet Absorption from an Ultrahot Jupiter
Authors: Patrick R. Behr, Kevin France, Luca Fossati, Tommi Koskinen, Patricio E. Cubillos, Arika Egan, P. Wilson Cauley
Figure caption: Same as Figure 1, but after data reduction. Events with SDQ flags and low PHA have been removed. The hot spot in segment B is not fully removed, so we shifted the lower background region upward 40 pixels in the cross-dispersion direction.
Paper: HST-COS Transit Spectroscopy of KELT-20b: First Detection of Excess Far-ultraviolet Absorption from an Ultrahot Jupiter
Authors: Patrick R. Behr, Kevin France, Luca Fossati, Tommi Koskinen, Patricio E. Cubillos, Arika Egan, P. Wilson Cauley
Figure caption: PHD for each COS detector segment. Distributions are shown as density plots to account for different exposure times. The dashed vertical lines show the upper and lower PHA limit set in calcos.
Paper: HST-COS Transit Spectroscopy of KELT-20b: First Detection of Excess Far-ultraviolet Absorption from an Ultrahot Jupiter
Authors: Patrick R. Behr, Kevin France, Luca Fossati, Tommi Koskinen, Patricio E. Cubillos, Arika Egan, P. Wilson Cauley
Figure caption: Comparison of the FUV Fe II line (1608 Å) and three coadded optical Fe II lines (5018, 5169, 5316 Å) from N. Casasayas-Barris et al. (2019). The light curves show the relative absorption of the line compared to the surrounding continuum. Beige squares show the HARPS-N optical light curve, and blue circles show the COS FUV light curve. The optical light curve is shown before applying corrections for the RM and CLV effects, resulting in a prominent “W” shape that does not appear in the FUV light curve.
Paper: HST-COS Transit Spectroscopy of KELT-20b: First Detection of Excess Far-ultraviolet Absorption from an Ultrahot Jupiter
Authors: Patrick R. Behr, Kevin France, Luca Fossati, Tommi Koskinen, Patricio E. Cubillos, Arika Egan, P. Wilson Cauley
Figure caption: Stellar intensity profile obtained from the averaged PHOENIX model with Teff ∼ 8800 K and ﹩\mathrm{log}(g)\sim 4.25﹩ cm s−2. The three intensity profiles shown are visible/near-IR as observed with Kepler (red), COS G160M segment A (blue), and COS G160M segment B (purple). Dashed gray lines over each intensity profile represent the best-fit model using the nonlinear limb-darkening law with coefficients retrieved from limb-darkening.
Paper: HST-COS Transit Spectroscopy of KELT-20b: First Detection of Excess Far-ultraviolet Absorption from an Ultrahot Jupiter
Authors: Patrick R. Behr, Kevin France, Luca Fossati, Tommi Koskinen, Patricio E. Cubillos, Arika Egan, P. Wilson Cauley
Figure caption: Top: overplot of the averaged PHOENIX model, convolved to the spectral resolution of COS G160M, with the coadded out-of-transit COS spectra. We note that because the PHOENIX model is in units of flux density, we have plotted the COS data using the flux-calibrated x1d files created by the calcos pipeline. Bottom: ratio of flux in the PHOENIX model to the out-of-transit COS spectrum.
Paper: HST-COS Transit Spectroscopy of KELT-20b: First Detection of Excess Far-ultraviolet Absorption from an Ultrahot Jupiter
Authors: Patrick R. Behr, Kevin France, Luca Fossati, Tommi Koskinen, Patricio E. Cubillos, Arika Egan, P. Wilson Cauley
Figure caption: Light curve of the KELT-20 b transit after removing all SDQ and low-PHA events. The light curves show a transit-level decrease in count rate over the five orbits. The solid black lines are linear fits to the count rates in orbits 1 and 5. Over the full duration of observation, the count rate decreases by 7.3 s−1 in segment B and by 28.1 s−1 in segment A. These trends are assumed to be due to instrument systematics as seen in other HST transit observations. The data are divided by the linear fits to obtain the final, fully corrected light curves.
Paper: HST-COS Transit Spectroscopy of KELT-20b: First Detection of Excess Far-ultraviolet Absorption from an Ultrahot Jupiter
Authors: Patrick R. Behr, Kevin France, Luca Fossati, Tommi Koskinen, Patricio E. Cubillos, Arika Egan, P. Wilson Cauley
Figure caption: Corner plot showing posterior distributions for the broadband planet-to-star radius ratio (Rp/R*) and time of midtransit (t0) retrieved from PyTransit. Blue distributions represent wavelengths 1410–1570 Å, and orange distributions represent wavelengths 1600–1760 Å. Time of midtransit (t0) is shown in hours.
Paper: HST-COS Transit Spectroscopy of KELT-20b: First Detection of Excess Far-ultraviolet Absorption from an Ultrahot Jupiter
Authors: Patrick R. Behr, Kevin France, Luca Fossati, Tommi Koskinen, Patricio E. Cubillos, Arika Egan, P. Wilson Cauley
Figure caption: CUTE broadband NUV light curves for visits 2–4. All data are shown after being processed with the CONTROL pipeline. Individual visits are shown with semitransparent circles at full temporal resolution. The final coadded light curve is shown with filled blue squares and is binned to a 90-minute cadence.
Paper: HST-COS Transit Spectroscopy of KELT-20b: First Detection of Excess Far-ultraviolet Absorption from an Ultrahot Jupiter
Authors: Patrick R. Behr, Kevin France, Luca Fossati, Tommi Koskinen, Patricio E. Cubillos, Arika Egan, P. Wilson Cauley
Figure caption: KELT-20 b transit light curve after removing events with SDQ flags or out-of-bounds PHA. The TESS optical light curve is plotted with green triangles for comparison.
Paper: HST-COS Transit Spectroscopy of KELT-20b: First Detection of Excess Far-ultraviolet Absorption from an Ultrahot Jupiter
Authors: Patrick R. Behr, Kevin France, Luca Fossati, Tommi Koskinen, Patricio E. Cubillos, Arika Egan, P. Wilson Cauley
Figure caption: Time series of low-PHA events in each detector segment for each orbit. Data are shown as the ratio of counts with PHA < 2 to the total counts in each bin. Orbit 1 shows excessive low-PHA counts in both detector segments.
Paper: HST-COS Transit Spectroscopy of KELT-20b: First Detection of Excess Far-ultraviolet Absorption from an Ultrahot Jupiter
Authors: Patrick R. Behr, Kevin France, Luca Fossati, Tommi Koskinen, Patricio E. Cubillos, Arika Egan, P. Wilson Cauley
Figure caption: R.A., decl., roll, and rms jitter during each orbit. R.A., decl., and roll are shown relative to the median value across all orbits.
Paper: HST-COS Transit Spectroscopy of KELT-20b: First Detection of Excess Far-ultraviolet Absorption from an Ultrahot Jupiter
Authors: Patrick R. Behr, Kevin France, Luca Fossati, Tommi Koskinen, Patricio E. Cubillos, Arika Egan, P. Wilson Cauley
Figure caption: Synthetic transmission spectra including various sets of opacities. The dashed–dotted blue line includes only CO. The dashed orange line includes CO, H, H2, He, and a Rayleigh scattering component. The solid red line includes all of the previous plus H I Lyα. The solid black line is the L. Fossati et al. (2023) NLTE model binned to the same resolution as the CO models (∼2 Å per bin). The NLTE model is provided in units of Rp/R* and has been converted to transit depth according to the simplified relation ﹩D={({R}_{p}/{R}_{* })}^{2}﹩, which we note does not account for stellar limb darkening. Purple circles represent our HST-COS observations.
Paper: HST-COS Transit Spectroscopy of KELT-20b: First Detection of Excess Far-ultraviolet Absorption from an Ultrahot Jupiter
Authors: Patrick R. Behr, Kevin France, Luca Fossati, Tommi Koskinen, Patricio E. Cubillos, Arika Egan, P. Wilson Cauley
Figure caption: Transit depth spectrum of KELT-20 b in the FUV through near-IR. Results from this work are shown with pentagon markers and are further divided by color: purple markers represent the COS 10 Å bins shown in Figure 15, yellow markers represent the COS broadband segment A and B depths, and red represents the CUTE NUV transit depth. The M. B. Lund et al. (2017) depth (circle) represents the photometric transit depth between 3900 and 9100 Å. The M. Stangret et al. (2024) data (diamonds) are measurements of several Fe II lines. The N. Casasayas-Barris et al. (2019) data (squares) are measurements of Hα, β, γ, Na I, Mg I, Fe II, and Ca II. The TESS transit depth (leftward-pointing triangle) is from the phase-folded light curve shown in Figure 7.
Paper: HST-COS Transit Spectroscopy of KELT-20b: First Detection of Excess Far-ultraviolet Absorption from an Ultrahot Jupiter
Authors: Patrick R. Behr, Kevin France, Luca Fossati, Tommi Koskinen, Patricio E. Cubillos, Arika Egan, P. Wilson Cauley
Figure caption: Comparison between the L. Fossati et al. (2023) NLTE transmission spectrum and the observed COS transit spectrum. The light-blue spectrum is the synthetic model convolved with a small boxcar kernel for visibility. The solid dark-blue line is the synthetic model binned to the same 10 Å bins as the COS spectrum. Horizontal dashed–dotted lines, circles, and squares represent the radii retrieved from PyTransit. Dashed–dotted lines represent the broadband values, circles the 10 Å wide spectral bins, and squares the atomic absorption lines discussed in Section 3.4.
Paper: A Deep Search for Exomoons around WISE 0855 with JWST
Authors: Mikayla J. Wilson, Mary Anne Limbach, Andrew J. Skemer, Johanna M. Vos, Brittany E. Miles, Melanie J. Rowland, Andrew Vanderburg, Adam C. Schneider, Caroline Morley, Brooke Kotten, Andrew Householder, Roxana Lupu, James Mang, Richard Freedman
Figure caption: Combined Spectrum of the 11 hr observation of WISE 0855 created from averaging the 44 spectra. The error bars are too small to be visible.
Paper: HST-COS Transit Spectroscopy of KELT-20b: First Detection of Excess Far-ultraviolet Absorption from an Ultrahot Jupiter
Authors: Patrick R. Behr, Kevin France, Luca Fossati, Tommi Koskinen, Patricio E. Cubillos, Arika Egan, P. Wilson Cauley
Figure caption: Top: broadband transit light-curve fit with the limb-darkened transit model described in Section 3.1.1. Blue circles represent wavelengths 1410–1570 Å, and orange squares represent wavelengths 1600–1760 Å. Solid lines show the respective best-fit model from PyTransit. Middle: residual of data and model fits. Marker shapes and colors are the same as in the top panel. Bottom: difference between segments A and B. Data are binned to 100 s.
Paper: HST-COS Transit Spectroscopy of KELT-20b: First Detection of Excess Far-ultraviolet Absorption from an Ultrahot Jupiter
Authors: Patrick R. Behr, Kevin France, Luca Fossati, Tommi Koskinen, Patricio E. Cubillos, Arika Egan, P. Wilson Cauley
Figure caption: Spectroscopic light curves in 10 Å bins at 300 s temporal cadence. Left: light curves for bins contained in detector segment B. Right: light curves for bins contained in detector segment A. Each panel is ordered with wavelength bins increasing along the y-axis, and each light curve has been shifted by 0.06 for clarity. Wavelengths are color-coded, with purple being the shortest and red being the longest. Each light curve has been fit with a PyTransit model using the radius and LDCs provided in Table 6.
Paper: HST-COS Transit Spectroscopy of KELT-20b: First Detection of Excess Far-ultraviolet Absorption from an Ultrahot Jupiter
Authors: Patrick R. Behr, Kevin France, Luca Fossati, Tommi Koskinen, Patricio E. Cubillos, Arika Egan, P. Wilson Cauley
Figure caption: Top: transit light curves of Al II and Si II binned to a 200 s cadence. Each transit has been fit with a “normal” limb-darkened transit model and a “W-shaped” limb-brightened model. Light-colored model fits are randomly drawn samples from the MCMC trials. Bottom: residuals between the COS observed transit and the two transit models.
Paper: HST-COS Transit Spectroscopy of KELT-20b: First Detection of Excess Far-ultraviolet Absorption from an Ultrahot Jupiter
Authors: Patrick R. Behr, Kevin France, Luca Fossati, Tommi Koskinen, Patricio E. Cubillos, Arika Egan, P. Wilson Cauley
Figure caption: Light curves for each of the atomic species listed in Table 4. For each panel, the blue squares represent the absorption-line light curve, and the orange circles represent the appropriate broadband region. The solid green line represents the PyTransit fit to the absorption line, and the thin orange line represents the fit to the broadband region.
Paper: A Deep Search for Exomoons around WISE 0855 with JWST
Authors: Mikayla J. Wilson, Mary Anne Limbach, Andrew J. Skemer, Johanna M. Vos, Brittany E. Miles, Melanie J. Rowland, Andrew Vanderburg, Adam C. Schneider, Caroline Morley, Brooke Kotten, Andrew Householder, Roxana Lupu, James Mang, Richard Freedman
Figure caption: Probability of an exomoon transit during the 11 hr WISE 0855 observation assuming a random orbital inclination angle. Different combinations of predicted radius and mass values for WISE 0855 are shown. The black line for each moon represents the extent of possible transit probabilities, given these various mass and radius uncertainties for the host. The largest Roche limit for an Io-like moon around the densest prediction of WISE 0855 is at 0.00177 au. Shown in gray is the distance range within which moons would be tidally disrupted.
Paper: A Deep Search for Exomoons around WISE 0855 with JWST
Authors: Mikayla J. Wilson, Mary Anne Limbach, Andrew J. Skemer, Johanna M. Vos, Brittany E. Miles, Melanie J. Rowland, Andrew Vanderburg, Adam C. Schneider, Caroline Morley, Brooke Kotten, Andrew Householder, Roxana Lupu, James Mang, Richard Freedman
Figure caption: The fraction of 50 transit injections recovered by the GP + transit model within 15 minutes of the injected time for each transit depth. The shaded regions represent the range of expected transit depths for Io and Titan mass analogs, based on the predicted mass and radii values of WISE 0855.
Paper: A Deep Search for Exomoons around WISE 0855 with JWST
Authors: Mikayla J. Wilson, Mary Anne Limbach, Andrew J. Skemer, Johanna M. Vos, Brittany E. Miles, Melanie J. Rowland, Andrew Vanderburg, Adam C. Schneider, Caroline Morley, Brooke Kotten, Andrew Householder, Roxana Lupu, James Mang, Richard Freedman
Figure caption: Probability of a transiting exomoon around WISE 0855, assuming a mass of 6.5 Mjup and a radius of ∼1 Rjup, random inclination angle, and 11 hr observation. Based off these conditions, we calculate the probability of a transit for exomoons at each of the Galilean moon separations for an increasing number of objects. The combined probability results in a 95% chance of a transiting exomoon after observing 18 WISE 0855–like objects that have Galilean analogs.
Paper: A Deep Search for Exomoons around WISE 0855 with JWST
Authors: Mikayla J. Wilson, Mary Anne Limbach, Andrew J. Skemer, Johanna M. Vos, Brittany E. Miles, Melanie J. Rowland, Andrew Vanderburg, Adam C. Schneider, Caroline Morley, Brooke Kotten, Andrew Householder, Roxana Lupu, James Mang, Richard Freedman
Figure caption: The time-series spectra with the full wavelength range (in microns) of the observations shown on the x-axis, observation time (in hours) on the y-axis, and a color bar representing the amplitude variability for any given flux value as a percentage deviation from the mean. The two wavelength regions used to construct the light curves are shown, where each has a distinct variability pattern. Region 1: negative, positive, negative positive amplitude; Region 2: negative, positive amplitude. The picket fence pattern (narrow striping) visible in region 2 is due to CO absorption.
Paper: A Deep Search for Exomoons around WISE 0855 with JWST
Authors: Mikayla J. Wilson, Mary Anne Limbach, Andrew J. Skemer, Johanna M. Vos, Brittany E. Miles, Melanie J. Rowland, Andrew Vanderburg, Adam C. Schneider, Caroline Morley, Brooke Kotten, Andrew Householder, Roxana Lupu, James Mang, Richard Freedman
Figure caption: Each curve represents transit duration for an edge-on system as a function of separation for a range of possible mass and radius values for WISE 0855 with the separations of the Galilean moons shown for reference. The black line emphasizes the extent of possible transit durations for each moon, given these various radius and mass combinations.
Paper: A Deep Search for Exomoons around WISE 0855 with JWST
Authors: Mikayla J. Wilson, Mary Anne Limbach, Andrew J. Skemer, Johanna M. Vos, Brittany E. Miles, Melanie J. Rowland, Andrew Vanderburg, Adam C. Schneider, Caroline Morley, Brooke Kotten, Andrew Householder, Roxana Lupu, James Mang, Richard Freedman
Figure caption: Panel (A): the light curves of WISE 0855 built from the two different wavelength regions are shown in black with an injected 0.3% transit (Mars-sized) at ∼4.2 hr. The solid lines represent the fit produced by the GP + transit model. Panel (B): the flattened light curves of each region are shown after subtracting the GP portion of the GP + transit model’s fit, revealing the injected Mars-sized 0.3% transit at ∼4.2 hr.
Paper: A Deep Search for Exomoons around WISE 0855 with JWST
Authors: Mikayla J. Wilson, Mary Anne Limbach, Andrew J. Skemer, Johanna M. Vos, Brittany E. Miles, Melanie J. Rowland, Andrew Vanderburg, Adam C. Schneider, Caroline Morley, Brooke Kotten, Andrew Householder, Roxana Lupu, James Mang, Richard Freedman
Figure caption: Histograms of the 50 Δlogz values for each transit depth, with nondetections in purple stacked on top of the successful detections (i.e., retrieved transit time within 15 minutes of injected time) in green.
Paper: A Deep Search for Exomoons around WISE 0855 with JWST
Authors: Mikayla J. Wilson, Mary Anne Limbach, Andrew J. Skemer, Johanna M. Vos, Brittany E. Miles, Melanie J. Rowland, Andrew Vanderburg, Adam C. Schneider, Caroline Morley, Brooke Kotten, Andrew Householder, Roxana Lupu, James Mang, Richard Freedman
Figure caption: The results of the 50 injection tests for each of the 6 transit depths, where the green points are detections (i.e., the retrieved time is within 15 minutes of the injected time) and purple Xs are nondetections.