adsabs/AstroCLIMB huggingface dataset:
Paper: Eleven New Transiting Brown Dwarfs and Very-low-mass Stars from TESS
Authors: Noah Vowell, Joseph E. Rodriguez, David W. Latham, Samuel N. Quinn, Jack Schulte, Jason D. Eastman, Allyson Bieryla, Khalid Barkaoui, David R. Ciardi, Karen A. Collins, Eric Girardin, Guillaume Hébrard, Elisabeth Heldridge, Marziye Jafariyazani, Brooke Kotten, Luigi Mancini, Felipe Murgas, Norio Narita, D. J. Radford, Howard M. Relles, Avi Shporer, Melinda Soares-Furtado, Ivan A. Strakhov, Carl Ziegler, Isabelle Boisse, César Briceño, Michael L. Calkins, Catherine A. Clark, Kevin I. Collins, Jerome de Leon, Gilbert A. Esquerdo, Sergio B. Fajardo-Acosta, Thierry Forveille, Akihiko Fukui, Cristilyn N. Watkins, Ruixuan He, Neda Heidari, Keith Horne, Jon M. Jenkins, Andrew W. Mann, Luca Naponiello, Enric Palle, Richard P. Schwarz, S. Seager, John Southworth, Gregor Srdoc, Jonathan J. Swift, Joshua N. Winn
Figure caption: Same as Figure 2 except for TOI-3577. TOI-3577’s fit resulted in a bimodal solution. We characterized both solutions independently as described in Section 3, and they are both are shown in the bottom-right plot.
Paper: Eleven New Transiting Brown Dwarfs and Very-low-mass Stars from TESS
Authors: Noah Vowell, Joseph E. Rodriguez, David W. Latham, Samuel N. Quinn, Jack Schulte, Jason D. Eastman, Allyson Bieryla, Khalid Barkaoui, David R. Ciardi, Karen A. Collins, Eric Girardin, Guillaume Hébrard, Elisabeth Heldridge, Marziye Jafariyazani, Brooke Kotten, Luigi Mancini, Felipe Murgas, Norio Narita, D. J. Radford, Howard M. Relles, Avi Shporer, Melinda Soares-Furtado, Ivan A. Strakhov, Carl Ziegler, Isabelle Boisse, César Briceño, Michael L. Calkins, Catherine A. Clark, Kevin I. Collins, Jerome de Leon, Gilbert A. Esquerdo, Sergio B. Fajardo-Acosta, Thierry Forveille, Akihiko Fukui, Cristilyn N. Watkins, Ruixuan He, Neda Heidari, Keith Horne, Jon M. Jenkins, Andrew W. Mann, Luca Naponiello, Enric Palle, Richard P. Schwarz, S. Seager, John Southworth, Gregor Srdoc, Jonathan J. Swift, Joshua N. Winn
Figure caption: Same as Figure 4 except for TOI-4462. Both TOI-4462 A and B are shown in the bottom left. The EXOFASTv2 models for TOI-4462 A and B are 5970 K and 4660 K, respectively.
Paper: Eleven New Transiting Brown Dwarfs and Very-low-mass Stars from TESS
Authors: Noah Vowell, Joseph E. Rodriguez, David W. Latham, Samuel N. Quinn, Jack Schulte, Jason D. Eastman, Allyson Bieryla, Khalid Barkaoui, David R. Ciardi, Karen A. Collins, Eric Girardin, Guillaume Hébrard, Elisabeth Heldridge, Marziye Jafariyazani, Brooke Kotten, Luigi Mancini, Felipe Murgas, Norio Narita, D. J. Radford, Howard M. Relles, Avi Shporer, Melinda Soares-Furtado, Ivan A. Strakhov, Carl Ziegler, Isabelle Boisse, César Briceño, Michael L. Calkins, Catherine A. Clark, Kevin I. Collins, Jerome de Leon, Gilbert A. Esquerdo, Sergio B. Fajardo-Acosta, Thierry Forveille, Akihiko Fukui, Cristilyn N. Watkins, Ruixuan He, Neda Heidari, Keith Horne, Jon M. Jenkins, Andrew W. Mann, Luca Naponiello, Enric Palle, Richard P. Schwarz, S. Seager, John Southworth, Gregor Srdoc, Jonathan J. Swift, Joshua N. Winn
Figure caption: Same as Figure 2 except for TOI-3122.
Paper: Eleven New Transiting Brown Dwarfs and Very-low-mass Stars from TESS
Authors: Noah Vowell, Joseph E. Rodriguez, David W. Latham, Samuel N. Quinn, Jack Schulte, Jason D. Eastman, Allyson Bieryla, Khalid Barkaoui, David R. Ciardi, Karen A. Collins, Eric Girardin, Guillaume Hébrard, Elisabeth Heldridge, Marziye Jafariyazani, Brooke Kotten, Luigi Mancini, Felipe Murgas, Norio Narita, D. J. Radford, Howard M. Relles, Avi Shporer, Melinda Soares-Furtado, Ivan A. Strakhov, Carl Ziegler, Isabelle Boisse, César Briceño, Michael L. Calkins, Catherine A. Clark, Kevin I. Collins, Jerome de Leon, Gilbert A. Esquerdo, Sergio B. Fajardo-Acosta, Thierry Forveille, Akihiko Fukui, Cristilyn N. Watkins, Ruixuan He, Neda Heidari, Keith Horne, Jon M. Jenkins, Andrew W. Mann, Luca Naponiello, Enric Palle, Richard P. Schwarz, S. Seager, John Southworth, Gregor Srdoc, Jonathan J. Swift, Joshua N. Winn
Figure caption: Same as Figure 2 except for TOI-3755.
Paper: Thermal and Optical Characterization of Near-Earth Objects: Science Commissioning of the Recently Upgraded Mid-infrared Camera MIRSI on the NASA Infrared Telescope Facility
Authors: Andy J. López-Oquendo, Joseph L. Hora, David E. Trilling, Howard A. Smith
Figure caption: Predicted N-band flux as a function of solar system absolute magnitude HV for all observable NEOs from the NASA-IRTF during a given observing semester. The top axis is the estimated diameter from HV assuming a 15% albedo in the A. W. Harris & J. S. V. Lagerros (2002) relationship. Each circle’s color indicates the visible magnitude of the NEO at the time it reached peak in brightness. Yellow represents fainter objects (larger visible magnitude), while purple represents brighter ones.
Paper: Thermal and Optical Characterization of Near-Earth Objects: Science Commissioning of the Recently Upgraded Mid-infrared Camera MIRSI on the NASA Infrared Telescope Facility
Authors: Andy J. López-Oquendo, Joseph L. Hora, David E. Trilling, Howard A. Smith
Figure caption: Mid-IR mosaics of NEO 7482 obtained with MIRSI’s 7.7 (top-left), 8.7 (top-right), 11.7 (bottom-left), and 12.5 μm (bottom-right) filters. Each image size is about 26﹩\mathop{.}\limits^{^{\prime\prime} }﹩7 horizontally and 21﹩\mathop{.}\limits^{^{\prime\prime} }﹩4 vertically.
Paper: A Detailed Investigation of HD 209458 b HST and JWST Transmission Spectra with SANSAR
Authors: Avinash Verma, Jayesh Goyal, Swaroop Avarsekar, Gaurav Shukla
Figure caption: Retrieved transmission spectra, abundance constraints, and P-T profile with free-chemistry retrievals. The top panel consists of median transmission spectra and P-T profiles of HD 209458 b for the three retrievals, JWST (NIRCam), HST WFC3 + JWST NIRCam, and HST STIS + HST WFC3 + JWST NIRCam. All the spectra shown here are generated with 5000 random equal-weighted samples from PyMultiNest and binned at a resolution of R ∼ 200. The shaded region indicates the 1σ uncertainty in the median fit. JWST observations are represented in green, while combined STIS and WFC3 observations are shown in brown. A retrieved median offset of 204 ppm is applied to the HST observations, whereas the offset for WFC3 in the case of the WFC3+NIRCam combination is not shown here. For all the retrievals, the corresponding P-T profiles are shown beside the median spectra. The middle panel shows the posteriors of the logarithm of mixing ratios of the ten molecules for three retrievals. The bottom panel shows the posteriors of the clouds and hazes parameters.
Paper: A Detailed Investigation of HD 209458 b HST and JWST Transmission Spectra with SANSAR
Authors: Avinash Verma, Jayesh Goyal, Swaroop Avarsekar, Gaurav Shukla
Figure caption: LBL transmission spectra comparison with opacity sampling at a resolution of 1000, 20,000, and 100,000 (all resolutions finally binned to R ∼ 100 for comparison) and with correlated-k at R ∼ 1000. Residuals compared with LBL are shown at the bottom, and the maximum error in each case is shown in the legend.
Paper: A Detailed Investigation of HD 209458 b HST and JWST Transmission Spectra with SANSAR
Authors: Avinash Verma, Jayesh Goyal, Swaroop Avarsekar, Gaurav Shukla
Figure caption: Benchmarking of SANSAR retrieval with other widely used retrieval models using WASP-96 b observations from M. Radica et al. (2023) and model results from J. Taylor et al. (2023). Opacity sampling and correlated-k median transmission spectra are represented by light blue and violet colors, respectively, with 1σ uncertainty. The temperature profile is shown for both opacity sampling and correlated-k along with the 1σ error bar, whereas the median retrieved temperature profiles from POSEIDON (black), CHIMERA (red), and Aurora (blue) are also plotted on top. The bottom panel shows the posteriors of different chemical species as well as cloud and haze parameters, along with the values retrieved by other models. The median values of the posteriors from POSEIDON, CHIMERA, and Aurora are shown as solid lines.
Paper: A Detailed Investigation of HD 209458 b HST and JWST Transmission Spectra with SANSAR
Authors: Avinash Verma, Jayesh Goyal, Swaroop Avarsekar, Gaurav Shukla
Figure caption: Contribution of different gases to the best-fit spectrum obtained from the free-chemistry retrieval, binned down to R ∼ 200, for STIS+WFC3+NIRCam observations.
Paper: A Detailed Investigation of HD 209458 b HST and JWST Transmission Spectra with SANSAR
Authors: Avinash Verma, Jayesh Goyal, Swaroop Avarsekar, Gaurav Shukla
Figure caption: Comparison between transmission spectra computed using the correlated-k opacity method and those from LBL calculations. The LBL spectra have been binned to a correlated-k wavelength grid (R ∼ 1000). Residuals are shown in the bottom panel.
Paper: A Detailed Investigation of HD 209458 b HST and JWST Transmission Spectra with SANSAR
Authors: Avinash Verma, Jayesh Goyal, Swaroop Avarsekar, Gaurav Shukla
Figure caption: Comparison of forward models generated with SANSAR and ATMO for a WASP-96 b–type planet. Both models were generated with the correlated-k method at a resolution of R ∼ 1000 and binned to R ∼ 200 for comparison.
Paper: A Detailed Investigation of HD 209458 b HST and JWST Transmission Spectra with SANSAR
Authors: Avinash Verma, Jayesh Goyal, Swaroop Avarsekar, Gaurav Shukla
Figure caption: Comparison of the SANSAR forward model with POSEIDON for a WASP-96 b–type planet. Both SANSAR and POSEIDON use the POKAZATEL line list here. SANSAR samples lines from a 0.001 cm−1 opacity file, contrary to POSEIDON, which uses an opacity file with a resolution of 0.01 cm−1.
Paper: A Detailed Investigation of HD 209458 b HST and JWST Transmission Spectra with SANSAR
Authors: Avinash Verma, Jayesh Goyal, Swaroop Avarsekar, Gaurav Shukla
Figure caption: Ray diagram showing the calculation of path length traveled by a ray in an exoplanetary atmosphere at an arbitrary impact parameter b. Here, riup is the upper boundary radius of a layer, ﹩d{l}_{\,\rm{agg}\,}^{i}﹩ is the total path length traveled by the ray in the half geometry until the i − 1 layer, and dli is the path length of the ray in the ith layer.
Paper: A Detailed Investigation of HD 209458 b HST and JWST Transmission Spectra with SANSAR
Authors: Avinash Verma, Jayesh Goyal, Swaroop Avarsekar, Gaurav Shukla
Figure caption: Heat map showing the predicted abundances of major chemical species in HD 209458 b at the 1 mbar pressure level. These values are obtained using FastChem while varying C/H for different C/O values.
Paper: A Detailed Investigation of HD 209458 b HST and JWST Transmission Spectra with SANSAR
Authors: Avinash Verma, Jayesh Goyal, Swaroop Avarsekar, Gaurav Shukla
Figure caption: Heat map showing the predicted abundances of major chemical species in HD 209458 b at the 1 mbar pressure level. These values are obtained using FastChem while varying O/H for different C/O values.
Paper: A Detailed Investigation of HD 209458 b HST and JWST Transmission Spectra with SANSAR
Authors: Avinash Verma, Jayesh Goyal, Swaroop Avarsekar, Gaurav Shukla
Figure caption: Retrieved posterior of different parameters for HD 209458b with free chemistry assumption obtained with WFC3+NIRCam observations. Here also, retrieval was performed with the correlated-k method.
Paper: Silkscreen: Direct Measurements of Galaxy Distances from Survey Image Cutouts
Authors: Tim B. Miller, Imad Pasha, Ava Polzin, Pieter van Dokkum
Figure caption: Silkscreen-inferred distances compared to previously measured values in the literature. Left: 1:1 plot comparing the literature distance to Silkscreen, with Silkscreen 1σ uncertainties generated from the learned posteriors. Though in this work we are considering literature distances as a ground truth, the SBF measurements do have formal uncertainties that are in some cases similar to those from Silkscreen; thus, for reference we show the SBF uncertainties as x errors. Reported uncertainties for TRGB distances measured with HST are typically much smaller (≲3%); we do not plot these here. The color of the points denotes which imaging survey is used for Silkscreen inference: blue for DECaLS (A. Dey et al. 2019) and purple for HSC-SSP (H. Aihara et al. 2018). The shape of the marker denotes how the literature value is measured, with a circle for TRGB measurements using HST imaging, and a square for SBF measurements from ground-based imaging. Note that the distance on each axis is on a log scale. We find generally good agreement: For 15 of the 20 galaxies, the Silkscreen measured distance matches that from the literature within uncertainties. For the other five, the literature distance lies outside the 5%–95% percentile of the posterior predicted by Silkscreen. Top Right: Precision of Silkscreen, measured as the ratio of the standard deviation of the distance estimate (calculated as half of the difference between the 16th and 84th percentile) and the median inferred distance. We find the median precision to be ∼15%, but we note that the precision is better for the HSC-SSP Wide sample than the overall average, while the shallower DECaLS is worse. Also shown is the precision of the injection test presented in Figure 3, which used HSC-SSP survey properties. Bottom Right: We assess the accuracy by plotting the ratio of Silkscreen-inferred distance to literature distance, normalized by the literature distance. In both precision and accuracy, we find no notable trends with galaxy distance.
Paper: Silkscreen: Direct Measurements of Galaxy Distances from Survey Image Cutouts
Authors: Tim B. Miller, Imad Pasha, Ava Polzin, Pieter van Dokkum
Figure caption: Comparison of the distances measured by Silkscreen using two different parameterizations of the youngest population of stars: Shown on the horizontal axis is the fiducial continuous SFH between 50 and 250 Myr, while that shown on the vertical axis assumes a fixed age of this population of 75 Myr. The color scheme is the same as in Figure 10, where blue denotes when DECaLs data are used and purple indicates HSC data. For most of the galaxies, the distances agree between the two parameterizations; however, there are some galaxies where the fixed age model produces a lower distance, by up to a factor of two.
Paper: Silkscreen: Direct Measurements of Galaxy Distances from Survey Image Cutouts
Authors: Tim B. Miller, Imad Pasha, Ava Polzin, Pieter van Dokkum
Figure caption: The joint posterior distributions and posterior predictive images produced by Silkscreen. Similar to Section 4.2 in the main text, here we show the posterior distribution for the four successive rounds of training and the observed image alongside posterior predictive images. Literature distances are denoted with a solid black line in the corner plots.
Paper: Silkscreen: Direct Measurements of Galaxy Distances from Survey Image Cutouts
Authors: Tim B. Miller, Imad Pasha, Ava Polzin, Pieter van Dokkum
Figure caption: Continuation of Figure 12, but focused on the galaxies for which the Silkscreen-inferred distance does match the literature value. We choose these when the literature distances lie outside the 5%–95% percentile range of the posteriors produced by Silkscreen.
Paper: Silkscreen: Direct Measurements of Galaxy Distances from Survey Image Cutouts
Authors: Tim B. Miller, Imad Pasha, Ava Polzin, Pieter van Dokkum
Figure caption: Continuation of Figure 17, focusing on two more galaxies with discrepant literature and Silkscreen distances.
Paper: Silkscreen: Direct Measurements of Galaxy Distances from Survey Image Cutouts
Authors: Tim B. Miller, Imad Pasha, Ava Polzin, Pieter van Dokkum
Figure caption: Continuation of Figure 12.
Paper: The Multiband Imaging Survey for High-alpha PlanetS (MISHAPS). I. Preliminary Constraints on the Occurrence Rate of Hot Jupiters in 47 Tucanae
Authors: Alison L. Crisp, Jonas Klüter, Marz L. Newman, Matthew T. Penny, Thomas G. Beatty, L. Ilsedore Cleeves, Karen A. Collins, Jennifer A. Johnson, Marshall C. Johnson, Michael B. Lund, Clara E. Martínez-Vázquez, Melissa K. Ness, Joseph E. Rodriguez, Robert Siverd, Daniel J. Stevens, Steven Villanueva, Carl Ziegler
Figure caption: Example of injected full and partial transits of a 1.26RJup planet orbiting a 0.59R⊙, r = 19.9 star in our data with P = 0.97 days. Each panel shows a different night, with the top two panels showing nights flagged as having full transits, and the bottom two showing nights flagged as partial. The r-band data are shown in blue, and the z-band data are shown in red. The black line is the injected model, and the green line is the best boxcar model. We note that the top-left transit is actually a partial transit since we do not capture the full egress in the data, but the algorithm flags it as a full transit based on its best S/N, tc, and τ. Our detection algorithm was able to successfully recover both the full and partial transits with S/N >7.
Paper: The Multiband Imaging Survey for High-alpha PlanetS (MISHAPS). I. Preliminary Constraints on the Occurrence Rate of Hot Jupiters in 47 Tucanae
Authors: Alison L. Crisp, Jonas Klüter, Marz L. Newman, Matthew T. Penny, Thomas G. Beatty, L. Ilsedore Cleeves, Karen A. Collins, Jennifer A. Johnson, Marshall C. Johnson, Michael B. Lund, Clara E. Martínez-Vázquez, Melissa K. Ness, Joseph E. Rodriguez, Robert Siverd, Daniel J. Stevens, Steven Villanueva, Carl Ziegler
Figure caption: r vs. (r − z) color–magnitude diagram of our field, with only the DOPHOT type cut applied (black). Our final selection of stars is overplotted in red, and the proper-motion-selected SMC stars (selected using the same procedure as for 47 Tuc stars) are overplotted in gold. The remaining black points are targets which either lie outside the 3σ 47 Tuc and SMC proper motion selections, or have no Gaia matches.
Paper: The Multiband Imaging Survey for High-alpha PlanetS (MISHAPS). I. Preliminary Constraints on the Occurrence Rate of Hot Jupiters in 47 Tucanae
Authors: Alison L. Crisp, Jonas Klüter, Marz L. Newman, Matthew T. Penny, Thomas G. Beatty, L. Ilsedore Cleeves, Karen A. Collins, Jennifer A. Johnson, Marshall C. Johnson, Michael B. Lund, Clara E. Martínez-Vázquez, Melissa K. Ness, Joseph E. Rodriguez, Robert Siverd, Daniel J. Stevens, Steven Villanueva, Carl Ziegler
Figure caption: Scaled median absolute deviation (MAD, a robust estimate of rms) of lightcurve photometry in our observations of 19,930 47 Tuc stars compared to the transit depths of planets orbiting 47 Tuc stars. Data from bad nights are removed prior to calculating this statistic. The black lines show predicted transit depths for 1.3RJup (dashed–dotted), 1RJup (dotted), and 0.8RJup (dashed) planets computed using a 47 Tuc–compatible isochrone to estimate stellar radii. The points show the MAD scaled to approximate the Gaussian σ of r-band (blue) and z-band (red) observations of 47 Tuc. The solid lines show the median MAD vs. r magnitude for r-band (blue) and z-band (red) observations.
Paper: The Multiband Imaging Survey for High-alpha PlanetS (MISHAPS). I. Preliminary Constraints on the Occurrence Rate of Hot Jupiters in 47 Tucanae
Authors: Alison L. Crisp, Jonas Klüter, Marz L. Newman, Matthew T. Penny, Thomas G. Beatty, L. Ilsedore Cleeves, Karen A. Collins, Jennifer A. Johnson, Marshall C. Johnson, Michael B. Lund, Clara E. Martínez-Vázquez, Melissa K. Ness, Joseph E. Rodriguez, Robert Siverd, Daniel J. Stevens, Steven Villanueva, Carl Ziegler
Figure caption: Vector-point proper motion diagram plotting Gaia DR3 μα and μδ. Our color- and proper-motion-based stellar selection for 47 Tuc is plotted in red. The gold points correspond with likely SMC stars. The black points scattered across the field are other stars, likely foreground Milky Way stars.
Paper: The Multiband Imaging Survey for High-alpha PlanetS (MISHAPS). I. Preliminary Constraints on the Occurrence Rate of Hot Jupiters in 47 Tucanae
Authors: Alison L. Crisp, Jonas Klüter, Marz L. Newman, Matthew T. Penny, Thomas G. Beatty, L. Ilsedore Cleeves, Karen A. Collins, Jennifer A. Johnson, Marshall C. Johnson, Michael B. Lund, Clara E. Martínez-Vázquez, Melissa K. Ness, Joseph E. Rodriguez, Robert Siverd, Daniel J. Stevens, Steven Villanueva, Carl Ziegler
Figure caption: Transformation plots to transform our data from NSC magnitudes to PS1 magnitudes (top row), and between PS1 magnitudes (bottom row). The CMDs of the data sets used to calculate the transforms are shown in black points. The functions generated by the spline fits are shown with the solid red lines in the upper panels. The binned medians of the fit data are shown with the dashed blue lines. The knots of the splines are indicated by the yellow circles. In the smaller panels, the residuals of sigma-clipped data are plotted as a function of magnitude with black points, their binned medians are plotted with solid red lines, and a residual of zero is noted with dashed blue lines.
Paper: The Multiband Imaging Survey for High-alpha PlanetS (MISHAPS). I. Preliminary Constraints on the Occurrence Rate of Hot Jupiters in 47 Tucanae
Authors: Alison L. Crisp, Jonas Klüter, Marz L. Newman, Matthew T. Penny, Thomas G. Beatty, L. Ilsedore Cleeves, Karen A. Collins, Jennifer A. Johnson, Marshall C. Johnson, Michael B. Lund, Clara E. Martínez-Vázquez, Melissa K. Ness, Joseph E. Rodriguez, Robert Siverd, Daniel J. Stevens, Steven Villanueva, Carl Ziegler
Figure caption: Radius estimation results. Top panel: the resultant radius estimates of our full field vs. r magnitude, with our final stellar selection highlighted in red. The radii for a MIST isochrone calculated for the Pan-STARRS photometric system are given by the gold line. Bottom panel: the residual between our stellar sample’s radii and the isochrone’s. The median residual is given by the red dashed line.
Paper: The Multiband Imaging Survey for High-alpha PlanetS (MISHAPS). I. Preliminary Constraints on the Occurrence Rate of Hot Jupiters in 47 Tucanae
Authors: Alison L. Crisp, Jonas Klüter, Marz L. Newman, Matthew T. Penny, Thomas G. Beatty, L. Ilsedore Cleeves, Karen A. Collins, Jennifer A. Johnson, Marshall C. Johnson, Michael B. Lund, Clara E. Martínez-Vázquez, Melissa K. Ness, Joseph E. Rodriguez, Robert Siverd, Daniel J. Stevens, Steven Villanueva, Carl Ziegler
Figure caption: Simplified version of the MISHAPS lightcurve classification workflow. The rightmost panel shows the tools users are given, while the rest show individual nights of the lightcurve. A blue panel indicates a full transit as flagged by the search algorithm, a gray panel indicates a partial transit, and a pink panel indicates a bad night (see Section 2.2 for discussion on how bad nights were selected). In the full Zooniverse workflow, users have the same tools but are presented with all 24 nights of the lightcurves.
Paper: The Multiband Imaging Survey for High-alpha PlanetS (MISHAPS). I. Preliminary Constraints on the Occurrence Rate of Hot Jupiters in 47 Tucanae
Authors: Alison L. Crisp, Jonas Klüter, Marz L. Newman, Matthew T. Penny, Thomas G. Beatty, L. Ilsedore Cleeves, Karen A. Collins, Jennifer A. Johnson, Marshall C. Johnson, Michael B. Lund, Clara E. Martínez-Vázquez, Melissa K. Ness, Joseph E. Rodriguez, Robert Siverd, Daniel J. Stevens, Steven Villanueva, Carl Ziegler
Figure caption: Histogram showing the S/N of nights with (yellow) and without (blue) injected transits. The dotted red line indicates our chosen S/N ≥ 7 threshold. The solid and dashed black lines represent the probability of a lightcurve containing a detection of a given S/N for nights with and without injected transits, respectively.