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Paper: The Lingering Death of Periodic Near-Sun Comet 323P/SOHO
Authors: Man-To Hui, 文韜 許, David J. Tholen, Rainer Kracht, Chan-Kao Chang, 展誥 章, Paul A. Wiegert, Quan-Zhi Ye, 泉志 葉, Max Mutchler
Figure caption: The appearance of 323P in our Subaru (2020 December 21, r-band), CFHT (2021 February 6, 8, and 11, gri filter), LDT (2021 February 16, r and VR filters), and GN (2021 February 13 and March 3, r-band) images from late 2020 December to early 2021 March. Each panel is median combined from individual exposures in the aforementioned corresponding filters from the same observing night, with registration on the comet and background sources masked out, except for the Subaru panel, which is an average from the background-offset image sequence and then convolved with a Gaussian of two pixels in FWHM so as to cosmetically suppress background noise. The antisolar direction ( −⊙ ) and the negative heliocentric velocity of the comet projected onto the sky plane (− V ) are shown as the arrows. Corresponding scale bars are given in each panel. Equatorial J2000 north is up and east is left.
Paper: The Lingering Death of Periodic Near-Sun Comet 323P/SOHO
Authors: Man-To Hui, 文韜 許, David J. Tholen, Rainer Kracht, Chan-Kao Chang, 展誥 章, Paul A. Wiegert, Quan-Zhi Ye, 泉志 葉, Max Mutchler
Figure caption: Same as Figure 1, but in HST/WFC3 median combined images from 2021 March. Two fragments, labeled “A” and “B,” respectively, and pointed out by the two arrows, can be seen in the upper two panels. A common scale bar of 5″ is shown at the bottom. Equatorial J2000 north is up and east is left.
Paper: The Lingering Death of Periodic Near-Sun Comet 323P/SOHO
Authors: Man-To Hui, 文韜 許, David J. Tholen, Rainer Kracht, Chan-Kao Chang, 展誥 章, Paul A. Wiegert, Quan-Zhi Ye, 泉志 葉, Max Mutchler
Figure caption: Folded rotational light curve of the nucleus of 323P/SOHO before (a) and after (b) removal of effects from the aspect change and the rotational light-curve amplitude enhancement, with rotation period P rot = 0.5220 hr and the 1σ formal error thereof ∼2 × 10−6 hr. The epoch at which the earliest Subaru observation from 2020 December 21 was taken is set to be the reference. The black dashed curve is the best-fit third-order Fourier function described in Section 4.2. Measurements from different observatories are distinguished according to the symbols shown in the legend. Note that the g- and i-band data in the plot (in colors different from the r-band data points) have already been converted to the r-band using the measured color indices from the corresponding nights (see Section 4.1).
Paper: The Lingering Death of Periodic Near-Sun Comet 323P/SOHO
Authors: Man-To Hui, 文韜 許, David J. Tholen, Rainer Kracht, Chan-Kao Chang, 展誥 章, Paul A. Wiegert, Quan-Zhi Ye, 泉志 葉, Max Mutchler
Figure caption: Color comparison of the dust and the nucleus of 323P from the two GN epochs (2021 February 12 and March 3) with various solar system bodies, including the Sun (Willmer 2018), near-Sun comets 322P (Knight et al. 2016) and 96P (Eisner et al. 2019), Kuiper-belt objects (KBOs; Solontoi et al. 2012, and citations therein), Centaurs, Jupiter Trojans, active Jupiter-family comets (JFCs) and their nuclei, active long-period comets and their nuclei, and Damocloids (Jewitt 2015, and citations therein), in the g − r vs. r − i space. Also plotted are typical colors of main-belt asteroid taxonomic classes (Dandy et al. 2003). Color transformations to the SDSS system were performed according to Jordi et al. (2006). The dashed curve is the locus of objects having linear reflectivity spectra. Objects below the curve have concave reflectivity spectra, otherwise convex, in the ﹩g-i﹩ regime.
Paper: The Lingering Death of Periodic Near-Sun Comet 323P/SOHO
Authors: Man-To Hui, 文韜 許, David J. Tholen, Rainer Kracht, Chan-Kao Chang, 展誥 章, Paul A. Wiegert, Quan-Zhi Ye, 泉志 葉, Max Mutchler
Figure caption: Colors of (a) the dust ejecta and (b) the nucleus of 323P/SOHO in the g − r (blue) and r − i (red) regimes. In the left panel, symbols in lighter colors are measurements from circular apertures of fixed linear radii, whereas those in darker colors are from annular apertures. In the right panel, the measurements with larger fixed seeing apertures are used as quality checks. Results from 2021 February 13 and March 3 are plotted as diamonds and squares, respectively. For comparison, the color indices of the Sun are shown as the light blue and red stripes in the background (associated uncertainties included) in either panel.
Paper: The Lingering Death of Periodic Near-Sun Comet 323P/SOHO
Authors: Man-To Hui, 文韜 許, David J. Tholen, Rainer Kracht, Chan-Kao Chang, 展誥 章, Paul A. Wiegert, Quan-Zhi Ye, 泉志 葉, Max Mutchler
Figure caption: Goodness of fit ﹩{\chi }_{\mathrm{rel}}^{2}﹩ as function of rotational pole orientation in terms of the J2000 ecliptic coordinates, obtained with the light-curve inversion software package from DAMIT using the relative light curves. As indicated by the color bar, the quality of the fit is color coded. The result with the calibrated light curves is visually similar and is therefore omitted for brevity. Basically, the best pole solutions are concentrated around λ p ≈ 90° ± 70° and 270° ± 70° (possible mirror solutions) in ecliptic longitude, and β p ≈ −50° ± 30° in ecliptic latitude.
Paper: The Lingering Death of Periodic Near-Sun Comet 323P/SOHO
Authors: Man-To Hui, 文韜 許, David J. Tholen, Rainer Kracht, Chan-Kao Chang, 展誥 章, Paul A. Wiegert, Quan-Zhi Ye, 泉志 葉, Max Mutchler
Figure caption: Convex shape model of the nucleus of 323P/SOHO in three orthogonal views, derived with the light-curve inversion software package from DAMIT using the calibrated light curves. The left and middle panels show edge-on views of the nucleus that are 90° apart from each other, with its spin axis (the Z-axis) pointing upwards, while the nucleus is viewed in a pole-on configuration (the line of sight along the negative Z direction) in the right panel.
Paper: The Lingering Death of Periodic Near-Sun Comet 323P/SOHO
Authors: Man-To Hui, 文韜 許, David J. Tholen, Rainer Kracht, Chan-Kao Chang, 展誥 章, Paul A. Wiegert, Quan-Zhi Ye, 泉志 葉, Max Mutchler
Figure caption: Periodogram of the nucleus of 323P/SOHO using relative light curves. The best solution (with a global minimum of ﹩{\chi }_{\mathrm{rel}}^{2}\approx 0.7﹩, corresponding to a rotation period of P rot ≈ 0.522 hr) is indicated by the red circle. The second best solution on the left side has half of the best period.
Paper: The Lingering Death of Periodic Near-Sun Comet 323P/SOHO
Authors: Man-To Hui, 文韜 許, David J. Tholen, Rainer Kracht, Chan-Kao Chang, 展誥 章, Paul A. Wiegert, Quan-Zhi Ye, 泉志 葉, Max Mutchler
Figure caption: Phase function of the nucleus of 323P/SOHO. For clarity, the data points are weighted mean values of individual measurements from the same runs. As indicated in the legend, different symbols correspond to measurements from different telescopes. The best-fitted linear, H, G, and H, G 12 phase-function models are shown as the blue dashed, red solid, and gold dashed lines, respectively.
Paper: The Lingering Death of Periodic Near-Sun Comet 323P/SOHO
Authors: Man-To Hui, 文韜 許, David J. Tholen, Rainer Kracht, Chan-Kao Chang, 展誥 章, Paul A. Wiegert, Quan-Zhi Ye, 泉志 葉, Max Mutchler
Figure caption: Mean rms residual of the best-fitted nongravitational orbital solution for 323P/SOHO vs. the slope index of the power-law nongravitational force model ﹩\sim {r}_{{\rm{H}}}^{-n}﹩. The local minimum of the rms residual is reached when n = 8.50.
Paper: The Lingering Death of Periodic Near-Sun Comet 323P/SOHO
Authors: Man-To Hui, 文韜 許, David J. Tholen, Rainer Kracht, Chan-Kao Chang, 展誥 章, Paul A. Wiegert, Quan-Zhi Ye, 泉志 葉, Max Mutchler
Figure caption: Temporal variation of the nightly mean apparent magnitude of 323P/SOHO measured with a circular aperture of fixed radius 2000 km projected at the distance of the comet except for the HST data points, which are photometric measurements of the nucleus. The perihelion epoch of the comet (TDB 2021 January 17.6) is marked by the vertical dotted line. Data points from different telescopes are discriminated according to symbols, and the reduced bandpasses are color coded.
Paper: The Lingering Death of Periodic Near-Sun Comet 323P/SOHO
Authors: Man-To Hui, 文韜 許, David J. Tholen, Rainer Kracht, Chan-Kao Chang, 展誥 章, Paul A. Wiegert, Quan-Zhi Ye, 泉志 葉, Max Mutchler
Figure caption: The left and middle panels show orbital evolution of the nominal orbit (dark) and the 300 MC variant clones (gray) of 323P/SOHO in terms of perihelion distance q, eccentricity e, inclination i, and the longitude of perihelion with respect to the one of Saturn, ϖ − ϖ ♄, from 2 kyr prior to J2000 to 3 kyr after, within which all of the clones but one collide with the Sun due to the ν 6 secular resonance. We plot the distribution of the Sun-impacting epochs as the histogram on the right, where the vertical red dashed line represents the Sun-impacting epoch of the nominal orbit. From the dynamical statistics alone, we obtain that the comet has a likelihood of ∼99.7% impacting the Sun 1.66 ± 0.14 kyr from J2000, in which the uncertainty is the standard deviation of the distribution.
Paper: The Lingering Death of Periodic Near-Sun Comet 323P/SOHO
Authors: Man-To Hui, 文韜 許, David J. Tholen, Rainer Kracht, Chan-Kao Chang, 展誥 章, Paul A. Wiegert, Quan-Zhi Ye, 泉志 葉, Max Mutchler
Figure caption: Effective scattering cross-section of the dust ejecta with respect to that of the bare nucleus as a function of time postperihelion, measured by a series of annular apertures whose inner radius was fixed to 1000 km from the nucleus projected at the distance of the comet, and the outer radii are as labeled in the plot. Only the r-band data points are used. Our best-fit physical models for the decline in the effective cross-section detailed in Section 4.4 are overplotted as dashed curves (color coded corresponding to the annular size). Data points from different observatories are distinguished by different symbols.
Paper: The Lingering Death of Periodic Near-Sun Comet 323P/SOHO
Authors: Man-To Hui, 文韜 許, David J. Tholen, Rainer Kracht, Chan-Kao Chang, 展誥 章, Paul A. Wiegert, Quan-Zhi Ye, 泉志 葉, Max Mutchler
Figure caption: Finson–Probstein models of 323P corresponding to Figure 1 for the ground-based observations (except the preperihelion Subaru observation in 2020 December). As indicated in the legend, syndynes and synchrones are plotted as blue solid and red dashed curves, respectively. Syndynes of β = 3 × 10−4 and 10−4 (the most crowded two almost overlapped with each other) are left unmarked in the middle left panel for clarity. In the middle right panel, since Earth was closest to the orbital plane of the comet, all of the syndynes and synchrones almost collapsed to a single line, and thus we simply leave all of the syndynes therein unmarked for clarity.
Paper: The Lingering Death of Periodic Near-Sun Comet 323P/SOHO
Authors: Man-To Hui, 文韜 許, David J. Tholen, Rainer Kracht, Chan-Kao Chang, 展誥 章, Paul A. Wiegert, Quan-Zhi Ye, 泉志 葉, Max Mutchler
Figure caption: Finson–Probstein models of 323P corresponding to Figure 2 for the HST observations. As in Figure 13, syndynes and synchrones are respectively plotted as blue solid and red dashed lines. Also marked in the upper two panels are the relative positions of Fragments A and B from the primary along with their associated uncertainties.
Paper: The Lingering Death of Periodic Near-Sun Comet 323P/SOHO
Authors: Man-To Hui, 文韜 許, David J. Tholen, Rainer Kracht, Chan-Kao Chang, 展誥 章, Paul A. Wiegert, Quan-Zhi Ye, 泉志 葉, Max Mutchler
Figure caption: Best-fit RTN components of the separation velocities (upper two panels, discriminated by colors) and goodness of fit (bottom, also see Section 4.7) of 323P’s two fragments around the time of perihelion passage of the primary in 2021. For clarity, the associated uncertainties in the separation velocity components are not shown. The minima in the goodness of fit for Fragments A and B (marked as the vertical dashed lines in the panels) are within ∼6 hr prior to the perihelion passage of the primary.
Paper: The Lingering Death of Periodic Near-Sun Comet 323P/SOHO
Authors: Man-To Hui, 文韜 許, David J. Tholen, Rainer Kracht, Chan-Kao Chang, 展誥 章, Paul A. Wiegert, Quan-Zhi Ye, 泉志 葉, Max Mutchler
Figure caption: Apparent magnitude of Fragments A (red) and B (blue) of 323P from the first two HST visits on UT 2021 March 2 and 3, respectively. The horizontal dotted lines in the corresponding lighter colors are the weighted mean values of apparent magnitudes of the two fragments in either of the visits, whose errors are not shown in the plots for clarity.
Paper: New Photometric Calibration of the Wide Field Camera 3 Detectors
Authors: Annalisa Calamida, Varun Bajaj, Jennifer Mack, Mariarosa Marinelli, Jennifer Medina, Aidan Pidgeon, Vera Kozhurina-Platais, Clare Shanahan, Debopam Som
Figure caption: Aperture photometry performed with a 10 pixel radius on _flc images collected with the F218W filter and the UVIS1-C512A-SUB (amp A; black) and UVIS1-C512B-SUB (amp B; red) subarrays for four CALSPEC WDs, namely, GRW 70 (circles), GD 153 (diamonds), GD 71 (squares), and G191B2B (triangles), plotted as percent change values versus the MJD of the observations. Photometry performed on scan images in the same filter and for GRW 70 (blue) and GD 153 (green) is also shown. The solid lines show the fit to the photometry of all stars before and after MJD = 55,738, indicated by a vertical dotted line. The sensitivity change rates in percent per year derived from fitting the data are labeled.
Paper: Optical Linear Polarization Study toward Czernik 3 Open Cluster at Different Spatial Scales
Authors: Namita Uppal, Shashikiran Ganesh, D. Bisht
Figure caption: Variation of degree of polarization, polarization angle of stars observed in the line of sight of Czernik 3, and 50th percentile reddening (E(B − V)) as a function of distance.
Paper: Optical Linear Polarization Study toward Czernik 3 Open Cluster at Different Spatial Scales
Authors: Namita Uppal, Shashikiran Ganesh, D. Bisht
Figure caption: Spectrum of neutral hydrogen clouds H I line (in blue color) within 16′ of the center of the Czernik 3 cluster and 12CO (orange) within 30′ of the center of the cluster. Y-axis represents the normalized brightness temperature for H I and normalized antenna temperature for 12CO.
Paper: Optical Linear Polarization Study toward Czernik 3 Open Cluster at Different Spatial Scales
Authors: Namita Uppal, Shashikiran Ganesh, D. Bisht
Figure caption: Variation of degree of polarization (panel (a)) and polarization angle (panel (b)) with distance of observed stars in the Czernik 3 direction. The errors in the Gaia EDR3 distances (r pgeo) and degree of polarization/polarization angle are also shown. The member stars are marked as red open circles.
Paper: Optical Linear Polarization Study toward Czernik 3 Open Cluster at Different Spatial Scales
Authors: Namita Uppal, Shashikiran Ganesh, D. Bisht
Figure caption: CMD (r − i vs. i in panel (a)) and color–color diagram (g − r vs. r − i in panel (b)) using Pan-STARRS data. The small gray dots represent the 10′ × 10′ field toward the Czernik 3 cluster. Black points with labels are the stars having polarization observations.
Paper: Optical Linear Polarization Study toward Czernik 3 Open Cluster at Different Spatial Scales
Authors: Namita Uppal, Shashikiran Ganesh, D. Bisht
Figure caption: Distribution of clusters (color and symbols represents different cluster) and Heiles (2000) stars (gray circles) in Galactic coordinates (ℓ–b) centered on Czernik 3.
Paper: Optical Linear Polarization Study toward Czernik 3 Open Cluster at Different Spatial Scales
Authors: Namita Uppal, Shashikiran Ganesh, D. Bisht
Figure caption: Variation of average polarization toward each cluster as a function of mean distance to the corresponding cluster.
Paper: Optical Linear Polarization Study toward Czernik 3 Open Cluster at Different Spatial Scales
Authors: Namita Uppal, Shashikiran Ganesh, D. Bisht
Figure caption: Variation of degree of polarization of stars toward different clusters as a function of distance. Heiles (2000) polarization within 15° is also shown with gray circles.
Paper: New Photometric Calibration of the Wide Field Camera 3 Detectors
Authors: Annalisa Calamida, Varun Bajaj, Jennifer Mack, Mariarosa Marinelli, Jennifer Medina, Aidan Pidgeon, Vera Kozhurina-Platais, Clare Shanahan, Debopam Som
Figure caption: (Top) Observed over synthetic count rates for the 42 UVIS1 (amp A) full-frame filters: wide (black), medium (red), X (green), long-pass (blue), and narrow (orange). These were calculated as a weighted mean over the standard stars. Error bars are displayed. The solid black line is a quadratic polynomial least-squares fit to the data of the wide, medium, and X filters only. (Bottom) Residual ratios after the polynomial fit. The dotted line shows a residual ratio of 1.0 (see text for more details).
Paper: New Photometric Calibration of the Wide Field Camera 3 Detectors
Authors: Annalisa Calamida, Varun Bajaj, Jennifer Mack, Mariarosa Marinelli, Jennifer Medina, Aidan Pidgeon, Vera Kozhurina-Platais, Clare Shanahan, Debopam Som
Figure caption: Comparison of old (DE16; magenta diamonds) and new (2020; filled black circles) synthetic detector sensitivity ratios, PHTRATIO, with observed values computed from WD (blue crosses) and ω Cen (orange triangles) observations. See text for more details.
Paper: New Photometric Calibration of the Wide Field Camera 3 Detectors
Authors: Annalisa Calamida, Varun Bajaj, Jennifer Mack, Mariarosa Marinelli, Jennifer Medina, Aidan Pidgeon, Vera Kozhurina-Platais, Clare Shanahan, Debopam Som
Figure caption: Same as Figure 11 but for the 42 UVIS2 (amp C) full-frame filters.
Paper: New Photometric Calibration of the Wide Field Camera 3 Detectors
Authors: Annalisa Calamida, Varun Bajaj, Jennifer Mack, Mariarosa Marinelli, Jennifer Medina, Aidan Pidgeon, Vera Kozhurina-Platais, Clare Shanahan, Debopam Som
Figure caption: Comparison between the new (2020) and old (2017) ZPs for WFC3 UVIS1 (amp A) in the ST photometric system for the wide- and medium-band filters over the entire WFC3-UVIS wavelength range. Error bars are also shown.
Paper: New Photometric Calibration of the Wide Field Camera 3 Detectors
Authors: Annalisa Calamida, Varun Bajaj, Jennifer Mack, Mariarosa Marinelli, Jennifer Medina, Aidan Pidgeon, Vera Kozhurina-Platais, Clare Shanahan, Debopam Som
Figure caption: Comparison between the new (2020) and old (2012) ZPs for WFC3-IR in the ST photometric system for the wide- and medium-band filters over the entire wavelength range. Error bars are also shown.
Paper: New Photometric Calibration of the Wide Field Camera 3 Detectors
Authors: Annalisa Calamida, Varun Bajaj, Jennifer Mack, Mariarosa Marinelli, Jennifer Medina, Aidan Pidgeon, Vera Kozhurina-Platais, Clare Shanahan, Debopam Som
Figure caption: Observed over synthetic count rates for WFC3-IR wide- and medium-band filters for the five standard stars used in the calibration as a function of the pivot wavelength.
Paper: New Photometric Calibration of the Wide Field Camera 3 Detectors
Authors: Annalisa Calamida, Varun Bajaj, Jennifer Mack, Mariarosa Marinelli, Jennifer Medina, Aidan Pidgeon, Vera Kozhurina-Platais, Clare Shanahan, Debopam Som
Figure caption: Same as Figure 17 but for the WFC3 UVIS2 (amp C) detector.
Paper: New Photometric Calibration of the Wide Field Camera 3 Detectors
Authors: Annalisa Calamida, Varun Bajaj, Jennifer Mack, Mariarosa Marinelli, Jennifer Medina, Aidan Pidgeon, Vera Kozhurina-Platais, Clare Shanahan, Debopam Som
Figure caption: Observed over synthetic count rates for UVIS1 (amp A) wide- and medium-band filters for the five standard stars used in the calibration as a function of the pivot wavelength. Error bars are displayed. Note that ratios for P330E were calculated for λ > 6000 Å only.
Paper: New Photometric Calibration of the Wide Field Camera 3 Detectors
Authors: Annalisa Calamida, Varun Bajaj, Jennifer Mack, Mariarosa Marinelli, Jennifer Medina, Aidan Pidgeon, Vera Kozhurina-Platais, Clare Shanahan, Debopam Som
Figure caption: Same as Figure 13 but for UVIS2 (amp C) filters.
Paper: The Featureless HST/WFC3 Transmission Spectrum of the Rocky Exoplanet GJ 1132b: No Evidence for a Cloud-free Primordial Atmosphere and Constraints on Starspot Contamination
Authors: Jessica E. Libby-Roberts, Zachory K. Berta-Thompson, Hannah Diamond-Lowe, Michael A. Gully-Santiago, Jonathan M. Irwin, Eliza M.-R. Kempton, Benjamin V. Rackham, David Charbonneau, Jean-Michel Désert, Jason A. Dittmann, Ryan Hofmann, Caroline V. Morley, Elisabeth R. Newton
Figure caption: Broadband light curves for each WFC3 transit of GJ 1132b, with each visit plotted left to right, including the raw light curves with transit and ramp-like systematics (first row), the transits with the RECTE systematic model divided out (second row), the systematics with the BATMAN transit model divided out (third row), and the final residuals (fourth row). Outlying points are noted as light gray points.
Paper: The Featureless HST/WFC3 Transmission Spectrum of the Rocky Exoplanet GJ 1132b: No Evidence for a Cloud-free Primordial Atmosphere and Constraints on Starspot Contamination
Authors: Jessica E. Libby-Roberts, Zachory K. Berta-Thompson, Hannah Diamond-Lowe, Michael A. Gully-Santiago, Jonathan M. Irwin, Eliza M.-R. Kempton, Benjamin V. Rackham, David Charbonneau, Jean-Michel Désert, Jason A. Dittmann, Ryan Hofmann, Caroline V. Morley, Elisabeth R. Newton
Figure caption: A comparison of the average stellar spectrum extracted for each visit. We find no evidence of significant contamination by other sources, as there is very little deviation in flux levels of the star across the five visits. The 1.15 μm and 1.63 μm are marked with dashed lines for comparison with Figure 2.
Paper: The Featureless HST/WFC3 Transmission Spectrum of the Rocky Exoplanet GJ 1132b: No Evidence for a Cloud-free Primordial Atmosphere and Constraints on Starspot Contamination
Authors: Jessica E. Libby-Roberts, Zachory K. Berta-Thompson, Hannah Diamond-Lowe, Michael A. Gully-Santiago, Jonathan M. Irwin, Eliza M.-R. Kempton, Benjamin V. Rackham, David Charbonneau, Jean-Michel Désert, Jason A. Dittmann, Ryan Hofmann, Caroline V. Morley, Elisabeth R. Newton
Figure caption: The deviation of each visit from the global medium-combined stellar spectrum created from the combination of all five visits. Visits 2−5 show <0.2% difference across 1.15 μm and 1.63 μm, while Visit 1 differs by <0.8%, most notably at shorter wavelengths. Dashed lines highlight the high-S/N region.
Paper: The Featureless HST/WFC3 Transmission Spectrum of the Rocky Exoplanet GJ 1132b: No Evidence for a Cloud-free Primordial Atmosphere and Constraints on Starspot Contamination
Authors: Jessica E. Libby-Roberts, Zachory K. Berta-Thompson, Hannah Diamond-Lowe, Michael A. Gully-Santiago, Jonathan M. Irwin, Eliza M.-R. Kempton, Benjamin V. Rackham, David Charbonneau, Jean-Michel Désert, Jason A. Dittmann, Ryan Hofmann, Caroline V. Morley, Elisabeth R. Newton
Figure caption: Each of the 22 spectroscopic light curves plotted with the smallest to largest wavelength bins being arranged from top to bottom. Point colors correspond to one of the five visits. Light curves are shown with systematics removed and with the transit model created from the weighted-average transit depth of the five visits (left), and residuals from this shared model are shown (right).