adsabs/AstroCLIMB huggingface dataset:
Paper: Candidate Main-belt Asteroids for Surface Heterogeneity
Authors: Sunao Hasegawa, Michaël Marsset, Francesca E. DeMeo, Josef Hanuš, Richard P. Binzel, Schelte J. Bus, Brian Burt, David Polishook, Cristina A. Thomas, Jooyeon Geem, Masateru Ishiguro, Daisuke Kuroda, Pierre Vernazza
Figure caption: Reflectance spectra of unpublished asteroids in Vernazza’s observations.
Paper: Candidate Main-belt Asteroids for Surface Heterogeneity
Authors: Sunao Hasegawa, Michaël Marsset, Francesca E. DeMeo, Josef Hanuš, Richard P. Binzel, Schelte J. Bus, Brian Burt, David Polishook, Cristina A. Thomas, Jooyeon Geem, Masateru Ishiguro, Daisuke Kuroda, Pierre Vernazza
Figure caption: Reflectance spectra of A-type asteroids identified as candidates for surface heterogeneity. The yellow error bars represent the observational uncertainty of Marsset et al. (2020b). To compare each absorption band, corrections were made to match the slope of one spectrum to the slope of the other.
Paper: Sites of Planet Formation in Binary Systems. I. Evidence for Disk−Orbit Alignment in the Close Binary FO Tau
Authors: Benjamin M. Tofflemire, Lisa Prato, Adam L. Kraus, Dominique Segura-Cox, G. H. Schaefer, Rachel Akeson, Sean Andrews, Eric L. N. Jensen, Christopher M. Johns-Krull, J. J. Zanazzi, M. Simon
Figure caption: Imaging of the FO Tau 12CO J = 2–1 visibilities. Left: the CO integrated intensity. All emission shown is ≥3σ above the background noise. Absorption from intervening cloud material contaminates the northwest side of the primary disk and the southeast side and center of the secondary disk. The synthesized beam is presented in the lower left corner, and a 10 au scale bar is provided in the lower right corner. The highest-likelihood orbital solution is overplotted in blue. White points mark the peak of continuum emission. Right: the CO intensity-weighted velocity map using the bettermoments quadratic method (Teague & Foreman-Mackey 2018). Extended CO gas disks are observed toward each component. Velocity channels heavily affected by cloud absorption are shown in the gray hatched region of the velocity color bar. Black contours are the 1.3 mm continuum emission, beginning at 5σ. The CO and continuum synthesized beams are presented in the white and black ellipses, respectively. In both panels a Keplerian mask, based on our best-fit disk model, is employed to reduce background noise for clarity (see Section 4.2).
Paper: Sites of Planet Formation in Binary Systems. I. Evidence for Disk−Orbit Alignment in the Close Binary FO Tau
Authors: Benjamin M. Tofflemire, Lisa Prato, Adam L. Kraus, Dominique Segura-Cox, G. H. Schaefer, Rachel Akeson, Sean Andrews, Eric L. N. Jensen, Christopher M. Johns-Krull, J. J. Zanazzi, M. Simon
Figure caption: Two-component SED fit to FO Tau photospheric flux measurements. The primary and secondary best-fit BT-Settl CFIST spectra are shown in blue and orange, respectively, with a combined spectrum in black. Model spectra have been smoothed to a resolution of R ∼ 3000 for clarity. Red points present measurements of the photospheric flux as they are fit. Horizontal bars represent the FWHM of the filter or spectral region considered in the measurement. Leftmost are spatially resolved HST-STIS flux measurements at 6100 Å from Hartigan & Kenyon (2003), highlighted in the inset in the upper left corner. The point at 7510 Å is the unresolved flux from Herczeg & Hillenbrand (2014). The lower inset presents the model agreement with the J-band contrast determined in this work. The ΔJ magnitude of the best-fit model is shown as the black point. Gray lines highlight the J-band spectral region. Rightmost are the H-band photospheric fluxes determined in this work. (Photometry values are provided in Table 3.)
Paper: Sites of Planet Formation in Binary Systems. I. Evidence for Disk−Orbit Alignment in the Close Binary FO Tau
Authors: Benjamin M. Tofflemire, Lisa Prato, Adam L. Kraus, Dominique Segura-Cox, G. H. Schaefer, Rachel Akeson, Sean Andrews, Eric L. N. Jensen, Christopher M. Johns-Krull, J. J. Zanazzi, M. Simon
Figure caption: On-sky projection of the FO Tau orbit. Observations are shown with blue circles. The orbit with the highest likelihood is shown in black. The dotted line signifies periastron passage. The dashed line is the line of nodes, with the Ω symbol signifying the ascending node. Random draws from the posterior distribution are shown in the background, color-coded by the orbital eccentricity. The secondary is farthest from Earth in the southwest portion of the orbit and closest in the northeast.
Paper: Sites of Planet Formation in Binary Systems. I. Evidence for Disk−Orbit Alignment in the Close Binary FO Tau
Authors: Benjamin M. Tofflemire, Lisa Prato, Adam L. Kraus, Dominique Segura-Cox, G. H. Schaefer, Rachel Akeson, Sean Andrews, Eric L. N. Jensen, Christopher M. Johns-Krull, J. J. Zanazzi, M. Simon
Figure caption: The FO Tau orbit fit. As a function of time, we present the projected separation, position angle, and RV difference from top to bottom, each with its associated residuals. Astrometry measurements are shown with blue circles. RV difference measurements are shown with red circles. The highest-likelihood orbital solution is shown in black. Random posterior draws are shown in the background, color-coded by the orbital eccentricity.
Paper: Sites of Planet Formation in Binary Systems. I. Evidence for Disk−Orbit Alignment in the Close Binary FO Tau
Authors: Benjamin M. Tofflemire, Lisa Prato, Adam L. Kraus, Dominique Segura-Cox, G. H. Schaefer, Rachel Akeson, Sean Andrews, Eric L. N. Jensen, Christopher M. Johns-Krull, J. J. Zanazzi, M. Simon
Figure caption: Spatially resolved spectra of FO Tau A (top) and B (bottom). The continuum-normalized spectra are presented in colored lines, and the best-fit model is overlaid in black.
Paper: Sites of Planet Formation in Binary Systems. I. Evidence for Disk−Orbit Alignment in the Close Binary FO Tau
Authors: Benjamin M. Tofflemire, Lisa Prato, Adam L. Kraus, Dominique Segura-Cox, G. H. Schaefer, Rachel Akeson, Sean Andrews, Eric L. N. Jensen, Christopher M. Johns-Krull, J. J. Zanazzi, M. Simon
Figure caption:  12CO J = 2–1 velocity channel maps (LRSK radio) of the observations (top panel set), the best-fit model (middle panel set), and the data−model residuals (bottom panel set). Each panel provides the channel’s central velocity in the upper left corner. White points signify peaks in the continuum emission. Channels contaminated by cloud absorption have a diagonal white line.
Paper: Sites of Planet Formation in Binary Systems. I. Evidence for Disk−Orbit Alignment in the Close Binary FO Tau
Authors: Benjamin M. Tofflemire, Lisa Prato, Adam L. Kraus, Dominique Segura-Cox, G. H. Schaefer, Rachel Akeson, Sean Andrews, Eric L. N. Jensen, Christopher M. Johns-Krull, J. J. Zanazzi, M. Simon
Figure caption: FO Tau orbital eccentricity posterior. The probability distribution function is represented with a Gaussian kernel density estimate. Line color matches the color bars in Figures 3 and 5.
Paper: Sites of Planet Formation in Binary Systems. I. Evidence for Disk−Orbit Alignment in the Close Binary FO Tau
Authors: Benjamin M. Tofflemire, Lisa Prato, Adam L. Kraus, Dominique Segura-Cox, G. H. Schaefer, Rachel Akeson, Sean Andrews, Eric L. N. Jensen, Christopher M. Johns-Krull, J. J. Zanazzi, M. Simon
Figure caption: TESS PDCSAP light curves of FO Tau. The variability is dominated by stochastic bursts associated with accretion- and inner-disk-related processes.
Paper: Sites of Planet Formation in Binary Systems. I. Evidence for Disk−Orbit Alignment in the Close Binary FO Tau
Authors: Benjamin M. Tofflemire, Lisa Prato, Adam L. Kraus, Dominique Segura-Cox, G. H. Schaefer, Rachel Akeson, Sean Andrews, Eric L. N. Jensen, Christopher M. Johns-Krull, J. J. Zanazzi, M. Simon
Figure caption: The FO Tau 1.3 mm continuum map. Circumstellar dust is detected, but not clearly resolved, toward each of the FO Tau binary components. The highest-likelihood orbital solution is overplotted in blue. The synthesized beam is presented in the lower left corner, and a 10 au scale bar is shown in the lower right corner.
Paper: Sites of Planet Formation in Binary Systems. I. Evidence for Disk−Orbit Alignment in the Close Binary FO Tau
Authors: Benjamin M. Tofflemire, Lisa Prato, Adam L. Kraus, Dominique Segura-Cox, G. H. Schaefer, Rachel Akeson, Sean Andrews, Eric L. N. Jensen, Christopher M. Johns-Krull, J. J. Zanazzi, M. Simon
Figure caption: Schematics of the binary−disk orbital planes for the two possible disk orientations allowed by our observation. The binary orbit is shown in black. The primary and secondary disks are displayed in blue and orange, respectively. Arrows indicate the angular momentum vectors. The dotted line marks periastron passage. The left column is the aligned solution in which the disks are rotating counterclockwise with the binary orbit. The right column is the misaligned solution where the disks rotate clockwise, retrograde with the binary orbit. The top row shows the on-sky projection where the projected disk inclinations are the same, despite having different directions of rotation. The bottom row presents an alternate projection where the difference between the solutions is more readily apparent.
Paper: Sites of Planet Formation in Binary Systems. I. Evidence for Disk−Orbit Alignment in the Close Binary FO Tau
Authors: Benjamin M. Tofflemire, Lisa Prato, Adam L. Kraus, Dominique Segura-Cox, G. H. Schaefer, Rachel Akeson, Sean Andrews, Eric L. N. Jensen, Christopher M. Johns-Krull, J. J. Zanazzi, M. Simon
Figure caption: Left: comparison of the projected inclination posteriors of the binary orbit and the individual protoplanetary disks. Measurements from both the continuum (dust) and CO visibility fits are included for each disk. Middle and right: disk−orbit obliquity posteriors for the FO Tau A and FO Tau B CO disks, respectively. In each panel, the dark and faint lines represent the aligned and misaligned solutions, respectively (as labeled). A schematic displaying these scenarios in presented in Figure 11. The gray curve in the right panel corresponds to the obliquity distribution of a randomly oriented disk.
Paper: Sites of Planet Formation in Binary Systems. I. Evidence for Disk−Orbit Alignment in the Close Binary FO Tau
Authors: Benjamin M. Tofflemire, Lisa Prato, Adam L. Kraus, Dominique Segura-Cox, G. H. Schaefer, Rachel Akeson, Sean Andrews, Eric L. N. Jensen, Christopher M. Johns-Krull, J. J. Zanazzi, M. Simon
Figure caption: Continuum visibility fitting. Results are shown for SPW 3. Left panel: data and model visibilities as a function of u-v distance. Middle panels: cleaned images of the data, model, and residuals. Contours in the residual image are set at −3σ and 3σ in dashed and solid lines, respectively. Right panel: best-fit radial intensity profile of the primary (blue) and secondary (orange).
Paper: Sites of Planet Formation in Binary Systems. I. Evidence for Disk−Orbit Alignment in the Close Binary FO Tau
Authors: Benjamin M. Tofflemire, Lisa Prato, Adam L. Kraus, Dominique Segura-Cox, G. H. Schaefer, Rachel Akeson, Sean Andrews, Eric L. N. Jensen, Christopher M. Johns-Krull, J. J. Zanazzi, M. Simon
Figure caption: Corner plot for parameters in the FO Tau orbit fit.
Paper: Sites of Planet Formation in Binary Systems. I. Evidence for Disk−Orbit Alignment in the Close Binary FO Tau
Authors: Benjamin M. Tofflemire, Lisa Prato, Adam L. Kraus, Dominique Segura-Cox, G. H. Schaefer, Rachel Akeson, Sean Andrews, Eric L. N. Jensen, Christopher M. Johns-Krull, J. J. Zanazzi, M. Simon
Figure caption: Corner plot for parameters in the FO Tau disk fit. Posteriors and two-parameter correlation contours are represented with a Gaussian kernel density estimate. The results for FO Tau A and B (fit simultaneously) are displayed in blue and orange, respectively.
Paper: High-precision Atmospheric Characterization of a Y Dwarf with JWST NIRSpec G395H Spectroscopy: Isotopologue, C/O Ratio, Metallicity, and the Abundances of Six Molecular Species
Authors: Ben W. P. Lew, Thomas Roellig, Natasha E. Batalha, Michael Line, Thomas Greene, Sagnick Murkherjee, Richard Freedman, Michael Meyer, Charles Beichman, Catarina Alves de Oliveira, Matthew De Furio, Doug Johnstone, Alexandra Z. Greenbaum, Mark Marley, Jonathan J. Fortney, Erick T. Young, Jarron Leisenring, Martha Boyer, Klaus Hodapp, Karl Misselt, John Stansberry, Marcia Rieke
Figure caption: Left panel: the TP profile of CHIMERA (T eff = ﹩{534}_{-25}^{+8}﹩ K, log(g) = 5.02 ± 0.01), the best-fit Elf-Owl model (T eff = ﹩{425}_{-0.3}^{+0.5}﹩ K, log(g) = 4.38 ± 0.01), and the petitRADTRANS retrieval in B23. The colored dots indicate the pressures at which the local temperatures are equal to the effective temperatures of the models. See Section 4.6 for the discussion of the thermal structure. Right panel: the contribution function of CHIMERA. The 3–5μm spectrum probes around 0.8–27 bars. The probed pressure range corresponds to the region in which the TP profiles have small uncertainties.(The data used to create this figure are available.)
Paper: High-precision Atmospheric Characterization of a Y Dwarf with JWST NIRSpec G395H Spectroscopy: Isotopologue, C/O Ratio, Metallicity, and the Abundances of Six Molecular Species
Authors: Ben W. P. Lew, Thomas Roellig, Natasha E. Batalha, Michael Line, Thomas Greene, Sagnick Murkherjee, Richard Freedman, Michael Meyer, Charles Beichman, Catarina Alves de Oliveira, Matthew De Furio, Doug Johnstone, Alexandra Z. Greenbaum, Mark Marley, Jonathan J. Fortney, Erick T. Young, Jarron Leisenring, Martha Boyer, Klaus Hodapp, Karl Misselt, John Stansberry, Marcia Rieke
Figure caption: Top panel: the best-fit Elf-Owl model (semitransparent green lines) and the CHIMERA atmospheric retrieval (semitransparent orange lines) spectra. For clarity, the Elf-Owl model spectra and a copy of the data spectra are shifted by −8 × 10−11 W m−3 on the y-axis. The original and shifted data spectra are plotted as semitransparent blue lines for comparison with the CHIMERA and Elf-Owl models, respectively. Middle and bottom panels: the residuals for the CHIMERA and Elf-Owl models plotted in orange and green lines, respectively. The sharp positive residual at 4.55 μm of the Elf-Owl model is because of the lower-than-solar CH3D abundance (see Section 3.5).(The data used to create this figure are available.)
Paper: High-precision Atmospheric Characterization of a Y Dwarf with JWST NIRSpec G395H Spectroscopy: Isotopologue, C/O Ratio, Metallicity, and the Abundances of Six Molecular Species
Authors: Ben W. P. Lew, Thomas Roellig, Natasha E. Batalha, Michael Line, Thomas Greene, Sagnick Murkherjee, Richard Freedman, Michael Meyer, Charles Beichman, Catarina Alves de Oliveira, Matthew De Furio, Doug Johnstone, Alexandra Z. Greenbaum, Mark Marley, Jonathan J. Fortney, Erick T. Young, Jarron Leisenring, Martha Boyer, Klaus Hodapp, Karl Misselt, John Stansberry, Marcia Rieke
Figure caption: The spectrum is plotted in dark gray lines along with the P(τ = 0.01) of the detected molecules. The left y-axis shows the flux density of the spectrum, while the right y-axis shows the photospheric pressure at which the molecular optical depth reaches 0.01. The three most abundant molecules, CH4, H2O, and NH3, are plotted in thin light blue, green, and orange lines, respectively. The three less abundant molecules, H2S, CO2, and CO, are plotted in thick red, purple, and blue lines, respectively. The P(τ = 0.01) lines of molecules are binned down into a resolution of R = 1350 for clarity.
Paper: High-precision Atmospheric Characterization of a Y Dwarf with JWST NIRSpec G395H Spectroscopy: Isotopologue, C/O Ratio, Metallicity, and the Abundances of Six Molecular Species
Authors: Ben W. P. Lew, Thomas Roellig, Natasha E. Batalha, Michael Line, Thomas Greene, Sagnick Murkherjee, Richard Freedman, Michael Meyer, Charles Beichman, Catarina Alves de Oliveira, Matthew De Furio, Doug Johnstone, Alexandra Z. Greenbaum, Mark Marley, Jonathan J. Fortney, Erick T. Young, Jarron Leisenring, Martha Boyer, Klaus Hodapp, Karl Misselt, John Stansberry, Marcia Rieke
Figure caption: Top panel: the best-fit CHIMERA model spectra with and without H2S opacity are plotted in blue and orange lines, respectively. The data are plotted with a black line. Middle panel: the fractional flux density change of the best-fit spectrum after the removal of H2S opacity. Bottom panel: the residuals relative to the data uncertainties for the CHIMERA retrieval results with and without H2S opacity are plotted in blue and orange lines. Exclusion of H2S opacity leads to an increase of χ 2 by over 900.
Paper: High-precision Atmospheric Characterization of a Y Dwarf with JWST NIRSpec G395H Spectroscopy: Isotopologue, C/O Ratio, Metallicity, and the Abundances of Six Molecular Species
Authors: Ben W. P. Lew, Thomas Roellig, Natasha E. Batalha, Michael Line, Thomas Greene, Sagnick Murkherjee, Richard Freedman, Michael Meyer, Charles Beichman, Catarina Alves de Oliveira, Matthew De Furio, Doug Johnstone, Alexandra Z. Greenbaum, Mark Marley, Jonathan J. Fortney, Erick T. Young, Jarron Leisenring, Martha Boyer, Klaus Hodapp, Karl Misselt, John Stansberry, Marcia Rieke
Figure caption: Top panel: the retrieved spectrum with the best fit and the 5σ upper limit 13CO abundance. Middle panel: the change of the spectra after removing 13CO and 5% 12CO opacity. Bottom panel: the spectral difference between the two model spectra relative to the observational data uncertainty.
Paper: High-precision Atmospheric Characterization of a Y Dwarf with JWST NIRSpec G395H Spectroscopy: Isotopologue, C/O Ratio, Metallicity, and the Abundances of Six Molecular Species
Authors: Ben W. P. Lew, Thomas Roellig, Natasha E. Batalha, Michael Line, Thomas Greene, Sagnick Murkherjee, Richard Freedman, Michael Meyer, Charles Beichman, Catarina Alves de Oliveira, Matthew De Furio, Doug Johnstone, Alexandra Z. Greenbaum, Mark Marley, Jonathan J. Fortney, Erick T. Young, Jarron Leisenring, Martha Boyer, Klaus Hodapp, Karl Misselt, John Stansberry, Marcia Rieke
Figure caption: The reduced spectrum of WISE 1828. The parts of the spectra covered by the NRS1 and NRS2 detectors are shown in the top and bottom panels, respectively. The 1σ uncertainties are plotted as gray shaded regions.
Paper: High-precision Atmospheric Characterization of a Y Dwarf with JWST NIRSpec G395H Spectroscopy: Isotopologue, C/O Ratio, Metallicity, and the Abundances of Six Molecular Species
Authors: Ben W. P. Lew, Thomas Roellig, Natasha E. Batalha, Michael Line, Thomas Greene, Sagnick Murkherjee, Richard Freedman, Michael Meyer, Charles Beichman, Catarina Alves de Oliveira, Matthew De Furio, Doug Johnstone, Alexandra Z. Greenbaum, Mark Marley, Jonathan J. Fortney, Erick T. Young, Jarron Leisenring, Martha Boyer, Klaus Hodapp, Karl Misselt, John Stansberry, Marcia Rieke
Figure caption: The corner plot of the Elf-Owl model grid fitting results. The nine model parameters are effective temperature, gravity (﹩\mathrm{log}(g)﹩), vertical mixing ﹩\mathrm{log}({K}_{{zz}})﹩, metallicity log(M/H), C/O ratio, radius (R Jup), wavelength shift in units of Å, and log(v sin i km s−1).
Paper: High-precision Atmospheric Characterization of a Y Dwarf with JWST NIRSpec G395H Spectroscopy: Isotopologue, C/O Ratio, Metallicity, and the Abundances of Six Molecular Species
Authors: Ben W. P. Lew, Thomas Roellig, Natasha E. Batalha, Michael Line, Thomas Greene, Sagnick Murkherjee, Richard Freedman, Michael Meyer, Charles Beichman, Catarina Alves de Oliveira, Matthew De Furio, Doug Johnstone, Alexandra Z. Greenbaum, Mark Marley, Jonathan J. Fortney, Erick T. Young, Jarron Leisenring, Martha Boyer, Klaus Hodapp, Karl Misselt, John Stansberry, Marcia Rieke
Figure caption: The fitted chemical abundances of the forward model Elf-Owl and the CHIMERA retrieval framework. The dashed and solid lines show the abundance of the best-fit model spectrum from the Elf-Owl models and CHIMERA, respectively.(The data used to create this figure are available.)
Paper: Planet Hunters NGTS: New Planet Candidates from a Citizen Science Search of the Next Generation Transit Survey Public Data
Authors: Sean M. O'Brien, Megan E. Schwamb, Samuel Gill, Christopher A. Watson, Matthew R. Burleigh, Alicia Kendall, Sarah L. Casewell, David R. Anderson, José I. Vines, James S. Jenkins, Douglas R. Alves, Laura Trouille, Solène Ulmer-Moll, Edward M. Bryant, Ioannis Apergis, Matthew Battley, Daniel Bayliss, Nora L. Eisner, Edward Gillen, Michael R. Goad, Maximilian N. Günther, Beth A. Henderson, Jeong-Eun Heo, David G. Jackson, Chris Lintott, James McCormac, Maximiliano Moyano, Louise D. Nielsen, Ares Osborn, Suman Saha, Ramotholo R. Sefako, Andrew W. Stephens, Rosanna H. Tilbrook, Stéphane Udry, Richard G. West, Peter J. Wheatley, Tafadzwa Zivave, See Min Lim, Arttu Sainio
Figure caption: PHNGTS classification interfaces. Top panel: Exoplanet Transit Search interface showing a phase-folded light curve with the response “A V-shaped dip in the middle” selected. Bottom-left panel: Secondary Eclipse Check interface showing the phase-folded light curve centered on phase = 0.5 with the response “A secondary eclipse” selected. Bottom-right panel: second task of the Odd/Even Transit Check workflow asking whether the green points (odd transits) and magenta points (even transits) have similar depths, the selected response is “Yes.” Note the example images for each workflow do not show data for the same star.
Paper: Planet Hunters NGTS: New Planet Candidates from a Citizen Science Search of the Next Generation Transit Survey Public Data
Authors: Sean M. O'Brien, Megan E. Schwamb, Samuel Gill, Christopher A. Watson, Matthew R. Burleigh, Alicia Kendall, Sarah L. Casewell, David R. Anderson, José I. Vines, James S. Jenkins, Douglas R. Alves, Laura Trouille, Solène Ulmer-Moll, Edward M. Bryant, Ioannis Apergis, Matthew Battley, Daniel Bayliss, Nora L. Eisner, Edward Gillen, Michael R. Goad, Maximilian N. Günther, Beth A. Henderson, Jeong-Eun Heo, David G. Jackson, Chris Lintott, James McCormac, Maximiliano Moyano, Louise D. Nielsen, Ares Osborn, Suman Saha, Ramotholo R. Sefako, Andrew W. Stephens, Rosanna H. Tilbrook, Stéphane Udry, Richard G. West, Peter J. Wheatley, Tafadzwa Zivave, See Min Lim, Arttu Sainio
Figure caption: Light curves for three different stars as presented in each of the three workflows. Top row: light curves for NGTS-8, which shows a clear U-shaped transit in the Exoplanet Transit Search. No secondary eclipse is visible in the Secondary Eclipse Check, and the depths of the odd and even transits match in the Odd/Even Transit Check. Middle row: light curves for TIC-389932515, which shows a U/V-shaped transit in the Exoplanet Transit Search. The depths of the odd and even transits match in the Odd/Even Transit Check; however, a secondary eclipse is visible in the Secondary Eclipse Check, indicating this is an eclipsing binary. Bottom row: light curves for TIC-441292449, which shows a clear V-shaped transit in the Exoplanet Transit Search. No secondary eclipse is visible in the Secondary Eclipse Check; however, the depths of the odd and even transits do not match in the Odd/Even Transit Check, indicating this is an eclipsing binary.