adsabs/AstroCLIMB huggingface dataset:
Paper: Census of Blue Straggler Stars in Distant Open Clusters and Maximum Fractional Mass Excess of Open Cluster Blue Straggler Stars
Authors: Qian Cui, Zhihong He, Shunhong Deng, Liming Peng, Chunyan Li, Yangping Luo, Kun Wang
Figure caption: The spatial distribution of OCs containing BSSs in the Milky Way. Left panel: a face-on view of the Galactic plane, showing all OCs (Z. He 2023) as gray points and OCs with BSSs as colored symbols, relative to the spiral arms. This is based on the spiral arm model from M. J. Reid et al. (2019), which includes the Scutum-Centaurus (black), Sagittarius (blue), Local (brown), Perseus (magenta), and Outer (yellow) arms. The Sun’s position is marked at (−8.15, 0) kpc. The newly identified OCs with BSSs studied in this work are primarily located in the outer regions of the Galaxy. Right panel: an edge-on view displays the vertical distribution of all OCs and OCs with BSSs along the Z-axis. The distribution indicates that most OC BSSs are confined to the Galactic disk with minimal vertical displacement, although some are associated with Galactic warp structures.
Paper: Census of Blue Straggler Stars in Distant Open Clusters and Maximum Fractional Mass Excess of Open Cluster Blue Straggler Stars
Authors: Qian Cui, Zhihong He, Shunhong Deng, Liming Peng, Chunyan Li, Yangping Luo, Kun Wang
Figure caption: Left panels: the OCs plotted within various mass ranges. Right panels: the maximum fractional mass excess of OC BSSs in different mass ranges presented as a function of cluster age. The dashed lines illustrate the running median values of maximum Me in relation to cluster age. The triangles indicate OCs containing Type 1 BSSs identified in this study, while solid circles denote BSSs cataloged in V. V. Jadhav & A. Subramaniam (2021). The brown solid and dotted lines correspond to Me = 1 and Me = 0.5, respectively. The colors indicate scatter point density, with cooler colors representing sparse areas and warmer colors indicating crowded areas.
Paper: Census of Blue Straggler Stars in Distant Open Clusters and Maximum Fractional Mass Excess of Open Cluster Blue Straggler Stars
Authors: Qian Cui, Zhihong He, Shunhong Deng, Liming Peng, Chunyan Li, Yangping Luo, Kun Wang
Figure caption: The maximum Me of BSSs in all-aged OCs as a function of cluster mass. The black line represents the running median values of maximum Me relative to cluster mass. The triangles denote OCs containing Type I BSSs identified in this study, while solid circles represent BSSs from V. V. Jadhav & A. Subramaniam (2021). The brown solid and dotted lines indicate Me = 1 and Me = 0.5, respectively. The colors indicate scatter point density, with cooler colors representing sparse areas and warmer colors indicating crowded areas. Two significant outliers, FSR 0542 and Teutsch 48, are also marked in the figure.
Paper: Census of Blue Straggler Stars in Distant Open Clusters and Maximum Fractional Mass Excess of Open Cluster Blue Straggler Stars
Authors: Qian Cui, Zhihong He, Shunhong Deng, Liming Peng, Chunyan Li, Yangping Luo, Kun Wang
Figure caption: The cross-match results between H23 and HR23 and the corresponding distribution of member stars in the H-R diagram. Star cluster members from H23 are depicted as black dots, with larger dots representing core members and smaller dots indicating border members. The orange pluses denote member stars from the clusters in HR23. Three clusters are identified as reliable in HR23: CWNU 3190 (FSR 0276), CWNU 2974 (HSC 2110), and FSR 0687.
Paper: Census of Blue Straggler Stars in Distant Open Clusters and Maximum Fractional Mass Excess of Open Cluster Blue Straggler Stars
Authors: Qian Cui, Zhihong He, Shunhong Deng, Liming Peng, Chunyan Li, Yangping Luo, Kun Wang
Figure caption: Statistics of BSSs in OCs from various studies. Panel (a) shows the age distribution of OCs containing BSSs. Panel (b) illustrates the relationship between cluster age and the number of BSSs. Panel (c) displays the apparent magnitudes of BSSs across different studies. The colors orange, magenta, black, and blue correspond to categories from V. V. Jadhav & A. Subramaniam (2021), M. J. Rain et al. (2021), C. Li et al. (2023), and Type I BSSs derived in this work, respectively.
Paper: Southern Binaries with the Zorro Speckle Camera @ Gemini South
Authors: Rene A. Mendez, Andrei Tokovinin, Edgardo Costa, Maximiliano Dirk
Figure caption: Example of power spectra for the data cube S20190519Z18, displayed with a negative logarithmic stretch. Top: blue channel; bottom: red channel. To the right of each spectrum, the spectrum of the associated PSF reference star is shown. The object is the 21 mas separation binary HIP 89000 observed at a zenith distance of 35°. The horizontal line in the reference spectra is an artifact caused by the image truncation due to imperfect centering of the star in the ROI.
Paper: Southern Binaries with the Zorro Speckle Camera @ Gemini South
Authors: Rene A. Mendez, Andrei Tokovinin, Edgardo Costa, Maximiliano Dirk
Figure caption: Comparison of measurements between the blue and red channels for 10 binary stars observed in the 2019A run. Top panel: ratio of red/blue separations; bottom panel: difference in position angle. This comparison is used to correct the red channel to the same scale and orientation as that of the blue channel. The solid line shows the mean, while the dashed lines indicate the  ±1σ range.
Paper: Southern Binaries with the Zorro Speckle Camera @ Gemini South
Authors: Rene A. Mendez, Andrei Tokovinin, Edgardo Costa, Maximiliano Dirk
Figure caption: Left panel: power spectrum in the blue channel of the cube S20190717Z0990b. Black circles are the consequence of a periodic noise. In this case, the reference spectrum on the right is the RAD model. Its similarity to the object spectrum illustrates the correctness of the AD model.
Paper: Southern Binaries with the Zorro Speckle Camera @ Gemini South
Authors: Rene A. Mendez, Andrei Tokovinin, Edgardo Costa, Maximiliano Dirk
Figure caption: Data flow diagram of the Zorro Speckle data reduction process, which has been adapted from the SOAR/HRCam pipeline (A. Tokovinin 2018b).
Paper: Low 4.5 μm Dayside Emission Disfavors a Dark Bare-rock Scenario for the Hot Super-Earth TOI-431 b
Authors: Christopher Monaghan, Pierre-Alexis Roy, Björn Benneke, Ian J. M. Crossfield, Louis-Philippe Coulombe, Caroline Piaulet-Ghorayeb, Laura Kreidberg, Courtney D. Dressing, Stephen R. Kane, Diana Dragomir, Michael W. Werner, Vivien Parmentier, Jessie L. Christiansen, Farisa Y. Morales, David Berardo, Varoujan Gorjian
Figure caption: Eclipse depth of TOI-431 b at 4.5 μm compared to a suite of theoretical emission spectra produced by SCARLET. The colored lines represent the five atmospheric models simulated by SCARLET using a nongray temperature profile and a well-mixed composition. The dashed gray lines show the blackbody eclipse spectra corresponding to different combinations of f and AB at uniform dayside temperatures. The black dot represents the measured eclipse depth, with the associated ±1σ error bars. Colored circles represent the models integrated over the IRAC2 bandpass between 4.05 and 4.95 μm. The exact compositions of the atmospheric models are shown in Table 3. Normalized opacity bands from dominating molecules in the models (CO, CO2, and SiO) are shown in the bottom panel.
Paper: Low 4.5 μm Dayside Emission Disfavors a Dark Bare-rock Scenario for the Hot Super-Earth TOI-431 b
Authors: Christopher Monaghan, Pierre-Alexis Roy, Björn Benneke, Ian J. M. Crossfield, Louis-Philippe Coulombe, Caroline Piaulet-Ghorayeb, Laura Kreidberg, Courtney D. Dressing, Stephen R. Kane, Diana Dragomir, Michael W. Werner, Vivien Parmentier, Jessie L. Christiansen, Farisa Y. Morales, David Berardo, Varoujan Gorjian
Figure caption: Eclipse depth of TOI-431 b at 4.5 μm compared to a suite of atmosphereless emission spectra from different mineralogical surface models, assuming a PHOENIX stellar model. The black dot represents the measured eclipse depth with the associated ±1σ and ±​​​​​​2σ error bars shown in black and gray, respectively. The colored lines represent the emission spectra of difference surface compositions assuming a nonuniform temperature gradient on the planet’s surface. Colored circles represent the models integrated over the IRAC2 bandpass between 4.05 and 4.95 μm. A blackbody model with a uniform dayside temperature is shown for comparison, indicating the difference between itself and the more accurate dark bare-rock model in blue.
Paper: Evidence of a Disk Wind Origin for Fluorescent H2 in Classical T Tauri Stars
Authors: Matt Kalscheur, Kevin France, Brunella Nisini, P. Christian Schneider, Richard Alexander, Jochen Eislöffel, Justyn Campbell-White, Hsien Shang, Manuele Gangi, Zhen Guo, Seok-Jun Chang
Figure caption: Correlations between the NC and BC kinematic properties for both progressions of fluorescent H2. We report the equation of the line (brown dot-dashed line) that best fits the data for statistically significant correlation pairs. The light-gray dotted line in the velocity plots (left panels) represents a hypothetical one-to-one correlation.
Paper: Evidence of a Disk Wind Origin for Fluorescent H2 in Classical T Tauri Stars
Authors: Matt Kalscheur, Kevin France, Brunella Nisini, P. Christian Schneider, Richard Alexander, Jochen Eislöffel, Justyn Campbell-White, Hsien Shang, Manuele Gangi, Zhen Guo, Seok-Jun Chang
Figure caption: Example individual and coadded emission line profiles of the [1,4] progression for a high-S/N (∼126 at the peak of the coadded profile) disk (top panel), and of the [1,7] progression for a low-S/N (∼16) disk (bottom panel). The averaged profile is indicated by the thick black line. Zero velocity is with respect to the rest wavelength of line center.
Paper: Evidence of a Disk Wind Origin for Fluorescent H2 in Classical T Tauri Stars
Authors: Matt Kalscheur, Kevin France, Brunella Nisini, P. Christian Schneider, Richard Alexander, Jochen Eislöffel, Justyn Campbell-White, Hsien Shang, Manuele Gangi, Zhen Guo, Seok-Jun Chang
Figure caption: Representative examples of one- (top panel) and two-component (bottom panel) model fits to coadded fluorescent H2 line profiles. The coadded profile is shown with the blue solid line, the best-fit model with the red solid line, and the linear continuum fit with the gray dashed line. The sum of the broad (green dashed line) and narrow (orange dashed line) Gaussian components exceeds the height of the best-fit model because the best-fit model is convolved with the HST-COS LSF (not shown). Velocities are not corrected for stellar RVs.
Paper: Evidence of a Disk Wind Origin for Fluorescent H2 in Classical T Tauri Stars
Authors: Matt Kalscheur, Kevin France, Brunella Nisini, P. Christian Schneider, Richard Alexander, Jochen Eislöffel, Justyn Campbell-White, Hsien Shang, Manuele Gangi, Zhen Guo, Seok-Jun Chang
Figure caption: Scatter plots of component centroid velocity and stellar RV (top panels), and histograms of the distribution of RV-corrected component velocities for both fluorescent H2 progressions (bottom panels). The markers clustered around zero RV in the top panels consist mostly of disks in the Lupus star-forming region, while markers clustered around 15 km s−1 pertain mostly to Taurus-Auriga.
Paper: Evidence of a Disk Wind Origin for Fluorescent H2 in Classical T Tauri Stars
Authors: Matt Kalscheur, Kevin France, Brunella Nisini, P. Christian Schneider, Richard Alexander, Jochen Eislöffel, Justyn Campbell-White, Hsien Shang, Manuele Gangi, Zhen Guo, Seok-Jun Chang
Figure caption: Example flux (top panel) and S/N (bottom panel) line profiles for the ﹩{B}^{1}{{\rm{\Sigma }}}_{u}^{+}-{X}^{1}{{\rm{\Sigma }}}_{g}^{+}﹩ (1–7) R(3) fluorescent emission line of H2 in ULLYSES target AA Tau. Zero velocity is with respect to the rest wavelength of the line. The average S/N per resolution element at the peak (denoted in red) of the profile is 61.25, the highest of the ULLYSES targets.
Paper: Evidence of a Disk Wind Origin for Fluorescent H2 in Classical T Tauri Stars
Authors: Matt Kalscheur, Kevin France, Brunella Nisini, P. Christian Schneider, Richard Alexander, Jochen Eislöffel, Justyn Campbell-White, Hsien Shang, Manuele Gangi, Zhen Guo, Seok-Jun Chang
Figure caption: Distribution of FWHM with respect to RV-corrected centroid velocity for both fluorescent progressions. Component FWHMs in excess of 125 km s−1 (BCs of RECX 11 and CS Cha) are excluded for easier visual comparison.
Paper: Searching for GEMS: Discovery and Characterization of Two Brown Dwarfs Around M Dwarfs 
Authors: Alexander Larsen, Tera N. Swaby, Henry A. Kobulnicky, Caleb I. Cañas, Shubham Kanodia, Jessica Libby-Roberts, Andrew Monson, Arvind F. Gupta, William Cochran, Suvrath Mahadevan, Chad Bender, Scott A. Diddams, Samuel Halverson, Andrea S. J. Lin, Maxwell Moe, Joe Ninan, Paul Robertson, Arpita Roy, Christian Schwab, Gudmundur Stefansson
Figure caption: Observed transits for TOI-5389Ab. From first to last: TESS Sector 22 (2020 March) and its phase-folded counterpart, TESS Sector 48 (2022 February) and its phase-folded counterpart, RBO I band 2023 February 28, and RBO I band 2024 February 6.
Paper: Searching for GEMS: Discovery and Characterization of Two Brown Dwarfs Around M Dwarfs 
Authors: Alexander Larsen, Tera N. Swaby, Henry A. Kobulnicky, Caleb I. Cañas, Shubham Kanodia, Jessica Libby-Roberts, Andrew Monson, Arvind F. Gupta, William Cochran, Suvrath Mahadevan, Chad Bender, Scott A. Diddams, Samuel Halverson, Andrea S. J. Lin, Maxwell Moe, Joe Ninan, Paul Robertson, Arpita Roy, Christian Schwab, Gudmundur Stefansson
Figure caption: Observed transits for TOI-5610b. From first to last: TESS Sector 21 (2020 February) and its phase-folded counterpart, TESS Sector 48 (2022 February) and its phase-folded counterpart, RBO I-band 2024 January 2, and RBO I-band 2024 February 11.
Paper: Searching for GEMS: Discovery and Characterization of Two Brown Dwarfs Around M Dwarfs 
Authors: Alexander Larsen, Tera N. Swaby, Henry A. Kobulnicky, Caleb I. Cañas, Shubham Kanodia, Jessica Libby-Roberts, Andrew Monson, Arvind F. Gupta, William Cochran, Suvrath Mahadevan, Chad Bender, Scott A. Diddams, Samuel Halverson, Andrea S. J. Lin, Maxwell Moe, Joe Ninan, Paul Robertson, Arpita Roy, Christian Schwab, Gudmundur Stefansson
Figure caption: NESSI contrast curves for TOI-5389A. NESSI rules out nearby sources down to ﹩{\rm{\Delta }}{r}^{{\prime} }=4.05﹩ mag and ﹩{\rm{\Delta }}{z}^{{\prime} }=3.84﹩ mag within 0﹩\mathop{.}\limits^{^{\prime\prime} }﹩2.
Paper: Searching for GEMS: Discovery and Characterization of Two Brown Dwarfs Around M Dwarfs 
Authors: Alexander Larsen, Tera N. Swaby, Henry A. Kobulnicky, Caleb I. Cañas, Shubham Kanodia, Jessica Libby-Roberts, Andrew Monson, Arvind F. Gupta, William Cochran, Suvrath Mahadevan, Chad Bender, Scott A. Diddams, Samuel Halverson, Andrea S. J. Lin, Maxwell Moe, Joe Ninan, Paul Robertson, Arpita Roy, Christian Schwab, Gudmundur Stefansson
Figure caption: NESSI contrast curves for TOI-5610. NESSI rules out nearby sources down to ﹩{\rm{\Delta }}r^{\prime} =4.16﹩ mag and ﹩{\rm{\Delta }}z^{\prime} =3.83﹩ mag within 0﹩\mathop{.}\limits^{^{\prime\prime} }﹩2.
Paper: Predicting Interstellar Object Chemodynamics with Gaia
Authors: Matthew J. Hopkins, Michele T. Bannister, Chris Lintott
Figure caption: Predicted distributions of ISOs with q < 5 au in velocity, on-sky radiant, composition proxied by water mass fraction ﹩{f}_{{{\rm{H}}}_{2}{\rm{O}}}﹩, parent-star metallicity, and age, analogous to Figure 1. On the radiant plot the ecliptic plane is marked in solid blue, the celestial equator is marked in dashed orange, and dashed horizontal lines encapsulate the b = ±10∘ region of high stellar density along the Galactic plane. Orange unfilled histograms plot the distribution of the sine morte stellar population for comparison.
Paper: Predicting Interstellar Object Chemodynamics with Gaia
Authors: Matthew J. Hopkins, Michele T. Bannister, Chris Lintott
Figure caption: Distributions of the sine morte stellar population in velocity, age, and [M/H]. U is the component of velocity toward the Galactic center, V in the direction of motion around the Galactic center, and W out of the plane of the Galaxy, each relative to the Sun's velocity. Both one-dimensional and two-dimensional histograms are normalized to integrate to unity. In orange unfilled histograms we have also plotted the distribution of the raw Gaia sample, without accounting for selection effects or stellar death, for comparison. The vertical lines on the [M/H] distribution are the limits of the protoplanetary disk chemical model.
Paper: Predicting Interstellar Object Chemodynamics with Gaia
Authors: Matthew J. Hopkins, Michele T. Bannister, Chris Lintott
Figure caption: Fraction of q < 5 au ISOs at each velocity, radiant, and age that are “sandy” (﹩{f}_{{{\rm{H}}}_{2}{\rm{O}}}\lt 0.25﹩). Sandy ISOs form the majority in moving groups and low V, and at higher ages.
Paper: Predicting Interstellar Object Chemodynamics with Gaia
Authors: Matthew J. Hopkins, Michele T. Bannister, Chris Lintott
Figure caption: Volume sampling rate scaled by 1/πq2 for different perihelia q. This is the combination of gravitational focusing, which increases the sampling rate of low-relative-speed ISOs, and the “refresh rate” effect, where faster ISOs are sampled at proportionally higher rates.
Paper: JWST-TST DREAMS: A Precise Water Abundance for Hot Jupiter WASP-17b from the NIRISS SOSS Transmission Spectrum
Authors: Dana R. Louie, Elijah Mullens, Lili Alderson, Ana Glidden, Nikole K. Lewis, Hannah R. Wakeford, Natasha E. Batalha, Knicole D. Colón, Amélie Gressier, Douglas Long, Michael Radica, Néstor Espinoza, Jayesh Goyal, Ryan J. MacDonald, Erin M. May, Sara Seager, Kevin B. Stevenson, Jeff A. Valenti, Natalie H. Allen, Caleb I. Cañas, Ryan C. Challener, David Grant, Jingcheng Huang, Zifan Lin, Daniel Valentine, Mark Clampin, Marshall Perrin, Laurent Pueyo, Roeland P. van der Marel, C. Matt Mountain
Figure caption: Comparison of one frame (integration 0, group 8) before and after supreme-SPOON group-level background subtraction applied in Ahsoka Stage 1. The order 1 spectral trace lies in the bottom part of the frame; the order 2 spectral trace lies in the middle; and the order 3 spectral trace is at the upper left. Top: frame shown after the jwst pipeline refpix step. The change in background level intensity near column ∼700 is clearly evident as a “step function.” Order 0 field star contaminants appear as chevron-shaped bright splotches on the right side of the “step.” Additionally, we show with red boxes the regions we use on either side of column 700 to scale the STScI background model to each side of this “step.” We chose these regions because they are relatively free of contaminants. Bottom: the same frame shown after the application of the supreme-SPOON group-level background subtraction. The “step function” near column 700 is no longer evident. The next step to be applied after group-level background subtraction is 1/f noise removal. The three spectral traces and order 0 field star contaminants are all masked during 1/f noise removal.
Paper: JWST-TST DREAMS: A Precise Water Abundance for Hot Jupiter WASP-17b from the NIRISS SOSS Transmission Spectrum
Authors: Dana R. Louie, Elijah Mullens, Lili Alderson, Ana Glidden, Nikole K. Lewis, Hannah R. Wakeford, Natasha E. Batalha, Knicole D. Colón, Amélie Gressier, Douglas Long, Michael Radica, Néstor Espinoza, Jayesh Goyal, Ryan J. MacDonald, Erin M. May, Sara Seager, Kevin B. Stevenson, Jeff A. Valenti, Natalie H. Allen, Caleb I. Cañas, Ryan C. Challener, David Grant, Jingcheng Huang, Zifan Lin, Daniel Valentine, Mark Clampin, Marshall Perrin, Laurent Pueyo, Roeland P. van der Marel, C. Matt Mountain
Figure caption: Ahsoka spectral traces and spectral widths. We employ the STScI-developed PASTASOSS package to determine the spectral traces and wavelength solutions to subpixel level accuracy (T. Baines et al. 2023a, 2023b). Our spectral extraction widths were chosen to minimize the raw white light curve MAD for OOT normalized flux values for each order (see Figure 3).
Paper: Demise of Kreutz Sungrazing Comet C/2024 S1 (ATLAS)
Authors: David Jewitt, Jane Luu, Jing Li
Figure caption: NOT image showing the preperihelion appearance of C/2024 S1 on UT 2024 October 11 at rH = 0.725 au. The image at the top shows raw data compiled from the median of five images each of 60 s integration. A Gaussian smoothed version of this image is shown in the middle panel while the difference image is at the bottom. Four discrete objects are labeled. A scale bar and cardinal directions are marked.
Paper: Demise of Kreutz Sungrazing Comet C/2024 S1 (ATLAS)
Authors: David Jewitt, Jane Luu, Jing Li
Figure caption: Cumulative ice ablation as a function of decreasing heliocentric distance for two sublimation models (solid blue line) a slab oriented perpendicular to the Sun–comet line and (dashed red line) a spherical ice surface sublimating only from the Sun-facing hemisphere. The orbit of C/2024 S1 and ice density ρ = 500 kg m−3 are assumed.
Paper: Demise of Kreutz Sungrazing Comet C/2024 S1 (ATLAS)
Authors: David Jewitt, Jane Luu, Jing Li
Figure caption: Photometry from the COR-2A data as a function of the heliocentric distance. The absolute magnitudes are shown within 48,000 km (blue diamonds) and 96,000 km (red circles) radius apertures. Isothermal, spherical blackbody temperatures are marked along the top axis. The vertical dashed line marks perihelion.
Paper: Demise of Kreutz Sungrazing Comet C/2024 S1 (ATLAS)
Authors: David Jewitt, Jane Luu, Jing Li
Figure caption: Absolute magnitude vs. heliocentric distance for preperihelion NOT observations, measured within circular apertures of fixed projected radii 5000 km (yellow diamonds), 10,000 km (red squares) and 15,000 km (green circles).
Paper: Demise of Kreutz Sungrazing Comet C/2024 S1 (ATLAS)
Authors: David Jewitt, Jane Luu, Jing Li
Figure caption: Cor-2A composite. Each panel has north to the top, east to the left, and is approximately 1°  wide (2.4 × 106 km at the comet). Yellow tick marks in the 0.039 and 0.047 au panels show the expected postperihelion location of the comet, which was not seen at these distances.
Paper: Demise of Kreutz Sungrazing Comet C/2024 S1 (ATLAS)
Authors: David Jewitt, Jane Luu, Jing Li
Figure caption: Preperihelion appearance of C/2024 S1 from NOT images on three dates, as shown. The scale bar and direction arrows are common to all six panels.
Paper: Eight New Candidate Multiplanet Systems among TESS Objects of Interest
Authors: Mohamed Jassim Munavar Hussain, Michelle Kunimoto
Figure caption: Vetting report produced by LEO-vetter. TIC-53498154.02 corresponds to one of our new candidates, which has since been alerted as TOI-5624.02. LEO shows the full observed and detrended stellar light curves from TESS, a phase-folded transit fit, the odd–even transits to compare morphology, a close-up of the light curve at phase 0.5 where secondary eclipses may occur, and models to compute difference images to identify off-target eclipsing signals. Finally, LEO reports stellar, transit fit, and inferred planetary properties.
Paper: Eight New Candidate Multiplanet Systems among TESS Objects of Interest
Authors: Mohamed Jassim Munavar Hussain, Michelle Kunimoto
Figure caption: O – C plots for TOI-6543.01 (top) and TIC-39015188.02 (bottom), showing the difference between observed transit times (O) and transit times computed assuming linear ephemerides (C). While these planets are near a 2:1 mean-motion resonance (Δ = 0.047), we do not detect measurable TTVs.
Paper: Eight New Candidate Multiplanet Systems among TESS Objects of Interest
Authors: Mohamed Jassim Munavar Hussain, Michelle Kunimoto
Figure caption: The binned phase diagrams for all of our new candidates, displaying the data and the transit model fit with residuals. The error bars represent the standard error for each bin. Original data points are plotted in gray, while data binned into 30 minute bins are plotted in black. The transit model fit to the data is plotted in orange. All plots are arranged in ascending order of TIC ID.