adsabs/AstroCLIMB huggingface dataset:
Paper: The TESS-Keck Survey. XVI. Mass Measurements for 12 Planets in Eight Systems
Authors: Joseph M. Akana Murphy, Natalie M. Batalha, Nicholas Scarsdale, Howard Isaacson, David R. Ciardi, Erica J. Gonzales, Steven Giacalone, Joseph D. Twicken, Anne Dattilo, Tara Fetherolf, Ryan A. Rubenzahl, Ian J. M. Crossfield, Courtney D. Dressing, Benjamin Fulton, Andrew W. Howard, Daniel Huber, Stephen R. Kane, Erik A. Petigura, Paul Robertson, Arpita Roy, Lauren M. Weiss, Corey Beard, Ashley Chontos, Fei Dai, Malena Rice, Judah Van Zandt, Jack Lubin, Sarah Blunt, Alex S. Polanski, Aida Behmard, Paul A. Dalba, Michelle L. Hill, Lee J. Rosenthal, Casey L. Brinkman, Andrew W. Mayo, Emma V. Turtelboom, Isabel Angelo, Teo Močnik, Mason G. MacDougall, Daria Pidhorodetska, Dakotah Tyler, Molly R. Kosiarek, Rae Holcomb, Emma M. Louden, Lea A. Hirsch, Emily A. Gilbert, Jay Anderson, Jeff A. Valenti
Figure caption: An example of our Savitzky–Golay filtering procedure for HD 42813’s Sector 6 PDCSAP photometry. The black points are the PDCSAP data, the green line is the data after being smoothed by the Savitzky–Golay filter, and the blue points are the in-transit data, which are not subjected to the outlier rejection. Outliers are marked in red.
Paper: A Noninteracting Galactic Black Hole Candidate in a Binary System with a Main-sequence Star
Authors: Sukanya Chakrabarti, Joshua D. Simon, Peter A. Craig, Henrique Reggiani, Timothy D. Brandt, Puragra Guhathakurta, Paul A. Dalba, Evan N. Kirby, Philip Chang, Daniel R. Hey, Alessandro Savino, Marla Geha, Ian B. Thompson
Figure caption: Phase-folded radial velocity curve for the data listed in Table 2 (top) and for all available data (bottom). The black line in the top panel represents the most likely orbit, and the light-blue curves illustrate a random selection of individual MCMC samples. The orbits shown in the top panel are restricted to periods between 175 and 195 days. The residuals, observed minus calculated, are shown in the lower panels. The agreement is within ∼5 km s−1 for all RV measurements, and all χ 2 values indicate satisfactory fits, with χ 2 per degree of freedom below 1 for both data sets.
Paper: A Noninteracting Galactic Black Hole Candidate in a Binary System with a Main-sequence Star
Authors: Sukanya Chakrabarti, Joshua D. Simon, Peter A. Craig, Henrique Reggiani, Timothy D. Brandt, Puragra Guhathakurta, Paul A. Dalba, Evan N. Kirby, Philip Chang, Daniel R. Hey, Alessandro Savino, Marla Geha, Ian B. Thompson
Figure caption: (Top) Radial velocity solution for Gaia DR3 4373465352415301632, for the velocity measurements listed in Table 2. The black curve is the most likely MCMC orbital solution determined from the spectroscopic measurements alone, and the light-blue curves are a random set of MCMC samples. Many periods are consistent with the RV data. (Bottom) Radial velocity solution including data from Table 2 and from El-Badry et al. (2023b). This fit yields a unimodal solution for the period even without incorporating any information from the astrometric solution (0.4% of the points in the chain are at P ≈ 218  day).
Paper: A Noninteracting Galactic Black Hole Candidate in a Binary System with a Main-sequence Star
Authors: Sukanya Chakrabarti, Joshua D. Simon, Peter A. Craig, Henrique Reggiani, Timothy D. Brandt, Puragra Guhathakurta, Paul A. Dalba, Evan N. Kirby, Philip Chang, Daniel R. Hey, Alessandro Savino, Marla Geha, Ian B. Thompson
Figure caption: MCMC results for the orbital solution determined from the radial velocity data listed in Table 2, showing only elements in the chain with periods between 175 and 195 days. Although some of the parameters exhibit significant correlations, the overall orbital properties are well constrained by the data, with results similar to those expected from the astrometric solution. Some parameters, such as K 1, do have significant uncertainties.
Paper: A Noninteracting Galactic Black Hole Candidate in a Binary System with a Main-sequence Star
Authors: Sukanya Chakrabarti, Joshua D. Simon, Peter A. Craig, Henrique Reggiani, Timothy D. Brandt, Puragra Guhathakurta, Paul A. Dalba, Evan N. Kirby, Philip Chang, Daniel R. Hey, Alessandro Savino, Marla Geha, Ian B. Thompson
Figure caption: Effective temperature and surface gravity of Gaia DR3 4373465352415301632 compared to MIST isochrones. The blue point shows the derived position of the star and the red curve is the 0.91 M ⊙ isochrone that provides the best fit to the combined photometric and spectroscopic data. The gray curves represent 0.89 M ⊙ and 0.93 M ⊙ isochrones for comparison.
Paper: A Noninteracting Galactic Black Hole Candidate in a Binary System with a Main-sequence Star
Authors: Sukanya Chakrabarti, Joshua D. Simon, Peter A. Craig, Henrique Reggiani, Timothy D. Brandt, Puragra Guhathakurta, Paul A. Dalba, Evan N. Kirby, Philip Chang, Daniel R. Hey, Alessandro Savino, Marla Geha, Ian B. Thompson
Figure caption: Joint orbital fit (see text for the description of the joint fit) to the astrometry (top) and radial velocities (middle) for the RV data set given in Table 2, and for all available radial velocity data (bottom). The black lines in the lower two panels show the steps in the RV chains that are most consistent with the Gaia astrometry. These orbits are in tension with the RVs. The light-blue points are drawn from weighted RV chains conditioned on the Gaia data as described in the text.
Paper: A Noninteracting Galactic Black Hole Candidate in a Binary System with a Main-sequence Star
Authors: Sukanya Chakrabarti, Joshua D. Simon, Peter A. Craig, Henrique Reggiani, Timothy D. Brandt, Puragra Guhathakurta, Paul A. Dalba, Evan N. Kirby, Philip Chang, Daniel R. Hey, Alessandro Savino, Marla Geha, Ian B. Thompson
Figure caption: 1, 2, and 3σ confidence levels resulting from fits to all available RV data (blue contours), compared to the reported constraints from Gaia astrometry (orange contours). Although the RV data are qualitatively consistent with the Gaia astrometry, most orbital parameters show discrepancies at the 2–3σ level, even with the full RV data set. Since the χ 2 value for RV fits indicates that the velocity uncertainties have not been underestimated, we conclude that the Gaia errors must have been underestimated.
Paper: A Noninteracting Galactic Black Hole Candidate in a Binary System with a Main-sequence Star
Authors: Sukanya Chakrabarti, Joshua D. Simon, Peter A. Craig, Henrique Reggiani, Timothy D. Brandt, Puragra Guhathakurta, Paul A. Dalba, Evan N. Kirby, Philip Chang, Daniel R. Hey, Alessandro Savino, Marla Geha, Ian B. Thompson
Figure caption: Astrometric orbit determined from the Gaia DR3 astrometric orbital solution as described in the text. The best-fit orbit calculated directly from the Gaia parameters is plotted as the thick black curve, and the thin blue curves represent orbits drawn randomly from the posterior distribution.
Paper: A Noninteracting Galactic Black Hole Candidate in a Binary System with a Main-sequence Star
Authors: Sukanya Chakrabarti, Joshua D. Simon, Peter A. Craig, Henrique Reggiani, Timothy D. Brandt, Puragra Guhathakurta, Paul A. Dalba, Evan N. Kirby, Philip Chang, Daniel R. Hey, Alessandro Savino, Marla Geha, Ian B. Thompson
Figure caption: MCMC results for the orbital solution determined from all available radial velocity data, including the measurements from El-Badry et al. (2023b). The orbital solution is much more strongly constrained by the full data set. We do not show a much sparser cluster of points at P ≈ 218 days, which contains ≈0.4% of the chain.
Paper: A Noninteracting Galactic Black Hole Candidate in a Binary System with a Main-sequence Star
Authors: Sukanya Chakrabarti, Joshua D. Simon, Peter A. Craig, Henrique Reggiani, Timothy D. Brandt, Puragra Guhathakurta, Paul A. Dalba, Evan N. Kirby, Philip Chang, Daniel R. Hey, Alessandro Savino, Marla Geha, Ian B. Thompson
Figure caption: (a) Single SED fit using the BaSeL model and the Fitzpatrick (1999) extinction law. (b) Composite SED fit, with the cooler component shown in yellow, the hotter component shown in blue, and the composite spectrum shown in black.
Paper: VaTEST. II. Statistical Validation of 11 TESS-detected Exoplanets Orbiting K-type Stars
Authors: Priyashkumar Mistry, Kamlesh Pathak, Aniket Prasad, Georgios Lekkas, Surendra Bhattarai, Sarvesh Gharat, Mousam Maity, Dhruv Kumar, Karen A. Collins, Richard P. Schwarz, Christopher R. Mann, Elise Furlan, Steve B. Howell, David Ciardi, Allyson Bieryla, Elisabeth C. Matthews, Erica Gonzales, Carl Ziegler, Ian Crossfield, Steven Giacalone, Thiam-Guan Tan, Phil Evans, Krzysztof G. Hełminiak, Kevin I. Collins, Norio Narita, Akihiko Fukui, Francisco J. Pozuelos, Courtney Dressing, Abderahmane Soubkiou, Zouhair Benkhaldoun, Joshua E. Schlieder, Olga Suarez, Khalid Barkaoui, Enric Palle, Felipe Murgas, Gregor Srdoc, Maria V. Goliguzova, Ivan A. Strakhov, Crystal Gnilka, Kathryn Lester, Colin Littlefield, Nic Scott, Rachel Matson, Michaël Gillon, Emmanuel Jehin, Mathilde Timmermans, Mourad Ghachoui, Lyu Abe, Philippe Bendjoya, Tristan Guillot, Amaury H. M. J. Triaud
Figure caption: Transmission spectroscopy values (left) and emission spectroscopy values (right) for the newly validated planets, color-coded by their equilibrium temperature. In each case the shaded regions indicate areas of interest (dark green region) as identified by Kempton et al. (2018). Big dots represent the planets amenable for transmission or emission spectroscopy.
Paper: Mid-to-late M Dwarfs Lack Jupiter Analogs
Authors: Emily K. Pass, Jennifer G. Winters, David Charbonneau, Jonathan M. Irwin, David W. Latham, Perry Berlind, Michael L. Calkins, Gilbert A. Esquerdo, Jessica Mink
Figure caption: The completeness of our survey, annotated with 95% confidence upper limits on the occurrence rate of giant planets around low-mass M dwarfs as a function of planetary mass and period/instellation/zero-albedo equilibrium temperature under the assumption of circular orbits. In regions where we are highly sensitive (i.e., short periods and large masses), we constrain the occurrence rate to <1.5% with 95% confidence. The color bar indicates N eff, the effective number of stars around which we are sensitive to the hypothetical planet. The arrows in the right-hand plot show instellations equivalent to that of the water snow line (Podolak & Zucker 2004; white), Jupiter (brown), and Neptune (blue). We are sensitive to M P sin i = 1 M J planets at the water snow line for 83% of stars (occurrence rate < 1.8% with 95% confidence) and at Jupiter-like instellations for 70% of stars (occurrence rate < 2.1%). We remain sensitive to M P sin i = 1 M J planets at Neptune-like instellations around 19% of stars (occurrence rate < 7.7%).
Paper: Mid-to-late M Dwarfs Lack Jupiter Analogs
Authors: Emily K. Pass, Jennifer G. Winters, David Charbonneau, Jonathan M. Irwin, David W. Latham, Perry Berlind, Michael L. Calkins, Gilbert A. Esquerdo, Jessica Mink
Figure caption: The mass distribution of our stars. We contrast this sample with Bonfils et al. (2013; B13), the largest radial velocity survey of M dwarfs in the literature, as well as Sabotta et al. (2021; S21)’s recent results from the CARMENES survey. Previous studies of giant planets around M dwarfs have been dominated by early Ms, with masses that are not so dissimilar to those of Sun-like stars. More poorly studied are low-mass, fully convective M dwarfs. Our sample is volume complete and contains 200 such stars with masses of 0.1–0.3 M ⊙. Previous studies have dramatically smaller samples over this mass range (46 in B13 and 15 in S21) and are not volume complete. Note that this figure compares total sample size; for a comparison of effective sample size as a function of planetary mass and period, an interested reader may compare our Figure 3 with Figure 15 of B13 and Figure 3 of S21.
Paper: Mid-to-late M Dwarfs Lack Jupiter Analogs
Authors: Emily K. Pass, Jennifer G. Winters, David Charbonneau, Jonathan M. Irwin, David W. Latham, Perry Berlind, Michael L. Calkins, Gilbert A. Esquerdo, Jessica Mink
Figure caption: The difference in survey sensitivity between the assumption of circular orbits and the assumption that all planets have e = 0.5 (left panel) or e = 0.8 (right panel). This difference is given in terms of ΔN eff, the change in the number of stars around which we could detect the planet, with a positive value indicating an increase in the effective number of stars for the eccentric case over the circular case. Given that our total sample contains 200 stars, the circular orbit assumption is generally appropriate for most regions of parameter space; the largest percent decrease in effective sample size is only 13% and 30% for the e = 0.5 and e = 0.8 assumptions, respectively. There are also previously inaccessible regions of parameter space to which we gain sensitivity when considering eccentric planets (in particular, the regime of super-Jupiters on wide orbits).
Paper: Mid-to-late M Dwarfs Lack Jupiter Analogs
Authors: Emily K. Pass, Jennifer G. Winters, David Charbonneau, Jonathan M. Irwin, David W. Latham, Perry Berlind, Michael L. Calkins, Gilbert A. Esquerdo, Jessica Mink
Figure caption: Radial velocity time series for the two candidate variables. The left panels show LHS 2899 and the right panels show G 125-34, while the upper panels show TRES observations and the lower panels show MAROON-X observations. The lower panels cover a much smaller range in time and radial velocity; the overlap is indicated by the red rectangles. Radial velocities from the blue arm of MAROON-X are shown in blue with thick crosses and from the red arm in red with thin crosses. The red arm achieves uncertainties as low as 70 cm s−1. The lack of radial velocity variability in the extreme precision MAROON-X observations refutes all possible orbital solutions consistent with the variability in the TRES data.
Paper: Mid-to-late M Dwarfs Lack Jupiter Analogs
Authors: Emily K. Pass, Jennifer G. Winters, David Charbonneau, Jonathan M. Irwin, David W. Latham, Perry Berlind, Michael L. Calkins, Gilbert A. Esquerdo, Jessica Mink
Figure caption: Our sensitivity to giant planets around the ten stars in our survey that are known to host a low-mass planet. The darkest blue line denotes a detection probability of 50%. The contours illustrate where our survey places 84% and 97.5% constraints on the existence of a planet. A hypothetical planet with the instellation and mass of Jupiter is indicated with a red X. Dashed lines show the locations of the known small planets. LHS 3844 b is located off the left edge of the plot.
Paper: A Noninteracting Galactic Black Hole Candidate in a Binary System with a Main-sequence Star
Authors: Sukanya Chakrabarti, Joshua D. Simon, Peter A. Craig, Henrique Reggiani, Timothy D. Brandt, Puragra Guhathakurta, Paul A. Dalba, Evan N. Kirby, Philip Chang, Daniel R. Hey, Alessandro Savino, Marla Geha, Ian B. Thompson
Figure caption: Selected portions of the Magellan/MIKE spectrum of Gaia DR3 4373465352415301632 (from left-hand to right-hand: the Mg triplet lines, Hα, and the Ca triplet). The spectrum of HD 126053, which has a spectral type of G1.5V (Gray et al. 2003), is overplotted in pink as a comparison. The close resemblance between the two stars in terms of line strengths and profiles is evident. The stellar parameters of HD 126053 are T eff = 5700 K, ﹩\mathrm{log}g=4.5﹩, [Fe/H]= − 0.35 (e.g., Brewer et al. 2016,Casali20). The small deviations in the wings of some strong lines are likely caused by a combination of continuum normalization uncertainties and the ∼200 K difference in temperature between the two stars.
Paper: A Noninteracting Galactic Black Hole Candidate in a Binary System with a Main-sequence Star
Authors: Sukanya Chakrabarti, Joshua D. Simon, Peter A. Craig, Henrique Reggiani, Timothy D. Brandt, Puragra Guhathakurta, Paul A. Dalba, Evan N. Kirby, Philip Chang, Daniel R. Hey, Alessandro Savino, Marla Geha, Ian B. Thompson
Figure caption: (Top) Posterior distributions of stellar parameters from ARIADNE using all of the available photometry except SkyMapper and Gaia, with the distance prior set from the measured Gaia parallax. (Bottom) Resultant best-fit SED. There is no evidence for an excess at short or long wavelengths that could indicate a second source contributing to the observed fluxes. The same points are shown in the residual plot below in circles (in the SED plot, they are overplotted with diamonds).
Paper: A Noninteracting Galactic Black Hole Candidate in a Binary System with a Main-sequence Star
Authors: Sukanya Chakrabarti, Joshua D. Simon, Peter A. Craig, Henrique Reggiani, Timothy D. Brandt, Puragra Guhathakurta, Paul A. Dalba, Evan N. Kirby, Philip Chang, Daniel R. Hey, Alessandro Savino, Marla Geha, Ian B. Thompson
Figure caption: Gaia color–magnitude diagram. The extinction-corrected absolute magnitude and color of Gaia DR3 4373465352415301632, based on the Gaia parallax and G-band extinction, are marked with a red cross; the Gaia main sequence is apparent.
Paper: A Noninteracting Galactic Black Hole Candidate in a Binary System with a Main-sequence Star
Authors: Sukanya Chakrabarti, Joshua D. Simon, Peter A. Craig, Henrique Reggiani, Timothy D. Brandt, Puragra Guhathakurta, Paul A. Dalba, Evan N. Kirby, Philip Chang, Daniel R. Hey, Alessandro Savino, Marla Geha, Ian B. Thompson
Figure caption: Selected portions of the Magellan/MIKE spectrum of Gaia DR3 4373465352415301632 (the Mg triplet lines, Hα, and the Ca triplet), shown here in the observed frame at the radial velocity extremes spanned by our data set.
Paper: A Noninteracting Galactic Black Hole Candidate in a Binary System with a Main-sequence Star
Authors: Sukanya Chakrabarti, Joshua D. Simon, Peter A. Craig, Henrique Reggiani, Timothy D. Brandt, Puragra Guhathakurta, Paul A. Dalba, Evan N. Kirby, Philip Chang, Daniel R. Hey, Alessandro Savino, Marla Geha, Ian B. Thompson
Figure caption: Available photometry of Gaia DR3 4373465352415301632 from the near-UV to the mid-infrared, with the data sources given in the legend.
Paper: A Noninteracting Galactic Black Hole Candidate in a Binary System with a Main-sequence Star
Authors: Sukanya Chakrabarti, Joshua D. Simon, Peter A. Craig, Henrique Reggiani, Timothy D. Brandt, Puragra Guhathakurta, Paul A. Dalba, Evan N. Kirby, Philip Chang, Daniel R. Hey, Alessandro Savino, Marla Geha, Ian B. Thompson
Figure caption: Orbit in the galaxy, integrated backwards from present day for 500 Myr; the red dot marks the present day (t = 0).
Paper: A Noninteracting Galactic Black Hole Candidate in a Binary System with a Main-sequence Star
Authors: Sukanya Chakrabarti, Joshua D. Simon, Peter A. Craig, Henrique Reggiani, Timothy D. Brandt, Puragra Guhathakurta, Paul A. Dalba, Evan N. Kirby, Philip Chang, Daniel R. Hey, Alessandro Savino, Marla Geha, Ian B. Thompson
Figure caption: Posterior distributions from our joints fits to all available velocity data (including RV data from El-Badry et al. 2023) and Gaia astrometry. The parameter constraints are tighter and correlations are reduced compared to the fit to the velocities alone.
Paper: A Noninteracting Galactic Black Hole Candidate in a Binary System with a Main-sequence Star
Authors: Sukanya Chakrabarti, Joshua D. Simon, Peter A. Craig, Henrique Reggiani, Timothy D. Brandt, Puragra Guhathakurta, Paul A. Dalba, Evan N. Kirby, Philip Chang, Daniel R. Hey, Alessandro Savino, Marla Geha, Ian B. Thompson
Figure caption: Posterior distributions from our joints fits to our velocity data and LAMOST data (as listed in Table 2), and Gaia astrometry. The parameter constraints are tighter and correlations are reduced compared to the fit to the velocities alone.
Paper: VaTEST. II. Statistical Validation of 11 TESS-detected Exoplanets Orbiting K-type Stars
Authors: Priyashkumar Mistry, Kamlesh Pathak, Aniket Prasad, Georgios Lekkas, Surendra Bhattarai, Sarvesh Gharat, Mousam Maity, Dhruv Kumar, Karen A. Collins, Richard P. Schwarz, Christopher R. Mann, Elise Furlan, Steve B. Howell, David Ciardi, Allyson Bieryla, Elisabeth C. Matthews, Erica Gonzales, Carl Ziegler, Ian Crossfield, Steven Giacalone, Thiam-Guan Tan, Phil Evans, Krzysztof G. Hełminiak, Kevin I. Collins, Norio Narita, Akihiko Fukui, Francisco J. Pozuelos, Courtney Dressing, Abderahmane Soubkiou, Zouhair Benkhaldoun, Joshua E. Schlieder, Olga Suarez, Khalid Barkaoui, Enric Palle, Felipe Murgas, Gregor Srdoc, Maria V. Goliguzova, Ivan A. Strakhov, Crystal Gnilka, Kathryn Lester, Colin Littlefield, Nic Scott, Rachel Matson, Michaël Gillon, Emmanuel Jehin, Mathilde Timmermans, Mourad Ghachoui, Lyu Abe, Philippe Bendjoya, Tristan Guillot, Amaury H. M. J. Triaud
Figure caption: Properties of newly validated systems. Top panel: new planets and their comparison with previously known planets (with < 100 day period), shaded region depicts the hot-Neptune desert, figure in right panel is a zoomed-in version of the left figure with labels for the planets in the hot-Neptune desert. Five of the planets lie in the hot-Neptune desert. Right panel: new host stars compared to hosts of known planets. Data for these plots were taken from the NASA Exoplanet Archive.
Paper: VaTEST. II. Statistical Validation of 11 TESS-detected Exoplanets Orbiting K-type Stars
Authors: Priyashkumar Mistry, Kamlesh Pathak, Aniket Prasad, Georgios Lekkas, Surendra Bhattarai, Sarvesh Gharat, Mousam Maity, Dhruv Kumar, Karen A. Collins, Richard P. Schwarz, Christopher R. Mann, Elise Furlan, Steve B. Howell, David Ciardi, Allyson Bieryla, Elisabeth C. Matthews, Erica Gonzales, Carl Ziegler, Ian Crossfield, Steven Giacalone, Thiam-Guan Tan, Phil Evans, Krzysztof G. Hełminiak, Kevin I. Collins, Norio Narita, Akihiko Fukui, Francisco J. Pozuelos, Courtney Dressing, Abderahmane Soubkiou, Zouhair Benkhaldoun, Joshua E. Schlieder, Olga Suarez, Khalid Barkaoui, Enric Palle, Felipe Murgas, Gregor Srdoc, Maria V. Goliguzova, Ivan A. Strakhov, Crystal Gnilka, Kathryn Lester, Colin Littlefield, Nic Scott, Rachel Matson, Michaël Gillon, Emmanuel Jehin, Mathilde Timmermans, Mourad Ghachoui, Lyu Abe, Philippe Bendjoya, Tristan Guillot, Amaury H. M. J. Triaud
Figure caption: Contrast curves extracted from the high-resolution follow-up observations, which allows us to rule out companions at a given separation above a certain Δ Magnitude.
Paper: VaTEST. II. Statistical Validation of 11 TESS-detected Exoplanets Orbiting K-type Stars
Authors: Priyashkumar Mistry, Kamlesh Pathak, Aniket Prasad, Georgios Lekkas, Surendra Bhattarai, Sarvesh Gharat, Mousam Maity, Dhruv Kumar, Karen A. Collins, Richard P. Schwarz, Christopher R. Mann, Elise Furlan, Steve B. Howell, David Ciardi, Allyson Bieryla, Elisabeth C. Matthews, Erica Gonzales, Carl Ziegler, Ian Crossfield, Steven Giacalone, Thiam-Guan Tan, Phil Evans, Krzysztof G. Hełminiak, Kevin I. Collins, Norio Narita, Akihiko Fukui, Francisco J. Pozuelos, Courtney Dressing, Abderahmane Soubkiou, Zouhair Benkhaldoun, Joshua E. Schlieder, Olga Suarez, Khalid Barkaoui, Enric Palle, Felipe Murgas, Gregor Srdoc, Maria V. Goliguzova, Ivan A. Strakhov, Crystal Gnilka, Kathryn Lester, Colin Littlefield, Nic Scott, Rachel Matson, Michaël Gillon, Emmanuel Jehin, Mathilde Timmermans, Mourad Ghachoui, Lyu Abe, Philippe Bendjoya, Tristan Guillot, Amaury H. M. J. Triaud
Figure caption: Difference between in and out transit flux for TOI-672. Left: Direct Image, Right: Difference Image. It can be understood by observing these images that variation in the brightness and target are approximately corelated.