adsabs/AstroCLIMB huggingface dataset:
Paper: Characterizing a World Within the Hot-Neptune Desert: Transit Observations of LTT 9779 b with the Hubble Space Telescope/WFC3
Authors: Billy Edwards, Quentin Changeat, Angelos Tsiaras, Andrew Allan, Patrick Behr, Simone R. Hagey, Michael D. Himes, Sushuang Ma, Keivan G. Stassun, Luis Thomas, Alexandra Thompson, Aaron Boley, Luke Booth, Jeroen Bouwman, Kevin France, Nataliea Lowson, Annabella Meech, Caprice L. Phillips, Aline A. Vidotto, Kai Hou Yip, Michelle Bieger, Amélie Gressier, Estelle Janin, Ing-Guey Jiang, Pietro Leonardi, Subhajit Sarkar, Nour Skaf, Jake Taylor, Ming Yang, Derek Ward-Thompson
Figure caption: SED of LTT 9779. Red symbols represent the observed photometric measurements, where the horizontal bars represent the effective width of the passband. Blue symbols are the model fluxes from the best-fit PHOENIX atmosphere model (black). The Gaia spectrum is also shown as a gray swathe; the inset plot shows a close up.
Paper: Characterizing a World Within the Hot-Neptune Desert: Transit Observations of LTT 9779 b with the Hubble Space Telescope/WFC3
Authors: Billy Edwards, Quentin Changeat, Angelos Tsiaras, Andrew Allan, Patrick Behr, Simone R. Hagey, Michael D. Himes, Sushuang Ma, Keivan G. Stassun, Luis Thomas, Alexandra Thompson, Aaron Boley, Luke Booth, Jeroen Bouwman, Kevin France, Nataliea Lowson, Annabella Meech, Caprice L. Phillips, Aline A. Vidotto, Kai Hou Yip, Michelle Bieger, Amélie Gressier, Estelle Janin, Ing-Guey Jiang, Pietro Leonardi, Subhajit Sarkar, Nour Skaf, Jake Taylor, Ming Yang, Derek Ward-Thompson
Figure caption: Epochs covered by existing data with CHEOPS, JWST, and HST WFC3 UVIS, as well as those that will be covered in TESS Sector 69. Overplotted are our best-fit models when the Spitzer transit timings are included in the analysis. With these data, the apsidal precession model is likely to be conclusively ruled out while the decay model will still be harder to distinguish from the linear period, although stronger constraints on the maximum decay rate could be placed.
Paper: Characterizing a World Within the Hot-Neptune Desert: Transit Observations of LTT 9779 b with the Hubble Space Telescope/WFC3
Authors: Billy Edwards, Quentin Changeat, Angelos Tsiaras, Andrew Allan, Patrick Behr, Simone R. Hagey, Michael D. Himes, Sushuang Ma, Keivan G. Stassun, Luis Thomas, Alexandra Thompson, Aaron Boley, Luke Booth, Jeroen Bouwman, Kevin France, Nataliea Lowson, Annabella Meech, Caprice L. Phillips, Aline A. Vidotto, Kai Hou Yip, Michelle Bieger, Amélie Gressier, Estelle Janin, Ing-Guey Jiang, Pietro Leonardi, Subhajit Sarkar, Nour Skaf, Jake Taylor, Ming Yang, Derek Ward-Thompson
Figure caption: High-resolution (δ λ = 30 Å, spaced by 0.1 Å) HST WFC3 G102 data for LTT 9779 b (top) and WASP-107 b (bottom). In the latter case, the excess absorption due to the helium triplet is clearly apparent.
Paper: Characterizing a World Within the Hot-Neptune Desert: Transit Observations of LTT 9779 b with the Hubble Space Telescope/WFC3
Authors: Billy Edwards, Quentin Changeat, Angelos Tsiaras, Andrew Allan, Patrick Behr, Simone R. Hagey, Michael D. Himes, Sushuang Ma, Keivan G. Stassun, Luis Thomas, Alexandra Thompson, Aaron Boley, Luke Booth, Jeroen Bouwman, Kevin France, Nataliea Lowson, Annabella Meech, Caprice L. Phillips, Aline A. Vidotto, Kai Hou Yip, Michelle Bieger, Amélie Gressier, Estelle Janin, Ing-Guey Jiang, Pietro Leonardi, Subhajit Sarkar, Nour Skaf, Jake Taylor, Ming Yang, Derek Ward-Thompson
Figure caption: Anticipated Lyα signature for LTT 9779 b assuming 2/98 He/H (dotted) and 10/90 He/H (solid). While no trace of atmospheric escape was found with the helium triplet, this tracer may offer another chance to detect and/or constrain the escape rate of LTT 9779 b’s atmosphere.
Paper: Mass Ratio of Single-line Spectroscopic Binaries with Visual Orbits Using Bayesian Inference and Suitable Priors 
Authors: Jennifer Anguita-Aguero, Rene A. Mendez, Miguel Videla, Edgardo Costa, Leonardo Vanzi, Nicolas Castro-Morales, Camila Caballero-Valdes
Figure caption: Orbit (left panel) and RV curve (right panel) for HIP 38414 based on the MAP values obtained from the SB1 + p(ϖ) + p(m 1∣θ) solution given in Table 2. The size and color of the dots in both plots depict the weight (uncertainty) of each observation: large clear dots indicate larger errors, and the opposite is true for small dark dots. In all astrometric orbits presented, smaller dots are from more recent interferometric measurements, including—but not limited to—our own (although in this particular case, all observations are from SOAR). For this system, we have a phase coverage of about 50% of the visual orbit. The large deviant point is from SOAR at 2011.9, so we gave it a smaller weight in our solution. For the RV curve, we supplemented good quality historical data with recent data acquired by us with FEROS and FIDEOS. The dashed horizontal line in the RV curve indicates the estimated systemic velocity, which is included, with its 95% HDPI range, at the right end of the line.
Paper: Mass Ratio of Single-line Spectroscopic Binaries with Visual Orbits Using Bayesian Inference and Suitable Priors 
Authors: Jennifer Anguita-Aguero, Rene A. Mendez, Miguel Videla, Edgardo Costa, Leonardo Vanzi, Nicolas Castro-Morales, Camila Caballero-Valdes
Figure caption: Similar to Figure 2, but for the HIP 43109 system. In this case, we have a good orbital coverage of the visual orbit (save for a small arc near periastron). The data points included are of different quality; some are historical RVs of decent quality and some are highly precise measurements at three consecutive epochs from HARPS at the ESO/La Silla 3.6 m telescope.
Paper: Mass Ratio of Single-line Spectroscopic Binaries with Visual Orbits Using Bayesian Inference and Suitable Priors 
Authors: Jennifer Anguita-Aguero, Rene A. Mendez, Miguel Videla, Edgardo Costa, Leonardo Vanzi, Nicolas Castro-Morales, Camila Caballero-Valdes
Figure caption: Similar to Figure 4, but for the HIP 43109 system.
Paper: Mass Ratio of Single-line Spectroscopic Binaries with Visual Orbits Using Bayesian Inference and Suitable Priors 
Authors: Jennifer Anguita-Aguero, Rene A. Mendez, Miguel Videla, Edgardo Costa, Leonardo Vanzi, Nicolas Castro-Morales, Camila Caballero-Valdes
Figure caption: Marginal PDFs and MAP estimates (vertical magenta lines) for the orbital and physical parameters of the HIP 38414 binary system, for the SB1 + p(ϖ) + p(m 1∣θ) solution. The magenta horizontal error bars (±2σ) indicate the priors adopted for ϖ and m 1, from Table 1.
Paper: Mass Ratio of Single-line Spectroscopic Binaries with Visual Orbits Using Bayesian Inference and Suitable Priors 
Authors: Jennifer Anguita-Aguero, Rene A. Mendez, Miguel Videla, Edgardo Costa, Leonardo Vanzi, Nicolas Castro-Morales, Camila Caballero-Valdes
Figure caption: Corner plots for HIP 38414. These plots are useful for a qualitative assessment of the quality of the fit, in the sense that better-defined orbits, with enough phase coverage, have tight (usually Gaussian-like) PDFs, while less-defined orbits have rather disperse, tangled, and/or asymmetrical PDFs with long tails. Corner plots can also be used to uncover possible correlations between parameters that, if found to be systematic, can eventually be used to reduce the dimensionality of the inference. This is especially useful in problems of high dimensionality. In some cases, we have used these corner plots to check the consistency of our solutions when the SpTy is ambiguous (see the case of HIP 96302 in Section 4).
Paper: Mass Ratio of Single-line Spectroscopic Binaries with Visual Orbits Using Bayesian Inference and Suitable Priors 
Authors: Jennifer Anguita-Aguero, Rene A. Mendez, Miguel Videla, Edgardo Costa, Leonardo Vanzi, Nicolas Castro-Morales, Camila Caballero-Valdes
Figure caption: (Pseudo) orbital parallaxes from this work vs. the adopted prior parallax (left panel). In the right panel, we show the residuals in the sense ΠOrb − ΠAdopted normalized by the parallax uncertainty of each target (see the text for details). The labels indicate the HIP numbers.
Paper: OGLE-2019-BLG-1180Lb: Discovery of a Wide-orbit Jupiter-mass Planet around a Late-type Star
Authors: Sun-Ju Chung, Andrzej Udalski, Jennifer C. Yee, Andrew Gould, Michael D. Albrow, Youn Kil Jung, Kyu-Ha Hwang, Cheongho Han, Yoon-Hyun Ryu, In-Gu Shin, Yossi Shvartzvald, Hongjing Yang, Weicheng Zang, Sang-Mok Cha, Dong-Jin Kim, Seung-Lee Kim, Chung-Uk Lee, Dong-Joo Lee, Yongseok Lee, Byeong-Gon Park, Richard W. Pogge, Radek Poleski, Przemek Mróz, Jan Skowron, Michał K. Szymański, Igor Soszyński, Paweł Pietrukowicz, Szymon Kozłowski, Krzysztof Ulaczyk, Krzysztof A. Rybicki, Patryk Iwanek, Marcin Wrona, Mariusz Gromadzki
Figure caption: Close-up view of the anomaly region. Here t 1 and t 2 represent the times before the source passes the cusp and right after the source exits the caustic, respectively (see Figure 3).
Paper: OGLE-2019-BLG-1180Lb: Discovery of a Wide-orbit Jupiter-mass Planet around a Late-type Star
Authors: Sun-Ju Chung, Andrzej Udalski, Jennifer C. Yee, Andrew Gould, Michael D. Albrow, Youn Kil Jung, Kyu-Ha Hwang, Cheongho Han, Yoon-Hyun Ryu, In-Gu Shin, Yossi Shvartzvald, Hongjing Yang, Weicheng Zang, Sang-Mok Cha, Dong-Jin Kim, Seung-Lee Kim, Chung-Uk Lee, Dong-Joo Lee, Yongseok Lee, Byeong-Gon Park, Richard W. Pogge, Radek Poleski, Przemek Mróz, Jan Skowron, Michał K. Szymański, Igor Soszyński, Paweł Pietrukowicz, Szymon Kozłowski, Krzysztof Ulaczyk, Krzysztof A. Rybicki, Patryk Iwanek, Marcin Wrona, Mariusz Gromadzki
Figure caption: Geometry of the best-fit parallax+orbital model. Top: the blue solid dots represent two lens components, while the red open circle represents the normalized source size. The dotted circle denotes the Einstein ring and the straight line with an arrow is the source trajectory. The black closed curve represents the planetary caustic. Bottom: close-up view of the planetary caustic region. The caustics at t 1 = 8741.2 and t 2 = 8743.5 are presented in black and gray, respectively.
Paper: OGLE-2019-BLG-1180Lb: Discovery of a Wide-orbit Jupiter-mass Planet around a Late-type Star
Authors: Sun-Ju Chung, Andrzej Udalski, Jennifer C. Yee, Andrew Gould, Michael D. Albrow, Youn Kil Jung, Kyu-Ha Hwang, Cheongho Han, Yoon-Hyun Ryu, In-Gu Shin, Yossi Shvartzvald, Hongjing Yang, Weicheng Zang, Sang-Mok Cha, Dong-Jin Kim, Seung-Lee Kim, Chung-Uk Lee, Dong-Joo Lee, Yongseok Lee, Byeong-Gon Park, Richard W. Pogge, Radek Poleski, Przemek Mróz, Jan Skowron, Michał K. Szymański, Igor Soszyński, Paweł Pietrukowicz, Szymon Kozłowski, Krzysztof Ulaczyk, Krzysztof A. Rybicki, Patryk Iwanek, Marcin Wrona, Mariusz Gromadzki
Figure caption: Light curve of the best-fit parallax+orbital lens model of OGLE-2019-BLG-1180. (The data used to create this figure are available.)
Paper: Detecting Solar System Analogs through Joint Radial Velocity/Astrometric Surveys
Authors: Daniel A. Yahalomi, Ruth Angus, David N. Spergel, Daniel Foreman-Mackey
Figure caption: Simulated “true” R.A. and decl. astrometry for an Earth-like exoplanet around a Sun-like star. Predicted Gaia R.A. and decl. observations, assuming white noise errors of 34.2 μas along the scan and 171 μas across the scan, with observations every 26 days for 10 yr. Predicted Roman R.A. and decl. observations assuming white noise errors of 5 μas, with observations every 40 days for 10 yr. And MCMC posterior results for the R.A. and decl.
Paper: Detecting Solar System Analogs through Joint Radial Velocity/Astrometric Surveys
Authors: Daniel A. Yahalomi, Ruth Angus, David N. Spergel, Daniel Foreman-Mackey
Figure caption: Left: Median and 1σ MCMC period and mass for an Earth-like exoplanet around a Sun-like star. The black dashed line shows the simulated values. Right: MCMC median and 1σ values for exoplanetary and orbital parameters as well as their corresponding simulated “true” values. Roman observing program with 10 yr of observations every 40 days and an assumed 1σ measurement error of 5 μas.
Paper: Detecting Solar System Analogs through Joint Radial Velocity/Astrometric Surveys
Authors: Daniel A. Yahalomi, Ruth Angus, David N. Spergel, Daniel Foreman-Mackey
Figure caption: Left: Median and 1σ MCMC period and mass for a Jupiter-like exoplanet around a Sun-like star. The black dashed line shows the simulated values. Right: MCMC median and 1σ values for exoplanetary and orbital parameters as well as their corresponding simulated “true” values. Roman observing program with 10 yr of observations every 40 days and an assumed 1σ measurement error of 5 μas.
Paper: Detecting Solar System Analogs through Joint Radial Velocity/Astrometric Surveys
Authors: Daniel A. Yahalomi, Ruth Angus, David N. Spergel, Daniel Foreman-Mackey
Figure caption: Simulated “true” R.A. and decl. astrometry for an Jupiter-like exoplanet around Sun-like star at 10 pc. Predicted Gaia R.A. and decl. observations assuming white noise errors of 60 μas with observations every 26 days for 10 yr. Predicted Roman R.A. and decl. observations, assuming white noise errors of 5 μas, with observations every 40 days for 10 yr. And MCMC posterior results for the R.A. and decl.
Paper: Estimating Distances from Parallaxes. VI. A Method for Inferring Distances and Transverse Velocities from Parallaxes and Proper Motions Demonstrated on Gaia Data Release 3
Authors: C. A. L. Bailer-Jones
Figure caption: Velocity prior for HEALpixel 6200 at (l, b) = (285.°7, 34.°8). The top left panel shows the positions of the midpoints of the shells and the number of sources in them (on a log scale). The two central panels show the distribution of the velocities (top v  α*, bottom v  δ ) for some selected shells, with the colors denoting the shell as in the top left panel. The dashed lines show the fitted Gaussians. The two right panels show the values of the fitted means (upper) and fitted standard deviations (lower) for all shells, as red circles for v  α* and as blue triangles for v  δ . The lines show the spline fits, which extend to the outer radius of the last shell, here 7597 pc. The bottom left panel shows the fitted correlations of the Gaussians in each shell along with their spline fits, but these are not used (the correlation is set to zero in the model).
Paper: Estimating Distances from Parallaxes. VI. A Method for Inferring Distances and Transverse Velocities from Parallaxes and Proper Motions Demonstrated on Gaia Data Release 3
Authors: C. A. L. Bailer-Jones
Figure caption: Median of the distance prior in each HEALpixel, computed from the mock catalog of Rybizki et al. (2020).
Paper: TOI-4010: A System of Three Large Short-period Planets with a Massive Long-period Companion
Authors: Michelle Kunimoto, Andrew Vanderburg, Chelsea X. Huang, M. Ryleigh Davis, Laura Affer, Andrew Collier Cameron, David Charbonneau, Rosario Cosentino, Mario Damasso, Xavier Dumusque, A. F. Martnez Fiorenzano, Adriano Ghedina, R. D. Haywood, Florian Lienhard, Mercedes López-Morales, Michel Mayor, Francesco Pepe, Matteo Pinamonti, Ennio Poretti, Jesús Maldonado, Ken Rice, Alessandro Sozzetti, Thomas G. Wilson, Stéphane Udry, Jay Baptista, Khalid Barkaoui, Juliette Becker, Paul Benni, Allyson Bieryla, Pau Bosch-Cabot, David R. Ciardi, Karen A. Collins, Kevin I. Collins, Elise Evans, Trent J. Dupuy, Maria V. Goliguzova, Pere Guerra, Adam Kraus, Jack J. Lissauer, Daniel Huber, Felipe Murgas, Enric Palle, Samuel N. Quinn, Boris S. Safonov, Richard P. Schwarz, Avi Shporer, Keivan G. Stassun, Jon M. Jenkins, David W. Latham, George R. Ricker, Sara Seager, Roland Vanderspek, Joshua Winn, Zahra Essack, Hannah M. Lewis, Mark E. Rose
Figure caption: Top: Difference images for TOI-4010.01, 4010.02, and 4010.03, made using 20 × 20 pixel cutouts of the Sector 25 TESS FFIs. Bottom: Close-up of the central 5 × 5 pixels. The fourth column shows the average of out-of-transit images, which should represent a direct image of the field near the target star. The color bars show the average pixel flux in electrons per second. The target TIC-352682207 is indicated with a pink star, while nearby stars up to ΔT = 4 mag fainter are plotted as white circles with sizes scaled by brightness. The difference images for all three planet candidates indicate the transit sources are co-located with the target star.
Paper: TOI-4010: A System of Three Large Short-period Planets with a Massive Long-period Companion
Authors: Michelle Kunimoto, Andrew Vanderburg, Chelsea X. Huang, M. Ryleigh Davis, Laura Affer, Andrew Collier Cameron, David Charbonneau, Rosario Cosentino, Mario Damasso, Xavier Dumusque, A. F. Martnez Fiorenzano, Adriano Ghedina, R. D. Haywood, Florian Lienhard, Mercedes López-Morales, Michel Mayor, Francesco Pepe, Matteo Pinamonti, Ennio Poretti, Jesús Maldonado, Ken Rice, Alessandro Sozzetti, Thomas G. Wilson, Stéphane Udry, Jay Baptista, Khalid Barkaoui, Juliette Becker, Paul Benni, Allyson Bieryla, Pau Bosch-Cabot, David R. Ciardi, Karen A. Collins, Kevin I. Collins, Elise Evans, Trent J. Dupuy, Maria V. Goliguzova, Pere Guerra, Adam Kraus, Jack J. Lissauer, Daniel Huber, Felipe Murgas, Enric Palle, Samuel N. Quinn, Boris S. Safonov, Richard P. Schwarz, Avi Shporer, Keivan G. Stassun, Jon M. Jenkins, David W. Latham, George R. Ricker, Sara Seager, Roland Vanderspek, Joshua Winn, Zahra Essack, Hannah M. Lewis, Mark E. Rose
Figure caption: Archival images showing the field within 40″ of TOI-4010 in blue (left), red (center left), and infrared (center right) filters from the second Palomar Sky Survey, and the y band (right) from the first Pan-STARRS survey. The location of TOI-4010 at the start of TESS Sector 24 in 2020 is marked with an orange cross. TOI-4010 has moved only ∼3″ since the oldest image in 1989, and is relatively isolated, with no nearby brighter stars.
Paper: The Star Formation Across Cosmic Time (SFACT) Survey. III. Spectroscopy of the Initial Catalog of Emission-line Objects
Authors: David J. Carr, Jennifer Sieben, John J. Salzer, Samantha W. Brunker, Bryce Cousins
Figure caption: Top: The redward half of the final processed multiobject spectral image from a pointing of SFF15. Each row in the image is a one-dimensional spectrum of an individual SFACT target. The red boxes show the wavelength coverage of the three narrowband filters. The leftmost box is NB2, the middle box shows NB1, and the right box shows NB3. In this pointing, many NB2 candidates were observed. Bottom: The spectral regions covered by SFACT’s filters are enlarged and presented in the same order from left to right as mentioned above.
Paper: Systematic KMTNet Planetary Anomaly Search. IX. Complete Sample of 2016 Prime-field Planets
Authors: In-Gu Shin, Jennifer C. Yee, Weicheng Zang, Hongjing Yang, Kyu-Ha Hwang, Cheongho Han, Andrew Gould, Andrzej Udalski, Ian A. Bond, Michael D. Albrow, Sun-Ju Chung, Youn Kil Jung, Yoon-Hyun Ryu, Yossi Shvartzvald, Sang-Mok Cha, Dong-Jin Kim, Seung-Lee Kim, Chung-Uk Lee, Dong-Joo Lee, Yongseok Lee, Byeong-Gon Park, Richard W. Pogge, Przemek Mróz, Michał K. Szymański, Jan Skowron, Radosław Poleski, Igor Soszyński, Paweł Pietrukowicz, Szymon Kozłowski, Krzysztof A. Rybicki, Patryk Iwanek, Krzysztof Ulaczyk, Marcin Wrona, Mariusz Gromadzki, Fumio Abe, Richard Barry, David P. Bennett, Aparna Bhattacharya, Hirosane Fujii, Akihiko Fukui, Ryusei Hamada, Yuki Hirao, Stela Ishitani Silva, Yoshitaka Itow, Rintaro Kirikawa, Iona Kondo, Naoki Koshimoto, Yutaka Matsubara, Shota Miyazaki, Yasushi Muraki, Greg Olmschenk, Clément Ranc, Nicholas J. Rattenbury, Yuki Satoh, Takahiro Sumi, Daisuke Suzuki, Mio Tomoyoshi, Paul J. Tristram, Aikaterini Vandorou, Hibiki Yama, Kansuke Yamashita
Figure caption: Light curve of MOA-2016-BLG-532 with the best-fit planetary model. We compare the planetary solution (black solid line) to the binary (blue dotted line) and 1L1S with finite-source (cyan dashed line) models. We also present caustic geometries of 2L1S models on the right side for comparison.
Paper: Systematic KMTNet Planetary Anomaly Search. IX. Complete Sample of 2016 Prime-field Planets
Authors: In-Gu Shin, Jennifer C. Yee, Weicheng Zang, Hongjing Yang, Kyu-Ha Hwang, Cheongho Han, Andrew Gould, Andrzej Udalski, Ian A. Bond, Michael D. Albrow, Sun-Ju Chung, Youn Kil Jung, Yoon-Hyun Ryu, Yossi Shvartzvald, Sang-Mok Cha, Dong-Jin Kim, Seung-Lee Kim, Chung-Uk Lee, Dong-Joo Lee, Yongseok Lee, Byeong-Gon Park, Richard W. Pogge, Przemek Mróz, Michał K. Szymański, Jan Skowron, Radosław Poleski, Igor Soszyński, Paweł Pietrukowicz, Szymon Kozłowski, Krzysztof A. Rybicki, Patryk Iwanek, Krzysztof Ulaczyk, Marcin Wrona, Mariusz Gromadzki, Fumio Abe, Richard Barry, David P. Bennett, Aparna Bhattacharya, Hirosane Fujii, Akihiko Fukui, Ryusei Hamada, Yuki Hirao, Stela Ishitani Silva, Yoshitaka Itow, Rintaro Kirikawa, Iona Kondo, Naoki Koshimoto, Yutaka Matsubara, Shota Miyazaki, Yasushi Muraki, Greg Olmschenk, Clément Ranc, Nicholas J. Rattenbury, Yuki Satoh, Takahiro Sumi, Daisuke Suzuki, Mio Tomoyoshi, Paul J. Tristram, Aikaterini Vandorou, Hibiki Yama, Kansuke Yamashita
Figure caption: Light curve of OGLE-2016-BLG-1635 with s ± models and their caustic geometries.
Paper: Systematic KMTNet Planetary Anomaly Search. IX. Complete Sample of 2016 Prime-field Planets
Authors: In-Gu Shin, Jennifer C. Yee, Weicheng Zang, Hongjing Yang, Kyu-Ha Hwang, Cheongho Han, Andrew Gould, Andrzej Udalski, Ian A. Bond, Michael D. Albrow, Sun-Ju Chung, Youn Kil Jung, Yoon-Hyun Ryu, Yossi Shvartzvald, Sang-Mok Cha, Dong-Jin Kim, Seung-Lee Kim, Chung-Uk Lee, Dong-Joo Lee, Yongseok Lee, Byeong-Gon Park, Richard W. Pogge, Przemek Mróz, Michał K. Szymański, Jan Skowron, Radosław Poleski, Igor Soszyński, Paweł Pietrukowicz, Szymon Kozłowski, Krzysztof A. Rybicki, Patryk Iwanek, Krzysztof Ulaczyk, Marcin Wrona, Mariusz Gromadzki, Fumio Abe, Richard Barry, David P. Bennett, Aparna Bhattacharya, Hirosane Fujii, Akihiko Fukui, Ryusei Hamada, Yuki Hirao, Stela Ishitani Silva, Yoshitaka Itow, Rintaro Kirikawa, Iona Kondo, Naoki Koshimoto, Yutaka Matsubara, Shota Miyazaki, Yasushi Muraki, Greg Olmschenk, Clément Ranc, Nicholas J. Rattenbury, Yuki Satoh, Takahiro Sumi, Daisuke Suzuki, Mio Tomoyoshi, Paul J. Tristram, Aikaterini Vandorou, Hibiki Yama, Kansuke Yamashita
Figure caption: Zoom-in of the anomaly part of OGLE-2016-BLG-1850 for comparing all models with their residuals.
Paper: Systematic KMTNet Planetary Anomaly Search. IX. Complete Sample of 2016 Prime-field Planets
Authors: In-Gu Shin, Jennifer C. Yee, Weicheng Zang, Hongjing Yang, Kyu-Ha Hwang, Cheongho Han, Andrew Gould, Andrzej Udalski, Ian A. Bond, Michael D. Albrow, Sun-Ju Chung, Youn Kil Jung, Yoon-Hyun Ryu, Yossi Shvartzvald, Sang-Mok Cha, Dong-Jin Kim, Seung-Lee Kim, Chung-Uk Lee, Dong-Joo Lee, Yongseok Lee, Byeong-Gon Park, Richard W. Pogge, Przemek Mróz, Michał K. Szymański, Jan Skowron, Radosław Poleski, Igor Soszyński, Paweł Pietrukowicz, Szymon Kozłowski, Krzysztof A. Rybicki, Patryk Iwanek, Krzysztof Ulaczyk, Marcin Wrona, Mariusz Gromadzki, Fumio Abe, Richard Barry, David P. Bennett, Aparna Bhattacharya, Hirosane Fujii, Akihiko Fukui, Ryusei Hamada, Yuki Hirao, Stela Ishitani Silva, Yoshitaka Itow, Rintaro Kirikawa, Iona Kondo, Naoki Koshimoto, Yutaka Matsubara, Shota Miyazaki, Yasushi Muraki, Greg Olmschenk, Clément Ranc, Nicholas J. Rattenbury, Yuki Satoh, Takahiro Sumi, Daisuke Suzuki, Mio Tomoyoshi, Paul J. Tristram, Aikaterini Vandorou, Hibiki Yama, Kansuke Yamashita
Figure caption: Light curve of OGLE-2016-BLG-1850 with STD (cyan) and APRX (black) models.
Paper: Astrometry and Photometry for ≈1000 L, T, and Y Dwarfs from the UKIRT Hemisphere Survey
Authors: Adam C. Schneider, Jeffrey A. Munn, Frederick J. Vrba, Justice Bruursema, Scott E. Dahm, Stephen J. Williams, Michael C. Liu, Bryan N. Dorland
Figure caption: The positions and proper motions of the four new Hyades candidate members identified in this work compared to the list of Hyades members from the Gaia Catalog of Nearby Stars (GCNS; Gaia Collaboration et al. 2021).