adsabs/AstroCLIMB huggingface dataset:
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 MLR from the 23 SB1 systems of luminosity class V in our sample. The plot inserted shows a zoom-in on the mass range from 0.5 to 1.5 M ⊙, with M  V  from +3.0 to +7.5. Primary components are depicted with a blue dot and secondaries with a red dot. The components of each binary are joined by a thin dashed line (the most massive object, HIP 7901, presented in Videla et al. 2022, does not have photometry for its secondary, hence only the primary star is shown here). The uncertainties on the mass of the primary and secondary are directly based on the values given in the last row of each entry in Table 2 (and the corresponding table in Videla et al. 2022), while we have assumed an uncertainty of ∼0.05 mag in M  V  as a representative value, considering the errors in the photometry and distance.
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 HIP 29860. For this system, the visual orbit is incomplete, with a severe lack of observations near periastron. Old RV data show a large scatter, while modern data and our own data from FEROS and FIDEOS (obtained in 2021 and 2022—indicated in the plot) are of much higher quality. This helped to constrain the final orbit, which, as indicated in Table 2, has a formal uncertainty of 0.3% in the period and 0.6% in the semimajor axis.
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: Same as Figure 4, but for the HIP 29860 binary 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: Residual O−C plots for HIP 78727, based on our MCMC solution with the orbital parameters indicated in Table 2. The dashed lines indicate the 3σ  boundaries computed from the overall rms of each panel. There is a clear indication of a significant wobble in position angle, with a period of about 50 yr (top panel), possibly due to an accounted-for companion to the AB system (see the text for details). There are hints of some periodicity in the separation residuals as well (middle panel), but these are less significant. Scarce RV data preclude us from any conclusion based on the lower panel.
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: Mass residuals for the 22 class V secondaries of Figure 7 (including those from Videla et al. 2022), in comparison with the expected mass, given their luminosity from the fiducial relationships from Abushattal et al. (2020; their Table 18). The dashed lines indicate the empirical ±1σ values, while the error on the mass in the abscissa comes from the upper and lower values presented in Table 2. The labels indicate the HIP numbers.
Paper: Clustering Properties of Intermediate and High-mass Young Stellar Objects 
Authors: Miguel Vioque, Manuel Cavieres, Michelangelo Pantaleoni González, Álvaro Ribas, René D. Oudmaijer, Ignacio Mendigutía, Lena Kilian, Héctor Cánovas, Michael A. Kuhn
Figure caption: Proportion of clustered (“3D or 5D”) intermediate- and high-mass YSOs as a function of stellar mass. Historically known YSOs have been separated from those identified homogeneously and in a position-unbiased way by Vioque et al. (2022). The top and bottom plots differ in the stellar mass bin used. Complete error is ﹩1/\sqrt{n}﹩, with n being the number of sources per bin.
Paper: Clustering Properties of Intermediate and High-mass Young Stellar Objects 
Authors: Miguel Vioque, Manuel Cavieres, Michelangelo Pantaleoni González, Álvaro Ribas, René D. Oudmaijer, Ignacio Mendigutía, Lena Kilian, Héctor Cánovas, Michael A. Kuhn
Figure caption: Comparison of the clustering rate between the YSO sample of this work and the YSO sample of Iglesias et al. (2023). Complete error is ﹩1/\sqrt{n}﹩, with n being the number of sources per bin. For visualization purposes, the plots show a smaller range of stellar masses with respect to Figure 4, as the Iglesias et al. (2023) sample is limited to 7 M ⊙.
Paper: Clustering Properties of Intermediate and High-mass Young Stellar Objects 
Authors: Miguel Vioque, Manuel Cavieres, Michelangelo Pantaleoni González, Álvaro Ribas, René D. Oudmaijer, Ignacio Mendigutía, Lena Kilian, Héctor Cánovas, Michael A. Kuhn
Figure caption: Same as Figure 4 “3D or 5D” with 2 M ⊙ bins but considering only certain distance ranges. The top-left panel is identical to the Figure 4 bottom-left “3D or 5D” panel. We show it here for comparison purposes. Complete error is ﹩1/\sqrt{n}﹩, with n being the number of sources per bin.
Paper: Clustering Properties of Intermediate and High-mass Young Stellar Objects 
Authors: Miguel Vioque, Manuel Cavieres, Michelangelo Pantaleoni González, Álvaro Ribas, René D. Oudmaijer, Ignacio Mendigutía, Lena Kilian, Héctor Cánovas, Michael A. Kuhn
Figure caption: Left: distance vs. stellar mass for all YSOs compiled in this work (337 sources). Density curves of clustered and isolated sources are shown at the top and right. Black dots indicate those sources that appear clustered both in 3D and 5D. Right: distance vs. Gaia G-band magnitude for all YSOs compiled in this work. Color scheme indicates stellar mass, with darker sources being more massive (linear scale). For the analysis, we have only considered sources between 350 and 4000 pc.
Paper: Clustering Properties of Intermediate and High-mass Young Stellar Objects 
Authors: Miguel Vioque, Manuel Cavieres, Michelangelo Pantaleoni González, Álvaro Ribas, René D. Oudmaijer, Ignacio Mendigutía, Lena Kilian, Héctor Cánovas, Michael A. Kuhn
Figure caption: Within 3′ of each intermediate- or high-mass YSO. Left: fraction of sources considered in our analysis (with Gaia DR3 five-parameter solution) with respect to all Gaia DR3 sources. Right: fraction of Gaia DR3 sources with all five astrometric quantities having values over three times their uncertainty with respect to the sources considered in our analysis. The stellar mass of the intermediate- or high-mass YSOs is shown in the horizontal axes. Density curves of clustered and isolated sources are shown at the top and right.
Paper: Clustering Properties of Intermediate and High-mass Young Stellar Objects 
Authors: Miguel Vioque, Manuel Cavieres, Michelangelo Pantaleoni González, Álvaro Ribas, René D. Oudmaijer, Ignacio Mendigutía, Lena Kilian, Héctor Cánovas, Michael A. Kuhn
Figure caption: Cluster properties as a function of the stellar mass of the intermediate- or high-mass YSO contained in each cluster. Left: number of sources in each cluster (N  c ). Center: cluster size (R 80%). Right: cluster density (﹩0.8{N}_{c}/\pi {R}_{80 \% }^{2}﹩).
Paper: Clustering Properties of Intermediate and High-mass Young Stellar Objects 
Authors: Miguel Vioque, Manuel Cavieres, Michelangelo Pantaleoni González, Álvaro Ribas, René D. Oudmaijer, Ignacio Mendigutía, Lena Kilian, Héctor Cánovas, Michael A. Kuhn
Figure caption: Within 3′ of each YSO, this plot shows the fraction of sources detected by IR surveys that were considered in our analysis (those with Gaia DR3 five-parameter solution). From left to right, VVV, UKIDSS, and 2MASS are shown. The horizontal axes show the stellar mass of each intermediate- or high-mass YSO. Density curves of clustered and isolated sources are shown at the top and right.
Paper: Clustering Properties of Intermediate and High-mass Young Stellar Objects 
Authors: Miguel Vioque, Manuel Cavieres, Michelangelo Pantaleoni González, Álvaro Ribas, René D. Oudmaijer, Ignacio Mendigutía, Lena Kilian, Héctor Cánovas, Michael A. Kuhn
Figure caption: Within 3′ of each YSO, this plot shows the fraction of sources appearing in the IR-based catalogs of Kuhn et al. (2021a; SPICY) and Winston et al. (2020), which were considered in our analysis (with Gaia DR3 five-parameter solution). The horizontal axes show the stellar mass of each intermediate- or high-mass YSO. Density curves of clustered and isolated sources are shown at the top and right.
Paper: Clustering Properties of Intermediate and High-mass Young Stellar Objects 
Authors: Miguel Vioque, Manuel Cavieres, Michelangelo Pantaleoni González, Álvaro Ribas, René D. Oudmaijer, Ignacio Mendigutía, Lena Kilian, Héctor Cánovas, Michael A. Kuhn
Figure caption: Top: distances of the intermediate- and high-mass YSOs to the geometrical center of their clusters as a function of their stellar mass. Bottom: distances of the intermediate- and high-mass YSOs to the geometrical center of their clusters divided by the cluster sizes (R 80%) vs. the stellar mass of the intermediate- and high-mass YSOs.
Paper: Atmospheric Retrieval of L Dwarfs: Benchmarking Results and Characterizing the Young Planetary Mass Companion HD 106906 b in the Near-infrared
Authors: Arthur D. Adams, Michael R. Meyer, Alex R. Howe, Ben Burningham, Sebastian Daemgen, Jonathan Fortney, Mike Line, Mark Marley, Sascha P. Quanz, Kamen Todorov
Figure caption: Spectra and contribution functions of the retrieved forward model fits to the HD 106906 b data. The forward model spectra (using the MLE parameter values) are in color, with the results from the cloudy model in red and those of a cloud-free model in blue. The data are shown in gray. The retrievals are performed with the data binned down to a resolution 4–8 times lower than its original, to mitigate the potential effects of binning errors from the opacity tables. Prominent alkali lines in the J-band data are marked with vertical dashed lines, including two K I doublets and a smaller Na I line. Immediately beneath the spectra are the contribution functions for the three principal carbon- and oxygen-bearing species. The deepest contours, outlined in solid colors, enclose the regions where the contribution function reaches >1% of the total contribution within the atmospheric column at a given wavelength bin. Each successive contour denotes 2 orders of magnitude smaller fractional contribution (here, 10−4).
Paper: Atmospheric Retrieval of L Dwarfs: Benchmarking Results and Characterizing the Young Planetary Mass Companion HD 106906 b in the Near-infrared
Authors: Arthur D. Adams, Michael R. Meyer, Alex R. Howe, Ben Burningham, Sebastian Daemgen, Jonathan Fortney, Mike Line, Mark Marley, Sascha P. Quanz, Kamen Todorov
Figure caption: Single-parameter (1D) and parameter vs. parameter (2D) posterior distributions of cloud parameters from the samples in the cloudy forward model fit to the HD 106906 b data. The cloud opacity is modeled as a power law in wavelength, as described in Section 3.3. The median value and 68% confidence interval of each parameter are shown at the top of each column; the full list of median, interval range, and MLE values is shown in Table 2.
Paper: Atmospheric Retrieval of L Dwarfs: Benchmarking Results and Characterizing the Young Planetary Mass Companion HD 106906 b in the Near-infrared
Authors: Arthur D. Adams, Michael R. Meyer, Alex R. Howe, Ben Burningham, Sebastian Daemgen, Jonathan Fortney, Mike Line, Mark Marley, Sascha P. Quanz, Kamen Todorov
Figure caption: The vertical temperature–pressure profiles of the retrieved forward model fits to the HD 106906 b data. We show the MLE, median, and 95% confidence interval of the retrieved T–P profiles for the cloud-free (blue) and cloudy (red) models, the latter of which is described in Section 3.3. Also plotted is the (cloud-free) SONORA model for a brown dwarf at the gravity and effective temperature of our best-fit cloudy model, with the change from radiative to convective behavior occurring at a few tenths of a bar. Our retrieved profiles, in contrast, vary much less in temperature with pressure down to the expected radiative–convective boundary for an object at this effective temperature.
Paper: Atmospheric Retrieval of L Dwarfs: Benchmarking Results and Characterizing the Young Planetary Mass Companion HD 106906 b in the Near-infrared
Authors: Arthur D. Adams, Michael R. Meyer, Alex R. Howe, Ben Burningham, Sebastian Daemgen, Jonathan Fortney, Mike Line, Mark Marley, Sascha P. Quanz, Kamen Todorov
Figure caption: A selection of parameters of the retrieved forward model fits to the HD 106906 b data, shown as 1D and 2D histograms in a corner plot of the retrieved posterior distributions for selected parameters. The median value and 68% confidence interval of each parameter are shown at the top of each column; the full list of median, interval range, and MLE values is shown in Table 2.
Paper: Atmospheric Retrieval of L Dwarfs: Benchmarking Results and Characterizing the Young Planetary Mass Companion HD 106906 b in the Near-infrared
Authors: Arthur D. Adams, Michael R. Meyer, Alex R. Howe, Ben Burningham, Sebastian Daemgen, Jonathan Fortney, Mike Line, Mark Marley, Sascha P. Quanz, Kamen Todorov
Figure caption: Single-parameter (1D) and parameter vs. parameter (2D) posterior distributions of gas parameters from the samples in the cloudy (red) and cloud-free (blue) forward model fit to the HD 106906 b data. The cloud opacity is modeled as a power law in wavelength, as described in Section 3.3. The median value and 68% confidence interval of each parameter are shown at the top of each column; the full list of median, interval range, and MLE values is shown in Table 2.
Paper: Spectral Retrieval with JWST Photometric data: a Case Study for HIP 65426 b
Authors: Ji Wang, 吉 王
Figure caption: Retrieved P-T profile (1σ region in red shaded region) for HIP 65426 b (assuming 1× solar metallcity and C/O = 0.4) The spectrally-averaged contribution function is shown as the black solid line, which completely overlaps with retrieved cloud layer (black dashed line). The pressure level of the retrieved cloud layer is consistent with that of a physical MgSiO3 cloud (blue dotted line). More results with other assumptions can be found in Table 4.
Paper: Spectral Retrieval with JWST Photometric data: a Case Study for HIP 65426 b
Authors: Ji Wang, 吉 王
Figure caption: Retrieved spectra for HIP 65426 b (assuming 1× solar metallcity and C/O = 0.4). Top three panels are the observed spectroscopic and photometric data (black) and the 1σ (16 to 84 percentile, darker red) and 2σ (2.5–97.5 percentile, lighter red) distribution of modeled spectra. The bottom panel is a residual plot with data minus model and divided by the individual errors. More results with other assumptions can be found in Table 4.
Paper: Spectral Retrieval with JWST Photometric data: a Case Study for HIP 65426 b
Authors: Ji Wang, 吉 王
Figure caption: Retrieved C and O abundances and C/O: C and O abundances from posterior samples are blue histograms, and stellar values are the black dashed lines. Free retrieval by varying all parameters returns nonphysical results (e.g., C/O∼0). More details can be found in Section 4.4.
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: Planets with s > 1.5 light-curve solutions from the 2018 and 2019 KMTNet seasons (black circles) and from data taken prior to 2015 (magenta triangles). Filled symbols are for planets with clear wide-orbit solutions; open symbols are for planets with s < 1 degeneracies. OGLE-2019-BLG-1180Lb is shown as a square in cyan. Events noted in the text are labeled. The dotted black line is at u anom = 0. The dashed black line shows u anom = s − 1/s.
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: CMD of stars around the event, which is constructed from combining OGLE and HST observations. The OGLE and HST CMDs are plotted as gray and green open dots, respectively. The red and blue solid dots indicate the positions of the red clump centroid and source, 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:  χ 2 distributions of the parallax and orbital parameters. Four models with Δχ 2 < 4 are marked as 1, 2, 3, and 4 in the distribution of u 0 > 0; their corresponding parameters are presented in Table 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:  χ 2 distributions of the best-fit parallax+orbital model with the partial data sets. The red, yellow, green, light blue, dark blue, and purple represent regions with Δχ 2 < (1, 4, 9, 16, 25, 36), from the best-fit model, 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: Bayesian probability distributions of the mass, distance, and brightness of the host lens star. The black solid vertical line and the two black dashed lines represent the median value and the 68% confidence intervals of the distribution.
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:  χ 2 distribution for the best-fit PSPL+parallax model (black and gray plots) together with the parallax+orbital model (colored plots). We note that the PSPL+parallax modeling was conducted using the data sets that had the planetary anomaly region ﹩8725\lt \mathrm{HJD}^{\prime} \lt 8755﹩ removed.
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:  χ 2 distributions of the parallax-only model for the partial data sets.
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:  χ 2 distribution for the best-fit xallarap solutions as a function of fixed binary source orbital period P. The red dot denotes the χ 2 of the best-fit parallax model.
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: Cumulative Δχ 2 between the standard and the parallax+orbital models.
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: Variation of the mean of the velocity prior over the Galactic sky at six different distances. The quantity shown is ﹩\sqrt{{v}_{\alpha * }^{2}+{v}_{\delta }^{2}}﹩, where v  α* and v  δ  are the means of the two components of the velocity prior at the specified distance in each HEALpixel. In each distance slice, the color bar covers the full range of velocities plotted, and it is different for each slice.