adsabs/AstroCLIMB huggingface dataset:
Paper: Erratum: “Improved Orbital Constraints and Hα Photometric Monitoring of the Directly Imaged Protoplanet Analog HD 142527 B” (2022, AJ, 164, 1)
Authors: William O. Balmer, Katherine B. Follette, Laird M. Close, Jared R. Males, Robert J. De Rosa, Jéa I. Adams Redai, Alex Watson, Alycia J. Weinberger, Katie M. Morzinski, Julio Morales, Kimberly Ward-Duong, Laurent Pueyo
Figure caption: Replacement for Figure 6 in Balmer et al. (2022). The visible-light contrast of HD 142527 B in two filters with respect to the continuum of HD 142527 A over time. Brown and blue diamonds mark our Hα and continuum contrast measurements, respectively. The gray shaded region represents the 1σ standard deviation of our measurements of continuum contrast, centered on the median. Squares mark the contrasts measured in nearly equivalent filters by Cugno et al. (2019) using VLT/SPHERE/ZIMPOL. The amount of Hα excess can no longer be said to vary convincingly between epochs.
Paper: Erratum: “Improved Orbital Constraints and Hα Photometric Monitoring of the Directly Imaged Protoplanet Analog HD 142527 B” (2022, AJ, 164, 1)
Authors: William O. Balmer, Katherine B. Follette, Laird M. Close, Jared R. Males, Robert J. De Rosa, Jéa I. Adams Redai, Alex Watson, Alycia J. Weinberger, Katie M. Morzinski, Julio Morales, Kimberly Ward-Duong, Laurent Pueyo
Figure caption: Replacement for Figure 15 in Balmer et al. (2022). Posterior distribution of fit (i ⋆, Ω⋆) and randomly sampled (i disk, Ωdisk) orientation angles for the binary orbit and disk components yields a posterior distribution of θs, the mutual inclination angles between the binary orbit and the disk components.
Paper: Stable Coronal X-Ray Emission over 20 yr of XZ Tau
Authors: Steven M. Silverberg, Hans Moritz Günther, Pragati Pradhan, David A. Principe, P. C. Schneider, Scott J. Wolk
Figure caption: XZ Tau AB and its environs; all three panels are on the same spatial scale. Left: 2004 HST/ACS/F625W image of XZ Tau AB. Middle: 2018 Chandra/ACIS observations (ObsID 21948 shown here) do not resolve XZ Tau AB but have a tight PSF with low background. Right: 2020 XMM-Newton observations (ObsID 0865040201 shown here) have more counts but a much wider PSF.
Paper: Stable Coronal X-Ray Emission over 20 yr of XZ Tau
Authors: Steven M. Silverberg, Hans Moritz Günther, Pragati Pradhan, David A. Principe, P. C. Schneider, Scott J. Wolk
Figure caption: Spectrum of one quiescent observation with XMM-Newton (blue), in comparison to the two observations with flares (orange and green). Left: the two flare spectra exhibit enhancement in overall brightness and show the Fe 6.7 keV emission line. Right: a detailed look at the 6–7 keV range shows that the Fe 6.7 keV line exhibited by the flare spectra is underfit by models and that flare spectra show no significant evidence for emission from the fluorescent Fe line at 6.4 keV.
Paper: Stable Coronal X-Ray Emission over 20 yr of XZ Tau
Authors: Steven M. Silverberg, Hans Moritz Günther, Pragati Pradhan, David A. Principe, P. C. Schneider, Scott J. Wolk
Figure caption: Broadband light curves of XZ Tau AB from XMM-Newton (top) and AAVSO (bottom). The top panels depict the individual XMM observations in chronological order, presenting the hard- (>1 keV; black) and soft-energy (<1 keV; red) count rates from the EPIC-PN. The bottom light curve depicts observations of XZ Tau AB from AAVSO, with the XMM-Newton observing windows highlighted in gray. Error bars are smaller than plot symbols. There is no apparent correlation in the X-ray and optical variability.
Paper: Stable Coronal X-Ray Emission over 20 yr of XZ Tau
Authors: Steven M. Silverberg, Hans Moritz Günther, Pragati Pradhan, David A. Principe, P. C. Schneider, Scott J. Wolk
Figure caption:  V-band light curve for XZ Tau AB from the AAVSO and ASAS-SN. The black dashed line represents the estimated baseline level for when XZ Tau B is not in an elevated state. Gray windows highlight times of X-ray observations in 2004, 2017, 2018, and 2020. “Zoomed-in” light curves for individual X-ray observations are shown in Figures 3 and 4.
Paper: Stable Coronal X-Ray Emission over 20 yr of XZ Tau
Authors: Steven M. Silverberg, Hans Moritz Günther, Pragati Pradhan, David A. Principe, P. C. Schneider, Scott J. Wolk
Figure caption: Bottom: zeroth-order observation-averaged net count rates for each Chandra observation of XZ Tau AB in Table 1. Error bars in the time dimension indicate the duration of each observation. Two observations (ObsIDs 20161 and 21951) show enhanced count rates compared to the other nine observations. Top: contemporaneous AAVSO data show some rolling variability with no obvious correlation to the Chandra variability.
Paper: Stable Coronal X-Ray Emission over 20 yr of XZ Tau
Authors: Steven M. Silverberg, Hans Moritz Günther, Pragati Pradhan, David A. Principe, P. C. Schneider, Scott J. Wolk
Figure caption: Chandra/HETG data for XZ Tau AB, combining both the MEG and HEG. Prominent lines in the spectrum are labeled. We exclude the spectrum at wavelengths longer than 15 Å, as there is minimal emission at these wavelengths owing to the contamination of the ACIS-S chip.
Paper: Revisiting the Transit Timing and Atmosphere Characterization of the Neptune-mass Planet HAT-P-26 b
Authors: Napaporn A-thano, Supachai Awiphan, Ing-Guey Jiang, Eamonn Kerins, Akshay Priyadarshi, Iain McDonald, Yogesh C. Joshi, Thansuda Chulikorn, Joshua J. C. Hayes, Stephen Charles, Chung-Kai Huang, Ronnakrit Rattanamala, Li-Chin Yeh, Vik S Dhillon
Figure caption: (a) GLS periodogram of timing residuals of all 39 midtransit times, showing three peaks with FAP < 3 × 10−13%. The dashed lines indicate the FAP levels. (b) O − C diagram and the best-fit sinusoid for the detected frequencies f 1 (top), f 2 (middle), and f 3 (bottom; purple dashed line). Notes: a: the midtransit times (T  m ) are adopted from the transit light curve observed by HATNet field 376 (Hartman et al. 2011); b: T  m  adopted from Stevenson et al. (2016); and c: T  m  adopted from the transit light curves observed by HST/STIS (Wakeford et al. 2017).
Paper: Revisiting the Transit Timing and Atmosphere Characterization of the Neptune-mass Planet HAT-P-26 b
Authors: Napaporn A-thano, Supachai Awiphan, Ing-Guey Jiang, Eamonn Kerins, Akshay Priyadarshi, Iain McDonald, Yogesh C. Joshi, Thansuda Chulikorn, Joshua J. C. Hayes, Stephen Charles, Chung-Kai Huang, Ronnakrit Rattanamala, Li-Chin Yeh, Vik S Dhillon
Figure caption: (a) GLS periodogram for the timing residuals of the 33 midtransit times obtained from TransitFit. The dashed lines indicate the FAP levels. (b) O − C diagram and the best fit of the sinusoidal variability from the frequency of the highest-power peak, where FAP = 1 × 10−7% (purple dashed line).
Paper: Revisiting the Transit Timing and Atmosphere Characterization of the Neptune-mass Planet HAT-P-26 b
Authors: Napaporn A-thano, Supachai Awiphan, Ing-Guey Jiang, Eamonn Kerins, Akshay Priyadarshi, Iain McDonald, Yogesh C. Joshi, Thansuda Chulikorn, Joshua J. C. Hayes, Stephen Charles, Chung-Kai Huang, Ronnakrit Rattanamala, Li-Chin Yeh, Vik S Dhillon
Figure caption: Top panel: the best-fit transmission spectrum of HAT-P-26 b, calculated using ground-based, TESS, and the HST/WFC3 data from TransitFit, with synthetic models generated by TauREx 3 (blue solid line), with their 1σ errors (blue bands). The blue squares are the binned best-fit transmission spectra. The gray stars are the transmission spectra obtained by Wakeford et al. (2017). The observed data are binned using the bandpass in the bottom panel.
Paper: Revisiting the Transit Timing and Atmosphere Characterization of the Neptune-mass Planet HAT-P-26 b
Authors: Napaporn A-thano, Supachai Awiphan, Ing-Guey Jiang, Eamonn Kerins, Akshay Priyadarshi, Iain McDonald, Yogesh C. Joshi, Thansuda Chulikorn, Joshua J. C. Hayes, Stephen Charles, Chung-Kai Huang, Ronnakrit Rattanamala, Li-Chin Yeh, Vik S Dhillon
Figure caption: The LDCs were calculated from TransitFit, PyLDTk, and ExoCTK. The colors of the bandpass filters are the same as those in Figures 5 and 6.
Paper: Revisiting the Transit Timing and Atmosphere Characterization of the Neptune-mass Planet HAT-P-26 b
Authors: Napaporn A-thano, Supachai Awiphan, Ing-Guey Jiang, Eamonn Kerins, Akshay Priyadarshi, Iain McDonald, Yogesh C. Joshi, Thansuda Chulikorn, Joshua J. C. Hayes, Stephen Charles, Chung-Kai Huang, Ronnakrit Rattanamala, Li-Chin Yeh, Vik S Dhillon
Figure caption: The planetary radii calculated from both models with fitted LDCs and fixed LDCs. The colors of the bandpass filters are the same as those in Figures 5 and 6.
Paper: Revisiting the Transit Timing and Atmosphere Characterization of the Neptune-mass Planet HAT-P-26 b
Authors: Napaporn A-thano, Supachai Awiphan, Ing-Guey Jiang, Eamonn Kerins, Akshay Priyadarshi, Iain McDonald, Yogesh C. Joshi, Thansuda Chulikorn, Joshua J. C. Hayes, Stephen Charles, Chung-Kai Huang, Ronnakrit Rattanamala, Li-Chin Yeh, Vik S Dhillon
Figure caption: Top panel: the best-fit transmission spectrum of HAT-P-26 b, based on fitting only the HST/WFC3 data from TransitFit with synthetic models generated by TauREx 3 (blue solid line), with their 1σ errors (blue bands). The blue squares are the binned best-fit transmission spectra. The data are binned using the bandpass in the bottom panel.
Paper: Revisiting the Transit Timing and Atmosphere Characterization of the Neptune-mass Planet HAT-P-26 b
Authors: Napaporn A-thano, Supachai Awiphan, Ing-Guey Jiang, Eamonn Kerins, Akshay Priyadarshi, Iain McDonald, Yogesh C. Joshi, Thansuda Chulikorn, Joshua J. C. Hayes, Stephen Charles, Chung-Kai Huang, Ronnakrit Rattanamala, Li-Chin Yeh, Vik S Dhillon
Figure caption: Posterior probability distribution for our HAT-P-26 b atmospheric model, using nested sampling and the TauREx 3 package.
Paper: Revisiting the Transit Timing and Atmosphere Characterization of the Neptune-mass Planet HAT-P-26 b
Authors: Napaporn A-thano, Supachai Awiphan, Ing-Guey Jiang, Eamonn Kerins, Akshay Priyadarshi, Iain McDonald, Yogesh C. Joshi, Thansuda Chulikorn, Joshua J. C. Hayes, Stephen Charles, Chung-Kai Huang, Ronnakrit Rattanamala, Li-Chin Yeh, Vik S Dhillon
Figure caption: Posterior probability distribution for our HAT-P-26 b atmospheric model, calculated using only the HST/WFC3 data, via nested sampling with TauREx 3.
Paper: Grid-based Atmospheric Retrievals for Reflected-light Spectra of Exoplanets Using PSGnest
Authors: Nicholas Susemiehl, Avi M. Mandell, Geronimo L. Villanueva, Giuliano Liuzzi, Michael Moore, Tyler Baines, Michael D. Himes, Adam J. R. W. Smith
Figure caption: Results of the bandpass study for the fiducial case. The gray regions represent the upper and lower limits of the 68% credible region, and the red line shows the (median) retrieved values, with circles at each bandpass center. The true value for each parameter is shown as a horizontal dashed black line. Regions where the gray region narrows indicate the increased certainty of the Bayesian retrieval algorithm. Colored points along the red line indicate the strength of a detection of the particular parameter at each bandpass center. Red points indicate a weak detection (﹩\mathrm{ln}B\lt 2.5﹩), purple points indicate a moderate detection (﹩2.5\leqslant \mathrm{ln}B\lt 5﹩), and blue points indicate a strong detection (﹩\mathrm{ln}B\gt 5﹩). Black points, present for each nongaseous parameter, represent the nonapplicability of Bayes factors to these parameters. Gray vertical lines mark the minimum bandpass centers for each planet where the most parameters can be constrained.
Paper: Grid-based Atmospheric Retrievals for Reflected-light Spectra of Exoplanets Using PSGnest
Authors: Nicholas Susemiehl, Avi M. Mandell, Geronimo L. Villanueva, Giuliano Liuzzi, Michael Moore, Tyler Baines, Michael D. Himes, Adam J. R. W. Smith
Figure caption: Spectra associated with retrievals in the high-O3, low-P 0, high-A  s  space. “Left,” “Middle,” and “Right” refer to the three darkest points in the 2D posterior of the left panel of Figure 9. The true spectrum corresponds to the blue vertical lines in that figure, while the retrieved spectrum corresponds to the orange ones. The bottom panel plots the difference between the true spectrum and each other spectrum. Despite differences in parameter values, all spectra are nearly identical.
Paper: Grid-based Atmospheric Retrievals for Reflected-light Spectra of Exoplanets Using PSGnest
Authors: Nicholas Susemiehl, Avi M. Mandell, Geronimo L. Villanueva, Giuliano Liuzzi, Michael Moore, Tyler Baines, Michael D. Himes, Adam J. R. W. Smith
Figure caption: Results of the bandpass study for the case with R = 90 and S/N = 12.5. Aspects of this plot are explained in the caption below Figure 11.
Paper: Grid-based Atmospheric Retrievals for Reflected-light Spectra of Exoplanets Using PSGnest
Authors: Nicholas Susemiehl, Avi M. Mandell, Geronimo L. Villanueva, Giuliano Liuzzi, Michael Moore, Tyler Baines, Michael D. Himes, Adam J. R. W. Smith
Figure caption: Posteriors of the bandpass study comparing the fiducial to the 20% bandwidth case. The marginalized posteriors for H2O, O3, O2, and P 0 are shown in blue for the fiducial (R = 140, S/N = 10, BW = 0.1) case and in orange for the 20% bandwidth case. Blue and orange vertical lines show the median values of these retrieval results, while a dashed black line shows the true value.
Paper: Grid-based Atmospheric Retrievals for Reflected-light Spectra of Exoplanets Using PSGnest
Authors: Nicholas Susemiehl, Avi M. Mandell, Geronimo L. Villanueva, Giuliano Liuzzi, Michael Moore, Tyler Baines, Michael D. Himes, Adam J. R. W. Smith
Figure caption: Posteriors of the bandpass studying comparing the fiducial to the R = 90 and S/N = 12.5 case. The marginalized posteriors for H2O, O3, O2, and P 0 are shown in blue for the fiducial (R = 140, S/N = 10, BW = 0.1) case and in green for the 20% bandwidth case. Blue and green vertical lines show the median values of these retrieval results, while a dashed black line shows the true value.
Paper: Grid-based Atmospheric Retrievals for Reflected-light Spectra of Exoplanets Using PSGnest
Authors: Nicholas Susemiehl, Avi M. Mandell, Geronimo L. Villanueva, Giuliano Liuzzi, Michael Moore, Tyler Baines, Michael D. Himes, Adam J. R. W. Smith
Figure caption: Posteriors of the bandpass study comparing the fiducial to the S/N = 20 case. The marginalized posteriors for H2O, O3, O2, and P 0 are shown in blue for the fiducial (R = 140, S/N = 10, BW = 0.1) case and in red for the 20% bandwidth case. Blue and red vertical lines show the median values of these retrieval results, while a dashed black line shows the true value.
Paper: Grid-based Atmospheric Retrievals for Reflected-light Spectra of Exoplanets Using PSGnest
Authors: Nicholas Susemiehl, Avi M. Mandell, Geronimo L. Villanueva, Giuliano Liuzzi, Michael Moore, Tyler Baines, Michael D. Himes, Adam J. R. W. Smith
Figure caption: Results of the bandpass study for the case with 20% bandwidth. Aspects of this plot are explained in the caption below Figure 11.
Paper: Grid-based Atmospheric Retrievals for Reflected-light Spectra of Exoplanets Using PSGnest
Authors: Nicholas Susemiehl, Avi M. Mandell, Geronimo L. Villanueva, Giuliano Liuzzi, Michael Moore, Tyler Baines, Michael D. Himes, Adam J. R. W. Smith
Figure caption: Results of the bandpass study for the case with S/N = 20. Aspects of this plot are explained in the caption below Figure 11.
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 KMT-2016-BLG-1855 with the best-fit (A) and degenerate (﹩{{\rm{A}}}^{{\prime} }﹩, B, and ﹩{{\rm{B}}}^{{\prime} }﹩) models.
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 KMT-2016-BLG-1855 with degenerate models C, ﹩{{\rm{C}}}^{{\prime} }﹩, D, and E.
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 KMT-2016-BLG-1855 with the best-fit model.
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: Caustic geometry of each solution of KMT-2016-BLG-1751. The color of the caustic is identical to the color of the light curve shown in Figure 10.
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: The s–q parameter space of KMT-2016-BLG-1751 showing possible solutions.
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: The ﹩{\mathrm{log}}_{10}(P)﹩ and χ 2 plots of the xallarap models of OGLE-2016-BLG-1850. The crosses indicate the χ 2 of the APRX models.
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: The CMDs of the five planetary events.