adsabs/AstroCLIMB huggingface dataset:
Paper: A Pioneering Experiment Combining Single-antenna and Aperture-synthesis Data to Measure Faraday Rotation with GMIMS and the CGPS
Authors: Anna Ordog, Jo-Anne C. Brown, T. L. Landecker, Alex S. Hill, Roland Kothes, Jennifer L. West, John M. Dickey, Marijke Haverkorn, Ettore Carretti, Alec J. M. Thomson, Andrea Bracco, D. A. Del Rizzo, Ryan R. Ransom, Robert I. Reid
Figure caption: The steps in feathering GMIMS-HBN and DRAO ST visibilities in order to combine the data sets. This example shows Stokes U for band B of field OB12. (a) The deconvolved, low-pass-filtered GMIMS-HBN map tapered to match the primary beam of the DRAO ST; (b) the original DRAO ST field; (c) GMIMS-HBN transformed to the uv-plane; (d) DRAO ST transformed to the uv-plane; (e) the GMIMS-HBN visibilities feathered to discard high spatial frequencies; (f) the DRAO ST visibilities feathered to discard low spatial frequencies; (g, h) the GMIMS-HBN and DRAO ST, respectively, transformed back to the image plane, ready to be added together.
Paper: A Pioneering Experiment Combining Single-antenna and Aperture-synthesis Data to Measure Faraday Rotation with GMIMS and the CGPS
Authors: Anna Ordog, Jo-Anne C. Brown, T. L. Landecker, Alex S. Hill, Roland Kothes, Jennifer L. West, John M. Dickey, Marijke Haverkorn, Ettore Carretti, Alec J. M. Thomson, Andrea Bracco, D. A. Del Rizzo, Ryan R. Ransom, Robert I. Reid
Figure caption: Sample linear fit RM values for three lines of sight, comparing the single-antenna-only data (GMIMS-HBN; purple, denoted “HBN”), aperture-synthesis-only data (DRAO ST; blue, denoted “ST”), and the combined full-scale data (red, denoted “full”). The bottom panels show the full-band GMIMS-HBN along with the linear fit to GMIMS-HBN for the four-channel 35 MHz bandwidth of the DRAO ST (indicated by the shaded gray λ2 range). The three lines of sight shown here (panels (a)–(c)) are indicated by crosses in Figures 16, 18, and 20.
Paper: A Pioneering Experiment Combining Single-antenna and Aperture-synthesis Data to Measure Faraday Rotation with GMIMS and the CGPS
Authors: Anna Ordog, Jo-Anne C. Brown, T. L. Landecker, Alex S. Hill, Roland Kothes, Jennifer L. West, John M. Dickey, Marijke Haverkorn, Ettore Carretti, Alec J. M. Thomson, Andrea Bracco, D. A. Del Rizzo, Ryan R. Ransom, Robert I. Reid
Figure caption: Combined full-scale RM and PI maps for 174° < ℓ < 194°, as in Figure 7. This region covers the high-longitude end of the previously unpublished CGPS Phase 3 data. The 1°-wide strip at ℓ = 180° is masked owing to a discontinuity in the GMIMS-HBN data at this longitude producing artifacts in the Fourier transform steps described in Section 3.2.
Paper: A Pioneering Experiment Combining Single-antenna and Aperture-synthesis Data to Measure Faraday Rotation with GMIMS and the CGPS
Authors: Anna Ordog, Jo-Anne C. Brown, T. L. Landecker, Alex S. Hill, Roland Kothes, Jennifer L. West, John M. Dickey, Marijke Haverkorn, Ettore Carretti, Alec J. M. Thomson, Andrea Bracco, D. A. Del Rizzo, Ryan R. Ransom, Robert I. Reid
Figure caption: The GMIMS-HBN, DRAO ST, and full-scale data in the Sh2-216 PN region. (a–c) PI calculated as ﹩\mathrm{PI}=\sqrt{{\langle Q\rangle }^{2}+{\langle U\rangle }^{2}}﹩. (d–f) RM for pixels with PI > 0.1 K. Left column: GMIMS-HBN single-antenna-only data. Middle column: DRAO ST aperture-synthesis-only data. Right column: combined full-scale data. Black circles in the lower left corners indicate the beam size (﹩4{0}^{{\prime} }﹩ for the single-antenna, ﹩\sim {3}^{{\prime} }﹩ for the aperture-synthesis and full-scale maps). The yellow cross indicates the LOS shown in Figure 15(a). Black contours indicate PI = 0.3 K on the full-scale map (panel (c)) and are shown in all panels for ease of comparison. The yellow dashed circle corresponds to the disk of the PN as determined in R08.
Paper: A Pioneering Experiment Combining Single-antenna and Aperture-synthesis Data to Measure Faraday Rotation with GMIMS and the CGPS
Authors: Anna Ordog, Jo-Anne C. Brown, T. L. Landecker, Alex S. Hill, Roland Kothes, Jennifer L. West, John M. Dickey, Marijke Haverkorn, Ettore Carretti, Alec J. M. Thomson, Andrea Bracco, D. A. Del Rizzo, Ryan R. Ransom, Robert I. Reid
Figure caption: Stokes Q (left) and Stokes U (right) power spectra for the GMIMS-HBN single-antenna (purple squares), the DRAO ST (blue circles), and the combined data (red diamonds). Rows (a)–(g) correspond to the regions shown in Figures 7–13, with the Cygnus X longitudes excluded from Figure 7. The light-gray regions indicate baselines between 100 and 200 m, where the DRAO ST data convolved to ﹩{3}^{{\prime} }﹩ start to decline in sensitivity, dropping to 20% at ∼200 m (∼600 m at the native ﹩{1}^{{\prime} }﹩ resolution; T. L. Landecker et al. 2000). The dark-gray regions indicate baselines at which the convolved DRAO ST is no longer reliable. The dashed lines correspond to a power law with slope −1 (not a fitted line; intended only to facilitate comparison between the regions). Vertical dotted lines indicate the overlap region for the uv-domain feathering of the single-antenna and interferometric data sets.
Paper: A Pioneering Experiment Combining Single-antenna and Aperture-synthesis Data to Measure Faraday Rotation with GMIMS and the CGPS
Authors: Anna Ordog, Jo-Anne C. Brown, T. L. Landecker, Alex S. Hill, Roland Kothes, Jennifer L. West, John M. Dickey, Marijke Haverkorn, Ettore Carretti, Alec J. M. Thomson, Andrea Bracco, D. A. Del Rizzo, Ryan R. Ransom, Robert I. Reid
Figure caption: The GMIMS-HBN, DRAO ST, and full-scale data in the ℓ = 173° H II complex. Panels are the same as in Figure 16. The yellow cross indicates the LOS shown in Figure 15(c). Black contours indicate PI = 0.2 K on the full-scale map (panel (c)).
Paper: A Pioneering Experiment Combining Single-antenna and Aperture-synthesis Data to Measure Faraday Rotation with GMIMS and the CGPS
Authors: Anna Ordog, Jo-Anne C. Brown, T. L. Landecker, Alex S. Hill, Roland Kothes, Jennifer L. West, John M. Dickey, Marijke Haverkorn, Ettore Carretti, Alec J. M. Thomson, Andrea Bracco, D. A. Del Rizzo, Ryan R. Ransom, Robert I. Reid
Figure caption: The northeastern arc of Sh2-216 showing the “polarization knots” studied by R08 and approximately matching the region shown in their Figure 3. As in Figure 16, the top row shows PI and the bottom row shows RMs, for DRAO ST data (panels (a) and (c)) and the combined data set (panels (b) and (d)). The white dashed arc corresponds to the disk of the PN as determined in R08 (also shown as a yellow circle in Figure 16). Note that the resolution is degraded to ﹩{3}^{{\prime} }﹩ compared to the ﹩{1}^{{\prime} }﹩ CGPS resolution in R08.
Paper: A Pioneering Experiment Combining Single-antenna and Aperture-synthesis Data to Measure Faraday Rotation with GMIMS and the CGPS
Authors: Anna Ordog, Jo-Anne C. Brown, T. L. Landecker, Alex S. Hill, Roland Kothes, Jennifer L. West, John M. Dickey, Marijke Haverkorn, Ettore Carretti, Alec J. M. Thomson, Andrea Bracco, D. A. Del Rizzo, Ryan R. Ransom, Robert I. Reid
Figure caption: Combined full-scale RM and PI maps for 156° < ℓ < 176°, as in Figure 7. These maps include the region in the bottom panel of Figure 7 in L10, as well as previously unpublished CGPS Phase 3 data.
Paper: A Pioneering Experiment Combining Single-antenna and Aperture-synthesis Data to Measure Faraday Rotation with GMIMS and the CGPS
Authors: Anna Ordog, Jo-Anne C. Brown, T. L. Landecker, Alex S. Hill, Roland Kothes, Jennifer L. West, John M. Dickey, Marijke Haverkorn, Ettore Carretti, Alec J. M. Thomson, Andrea Bracco, D. A. Del Rizzo, Ryan R. Ransom, Robert I. Reid
Figure caption: The GMIMS-HBN, DRAO ST, and full-scale data in the IC 443 SNR region. Panels are the same as in Figure 16. The yellow cross indicates the LOS shown in Figure 15(b). Black contours indicate PI = 0.25 K on the full-scale map (panel (c)).
Paper: A Pioneering Experiment Combining Single-antenna and Aperture-synthesis Data to Measure Faraday Rotation with GMIMS and the CGPS
Authors: Anna Ordog, Jo-Anne C. Brown, T. L. Landecker, Alex S. Hill, Roland Kothes, Jennifer L. West, John M. Dickey, Marijke Haverkorn, Ettore Carretti, Alec J. M. Thomson, Andrea Bracco, D. A. Del Rizzo, Ryan R. Ransom, Robert I. Reid
Figure caption: CGPS Stokes I in the IC 443 SNR region. Black contours indicate PI = 0.25 K on the full-scale map.
Paper: The Thermal Emission Spectrum of the Nearby Rocky Exoplanet LTT 1445A b from JWST MIRI/LRS
Authors: Patcharapol Wachiraphan, Zachory K. Berta-Thompson, Hannah Diamond-Lowe, Jennifer G. Winters, Catriona Murray, Michael Zhang, Qiao Xue, Caroline V. Morley, Marialis Rosario-Franco, Girish M. Duvvuri
Figure caption: Emission spectra in terms of measured secondary eclipse depth (ppm), at different spectral resolutions of 1, 5, 10, and 20 wavelength bins (rows), for the three individual visits and an inverse-variance weighted average (columns). Each data point shows eclipse depth with 1σ error bar on the y-axis and the width of the wavelength bin on the x-axis; depth uncertainties in the combined spectrum have been inflated to bring the three visits into consistency with each other. Each gray line indicates the planet isothermal model as described in Equation (6) with uncertainty (gray shaded region) discussed in Equation (8). The dark rock, thick atmosphere, and Venus-like (brown) lines are Planck planet models calculated at 549 K (0 albedo and instant reradiation; f = 2/3), 430 K (0 albedo and perfect heat redistribution; f = 1/4), and 297 K (0.77 albedo and perfect heat redistribution; f = 1/4), respectively. The binned model depths are shown as brown dots along each line model.
Paper: The Thermal Emission Spectrum of the Nearby Rocky Exoplanet LTT 1445A b from JWST MIRI/LRS
Authors: Patcharapol Wachiraphan, Zachory K. Berta-Thompson, Hannah Diamond-Lowe, Jennifer G. Winters, Catriona Murray, Michael Zhang, Qiao Xue, Caroline V. Morley, Marialis Rosario-Franco, Girish M. Duvvuri
Figure caption: The average emission spectrum of LTT 1445A b compared to models with and without atmospheres. Left panel: forward models are shown for 100% CO2, αB = 0.1 atmospheres with at different surface pressures (ps). Right panel: Planck thermal spectra are shown at 0 K (no eclipse), 297 K (αB = 0.77, f-factor = 1/4), 431 K (αB = 0, f-factor = 1/4), 549 K (αB = 0, f-factor = 2/3), and best-fit dayside temperature (525 K; blue line). The displayed χ2 (i) incorporates model uncertainty from the uncertain system parameters, (ii) is for 16 degrees of freedom (dof), and (iii) is translated into a probability with which each model can be disfavored, expressed as a number of σ in a Gaussian distribution.
Paper: The Thermal Emission Spectrum of the Nearby Rocky Exoplanet LTT 1445A b from JWST MIRI/LRS
Authors: Patcharapol Wachiraphan, Zachory K. Berta-Thompson, Hannah Diamond-Lowe, Jennifer G. Winters, Catriona Murray, Michael Zhang, Qiao Xue, Caroline V. Morley, Marialis Rosario-Franco, Girish M. Duvvuri
Figure caption: LTT 1445A b in the context of other worlds with and without atmospheres, considering both instantaneous bolometric instellation (top) and a crudely estimated proxy for time-integrated high-energy received (bottom). Two relevant boundaries are shown, each normalized to Mars: an empirical ﹩I\propto {v}_{escape}^{4}﹩ “cosmic shoreline” proposed by K. J. Zahnle & D. C. Catling (2017) and a simpler vthermal ∝ vescape energy-balance shoreline.
Paper: The Thermal Emission Spectrum of the Nearby Rocky Exoplanet LTT 1445A b from JWST MIRI/LRS
Authors: Patcharapol Wachiraphan, Zachory K. Berta-Thompson, Hannah Diamond-Lowe, Jennifer G. Winters, Catriona Murray, Michael Zhang, Qiao Xue, Caroline V. Morley, Marialis Rosario-Franco, Girish M. Duvvuri
Figure caption: A map of expected dayside temperature ratio (﹩R={T}_{{\rm{day}}}/{T}_{{\rm{\max }}}﹩) as a function of Bond albedo and surface pressure, according to the D. D. B. Koll (2022) analytic estimates. Contours indicate LTT 1445A b’s temperature ratio of R = 0.952 ± 0.057 measured from the 16-bin emission spectrum, showing the central value (solid line), 1σ range (dotted line), and 3σ range (dashed line), accounting for both measurement uncertainties in the emission spectrum and underlying uncertainties in the system parameters. Several solar system planetary bodies are shown for reference.
Paper: The Thermal Emission Spectrum of the Nearby Rocky Exoplanet LTT 1445A b from JWST MIRI/LRS
Authors: Patcharapol Wachiraphan, Zachory K. Berta-Thompson, Hannah Diamond-Lowe, Jennifer G. Winters, Catriona Murray, Michael Zhang, Qiao Xue, Caroline V. Morley, Marialis Rosario-Franco, Girish M. Duvvuri
Figure caption: Analytical dayside temperature estimates as a function of surface pressure and Bond albedo (αB) from D. D. B. Koll (2022; gray dashed lines in left panel) with observed dayside temperature posteriors from different binning strategies (right panel). Horizontal lines indicate 3σ temperature limits from the observations. The uncertainties shown here do not account for uncertainties in the system’s parameters.
Paper: The Thermal Emission Spectrum of the Nearby Rocky Exoplanet LTT 1445A b from JWST MIRI/LRS
Authors: Patcharapol Wachiraphan, Zachory K. Berta-Thompson, Hannah Diamond-Lowe, Jennifer G. Winters, Catriona Murray, Michael Zhang, Qiao Xue, Caroline V. Morley, Marialis Rosario-Franco, Girish M. Duvvuri
Figure caption: The flux contrast between LTT 1445A’s SPHINX model (solid blue line) and planet b’s Planck thermal emission model at the best-fit temperature (525 K). The y-axis expresses the flux received at the telescope, given LTT 1445A’s distance.
Paper: The Thermal Emission Spectrum of the Nearby Rocky Exoplanet LTT 1445A b from JWST MIRI/LRS
Authors: Patcharapol Wachiraphan, Zachory K. Berta-Thompson, Hannah Diamond-Lowe, Jennifer G. Winters, Catriona Murray, Michael Zhang, Qiao Xue, Caroline V. Morley, Marialis Rosario-Franco, Girish M. Duvvuri
Figure caption: Emission spectra comparison in terms of measured secondary eclipse depth (ppm). We constructed this plot in the same fashion as Figure 8. The gray error bars indicate eclipse depths from Eureka! pipeline and were offset in by −0.1 μm on the x-axis for better visualization, while colored error bars showed eclipse depths from SPARTA pipeline.
Paper: The Herbig–Haro Outflow Content and Star-forming Environment of Circinus West and East
Authors: T. A. Rector, L. Prato, R. Kerr, E. Papraniku, K. Fisk
Figure caption: The fields of view for the Cir-E (left) and Cir-W (right) DECam pointings. The two fields slightly overlap. The field of view of the Swope 1 m observations from T. A. Rector et al. (2020) is shown in the Cir-W image for comparison. Note that each image is composited slightly differently to maximize sensitivity to faint outflows within the dynamic range of the nebulosity– the color differences between the two images therefore are not meaningful.
Paper: The Herbig–Haro Outflow Content and Star-forming Environment of Circinus West and East
Authors: T. A. Rector, L. Prato, R. Kerr, E. Papraniku, K. Fisk
Figure caption: Cutouts of newly detected components of the HH 76 outflow. Each cutout is 200 pixels (52″) on side. Color-composite images were made with the g (cyan), i (yellow), and N662 Hα (red) filters so that the Hα emission from the HH objects is distinctly red. The grayscale images are from follow-up N673 [S II] observations. HH objects are therefore deep red in the color images and are also detected in [S II].
Paper: The Herbig–Haro Outflow Content and Star-forming Environment of Circinus West and East
Authors: T. A. Rector, L. Prato, R. Kerr, E. Papraniku, K. Fisk
Figure caption: This region of Cir-W, shown here in Hα, contains all of the known HH objects in this nebula except for HH 1259, which lies at the southeastern tip of the cloud. Red circles show the locations of previously known HH objects; and green circles show new ones reported in this paper. The size of each circle roughly reflects the size of the HH object. North is up, east is left.
Paper: The Herbig–Haro Outflow Content and Star-forming Environment of Circinus West and East
Authors: T. A. Rector, L. Prato, R. Kerr, E. Papraniku, K. Fisk
Figure caption: Cutouts of new HH objects within Cir-W. HH 1244 is just east of the HH 76 outflow (seen just below the blue charge bleed in the color image above). And HH 1245 is west of the HH 1246-1249 group. Cutout size and color schemes are the same as for Figure 3.
Paper: The Herbig–Haro Outflow Content and Star-forming Environment of Circinus West and East
Authors: T. A. Rector, L. Prato, R. Kerr, E. Papraniku, K. Fisk
Figure caption: Cutouts of newly discovered HH objects within Cir-W, to the west of the HH 76 outflow. Cutout size and color schemes are the same as for Figure 3.
Paper: The Herbig–Haro Outflow Content and Star-forming Environment of Circinus West and East
Authors: T. A. Rector, L. Prato, R. Kerr, E. Papraniku, K. Fisk
Figure caption: Cutouts of six new HH objects in the highly obscured area south of the Cir-MMS complex. Cutout size and color schemes are the same as for Figure 3.
Paper: The Herbig–Haro Outflow Content and Star-forming Environment of Circinus West and East
Authors: T. A. Rector, L. Prato, R. Kerr, E. Papraniku, K. Fisk
Figure caption: Motions of Circinus members with PAge < 50 Myr > 0.95 in R. Kerr et al. (2025), overlaid on the Hα DECam frames. Velocities are shown relative to ASCC 79, the central cluster in the Circinus Complex, and corrected for virtual expansion. The left panel shows Cir-E, and the right panel shows Cir-W. We split up the membership of Cir-E according to its two components defined in (R. Kerr et al. 2025), which correspond roughly to the Cir-Ea (south) and Cir-Eb (north) subcomponents from T. Shimoikura & K. Dobashi (2011).
Paper: The Herbig–Haro Outflow Content and Star-forming Environment of Circinus West and East
Authors: T. A. Rector, L. Prato, R. Kerr, E. Papraniku, K. Fisk
Figure caption: In the left panel, a sky-plane map of the Circinus Complex subgroups defined by R. Kerr et al. (2025), colored by their ages and with subgroup IDs annotated in black. Subgroups 3 and 4 contain the populations associated with the Cir-W and Cir-E clouds, respectively. In the right panel, the mean stellar velocities by on-sky bin relative to the velocity of ASCC 79 with the locations of notable structures labeled, as previously presented in Figure 9 of R. Kerr et al. (2025).
Paper: The Herbig–Haro Outflow Content and Star-forming Environment of Circinus West and East
Authors: T. A. Rector, L. Prato, R. Kerr, E. Papraniku, K. Fisk
Figure caption: Cutouts of the field around HH 1260b (lower-left) and HH 1260a (upper-right) within Cir-E. WISEA J151319.86-623522.3 is located in the cloud between them. Each cutout is 400 pixels (104″) on a side. Color schemes are the same as for Figure 3.
Paper: The Herbig–Haro Outflow Content and Star-forming Environment of Circinus West and East
Authors: T. A. Rector, L. Prato, R. Kerr, E. Papraniku, K. Fisk
Figure caption: Cutouts of the field around HH 1261 (center-top) and HH 1262 (center-bottom) within Cir-E. HH 1261a is only faintly detected in [S II]. Cutout size and color schemes are the same as for Figure 10.
Paper: The Herbig–Haro Outflow Content and Star-forming Environment of Circinus West and East
Authors: T. A. Rector, L. Prato, R. Kerr, E. Papraniku, K. Fisk
Figure caption: Cutouts of the field around HH 1263a (center-top) and HH 1263b (center-bottom) within Cir-E. A faint stream with one or more knots appears to connect the two. Cutout size and color schemes are the same as for Figure 10.
Paper: The Herbig–Haro Outflow Content and Star-forming Environment of Circinus West and East
Authors: T. A. Rector, L. Prato, R. Kerr, E. Papraniku, K. Fisk
Figure caption: Cutouts of four new HH objects in the southeastern region of Cir-W. Cutout size and color schemes are the same as for Figure 3.
Paper: The Herbig–Haro Outflow Content and Star-forming Environment of Circinus West and East
Authors: T. A. Rector, L. Prato, R. Kerr, E. Papraniku, K. Fisk
Figure caption: Cutouts of seven new HH objects in the VdBH 65b region. Cutout size and color schemes are the same as for Figure 3.
Paper: The Herbig–Haro Outflow Content and Star-forming Environment of Circinus West and East
Authors: T. A. Rector, L. Prato, R. Kerr, E. Papraniku, K. Fisk
Figure caption: Cutouts of five new HH objects between the VdBH 65b and Cir-MMS regions. Cutout size and color schemes are the same as for Figure 3.
Paper: The Herbig–Haro Outflow Content and Star-forming Environment of Circinus West and East
Authors: T. A. Rector, L. Prato, R. Kerr, E. Papraniku, K. Fisk
Figure caption: Cutouts of new HH components in Cir-E. Each cutout is 200 pixels (52″) on side. Cutout size and color schemes are the same as for Figure 3.
Paper: Systematic Reanalysis of KMTNet Microlensing Events. II. Two New Planets in Giant-source Events
Authors: Hongjing Yang, 弘靖 杨, Jennifer C. Yee, Jiyuan Zhang, 纪元 张, Chung-Uk Lee, Dong-Jin Kim, Ian A. Bond, Andrzej Udalski, Kyu-Ha Hwang, Weicheng Zang, 伟呈 臧, Qiyue Qian, 奇玥 钱, Andrew Gould, Shude Mao, 淑德 毛, Michael D. Albrow, Sun-Ju Chung, Cheongho Han, Youn Kil Jung, Yoon-Hyun Ryu, In-Gu Shin, Yossi Shvartzvald, Sang-Mok Cha, Hyoun-Woo Kim, Seung-Lee Kim, Dong-Joo Lee, Yongseok Lee, Byeong-Gon Park, Richard W. Pogge, Fumio Abe, Ken Bando, David P. Bennett, Aparna Bhattacharya, Akihiko Fukui, Ryusei Hamada, Shunya Hamada, Naoto Hamasaki, Yuki Hirao, Stela Ishitani Silva, Yoshitaka Itow, Naoki Koshimoto, Yutaka Matsubara, Shota Miyazaki, Yasushi Muraki, Tutumi Nagai, Kansuke Nunota, Greg Olmschenk, Clément Ranc, Nicholas J. Rattenbury, Yuki Satoh, Takahiro Sumi, Daisuke Suzuki, Sean K. Terry, Paul . J. Tristram, Aikaterini Vandorou, Hibiki Yama, Przemek Mróz, Jan Skowron, Radoslaw Poleski, Michał K. Szymański, Igor Soszyński, Paweł Pietrukowicz, Szymon Kozłowski, Krzysztof Ulaczyk, Krzysztof A. Rybicki, Patryk Iwanek, Marcin Wrona
Figure caption: Left panels: the light curve, models, and residuals of KMT-2021-BLG-0736 around the anomalous region. The residuals of each model are shown in separate panels, and their χ2 are presented. Right panels: caustics and trajectories of 2L1S models for KMT-2021-BLG-0736. The curves are the (planetary) caustics, and the lines with arrows are the trajectories of the source-to-lens motion. The magenta dashed circles mark the (1, 2, 3)σ upper limits of ρ, and the solid circle (bottom right) marks the measured values of ρ. The blue (nearly vertical) lines represent the Einstein radius.
Paper: Systematic Reanalysis of KMTNet Microlensing Events. II. Two New Planets in Giant-source Events
Authors: Hongjing Yang, 弘靖 杨, Jennifer C. Yee, Jiyuan Zhang, 纪元 张, Chung-Uk Lee, Dong-Jin Kim, Ian A. Bond, Andrzej Udalski, Kyu-Ha Hwang, Weicheng Zang, 伟呈 臧, Qiyue Qian, 奇玥 钱, Andrew Gould, Shude Mao, 淑德 毛, Michael D. Albrow, Sun-Ju Chung, Cheongho Han, Youn Kil Jung, Yoon-Hyun Ryu, In-Gu Shin, Yossi Shvartzvald, Sang-Mok Cha, Hyoun-Woo Kim, Seung-Lee Kim, Dong-Joo Lee, Yongseok Lee, Byeong-Gon Park, Richard W. Pogge, Fumio Abe, Ken Bando, David P. Bennett, Aparna Bhattacharya, Akihiko Fukui, Ryusei Hamada, Shunya Hamada, Naoto Hamasaki, Yuki Hirao, Stela Ishitani Silva, Yoshitaka Itow, Naoki Koshimoto, Yutaka Matsubara, Shota Miyazaki, Yasushi Muraki, Tutumi Nagai, Kansuke Nunota, Greg Olmschenk, Clément Ranc, Nicholas J. Rattenbury, Yuki Satoh, Takahiro Sumi, Daisuke Suzuki, Sean K. Terry, Paul . J. Tristram, Aikaterini Vandorou, Hibiki Yama, Przemek Mróz, Jan Skowron, Radoslaw Poleski, Michał K. Szymański, Igor Soszyński, Paweł Pietrukowicz, Szymon Kozłowski, Krzysztof Ulaczyk, Krzysztof A. Rybicki, Patryk Iwanek, Marcin Wrona
Figure caption: Light curves and reported signals of some example candidate anomalies. In each subfigure, the upper panel is the full light curve of the event, and the lower is the zoomed-in plot of the candidate signal region. The shadowed region marks the reported time window that has the candidate signal. The colors represent data from different sites and fields. The PSPL models are shown as black curves.