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Planetary

planetary

Authors:
(1) Youn Kil Jung, Korea Astronomy and Space Science Institute, University of Science and Technology, and The KMTNet Collaboration;
(2) Cheongho Han, Department of Physics, Chungbuk National University and The KMTNet Collaboration;
(3) Andrzej Udalski, Warsaw University Observatory and The OGLE Collaboration;
(4) Andrew Gould, Korea Astronomy and Space Science Institute, Department of Astronomy, Ohio State University, Max-Planck-Institute for Astronomy and The KMTNet Collaboration;
(5) Jennifer C. Yee, Center for Astrophysics | Harvard & Smithsonian and The KMTNet Collaboration;
(6) Michael D. Albrow, University of Canterbury, Department of Physics and Astronomy;
(7) Sun-Ju Chung, Korea Astronomy and Space Science Institute and University of Science and Technology;
(8) Kyu-Ha Hwang, Korea Astronomy and Space Science Institute;
(9) Yoon-Hyun Ryu, Korea Astronomy and Space Science Institute;
(10) In-Gu Shin, Korea Astronomy and Space Science Institute;
(11) Yossi Shvartzvald, Department of Particle Physics and Astrophysics, Weizmann Institute of Science;
(12) Wei Zhu, Canadian Institute for Theoretical Astrophysics, University of Toronto;
(13) Weicheng Zang, Department of Astronomy, Tsinghua University;
(14) Sang-Mok Cha, Korea Astronomy and Space Science Institute and 2School of Space Research, Kyung Hee University;
(15) Dong-Jin Kim, Korea Astronomy and Space Science Institute;
(16) Hyoun-Woo Kim, Korea Astronomy and Space Science Institute;
(17) Seung-Lee Kim, Korea Astronomy and Space Science Institute and University of Science and Technology;
(18) Chung-Uk Lee, Korea Astronomy and Space Science Institute and University of Science and Technology;
(19) Dong-Joo Lee, Korea Astronomy and Space Science Institute;
(20) Yongseok Lee, Korea Astronomy and Space Science Institute and School of Space Research, Kyung Hee University;
(21) Byeong-Gon Park, Korea Astronomy and Space Science Institute and University of Science and Technology;
(22) Richard W. Pogge, Department of Astronomy, Ohio State University;
(23) Przemek Mroz, Warsaw University Observatory and Division of Physics, Mathematics, and Astronomy, California Institute of Technology;
(24) Michal K. Szymanski, Warsaw University Observatory;
(25) Jan Skowron, Warsaw University Observatory;
(26) Radek Poleski, Warsaw University Observatory and Department of Astronomy, Ohio State University;
(27) Igor Soszynski, Warsaw University Observatory;
(28) Pawel Pietrukowicz, Warsaw University Observatory;
(29) Szymon Kozlowski, Warsaw University Observatory;
(30) Krzystof Ulaczyk, Department of Physics, University of Warwick, Gibbet;
(31) Krzysztof A. Rybicki, Warsaw University Observatory;
(32) Patryk Iwanek, Warsaw University Observatory;
(33) Marcin Wrona, Warsaw University Observatory. Table of Links Abstract and Intro
Observation
Light Curve Analysis
Physical Parameters
Microlensing Planets in the (log s, log q) plane
Summary and Conclusions
References 6. Summary and Conclusions This research has made use of the KMTNet system operated by the Korea Astronomy and Space Science Institute (KASI) and the data were obtained at three host sites of CTIO in Chile, SAAO in South Africa, and SSO in Australia. Work by CH was supported by the grants of National Research Foundation of Korea (2017R1A4A1015178 and 2019R1A2C2085965). The OGLE has received funding from the National Science Centre, Poland, grant MAESTRO 2014/14/A/ST9/00121 to A.U. This paper is available on arxiv under CC0 1.0 DEED license. Authors: (1) Youn Kil Jung, Korea Astronomy and Space Science Institute, University of Science and Technology, and The KMTNet Collaboration; (2) Cheongho Han, Department of Physics, Chungbuk National University and The KMTNet Collaboration; (3) Andrzej Udalski, Warsaw University Observatory and The OGLE Collaboration; (4) Andrew Gould, Korea Astronomy and Space Science Institute, Department of Astronomy, Ohio State University, Max-Planck-Institute for Astronomy and The KMTNet Collaboration; (5) Jennifer C. Yee, Center for Astrophysics | Harvard & Smithsonian and The KMTNet Collaboration; (6) Michael D. Albrow, University of Canterbury, Department of Physics and Astronomy; (7) Sun-Ju Chung, Korea Astronomy and Space Science Institute and University of Science and Technology; (8) Kyu-Ha Hwang, Korea Astronomy and Space Science Institute; (9) Yoon-Hyun Ryu, Korea Astronomy and Space Science Institute; (10) In-Gu Shin, Korea Astronomy and Space Science Institute; (11) Yossi Shvartzvald, Department of Particle Physics and Astrophysics, Weizmann Institute of Science; (12) Wei Zhu, Canadian Institute for Theoretical Astrophysics, University of Toronto; (13) Weicheng Zang, Department of Astronomy, Tsinghua University; (14) Sang-Mok Cha, Korea Astronomy and Space Science Institute and 2School of Space Research, Kyung Hee University; (15) Dong-Jin Kim, Korea Astronomy and Space Science Institute; (16) Hyoun-Woo Kim, Korea Astronomy and Space Science Institute; (17) Seung-Lee Kim, Korea Astronomy and Space Science Institute and University of Science and Technology; (18) Chung-Uk Lee, Korea Astronomy and Space Science Institute and University of Science and Technology; (19) Dong-Joo Lee, Korea Astronomy and Space Science Institute; (20) Yongseok Lee, Korea Astronomy and Space Science Institute and School of Space Research, Kyung Hee University; (21) Byeong-Gon Park, Korea Astronomy and Space Science Institute and University of Science and Technology; (22) Richard W. Pogge, Department of Astronomy, Ohio State University; (23) Przemek Mroz, Warsaw University Observatory and Division of Physics, Mathematics, and Astronomy, California Institute of Technology; (24) Michal K. Szymanski, Warsaw University Observatory; (25) Jan Skowron, Warsaw University Observatory; (26) Radek Poleski, Warsaw University Observatory and Department of Astronomy, Ohio State University; (27) Igor Soszynski, Warsaw University Observatory; (28) Pawel Pietrukowicz, Warsaw University Observatory; (29) Szymon Kozlowski, Warsaw University Observatory; (30) Krzystof Ulaczyk, Department of Physics, University of Warwick, Gibbet; (31) Krzysztof A. Rybicki, Warsaw University Observatory; (32) Patryk Iwanek, Warsaw University Observatory; (33) Marcin Wrona, Warsaw University Observatory. Authors: Authors: (1) Youn Kil Jung, Korea Astronomy and Space Science Institute, University of Science and Technology, and The KMTNet Collaboration; (2) Cheongho Han, Department of Physics, Chungbuk National University and The KMTNet Collaboration; (3) Andrzej Udalski, Warsaw University Observatory and The OGLE Collaboration; (4) Andrew Gould, Korea Astronomy and Space Science Institute, Department of Astronomy, Ohio State University, Max-Planck-Institute for Astronomy and The KMTNet Collaboration; (5) Jennifer C. Yee, Center for Astrophysics | Harvard & Smithsonian and The KMTNet Collaboration; (6) Michael D. Albrow, University of Canterbury, Department of Physics and Astronomy; (7) Sun-Ju Chung, Korea Astronomy and Space Science Institute and University of Science and Technology; (8) Kyu-Ha Hwang, Korea Astronomy and Space Science Institute; (9) Yoon-Hyun Ryu, Korea Astronomy and Space Science Institute; (10) In-Gu Shin, Korea Astronomy and Space Science Institute; (11) Yossi Shvartzvald, Department of Particle Physics and Astrophysics, Weizmann Institute of Science; (12) Wei Zhu, Canadian Institute for Theoretical Astrophysics, University of Toronto; (13) Weicheng Zang, Department of Astronomy, Tsinghua University; (14) Sang-Mok Cha, Korea Astronomy and Space Science Institute and 2School of Space Research, Kyung Hee University; (15) Dong-Jin Kim, Korea Astronomy and Space Science Institute; (16) Hyoun-Woo Kim, Korea Astronomy and Space Science Institute; (17) Seung-Lee Kim, Korea Astronomy and Space Science Institute and University of Science and Technology; (18) Chung-Uk Lee, Korea Astronomy and Space Science Institute and University of Science and Technology; (19) Dong-Joo Lee, Korea Astronomy and Space Science Institute; (20) Yongseok Lee, Korea Astronomy and Space Science Institute and School of Space Research, Kyung Hee University; (21) Byeong-Gon Park, Korea Astronomy and Space Science Institute and University of Science and Technology; (22) Richard W. Pogge, Department of Astronomy, Ohio State University; (23) Przemek Mroz, Warsaw University Observatory and Division of Physics, Mathematics, and Astronomy, California Institute of Technology; (24) Michal K. Szymanski, Warsaw University Observatory; (25) Jan Skowron, Warsaw University Observatory; (26) Radek Poleski, Warsaw University Observatory and Department of Astronomy, Ohio State University; (27) Igor Soszynski, Warsaw University Observatory; (28) Pawel Pietrukowicz, Warsaw University Observatory; (29) Szymon Kozlowski, Warsaw University Observatory; (30) Krzystof Ulaczyk, Department of Physics, University of Warwick, Gibbet; (31) Krzysztof A. Rybicki, Warsaw University Observatory; (32) Patryk Iwanek, Warsaw University Observatory; (33) Marcin Wrona, Warsaw University Observatory. Table of Links Abstract and Intro Observation Light Curve Analysis Physical Parameters Microlensing Planets in the (log s, log q) plane Summary and Conclusions References Abstract and Intro Abstract and Intro Observation Observation Light Curve Analysis Light Curve Analysis Physical Parameters Physical Parameters Microlensing Planets in the (log s , log q ) plane Microlensing Planets in the (log s s , log q q ) plane Summary and Conclusions Summary and Conclusions References References 6. Summary and Conclusions This research has made use of the KMTNet system operated by the Korea Astronomy and Space Science Institute (KASI) and the data were obtained at three host sites of CTIO in Chile, SAAO in South Africa, and SSO in Australia. Work by CH was supported by the grants of National Research Foundation of Korea (2017R1A4A1015178 and 2019R1A2C2085965). The OGLE has received funding from the National Science Centre, Poland, grant MAESTRO 2014/14/A/ST9/00121 to A.U. This paper is available on arxiv under CC0 1.0 DEED license. This paper is available on arxiv under CC0 1.0 DEED license. available on arxiv

Two Microlensing Planets through Planetary-Caustic Channel: Summary and Conclusions

প্ল্যানেটারি-কস্টিক চ্যানেলের মাধ্যমে দুটি মাইক্রোলেনসিং গ্রহ: সারাংশ এবং উপসংহার

Zwei Mikrolinsenplaneten durch den planetar-kaustischen Kanal: Zusammenfassung und Schlussfolgerungen

Dos planetas microlentes a través del canal planetario-cáustico: resumen y conclusiones

Deux planètes à microlentille via un canal planétaire-caustique : résumé et conclusions

ग्रहीय-कास्टिक चैनल के माध्यम से दो माइक्रोलेंसिंग ग्रह: सारांश और निष्कर्ष

惑星-コースティックチャネルを通した2つのマイクロレンズ効果を持つ惑星：要約と結論

행성 가성 채널을 통한 두 개의 미세 렌즈 행성: 요약 및 결론

Dois planetas microlentes através do canal planetário-cáustico: resumo e conclusões

Две микролинзирующие планеты через планетарно-каустический канал: итоги и выводы

Gezegensel-Kostik Kanal Üzerinden İki Mikro Mercekleme Gezegeni: Özet ve Sonuçlar

Hai hành tinh vi thấu kính thông qua Kênh ăn da hành tinh: Tóm tắt và kết luận

通过行星焦散通道观察两颗微透镜行星：总结和结论

Authors:
(1) Youn Kil Jung, Korea Astronomy and Space Science Institute, University of Science and Technology, and The KMTNet Collaboration;
(2) Cheongho Han, Department of Physics, Chungbuk National University and The KMTNet Collaboration;
(3) Andrzej Udalski, Warsaw University Observatory and The OGLE Collaboration;
(4) Andrew Gould, Korea Astronomy and Space Science Institute, Department of Astronomy, Ohio State University, Max-Planck-Institute for Astronomy and The KMTNet Collaboration;
(5) Jennifer C. Yee, Center for Astrophysics | Harvard & Smithsonian and The KMTNet Collaboration;
(6) Michael D. Albrow, University of Canterbury, Department of Physics and Astronomy;
(7) Sun-Ju Chung, Korea Astronomy and Space Science Institute and University of Science and Technology;
(8) Kyu-Ha Hwang, Korea Astronomy and Space Science Institute;
(9) Yoon-Hyun Ryu, Korea Astronomy and Space Science Institute;
(10) In-Gu Shin, Korea Astronomy and Space Science Institute;
(11) Yossi Shvartzvald, Department of Particle Physics and Astrophysics, Weizmann Institute of Science;
(12) Wei Zhu, Canadian Institute for Theoretical Astrophysics, University of Toronto;
(13) Weicheng Zang, Department of Astronomy, Tsinghua University;
(14) Sang-Mok Cha, Korea Astronomy and Space Science Institute and 2School of Space Research, Kyung Hee University;
(15) Dong-Jin Kim, Korea Astronomy and Space Science Institute;
(16) Hyoun-Woo Kim, Korea Astronomy and Space Science Institute;
(17) Seung-Lee Kim, Korea Astronomy and Space Science Institute and University of Science and Technology;
(18) Chung-Uk Lee, Korea Astronomy and Space Science Institute and University of Science and Technology;
(19) Dong-Joo Lee, Korea Astronomy and Space Science Institute;
(20) Yongseok Lee, Korea Astronomy and Space Science Institute and School of Space Research, Kyung Hee University;
(21) Byeong-Gon Park, Korea Astronomy and Space Science Institute and University of Science and Technology;
(22) Richard W. Pogge, Department of Astronomy, Ohio State University;
(23) Przemek Mroz, Warsaw University Observatory and Division of Physics, Mathematics, and Astronomy, California Institute of Technology;
(24) Michal K. Szymanski, Warsaw University Observatory;
(25) Jan Skowron, Warsaw University Observatory;
(26) Radek Poleski, Warsaw University Observatory and Department of Astronomy, Ohio State University;
(27) Igor Soszynski, Warsaw University Observatory;
(28) Pawel Pietrukowicz, Warsaw University Observatory;
(29) Szymon Kozlowski, Warsaw University Observatory;
(30) Krzystof Ulaczyk, Department of Physics, University of Warwick, Gibbet;
(31) Krzysztof A. Rybicki, Warsaw University Observatory;
(32) Patryk Iwanek, Warsaw University Observatory;
(33) Marcin Wrona, Warsaw University Observatory. Table of Links Abstract and Intro
Observation
Light Curve Analysis
Physical Parameters
Microlensing Planets in the (log s, log q) plane
Summary and Conclusions
References 3. Light Curve Analysis In Figures 3 and 4, we present the lens-system configurations of the individual events, showing the source trajectory with respect to the lens components and resulting caustics. From the configurations, it is found that the anomalies of both events are produced by the source crossing over the planetary caustic of the lens system. For OGLE-2018-BLG-0567, the source size is comparable to the caustic size, and thus the detailed caustic-crossing features, two caustic spikes and a U-shape trough region between the spikes, was smeared out by finite source effects. For OGLE-2018-BLG-0962, on the other hand, the caustic is much bigger than the source size, and thus detailed caustic-crossing feature of the anomaly is well delineated. It is found the first part of the anomaly, centered at HJD′ (= HJD − 2, 450, 000 days) ∼ 8271.5, was produced by the source passing over the two caustic segments that flank the inner cusp (on the binary axis) of the planetary caustic, and the second part, centered at HJD′ ∼ 8273.8, was generated by the source passage over the adjacent (off-axis) cusp. This paper is available on arxiv under CC0 1.0 DEED license. Authors: (1) Youn Kil Jung, Korea Astronomy and Space Science Institute, University of Science and Technology, and The KMTNet Collaboration; (2) Cheongho Han, Department of Physics, Chungbuk National University and The KMTNet Collaboration; (3) Andrzej Udalski, Warsaw University Observatory and The OGLE Collaboration; (4) Andrew Gould, Korea Astronomy and Space Science Institute, Department of Astronomy, Ohio State University, Max-Planck-Institute for Astronomy and The KMTNet Collaboration; (5) Jennifer C. Yee, Center for Astrophysics | Harvard & Smithsonian and The KMTNet Collaboration; (6) Michael D. Albrow, University of Canterbury, Department of Physics and Astronomy; (7) Sun-Ju Chung, Korea Astronomy and Space Science Institute and University of Science and Technology; (8) Kyu-Ha Hwang, Korea Astronomy and Space Science Institute; (9) Yoon-Hyun Ryu, Korea Astronomy and Space Science Institute; (10) In-Gu Shin, Korea Astronomy and Space Science Institute; (11) Yossi Shvartzvald, Department of Particle Physics and Astrophysics, Weizmann Institute of Science; (12) Wei Zhu, Canadian Institute for Theoretical Astrophysics, University of Toronto; (13) Weicheng Zang, Department of Astronomy, Tsinghua University; (14) Sang-Mok Cha, Korea Astronomy and Space Science Institute and 2School of Space Research, Kyung Hee University; (15) Dong-Jin Kim, Korea Astronomy and Space Science Institute; (16) Hyoun-Woo Kim, Korea Astronomy and Space Science Institute; (17) Seung-Lee Kim, Korea Astronomy and Space Science Institute and University of Science and Technology; (18) Chung-Uk Lee, Korea Astronomy and Space Science Institute and University of Science and Technology; (19) Dong-Joo Lee, Korea Astronomy and Space Science Institute; (20) Yongseok Lee, Korea Astronomy and Space Science Institute and School of Space Research, Kyung Hee University; (21) Byeong-Gon Park, Korea Astronomy and Space Science Institute and University of Science and Technology; (22) Richard W. Pogge, Department of Astronomy, Ohio State University; (23) Przemek Mroz, Warsaw University Observatory and Division of Physics, Mathematics, and Astronomy, California Institute of Technology; (24) Michal K. Szymanski, Warsaw University Observatory; (25) Jan Skowron, Warsaw University Observatory; (26) Radek Poleski, Warsaw University Observatory and Department of Astronomy, Ohio State University; (27) Igor Soszynski, Warsaw University Observatory; (28) Pawel Pietrukowicz, Warsaw University Observatory; (29) Szymon Kozlowski, Warsaw University Observatory; (30) Krzystof Ulaczyk, Department of Physics, University of Warwick, Gibbet; (31) Krzysztof A. Rybicki, Warsaw University Observatory; (32) Patryk Iwanek, Warsaw University Observatory; (33) Marcin Wrona, Warsaw University Observatory. Authors: Authors: (1) Youn Kil Jung, Korea Astronomy and Space Science Institute, University of Science and Technology, and The KMTNet Collaboration; (2) Cheongho Han, Department of Physics, Chungbuk National University and The KMTNet Collaboration; (3) Andrzej Udalski, Warsaw University Observatory and The OGLE Collaboration; (4) Andrew Gould, Korea Astronomy and Space Science Institute, Department of Astronomy, Ohio State University, Max-Planck-Institute for Astronomy and The KMTNet Collaboration; (5) Jennifer C. Yee, Center for Astrophysics | Harvard & Smithsonian and The KMTNet Collaboration; (6) Michael D. Albrow, University of Canterbury, Department of Physics and Astronomy; (7) Sun-Ju Chung, Korea Astronomy and Space Science Institute and University of Science and Technology; (8) Kyu-Ha Hwang, Korea Astronomy and Space Science Institute; (9) Yoon-Hyun Ryu, Korea Astronomy and Space Science Institute; (10) In-Gu Shin, Korea Astronomy and Space Science Institute; (11) Yossi Shvartzvald, Department of Particle Physics and Astrophysics, Weizmann Institute of Science; (12) Wei Zhu, Canadian Institute for Theoretical Astrophysics, University of Toronto; (13) Weicheng Zang, Department of Astronomy, Tsinghua University; (14) Sang-Mok Cha, Korea Astronomy and Space Science Institute and 2School of Space Research, Kyung Hee University; (15) Dong-Jin Kim, Korea Astronomy and Space Science Institute; (16) Hyoun-Woo Kim, Korea Astronomy and Space Science Institute; (17) Seung-Lee Kim, Korea Astronomy and Space Science Institute and University of Science and Technology; (18) Chung-Uk Lee, Korea Astronomy and Space Science Institute and University of Science and Technology; (19) Dong-Joo Lee, Korea Astronomy and Space Science Institute; (20) Yongseok Lee, Korea Astronomy and Space Science Institute and School of Space Research, Kyung Hee University; (21) Byeong-Gon Park, Korea Astronomy and Space Science Institute and University of Science and Technology; (22) Richard W. Pogge, Department of Astronomy, Ohio State University; (23) Przemek Mroz, Warsaw University Observatory and Division of Physics, Mathematics, and Astronomy, California Institute of Technology; (24) Michal K. Szymanski, Warsaw University Observatory; (25) Jan Skowron, Warsaw University Observatory; (26) Radek Poleski, Warsaw University Observatory and Department of Astronomy, Ohio State University; (27) Igor Soszynski, Warsaw University Observatory; (28) Pawel Pietrukowicz, Warsaw University Observatory; (29) Szymon Kozlowski, Warsaw University Observatory; (30) Krzystof Ulaczyk, Department of Physics, University of Warwick, Gibbet; (31) Krzysztof A. Rybicki, Warsaw University Observatory; (32) Patryk Iwanek, Warsaw University Observatory; (33) Marcin Wrona, Warsaw University Observatory. Table of Links Abstract and Intro Observation Light Curve Analysis Physical Parameters Microlensing Planets in the (log s, log q) plane Summary and Conclusions References Abstract and Intro Abstract and Intro Observation Observation Light Curve Analysis Light Curve Analysis Physical Parameters Physical Parameters Microlensing Planets in the (log s , log q ) plane Microlensing Planets in the (log s s , log q q ) plane Summary and Conclusions Summary and Conclusions References References 3. Light Curve Analysis In Figures 3 and 4, we present the lens-system configurations of the individual events, showing the source trajectory with respect to the lens components and resulting caustics. From the configurations, it is found that the anomalies of both events are produced by the source crossing over the planetary caustic of the lens system. For OGLE-2018-BLG-0567, the source size is comparable to the caustic size, and thus the detailed caustic-crossing features, two caustic spikes and a U-shape trough region between the spikes, was smeared out by finite source effects. For OGLE-2018-BLG-0962, on the other hand, the caustic is much bigger than the source size, and thus detailed caustic-crossing feature of the anomaly is well delineated. It is found the first part of the anomaly, centered at HJD′ (= HJD − 2, 450, 000 days) ∼ 8271.5, was produced by the source passing over the two caustic segments that flank the inner cusp (on the binary axis) of the planetary caustic, and the second part, centered at HJD′ ∼ 8273.8, was generated by the source passage over the adjacent (off-axis) cusp. This paper is available on arxiv under CC0 1.0 DEED license. This paper is available on arxiv under CC0 1.0 DEED license. available on arxiv

Two Microlensing Planets through Planetary-Caustic Channel: Light Curve Analysis

প্ল্যানেটারি-কস্টিক চ্যানেলের মাধ্যমে দুটি মাইক্রোলেনসিং গ্রহ: হালকা বক্ররেখা বিশ্লেষণ

Zwei Mikrolinsenplaneten durch den planetarisch-kaustischen Kanal: Lichtkurvenanalyse

Dos planetas con microlentes a través del canal cáustico planetario: análisis de la curva de luz

Deux planètes à microlentille à travers un canal planétaire-caustique : analyse de la courbe de lumière

ग्रहीय-कास्टिक चैनल के माध्यम से दो माइक्रोलेंसिंग ग्रह: प्रकाश वक्र विश्लेषण

惑星-コースティックチャンネルを通した2つのマイクロレンズ惑星：光度曲線解析

행성 가성 채널을 통한 두 개의 미세 렌즈 행성: 광 곡선 분석

Dois planetas microlentes através do canal planetário-cáustico: análise da curva de luz

Две микролинзирующие планеты через планетарно-каустический канал: анализ кривой блеска

Gezegensel-Kostik Kanal Üzerinden İki Mikro Mercekleme Gezegeni: Işık Eğrisi Analizi

Hai hành tinh vi thấu kính thông qua Kênh Caustic-Hành tinh: Phân tích đường cong ánh sáng

通过行星焦散通道观察两颗微透镜行星：光变曲线分析

Authors:
(1) Youn Kil Jung, Korea Astronomy and Space Science Institute, University of Science and Technology, and The KMTNet Collaboration;
(2) Cheongho Han, Department of Physics, Chungbuk National University and The KMTNet Collaboration;
(3) Andrzej Udalski, Warsaw University Observatory and The OGLE Collaboration;
(4) Andrew Gould, Korea Astronomy and Space Science Institute, Department of Astronomy, Ohio State University, Max-Planck-Institute for Astronomy and The KMTNet Collaboration;
(5) Jennifer C. Yee, Center for Astrophysics | Harvard & Smithsonian and The KMTNet Collaboration;
(6) Michael D. Albrow, University of Canterbury, Department of Physics and Astronomy;
(7) Sun-Ju Chung, Korea Astronomy and Space Science Institute and University of Science and Technology;
(8) Kyu-Ha Hwang, Korea Astronomy and Space Science Institute;
(9) Yoon-Hyun Ryu, Korea Astronomy and Space Science Institute;
(10) In-Gu Shin, Korea Astronomy and Space Science Institute;
(11) Yossi Shvartzvald, Department of Particle Physics and Astrophysics, Weizmann Institute of Science;
(12) Wei Zhu, Canadian Institute for Theoretical Astrophysics, University of Toronto;
(13) Weicheng Zang, Department of Astronomy, Tsinghua University;
(14) Sang-Mok Cha, Korea Astronomy and Space Science Institute and 2School of Space Research, Kyung Hee University;
(15) Dong-Jin Kim, Korea Astronomy and Space Science Institute;
(16) Hyoun-Woo Kim, Korea Astronomy and Space Science Institute;
(17) Seung-Lee Kim, Korea Astronomy and Space Science Institute and University of Science and Technology;
(18) Chung-Uk Lee, Korea Astronomy and Space Science Institute and University of Science and Technology;
(19) Dong-Joo Lee, Korea Astronomy and Space Science Institute;
(20) Yongseok Lee, Korea Astronomy and Space Science Institute and School of Space Research, Kyung Hee University;
(21) Byeong-Gon Park, Korea Astronomy and Space Science Institute and University of Science and Technology;
(22) Richard W. Pogge, Department of Astronomy, Ohio State University;
(23) Przemek Mroz, Warsaw University Observatory and Division of Physics, Mathematics, and Astronomy, California Institute of Technology;
(24) Michal K. Szymanski, Warsaw University Observatory;
(25) Jan Skowron, Warsaw University Observatory;
(26) Radek Poleski, Warsaw University Observatory and Department of Astronomy, Ohio State University;
(27) Igor Soszynski, Warsaw University Observatory;
(28) Pawel Pietrukowicz, Warsaw University Observatory;
(29) Szymon Kozlowski, Warsaw University Observatory;
(30) Krzystof Ulaczyk, Department of Physics, University of Warwick, Gibbet;
(31) Krzysztof A. Rybicki, Warsaw University Observatory;
(32) Patryk Iwanek, Warsaw University Observatory;
(33) Marcin Wrona, Warsaw University Observatory. Table of Links Abstract and Intro
Observation
Light Curve Analysis
Physical Parameters
Microlensing Planets in the (log s, log q) plane
Summary and Conclusions
References REFERENCES Alard, C., & Lupton, Robert H. 1998, ApJ, 503, 325 Alcock, C., Allsman, R. A., Axelrod, T. S., et al. 1995, ApJ, 445, 133 Albrow, M. D. 2017, MichaelDAlbrow/pyDIA: Initial release on github, V1.0.0, Zenodo, doi:10.5281/zenodo.268049 Albrow, M. D., Horne, K., Bramich, D. M., et al. 2009, MNRAS, 397, 2099 Beaulieu, J.-P., Bennett, D. P., Fouqu´e, P., et al. 2006, Nature, 439, 437 Bennett, D.P., Rhie, S.H., Nikolaev, S. et al. 2010, ApJ, 713, 837 Bennett, D. P., Sumi, T., Bond, I. A., et al. 2012, ApJ, 757, 119 Bensby, T., Yee, J. C., Feltzing, S., et al. 2013, A&A, 549, 147 Bessell, M. S., & Brett, J. M. 1988, PASP, 100, 1134 Bond, I. A., Abe, F., Dodd, R. J. 2001, MNRAS, 327, 868 Bond, I.A., Udalski, A., Jaroszy´nski, M. et al. 2004, ApJ, 606, L155 Dominik, M. 1998, A&A, 329, 361 Dominik, M. 1999, A&A, 349, 108 Dong, S., Gould, A., Udalski, A. et al. 2009, ApJ, 695, 970 Gaia Collaboration, Brown, A. G. A., Vallenari, A., et al. 2018, A&A, 616, 1 Gaia Collaboration, Prusti, T., de Bruijne, J. H. J., et al. 2016, A&A, 595, A1 Gaudi, B.S. 1998, ApJ, 506, 533 Gaudi, B. S. 2012, ARA&A, 50, 411 Gaudi, B.S., Bennett, D.P., Udalski, A. et al. 2008, Science, 319, 927 Gould, A. 1992, ApJ, 392, 442 Gould, A. 1997, in Variables Stars and the Astrophysical Returns of the Microlensing Surveys, ed. R. Ferlet, J.-P. Maillard, & B. Raban (Gif-sur-Yvette, France: Editions Frontieres), 125 Gould, A. 2000, ApJ, 542, 785 Gould, A. & Gaucherel, C. 1997, ApJ, 477, 580 Gould, A., & Loeb, A. 1992, ApJ, 396, 104 Gould, A., Dong, S., Gaudi, B. S., et al. 2010, ApJ, 720, 1073 Gould, A., Udalski, A., Shin, I.-G. et al. 2014, Science, 345, 46 Griest, K., & Safizadeh, N. 1998, ApJ, 500, 37 Han, C., & Gould, A. 1995, ApJ, 447, 53 Han, C., & Gould, A. 2003, ApJ, 592, 172 Han, C., Udalski, A., Gould, A., et al. 2017, AJ, 154, 133 Han, C., Udalski, A., Gould, A., et al. 2020, AJ, 159, 91 Holtzman, J. A., Watson, A. M., Baum, W. A., et al. 1998, AJ, 115, 1946 Hwang, K.-H., Ryu, Y.-H., Kim, H.-W., et al. 2019, AJ, 157, 23 Hwang, K.-H., Udalski, A., Shvartzvald, Y., et al. 2018, AJ, 155, 20 Ida, S., & Lin, D. N. C. 2004, ApJ, 616, 567 Jung, Y. K., Gould, A., Udalski, A, et al. 2019, AJ, 158, 28 Jung, Y. K., Udalski, A., Gould, A., et al. 2018, AJ, 155, 219 Jung, Y. K., Udalski, A., Sumi, T., et al. 2015, ApJ, 798, 123 Jung, Y. K., Udalski, A., Yee, J. C., et al. 2017, AJ, 153, 129 Han, C. 2006, ApJ, 638, 1080 Kayser, R., Refsdal S., & Stabell, R. 1986, A&A, 166, 36 Kennedy, G. M., & Kenyon, S. J. 2008, ApJ, 673, 502 Kervella, P., Bersier, D., Mourard, D., et al. 2004a, A&A, 428, 587 Kervella, P., Th´evenin, F., Di Folco, E., & S´egransan, D. 2004b, A&A, 426, 297 Kim, D.-J., Kim, H.-W., Hwang, K.-H., et al. 2018, AJ, 155, 76 Kim, S.-L., Lee, C.-U., Park, B.-G., et al. 2016, JKAS, 49, 37 Nataf, D. M., Gould, A., Fouqu´e, P., et al. 2013, ApJ, 769, 88 Paczy´nski, B. 1986, ApJ, 304, 1 Pecaut, M. J., & Mamajek, E. E. 2013, ApJS, 208, 9 Poleski, R., Skowron, J., Udalski, A., et al. 2014, ApJ, 795, 42 Poleski, R., Suzuki, D., Udalski, A., et al. 2020, AJ, 159, 261 Poleski, R., Udalski, A., Bond, I. A., et al. 2017, A&A, 604A, 103 Rattenbury, N. J., Bennett, D. P., Sumi, T., et al. 2015, MNRAS, 454, 946 Rhie, S. H., Bennett, D. P., Becker, A. C., et al. 2000, ApJ, 533, 378 Robin, A. C., Reyl´e, C., Derri´ere, S., & Picaud, S. 2003, A&A, 409, 523 Schneider, P., & Weiss, A. 1986, A&A, 164, 237 Schneider, P., & Weiss, A. 1987, A&A, 171, 49 Skowron, J., Udalski, A., Poleski, R., et al. 2016, ApJ, 820, 4 Skowron, J., Ryu, Y.-H., Hwang, K.-H., et al. 2018, AcA, 68, 43 Sumi, T., Bennett, D. P., Bond, I. A., et al. 2013, ApJ, 778, 150 Sumi, T., Udalski, A., Bennett, D. P., et al. 2016, ApJ, 825, 112 Suzuki, D., Bennett, D. P., Udalski, A., et al. 2018, AJ, 155, 263 Szyma´nski, M. K., Udalski, A., Soszy´nski, I., et al. 2011, AcA, 61, 83 Tomaney, A.B. & Crotts, A.P.S. 1996, AJ, 112, 2872 Udalski, A. 2003, Acta Astron., 53, 291 Udalski, A., Szyma´nski, M., Ka lu˙zny, J., Kubiak, M., & Mateo, M. 1992, AcA, 42, 253 Udalski, A., Szyma´nski, M. K., & Szyma´nski, G. 2015, AcA, 65, 1 Udalski, A., Jaroszy´nski, M., Paczy´nski, B., et al. 2005, ApJ, 628, L109 Wo´zniak, P. R. 2000, AcA, 50, 42 Yee, J. C., Shvartzvald, Y., Gal-Yam, A., et al. 2012, ApJ, 755, 102 Yee, J. C., Zang, W., Udalski, A., et al. 2021, arXiv:2101.04696 Yoo, J., DePoy, D. L., Gal-Yam, A., et al. 2004, ApJ, 603, 139 This paper is available on arxiv under CC0 1.0 DEED license. Authors: (1) Youn Kil Jung, Korea Astronomy and Space Science Institute, University of Science and Technology, and The KMTNet Collaboration; (2) Cheongho Han, Department of Physics, Chungbuk National University and The KMTNet Collaboration; (3) Andrzej Udalski, Warsaw University Observatory and The OGLE Collaboration; (4) Andrew Gould, Korea Astronomy and Space Science Institute, Department of Astronomy, Ohio State University, Max-Planck-Institute for Astronomy and The KMTNet Collaboration; (5) Jennifer C. Yee, Center for Astrophysics | Harvard & Smithsonian and The KMTNet Collaboration; (6) Michael D. Albrow, University of Canterbury, Department of Physics and Astronomy; (7) Sun-Ju Chung, Korea Astronomy and Space Science Institute and University of Science and Technology; (8) Kyu-Ha Hwang, Korea Astronomy and Space Science Institute; (9) Yoon-Hyun Ryu, Korea Astronomy and Space Science Institute; (10) In-Gu Shin, Korea Astronomy and Space Science Institute; (11) Yossi Shvartzvald, Department of Particle Physics and Astrophysics, Weizmann Institute of Science; (12) Wei Zhu, Canadian Institute for Theoretical Astrophysics, University of Toronto; (13) Weicheng Zang, Department of Astronomy, Tsinghua University; (14) Sang-Mok Cha, Korea Astronomy and Space Science Institute and 2School of Space Research, Kyung Hee University; (15) Dong-Jin Kim, Korea Astronomy and Space Science Institute; (16) Hyoun-Woo Kim, Korea Astronomy and Space Science Institute; (17) Seung-Lee Kim, Korea Astronomy and Space Science Institute and University of Science and Technology; (18) Chung-Uk Lee, Korea Astronomy and Space Science Institute and University of Science and Technology; (19) Dong-Joo Lee, Korea Astronomy and Space Science Institute; (20) Yongseok Lee, Korea Astronomy and Space Science Institute and School of Space Research, Kyung Hee University; (21) Byeong-Gon Park, Korea Astronomy and Space Science Institute and University of Science and Technology; (22) Richard W. Pogge, Department of Astronomy, Ohio State University; (23) Przemek Mroz, Warsaw University Observatory and Division of Physics, Mathematics, and Astronomy, California Institute of Technology; (24) Michal K. Szymanski, Warsaw University Observatory; (25) Jan Skowron, Warsaw University Observatory; (26) Radek Poleski, Warsaw University Observatory and Department of Astronomy, Ohio State University; (27) Igor Soszynski, Warsaw University Observatory; (28) Pawel Pietrukowicz, Warsaw University Observatory; (29) Szymon Kozlowski, Warsaw University Observatory; (30) Krzystof Ulaczyk, Department of Physics, University of Warwick, Gibbet; (31) Krzysztof A. Rybicki, Warsaw University Observatory; (32) Patryk Iwanek, Warsaw University Observatory; (33) Marcin Wrona, Warsaw University Observatory. Authors: Authors: (1) Youn Kil Jung, Korea Astronomy and Space Science Institute, University of Science and Technology, and The KMTNet Collaboration; (2) Cheongho Han, Department of Physics, Chungbuk National University and The KMTNet Collaboration; (3) Andrzej Udalski, Warsaw University Observatory and The OGLE Collaboration; (4) Andrew Gould, Korea Astronomy and Space Science Institute, Department of Astronomy, Ohio State University, Max-Planck-Institute for Astronomy and The KMTNet Collaboration; (5) Jennifer C. Yee, Center for Astrophysics | Harvard & Smithsonian and The KMTNet Collaboration; (6) Michael D. Albrow, University of Canterbury, Department of Physics and Astronomy; (7) Sun-Ju Chung, Korea Astronomy and Space Science Institute and University of Science and Technology; (8) Kyu-Ha Hwang, Korea Astronomy and Space Science Institute; (9) Yoon-Hyun Ryu, Korea Astronomy and Space Science Institute; (10) In-Gu Shin, Korea Astronomy and Space Science Institute; (11) Yossi Shvartzvald, Department of Particle Physics and Astrophysics, Weizmann Institute of Science; (12) Wei Zhu, Canadian Institute for Theoretical Astrophysics, University of Toronto; (13) Weicheng Zang, Department of Astronomy, Tsinghua University; (14) Sang-Mok Cha, Korea Astronomy and Space Science Institute and 2School of Space Research, Kyung Hee University; (15) Dong-Jin Kim, Korea Astronomy and Space Science Institute; (16) Hyoun-Woo Kim, Korea Astronomy and Space Science Institute; (17) Seung-Lee Kim, Korea Astronomy and Space Science Institute and University of Science and Technology; (18) Chung-Uk Lee, Korea Astronomy and Space Science Institute and University of Science and Technology; (19) Dong-Joo Lee, Korea Astronomy and Space Science Institute; (20) Yongseok Lee, Korea Astronomy and Space Science Institute and School of Space Research, Kyung Hee University; (21) Byeong-Gon Park, Korea Astronomy and Space Science Institute and University of Science and Technology; (22) Richard W. Pogge, Department of Astronomy, Ohio State University; (23) Przemek Mroz, Warsaw University Observatory and Division of Physics, Mathematics, and Astronomy, California Institute of Technology; (24) Michal K. Szymanski, Warsaw University Observatory; (25) Jan Skowron, Warsaw University Observatory; (26) Radek Poleski, Warsaw University Observatory and Department of Astronomy, Ohio State University; (27) Igor Soszynski, Warsaw University Observatory; (28) Pawel Pietrukowicz, Warsaw University Observatory; (29) Szymon Kozlowski, Warsaw University Observatory; (30) Krzystof Ulaczyk, Department of Physics, University of Warwick, Gibbet; (31) Krzysztof A. Rybicki, Warsaw University Observatory; (32) Patryk Iwanek, Warsaw University Observatory; (33) Marcin Wrona, Warsaw University Observatory. Table of Links Abstract and Intro Observation Light Curve Analysis Physical Parameters Microlensing Planets in the (log s, log q) plane Summary and Conclusions References Abstract and Intro Abstract and Intro Observation Observation Light Curve Analysis Light Curve Analysis Physical Parameters Physical Parameters Microlensing Planets in the (log s , log q ) plane Microlensing Planets in the (log s s , log q q ) plane Summary and Conclusions Summary and Conclusions References References REFERENCES Alard, C., & Lupton, Robert H. 1998, ApJ, 503, 325 Alcock, C., Allsman, R. A., Axelrod, T. S., et al. 1995, ApJ, 445, 133 Albrow, M. D. 2017, MichaelDAlbrow/pyDIA: Initial release on github, V1.0.0, Zenodo, doi:10.5281/zenodo.268049 Albrow, M. D., Horne, K., Bramich, D. M., et al. 2009, MNRAS, 397, 2099 Beaulieu, J.-P., Bennett, D. P., Fouqu´e, P., et al. 2006, Nature, 439, 437 Bennett, D.P., Rhie, S.H., Nikolaev, S. et al. 2010, ApJ, 713, 837 Bennett, D. P., Sumi, T., Bond, I. A., et al. 2012, ApJ, 757, 119 Bensby, T., Yee, J. C., Feltzing, S., et al. 2013, A&A, 549, 147 Bessell, M. S., & Brett, J. M. 1988, PASP, 100, 1134 Bond, I. A., Abe, F., Dodd, R. J. 2001, MNRAS, 327, 868 Bond, I.A., Udalski, A., Jaroszy´nski, M. et al. 2004, ApJ, 606, L155 Dominik, M. 1998, A&A, 329, 361 Dominik, M. 1999, A&A, 349, 108 Dong, S., Gould, A., Udalski, A. et al. 2009, ApJ, 695, 970 Gaia Collaboration, Brown, A. G. A., Vallenari, A., et al. 2018, A&A, 616, 1 Gaia Collaboration, Prusti, T., de Bruijne, J. H. J., et al. 2016, A&A, 595, A1 Gaudi, B.S. 1998, ApJ, 506, 533 Gaudi, B. S. 2012, ARA&A, 50, 411 Gaudi, B.S., Bennett, D.P., Udalski, A. et al. 2008, Science, 319, 927 Gould, A. 1992, ApJ, 392, 442 Gould, A. 1997, in Variables Stars and the Astrophysical Returns of the Microlensing Surveys, ed. R. Ferlet, J.-P. Maillard, & B. Raban (Gif-sur-Yvette, France: Editions Frontieres), 125 Gould, A. 2000, ApJ, 542, 785 Gould, A. & Gaucherel, C. 1997, ApJ, 477, 580 Gould, A., & Loeb, A. 1992, ApJ, 396, 104 Gould, A., Dong, S., Gaudi, B. S., et al. 2010, ApJ, 720, 1073 Gould, A., Udalski, A., Shin, I.-G. et al. 2014, Science, 345, 46 Griest, K., & Safizadeh, N. 1998, ApJ, 500, 37 Han, C., & Gould, A. 1995, ApJ, 447, 53 Han, C., & Gould, A. 2003, ApJ, 592, 172 Han, C., Udalski, A., Gould, A., et al. 2017, AJ, 154, 133 Han, C., Udalski, A., Gould, A., et al. 2020, AJ, 159, 91 Holtzman, J. A., Watson, A. M., Baum, W. A., et al. 1998, AJ, 115, 1946 Hwang, K.-H., Ryu, Y.-H., Kim, H.-W., et al. 2019, AJ, 157, 23 Hwang, K.-H., Udalski, A., Shvartzvald, Y., et al. 2018, AJ, 155, 20 Ida, S., & Lin, D. N. C. 2004, ApJ, 616, 567 Jung, Y. K., Gould, A., Udalski, A, et al. 2019, AJ, 158, 28 Jung, Y. K., Udalski, A., Gould, A., et al. 2018, AJ, 155, 219 Jung, Y. K., Udalski, A., Sumi, T., et al. 2015, ApJ, 798, 123 Jung, Y. K., Udalski, A., Yee, J. C., et al. 2017, AJ, 153, 129 Han, C. 2006, ApJ, 638, 1080 Kayser, R., Refsdal S., & Stabell, R. 1986, A&A, 166, 36 Kennedy, G. M., & Kenyon, S. J. 2008, ApJ, 673, 502 Kervella, P., Bersier, D., Mourard, D., et al. 2004a, A&A, 428, 587 Kervella, P., Th´evenin, F., Di Folco, E., & S´egransan, D. 2004b, A&A, 426, 297 Kim, D.-J., Kim, H.-W., Hwang, K.-H., et al. 2018, AJ, 155, 76 Kim, S.-L., Lee, C.-U., Park, B.-G., et al. 2016, JKAS, 49, 37 Nataf, D. M., Gould, A., Fouqu´e, P., et al. 2013, ApJ, 769, 88 Paczy´nski, B. 1986, ApJ, 304, 1 Pecaut, M. J., & Mamajek, E. E. 2013, ApJS, 208, 9 Poleski, R., Skowron, J., Udalski, A., et al. 2014, ApJ, 795, 42 Poleski, R., Suzuki, D., Udalski, A., et al. 2020, AJ, 159, 261 Poleski, R., Udalski, A., Bond, I. A., et al. 2017, A&A, 604A, 103 Rattenbury, N. J., Bennett, D. P., Sumi, T., et al. 2015, MNRAS, 454, 946 Rhie, S. H., Bennett, D. P., Becker, A. C., et al. 2000, ApJ, 533, 378 Robin, A. C., Reyl´e, C., Derri´ere, S., & Picaud, S. 2003, A&A, 409, 523 Schneider, P., & Weiss, A. 1986, A&A, 164, 237 Schneider, P., & Weiss, A. 1987, A&A, 171, 49 Skowron, J., Udalski, A., Poleski, R., et al. 2016, ApJ, 820, 4 Skowron, J., Ryu, Y.-H., Hwang, K.-H., et al. 2018, AcA, 68, 43 Sumi, T., Bennett, D. P., Bond, I. A., et al. 2013, ApJ, 778, 150 Sumi, T., Udalski, A., Bennett, D. P., et al. 2016, ApJ, 825, 112 Suzuki, D., Bennett, D. P., Udalski, A., et al. 2018, AJ, 155, 263 Szyma´nski, M. K., Udalski, A., Soszy´nski, I., et al. 2011, AcA, 61, 83 Tomaney, A.B. & Crotts, A.P.S. 1996, AJ, 112, 2872 Udalski, A. 2003, Acta Astron., 53, 291 Udalski, A., Szyma´nski, M., Ka lu˙zny, J., Kubiak, M., & Mateo, M. 1992, AcA, 42, 253 Udalski, A., Szyma´nski, M. K., & Szyma´nski, G. 2015, AcA, 65, 1 Udalski, A., Jaroszy´nski, M., Paczy´nski, B., et al. 2005, ApJ, 628, L109 Wo´zniak, P. R. 2000, AcA, 50, 42 Yee, J. C., Shvartzvald, Y., Gal-Yam, A., et al. 2012, ApJ, 755, 102 Yee, J. C., Zang, W., Udalski, A., et al. 2021, arXiv:2101.04696 Yoo, J., DePoy, D. L., Gal-Yam, A., et al. 2004, ApJ, 603, 139 This paper is available on arxiv under CC0 1.0 DEED license. This paper is available on arxiv under CC0 1.0 DEED license. available on arxiv

Two Microlensing Planets through Planetary-Caustic Channel: References

প্ল্যানেটারি-কস্টিক চ্যানেলের মাধ্যমে দুটি মাইক্রোলেনসিং গ্রহ: তথ্যসূত্র

Zwei Mikrolinsenplaneten durch den planetar-kaustischen Kanal: Referenzen

Dos planetas con microlentes a través del canal cáustico planetario: referencias

Deux planètes à microlentille via un canal planétaire-caustique : références

ग्रहीय-कास्टिक चैनल के माध्यम से दो माइक्रोलेंसिंग ग्रह: संदर्भ

惑星-コースティックチャネルを通した2つのマイクロレンズ効果を持つ惑星: 参考文献

행성 가성 채널을 통한 두 개의 미세 렌즈 행성: 참고 자료

Dois planetas microlentes através do canal cáustico-planetário: referências

Две микролинзирующие планеты через планетарно-каустический канал: ссылки

Gezegensel-Kostik Kanal Üzerinden İki Mikro Mercekleme Gezegeni: Referanslar

Hai hành tinh vi thấu kính thông qua Kênh ăn da hành tinh: Tài liệu tham khảo

通过行星焦散通道观察两颗微透镜行星：参考文献

Authors:
(1) Youn Kil Jung, Korea Astronomy and Space Science Institute, University of Science and Technology, and The KMTNet Collaboration;
(2) Cheongho Han, Department of Physics, Chungbuk National University and The KMTNet Collaboration;
(3) Andrzej Udalski, Warsaw University Observatory and The OGLE Collaboration;
(4) Andrew Gould, Korea Astronomy and Space Science Institute, Department of Astronomy, Ohio State University, Max-Planck-Institute for Astronomy and The KMTNet Collaboration;
(5) Jennifer C. Yee, Center for Astrophysics | Harvard & Smithsonian and The KMTNet Collaboration;
(6) Michael D. Albrow, University of Canterbury, Department of Physics and Astronomy;
(7) Sun-Ju Chung, Korea Astronomy and Space Science Institute and University of Science and Technology;
(8) Kyu-Ha Hwang, Korea Astronomy and Space Science Institute;
(9) Yoon-Hyun Ryu, Korea Astronomy and Space Science Institute;
(10) In-Gu Shin, Korea Astronomy and Space Science Institute;
(11) Yossi Shvartzvald, Department of Particle Physics and Astrophysics, Weizmann Institute of Science;
(12) Wei Zhu, Canadian Institute for Theoretical Astrophysics, University of Toronto;
(13) Weicheng Zang, Department of Astronomy, Tsinghua University;
(14) Sang-Mok Cha, Korea Astronomy and Space Science Institute and 2School of Space Research, Kyung Hee University;
(15) Dong-Jin Kim, Korea Astronomy and Space Science Institute;
(16) Hyoun-Woo Kim, Korea Astronomy and Space Science Institute;
(17) Seung-Lee Kim, Korea Astronomy and Space Science Institute and University of Science and Technology;
(18) Chung-Uk Lee, Korea Astronomy and Space Science Institute and University of Science and Technology;
(19) Dong-Joo Lee, Korea Astronomy and Space Science Institute;
(20) Yongseok Lee, Korea Astronomy and Space Science Institute and School of Space Research, Kyung Hee University;
(21) Byeong-Gon Park, Korea Astronomy and Space Science Institute and University of Science and Technology;
(22) Richard W. Pogge, Department of Astronomy, Ohio State University;
(23) Przemek Mroz, Warsaw University Observatory and Division of Physics, Mathematics, and Astronomy, California Institute of Technology;
(24) Michal K. Szymanski, Warsaw University Observatory;
(25) Jan Skowron, Warsaw University Observatory;
(26) Radek Poleski, Warsaw University Observatory and Department of Astronomy, Ohio State University;
(27) Igor Soszynski, Warsaw University Observatory;
(28) Pawel Pietrukowicz, Warsaw University Observatory;
(29) Szymon Kozlowski, Warsaw University Observatory;
(30) Krzystof Ulaczyk, Department of Physics, University of Warwick, Gibbet;
(31) Krzysztof A. Rybicki, Warsaw University Observatory;
(32) Patryk Iwanek, Warsaw University Observatory;
(33) Marcin Wrona, Warsaw University Observatory. Table of Links Abstract and Intro
Observation
Light Curve Analysis
Physical Parameters
Microlensing Planets in the (log s, log q) plane
Summary and Conclusions
References 4. Physical Parameters The bulge VD is modeled based on stars in the Gaia catalog (Gaia Collaboration et al. 2016, 2018). That is, we first find red giant stars in the catalog within 2 arcmin centered on the event location. We then derive their mean velocity and its dispersion in Galactocentric Cartesian coordinates (x, y, z) as defined in Han & Gould (1995). This paper is available on arxiv under CC0 1.0 DEED license. Authors: (1) Youn Kil Jung, Korea Astronomy and Space Science Institute, University of Science and Technology, and The KMTNet Collaboration; (2) Cheongho Han, Department of Physics, Chungbuk National University and The KMTNet Collaboration; (3) Andrzej Udalski, Warsaw University Observatory and The OGLE Collaboration; (4) Andrew Gould, Korea Astronomy and Space Science Institute, Department of Astronomy, Ohio State University, Max-Planck-Institute for Astronomy and The KMTNet Collaboration; (5) Jennifer C. Yee, Center for Astrophysics | Harvard & Smithsonian and The KMTNet Collaboration; (6) Michael D. Albrow, University of Canterbury, Department of Physics and Astronomy; (7) Sun-Ju Chung, Korea Astronomy and Space Science Institute and University of Science and Technology; (8) Kyu-Ha Hwang, Korea Astronomy and Space Science Institute; (9) Yoon-Hyun Ryu, Korea Astronomy and Space Science Institute; (10) In-Gu Shin, Korea Astronomy and Space Science Institute; (11) Yossi Shvartzvald, Department of Particle Physics and Astrophysics, Weizmann Institute of Science; (12) Wei Zhu, Canadian Institute for Theoretical Astrophysics, University of Toronto; (13) Weicheng Zang, Department of Astronomy, Tsinghua University; (14) Sang-Mok Cha, Korea Astronomy and Space Science Institute and 2School of Space Research, Kyung Hee University; (15) Dong-Jin Kim, Korea Astronomy and Space Science Institute; (16) Hyoun-Woo Kim, Korea Astronomy and Space Science Institute; (17) Seung-Lee Kim, Korea Astronomy and Space Science Institute and University of Science and Technology; (18) Chung-Uk Lee, Korea Astronomy and Space Science Institute and University of Science and Technology; (19) Dong-Joo Lee, Korea Astronomy and Space Science Institute; (20) Yongseok Lee, Korea Astronomy and Space Science Institute and School of Space Research, Kyung Hee University; (21) Byeong-Gon Park, Korea Astronomy and Space Science Institute and University of Science and Technology; (22) Richard W. Pogge, Department of Astronomy, Ohio State University; (23) Przemek Mroz, Warsaw University Observatory and Division of Physics, Mathematics, and Astronomy, California Institute of Technology; (24) Michal K. Szymanski, Warsaw University Observatory; (25) Jan Skowron, Warsaw University Observatory; (26) Radek Poleski, Warsaw University Observatory and Department of Astronomy, Ohio State University; (27) Igor Soszynski, Warsaw University Observatory; (28) Pawel Pietrukowicz, Warsaw University Observatory; (29) Szymon Kozlowski, Warsaw University Observatory; (30) Krzystof Ulaczyk, Department of Physics, University of Warwick, Gibbet; (31) Krzysztof A. Rybicki, Warsaw University Observatory; (32) Patryk Iwanek, Warsaw University Observatory; (33) Marcin Wrona, Warsaw University Observatory. Authors: Authors: (1) Youn Kil Jung, Korea Astronomy and Space Science Institute, University of Science and Technology, and The KMTNet Collaboration; (2) Cheongho Han, Department of Physics, Chungbuk National University and The KMTNet Collaboration; (3) Andrzej Udalski, Warsaw University Observatory and The OGLE Collaboration; (4) Andrew Gould, Korea Astronomy and Space Science Institute, Department of Astronomy, Ohio State University, Max-Planck-Institute for Astronomy and The KMTNet Collaboration; (5) Jennifer C. Yee, Center for Astrophysics | Harvard & Smithsonian and The KMTNet Collaboration; (6) Michael D. Albrow, University of Canterbury, Department of Physics and Astronomy; (7) Sun-Ju Chung, Korea Astronomy and Space Science Institute and University of Science and Technology; (8) Kyu-Ha Hwang, Korea Astronomy and Space Science Institute; (9) Yoon-Hyun Ryu, Korea Astronomy and Space Science Institute; (10) In-Gu Shin, Korea Astronomy and Space Science Institute; (11) Yossi Shvartzvald, Department of Particle Physics and Astrophysics, Weizmann Institute of Science; (12) Wei Zhu, Canadian Institute for Theoretical Astrophysics, University of Toronto; (13) Weicheng Zang, Department of Astronomy, Tsinghua University; (14) Sang-Mok Cha, Korea Astronomy and Space Science Institute and 2School of Space Research, Kyung Hee University; (15) Dong-Jin Kim, Korea Astronomy and Space Science Institute; (16) Hyoun-Woo Kim, Korea Astronomy and Space Science Institute; (17) Seung-Lee Kim, Korea Astronomy and Space Science Institute and University of Science and Technology; (18) Chung-Uk Lee, Korea Astronomy and Space Science Institute and University of Science and Technology; (19) Dong-Joo Lee, Korea Astronomy and Space Science Institute; (20) Yongseok Lee, Korea Astronomy and Space Science Institute and School of Space Research, Kyung Hee University; (21) Byeong-Gon Park, Korea Astronomy and Space Science Institute and University of Science and Technology; (22) Richard W. Pogge, Department of Astronomy, Ohio State University; (23) Przemek Mroz, Warsaw University Observatory and Division of Physics, Mathematics, and Astronomy, California Institute of Technology; (24) Michal K. Szymanski, Warsaw University Observatory; (25) Jan Skowron, Warsaw University Observatory; (26) Radek Poleski, Warsaw University Observatory and Department of Astronomy, Ohio State University; (27) Igor Soszynski, Warsaw University Observatory; (28) Pawel Pietrukowicz, Warsaw University Observatory; (29) Szymon Kozlowski, Warsaw University Observatory; (30) Krzystof Ulaczyk, Department of Physics, University of Warwick, Gibbet; (31) Krzysztof A. Rybicki, Warsaw University Observatory; (32) Patryk Iwanek, Warsaw University Observatory; (33) Marcin Wrona, Warsaw University Observatory. Table of Links Abstract and Intro Observation Light Curve Analysis Physical Parameters Microlensing Planets in the (log s, log q) plane Summary and Conclusions References Abstract and Intro Abstract and Intro Observation Observation Light Curve Analysis Light Curve Analysis Physical Parameters Physical Parameters Microlensing Planets in the (log s , log q ) plane Microlensing Planets in the (log s s , log q q ) plane Summary and Conclusions Summary and Conclusions References References 4. Physical Parameters The bulge VD is modeled based on stars in the Gaia catalog (Gaia Collaboration et al. 2016, 2018). That is, we first find red giant stars in the catalog within 2 arcmin centered on the event location. We then derive their mean velocity and its dispersion in Galactocentric Cartesian coordinates ( x, y, z ) as defined in Han & Gould (1995). x, y, z This paper is available on arxiv under CC0 1.0 DEED license. This paper is available on arxiv under CC0 1.0 DEED license. available on arxiv

Two Microlensing Planets through Planetary-Caustic Channel: Physical Parameters

প্ল্যানেটারি-কস্টিক চ্যানেলের মাধ্যমে দুটি মাইক্রোলেনসিং গ্রহ: শারীরিক পরামিতি

Zwei Mikrolinsenplaneten durch den planetar-kaustischen Kanal: Physikalische Parameter

Dos planetas microlentes a través del canal cáustico planetario: parámetros físicos

Deux planètes à microlentille via un canal planétaire-caustique : paramètres physiques

ग्रहीय-कास्टिक चैनल के माध्यम से दो माइक्रोलेंसिंग ग्रह: भौतिक पैरामीटर

惑星-コースティックチャンネルを通した2つのマイクロレンズ惑星: 物理的パラメータ

행성 가성 채널을 통한 두 개의 미세 렌즈 행성: 물리적 매개변수

Dois planetas microlentes através do canal cáustico-planetário: parâmetros físicos

Две микролинзирующие планеты через планетарно-каустический канал: физические параметры

Gezegensel-Kostik Kanal Üzerinden İki Mikro Mercekleme Gezegeni: Fiziksel Parametreler

Hai hành tinh vi thấu kính thông qua Kênh ăn da hành tinh: Các thông số vật lý

通过行星焦散通道观察两颗微透镜行星：物理参数

This paper is available on arxiv under CC0 1.0 DEED license.
Authors:
(1) Youn Kil Jung, Korea Astronomy and Space Science Institute, University of Science and Technology, and The KMTNet Collaboration;
(2) Cheongho Han, Department of Physics, Chungbuk National University and The KMTNet Collaboration;
(3) Andrzej Udalski, Warsaw University Observatory and The OGLE Collaboration;
(4) Andrew Gould, Korea Astronomy and Space Science Institute, Department of Astronomy, Ohio State University, Max-Planck-Institute for Astronomy and The KMTNet Collaboration;
(5) Jennifer C. Yee, Center for Astrophysics | Harvard & Smithsonian and The KMTNet Collaboration;
(6) Michael D. Albrow, University of Canterbury, Department of Physics and Astronomy;
(7) Sun-Ju Chung, Korea Astronomy and Space Science Institute and University of Science and Technology;
(8) Kyu-Ha Hwang, Korea Astronomy and Space Science Institute;
(9) Yoon-Hyun Ryu, Korea Astronomy and Space Science Institute;
(10) In-Gu Shin, Korea Astronomy and Space Science Institute;
(11) Yossi Shvartzvald, Department of Particle Physics and Astrophysics, Weizmann Institute of Science;
(12) Wei Zhu, Canadian Institute for Theoretical Astrophysics, University of Toronto;
(13) Weicheng Zang, Department of Astronomy, Tsinghua University;
(14) Sang-Mok Cha, Korea Astronomy and Space Science Institute and 2School of Space Research, Kyung Hee University;
(15) Dong-Jin Kim, Korea Astronomy and Space Science Institute;
(16) Hyoun-Woo Kim, Korea Astronomy and Space Science Institute;
(17) Seung-Lee Kim, Korea Astronomy and Space Science Institute and University of Science and Technology;
(18) Chung-Uk Lee, Korea Astronomy and Space Science Institute and University of Science and Technology;
(19) Dong-Joo Lee, Korea Astronomy and Space Science Institute;
(20) Yongseok Lee, Korea Astronomy and Space Science Institute and School of Space Research, Kyung Hee University;
(21) Byeong-Gon Park, Korea Astronomy and Space Science Institute and University of Science and Technology;
(22) Richard W. Pogge, Department of Astronomy, Ohio State University;
(23) Przemek Mroz, Warsaw University Observatory and Division of Physics, Mathematics, and Astronomy, California Institute of Technology;
(24) Michal K. Szymanski, Warsaw University Observatory;
(25) Jan Skowron, Warsaw University Observatory;
(26) Radek Poleski, Warsaw University Observatory and Department of Astronomy, Ohio State University;
(27) Igor Soszynski, Warsaw University Observatory;
(28) Pawel Pietrukowicz, Warsaw University Observatory;
(29) Szymon Kozlowski, Warsaw University Observatory;
(30) Krzystof Ulaczyk, Department of Physics, University of Warwick, Gibbet;
(31) Krzysztof A. Rybicki, Warsaw University Observatory;
(32) Patryk Iwanek, Warsaw University Observatory;
(33) Marcin Wrona, Warsaw University Observatory. Table of Links Abstract and Intro
Observation
Light Curve Analysis
Physical Parameters
Microlensing Planets in the (log s, log q) plane
Summary and Conclusions
References 2. Observation The two planetary events were observed by the two lensing surveys conducted by the OGLE and KMTNet groups. The OGLE survey uses the 1.3 m telescope that is located at the Las Campanas Observatory in Chile. The KMTNet survey utilizes three 1.6 m telescopes that are located at the Siding Spring Observatory in Australia (KMTA), the Cerro Tololo Interamerican Observatory in Chile (KMTC), and the South African Astronomical Observatory in South Africa (KMTS). The global distribution of the KMTNet telescopes makes it possible to continuously monitor the events. In both surveys, observations were mainly conducted in the I-band, and a fraction of the images were taken in the V -band to determine the color of the microlensed source stars. For both events, the data sets were reduced based on the image subtraction methodology (Tomaney & Crotts 1996; Alard & Lupton 1998), specifically Albrow et al. (2009) for KMTNet and Wo´zniak (2000) for OGLE. The photometric error bars were then readjusted following the prescription presented in Yee et al. (2012). We note that for the source color measurement, we additionally carried out pyDIA (Albrow 2017) reductions for a subset of the KMTNet data, which simultaneously returns the light curve and field-star photometry on the same system. This paper is available on arxiv under CC0 1.0 DEED license. This paper is available on arxiv under CC0 1.0 DEED license. Authors: (1) Youn Kil Jung, Korea Astronomy and Space Science Institute, University of Science and Technology, and The KMTNet Collaboration; (2) Cheongho Han, Department of Physics, Chungbuk National University and The KMTNet Collaboration; (3) Andrzej Udalski, Warsaw University Observatory and The OGLE Collaboration; (4) Andrew Gould, Korea Astronomy and Space Science Institute, Department of Astronomy, Ohio State University, Max-Planck-Institute for Astronomy and The KMTNet Collaboration; (5) Jennifer C. Yee, Center for Astrophysics | Harvard & Smithsonian and The KMTNet Collaboration; (6) Michael D. Albrow, University of Canterbury, Department of Physics and Astronomy; (7) Sun-Ju Chung, Korea Astronomy and Space Science Institute and University of Science and Technology; (8) Kyu-Ha Hwang, Korea Astronomy and Space Science Institute; (9) Yoon-Hyun Ryu, Korea Astronomy and Space Science Institute; (10) In-Gu Shin, Korea Astronomy and Space Science Institute; (11) Yossi Shvartzvald, Department of Particle Physics and Astrophysics, Weizmann Institute of Science; (12) Wei Zhu, Canadian Institute for Theoretical Astrophysics, University of Toronto; (13) Weicheng Zang, Department of Astronomy, Tsinghua University; (14) Sang-Mok Cha, Korea Astronomy and Space Science Institute and 2School of Space Research, Kyung Hee University; (15) Dong-Jin Kim, Korea Astronomy and Space Science Institute; (16) Hyoun-Woo Kim, Korea Astronomy and Space Science Institute; (17) Seung-Lee Kim, Korea Astronomy and Space Science Institute and University of Science and Technology; (18) Chung-Uk Lee, Korea Astronomy and Space Science Institute and University of Science and Technology; (19) Dong-Joo Lee, Korea Astronomy and Space Science Institute; (20) Yongseok Lee, Korea Astronomy and Space Science Institute and School of Space Research, Kyung Hee University; (21) Byeong-Gon Park, Korea Astronomy and Space Science Institute and University of Science and Technology; (22) Richard W. Pogge, Department of Astronomy, Ohio State University; (23) Przemek Mroz, Warsaw University Observatory and Division of Physics, Mathematics, and Astronomy, California Institute of Technology; (24) Michal K. Szymanski, Warsaw University Observatory; (25) Jan Skowron, Warsaw University Observatory; (26) Radek Poleski, Warsaw University Observatory and Department of Astronomy, Ohio State University; (27) Igor Soszynski, Warsaw University Observatory; (28) Pawel Pietrukowicz, Warsaw University Observatory; (29) Szymon Kozlowski, Warsaw University Observatory; (30) Krzystof Ulaczyk, Department of Physics, University of Warwick, Gibbet; (31) Krzysztof A. Rybicki, Warsaw University Observatory; (32) Patryk Iwanek, Warsaw University Observatory; (33) Marcin Wrona, Warsaw University Observatory. This paper is available on arxiv under CC0 1.0 DEED license. Authors: Authors: (1) Youn Kil Jung, Korea Astronomy and Space Science Institute, University of Science and Technology, and The KMTNet Collaboration; (2) Cheongho Han, Department of Physics, Chungbuk National University and The KMTNet Collaboration; (3) Andrzej Udalski, Warsaw University Observatory and The OGLE Collaboration; (4) Andrew Gould, Korea Astronomy and Space Science Institute, Department of Astronomy, Ohio State University, Max-Planck-Institute for Astronomy and The KMTNet Collaboration; (5) Jennifer C. Yee, Center for Astrophysics | Harvard & Smithsonian and The KMTNet Collaboration; (6) Michael D. Albrow, University of Canterbury, Department of Physics and Astronomy; (7) Sun-Ju Chung, Korea Astronomy and Space Science Institute and University of Science and Technology; (8) Kyu-Ha Hwang, Korea Astronomy and Space Science Institute; (9) Yoon-Hyun Ryu, Korea Astronomy and Space Science Institute; (10) In-Gu Shin, Korea Astronomy and Space Science Institute; (11) Yossi Shvartzvald, Department of Particle Physics and Astrophysics, Weizmann Institute of Science; (12) Wei Zhu, Canadian Institute for Theoretical Astrophysics, University of Toronto; (13) Weicheng Zang, Department of Astronomy, Tsinghua University; (14) Sang-Mok Cha, Korea Astronomy and Space Science Institute and 2School of Space Research, Kyung Hee University; (15) Dong-Jin Kim, Korea Astronomy and Space Science Institute; (16) Hyoun-Woo Kim, Korea Astronomy and Space Science Institute; (17) Seung-Lee Kim, Korea Astronomy and Space Science Institute and University of Science and Technology; (18) Chung-Uk Lee, Korea Astronomy and Space Science Institute and University of Science and Technology; (19) Dong-Joo Lee, Korea Astronomy and Space Science Institute; (20) Yongseok Lee, Korea Astronomy and Space Science Institute and School of Space Research, Kyung Hee University; (21) Byeong-Gon Park, Korea Astronomy and Space Science Institute and University of Science and Technology; (22) Richard W. Pogge, Department of Astronomy, Ohio State University; (23) Przemek Mroz, Warsaw University Observatory and Division of Physics, Mathematics, and Astronomy, California Institute of Technology; (24) Michal K. Szymanski, Warsaw University Observatory; (25) Jan Skowron, Warsaw University Observatory; (26) Radek Poleski, Warsaw University Observatory and Department of Astronomy, Ohio State University; (27) Igor Soszynski, Warsaw University Observatory; (28) Pawel Pietrukowicz, Warsaw University Observatory; (29) Szymon Kozlowski, Warsaw University Observatory; (30) Krzystof Ulaczyk, Department of Physics, University of Warwick, Gibbet; (31) Krzysztof A. Rybicki, Warsaw University Observatory; (32) Patryk Iwanek, Warsaw University Observatory; (33) Marcin Wrona, Warsaw University Observatory. Table of Links Abstract and Intro Observation Light Curve Analysis Physical Parameters Microlensing Planets in the (log s, log q) plane Summary and Conclusions References Abstract and Intro Abstract and Intro Observation Observation Light Curve Analysis Light Curve Analysis Physical Parameters Physical Parameters Microlensing Planets in the (log s , log q ) plane Microlensing Planets in the (log s s , log q q ) plane Summary and Conclusions Summary and Conclusions References References 2. Observation The two planetary events were observed by the two lensing surveys conducted by the OGLE and KMTNet groups. The OGLE survey uses the 1.3 m telescope that is located at the Las Campanas Observatory in Chile. The KMTNet survey utilizes three 1.6 m telescopes that are located at the Siding Spring Observatory in Australia (KMTA), the Cerro Tololo Interamerican Observatory in Chile (KMTC), and the South African Astronomical Observatory in South Africa (KMTS). The global distribution of the KMTNet telescopes makes it possible to continuously monitor the events. In both surveys, observations were mainly conducted in the I-band, and a fraction of the images were taken in the V -band to determine the color of the microlensed source stars. For both events, the data sets were reduced based on the image subtraction methodology (Tomaney & Crotts 1996; Alard & Lupton 1998), specifically Albrow et al. (2009) for KMTNet and Wo´zniak (2000) for OGLE. The photometric error bars were then readjusted following the prescription presented in Yee et al. (2012). We note that for the source color measurement, we additionally carried out pyDIA (Albrow 2017) reductions for a subset of the KMTNet data, which simultaneously returns the light curve and field-star photometry on the same system. This paper is available on arxiv under CC0 1.0 DEED license. This paper is available on arxiv under CC0 1.0 DEED license. available on arxiv

Two Microlensing Planets through Planetary-Caustic Channel: Observation

প্ল্যানেটারি-কস্টিক চ্যানেলের মাধ্যমে দুটি মাইক্রোলেনসিং গ্রহ: পর্যবেক্ষণ

Zwei Mikrolinsenplaneten durch den planetar-kaustischen Kanal: Beobachtung

Dos planetas microlentes a través del canal cáustico planetario: observación

Deux planètes à microlentille à travers un canal planétaire-caustique : observation

ग्रहीय-कास्टिक चैनल के माध्यम से दो माइक्रोलेंसिंग ग्रह: अवलोकन

惑星-コースティックチャンネルを通した2つのマイクロレンズ効果を持つ惑星の観測

행성 가성 채널을 통한 두 개의 미세 렌즈 행성: 관측

Dois planetas microlentes através do canal planetário-cáustico: observação

Две микролинзирующие планеты через планетарно-каустический канал: наблюдение

Gezegensel-Kostik Kanal Üzerinden İki Mikro Mercekleyici Gezegen: Gözlem

Hai hành tinh vi thấu kính thông qua Kênh ăn da hành tinh: Quan sát

通过行星焦散通道观察两颗微透镜行星

Two Microlensing Planets through Planetary-Caustic Channel: Abstract and Intro

প্ল্যানেটারি-কস্টিক চ্যানেলের মাধ্যমে দুটি মাইক্রোলেনসিং গ্রহ: বিমূর্ত এবং ভূমিকা

Zwei Mikrolinsenplaneten durch den planetar-kaustischen Kanal: Zusammenfassung und Einführung

Dos planetas microlentes a través del canal planetario-cáustico: resumen e introducción

Deux planètes à microlentille via un canal planétaire-caustique : résumé et introduction

ग्रहीय-कास्टिक चैनल के माध्यम से दो माइक्रोलेंसिंग ग्रह: सार और परिचय

惑星腐食チャネルを通した2つのマイクロレンズ効果を持つ惑星：概要と序論

행성 가성 채널을 통한 두 개의 미세 렌즈 행성: 요약 및 소개

Dois planetas microlentes através do canal planetário-cáustico: resumo e introdução

Две микролинзирующие планеты через планетарно-каустический канал: Аннотация и введение

Gezegensel-Kostik Kanal Üzerinden İki Mikro Mercekleme Gezegeni: Özet ve Giriş

Hai hành tinh vi thấu kính thông qua Kênh ăn da hành tinh: Tóm tắt và giới thiệu

通过行星焦散通道观察两颗微透镜行星：摘要和简介

Off on a Comet! a Journey through Planetary Space by Jules Verne is part of the HackerNoon Books Series. Read this book online for free on HackerNoon! : Off on a Comet! a Journey through Planetary Space Title : Jules Verne Author : June 1, 1998 [eBook #1353] Most recently updated: February 26, 2021 Release date : English Language TABLE OF LINKS INTRODUCTION TO VOLUME NINE BOOK I. CHAPTER I. A CHALLENGE CHAPTER II. CAPTAIN SERVADAC AND HIS ORDERLY CHAPTER III. INTERRUPTED EFFUSIONS CHAPTER IV. A CONVULSION OF NATURE CHAPTER V. A MYSTERIOUS SEA CHAPTER VI. THE CAPTAIN MAKES AN EXPLORATION CHAPTER VII. BEN ZOOF WATCHES IN VAIN CHAPTER VIII. VENUS IN PERILOUS PROXIMITY CHAPTER IX. INQUIRIES UNSATISFIED CHAPTER X. A SEARCH FOR ALGERIA CHAPTER XI. AN ISLAND TOMB CHAPTER XII. AT THE MERCY OF THE WINDS CHAPTER XIII. A ROYAL SALUTE CHAPTER XIV. SENSITIVE NATIONALITY CHAPTER XV. AN ENIGMA FROM THE SEA CHAPTER XVI. THE RESIDUUM OF A CONTINENT CHAPTER XVII. A SECOND ENIGMA CHAPTER XVIII. AN UNEXPECTED POPULATION CHAPTER XIX. GALLIA’S GOVERNOR GENERAL CHAPTER XX. A LIGHT ON THE HORIZON CHAPTER XXI. WINTER QUARTERS CHAPTER XXII. A FROZEN OCEAN CHAPTER XXIII. A CARRIER-PIGEON CHAPTER XXIV. A SLEDGE-RIDE BOOK II. CHAPTER I. THE ASTRONOMER CHAPTER II. A REVELATION CHAPTER III. THE PROFESSOR’S EXPERIENCES CHAPTER IV. A REVISED CALENDAR CHAPTER V. WANTED: A STEELYARD CHAPTER VI. MONEY AT A PREMIUM CHAPTER VII. GALLIA WEIGHED CHAPTER VIII. JUPITER SOMEWHAT CLOSE CHAPTER IX MARKET PRICES IN GALLIA CHAPTER X. FAR INTO SPACE CHAPTER XI. A FETE DAY CHAPTER XII. THE BOWELS OF THE COMET CHAPTER XIII. DREARY MONTHS CHAPTER XIV. THE PROFESSOR PERPLEXED CHAPTER XV. A JOURNEY AND A DISAPPOINTMENT CHAPTER XVI. A BOLD PROPOSITION CHAPTER XVII. THE VENTURE MADE CHAPTER XVIII. SUSPENSE CHAPTER XIX. BACK AGAIN About HackerNoon Book Series: We bring you the most important technical, scientific, and insightful public domain books. This book is part of the public domain. Jules Verne (1998). Off on a Comet! a Journey through Planetary Space. Urbana, Illinois: Project Gutenberg. Retrieved October 2022 https://www.gutenberg.org/cache/epub/1353/pg1353-images.html This eBook is for the use of anyone anywhere at no cost and with almost no restrictions whatsoever. You may copy it, give it away or re-use it under the terms of the Project Gutenberg License included with this eBook or online at , located at . www.gutenberg.org https://www.gutenberg.org/policy/license.html

Off on a Comet! a Journey through Planetary Space by Jules Verne - Table of Links

SPIRAL AND PLANETARY NEBULÆ

A Columbus of Space by Garrett Putman Serviss is part of the HackerNoon Books Series. You can jump to any chapter in this book here . THE PLANETARY LIMITED THE PLANETARY LIMITED But Edmund had seen the meteor sooner than I, and as quick as thought he swerved the car, and threw us all off our feet once more. But we should have been thankful if he had broken our heads, since he had saved us from instant destruction. The danger, however, was not yet passed. Scarcely had the immense dumb-bell (which Edmund declared must have been composed of solid iron, so great was its effect on his needles) disappeared, before there came from outside a blaze so fierce that it fairly slapped our lids shut. "A collision!" Edmund exclaimed. "The thing has struck another big meteor, and they are exchanging fiery compliments." He threw himself flat on the floor, and stared out of the peephole. Then he jumped to his feet and gave us another tumble. "They're all about us," he faltered, breathless with exertion; then, having drawn a deep inspiration, he continued: "We're like a boat in a raging freshet, with rocks, tree trunks, and cakes of ice threatening it on all sides. But we'll get out of it. The car obeys its helm as if it appreciated the danger. Why, I got away from that last fellow by setting up atomic reaction against it, as a boatman pushes with his pole." Even in the midst of our terror we could not but admire our leader. His resources seemed boundless, and our confidence in him grew with every escape. While he kept guard at the peepholes we watched for meteors from the windows. We must have come almost within striking distance of a thousand in the course of an hour, but Edmund decided not to diminish our speed, for he said that he could control the car quicker when it was under full headway. So on we rushed, dodging the things like a crow in a flock of pestering jays, and we really enjoyed the excitement. It was more fascinating sport than shooting rapids in a careening skiff, and at last we grew so confident in the powers of our car and its commander that we were rather sorry when the last meteor passed, and we found ourselves once more in open, unimpeded space. After that the time passed quietly. We ate our meals and went to bed and rose as regularly as if we had been at home. In one respect, however, things were very different from what they were on the earth. We had no night! The sun shone continually, although the sky was black and always glittering with stars. None of us needed to be told by our conductor that this was due to the fact that we no longer had the shadow of the earth to make night for us when the sun was behind it. The sun was now never behind the earth, or any other great opaque body, and when we wished to sleep we made an artificial night, for our special use, by closing all the shutters. And there was no atmosphere about us to diffuse the sunlight, and so to hide the stars. We kept count of the days by the aid of a calendar clock; there seemed to be nothing that Edmund had forgotten. And it was a delightful experience, the wonder of which grew upon us hour by hour. It was too marvelous, too incredible, to be believed, and yet—there we were! Once the idea suddenly came to me that it was astonishing that we had not long ago perished for lack of oxygen. I understood, of course, from what Edmund had said, that the mysterious machines along the wall absorbed the carbonic acid, but we must be constantly using up the oxygen. When I put my difficulty before Edmund he laughed. "That's the easiest thing of all," he said. "Look here." He threw open a little grating. "In there," he continued, "there's an apparatus which manufactures just enough oxygen to keep the air in good condition. It is supplied with materials to last a month, which will be much longer than this expedition will take." "There you are again," exclaimed Jack. "I was asking you about that when we ran into those pesky meteors. What is this expedition? Where are we going, anyway?" "Well," Edmund replied, "since we have become pretty good shipmates, I don't see any objection to telling you. We are going to Venus." "Going to Venus!" we all cried in a breath. "To be sure. Why not? We've got the proper sort of conveyance, haven't we?" There was no denying that. Our conveyance had already brought us some millions of miles out into space; why, indeed, should it not be able to carry us to Venus, or any other planet? "How far is it to Venus?" asked Jack. "When we quit the earth," Edmund answered, "Venus was rapidly approaching inferior conjunction. You know what that is," addressing me, "it's when the planet comes between the sun and the earth. The distance from the earth is not always the same at such a conjunction, but I figured out that on this occasion, after allowing for the circuit we should have to make, there would be just twenty-seven million miles to travel. At an average speed of twenty miles a second we could do that distance in fifteen days, fourteen and one half hours. But, of course, I had to lose some time going slow through the earth's atmosphere, for otherwise the car would have taken fire, like a meteor, on account of the friction. Then, too, I shall have to slow up on entering the atmosphere of Venus, which appears to be very deep and dense; so, upon the whole, I don't count on landing upon Venus in less than sixteen days from the time of our departure. We've already been out five days, and within eleven more I expect to introduce you to the inhabitants of another world." The inhabitants of another world! Again Edmund had thrown out an idea which took us all aback. "Do you believe there are any inhabitants on Venus?" I asked at length. "Certainly. I know there are." "For sure," put in Jack, stretching out his legs and pulling at his pipe. "Who'd go twenty-seven million miles to pay a visit if he didn't know there was somebody at home?" "Then that's what you put the arms aboard for," I remarked. "Yes, but I hope we shall not have to use them." "Strikes me that this is a sort of pirate ship," said Jack. "But what kind of arms have you got, Edmund?" For answer Edmund threw open a locker and showed us a gleaming array of automatic guns and pistols and even some cutlasses. "Decidedly piratical!" exclaimed the incorrigible Jack. "You'd better hoist the black flag. But, see here, Edmund, with all this inter-atomic energy that you talk about, why in the world didn't you invent something new—something that would just knock the Venustians silly, and blow their old planet up if necessary? Automatic arms are pretty good at home, on that unprogressive earth that you have spurned with your heels, but they'll likely be rather small pumpkins on Venus." "I didn't prepare anything else," Edmund replied, "because, in the first place, I was too busy with more important things, and in the second place because I don't really anticipate that we shall have any use for arms. I only took these as a precaution." "You mean to try moral suasion, I suppose," drawled Jack. "Well, anyhow, I hope they'll be glad to see us, and since it is Venus that we are going to visit, I don't look for much fighting. I'm glad you made it Venus instead of Mars, Edmund, for, from all I've heard of Mars with its fourteen-foot giants, I don't think I should like to try the pirate business in that direction." We all laughed at Jack's fancies; but there was something tremendously thrilling in the idea. Think of landing on another world! Think of meeting inhabitants there! Really, it made one's head spin. "Confound it, this is all a dream," I said to myself. "I'm on my back in bed with a nightmare. I'll kick myself awake." But do what I would I could make no dream of it. On the contrary, I felt that I had never been quite so much awake in all my life before. After a while we all settled down to take the thing in earnest. And then the charm of it began to master our imaginations. We talked over the prospects in all their aspects. Edmund said little, and Henry nothing, but Jack and I were stirred to the bottom of our romantic souls. Henry was different. He had no romance in his make-up. He always looked at the money in a thing. To his mind, going to Venus was playing the fool, when we had at our command the means of owning the earth. "Edmund," he said, after mumbling for a while under his breath, "this is the most utter tomfoolery that ever I heard of. Here you've got an invention that would revolutionize mechanics, and instead of utilizing it you rush off into space on a hairbrained adventure. You might have been twenty times a billionaire inside of a year if you had stayed at home and developed the thing. Why, it's folly; pure, beastly folly! Going to Venus! What can you make on Venus?" Edmund only smiled. After a little he said: "Well, I'm sorry for you, Henry. But then you're cut out on the ordinary pattern. But cheer up. When we go back, perhaps I'll let you take out a patent, and you can make the billions. For my part, Venus is more interesting to me than all the money you could pile up between the Atlantic Ocean and the Rocky Mountains. Why," he continued, warming up, and straightening with a certain pride which he had, "am I not the Columbus of Space?—And you my lieutenants," he added, with a smile. "Right you are," cried Jack enthusiastically. "The Columbus of Space, that's the ticket! Where's old Archimedes now? Buried, by Jo! He couldn't go to Venus! And what need we care for your billionaires?" Edmund patted Jack on the back, and I rather sympathized with his enthusiasm myself. The time ran on, and we watched anxiously the day-hand of the calendar clock. Soon it had marked a week; then ten days; then a fortnight. We knew we must be getting very close to our goal, yet up to this time neither Jack, nor Henry, nor I had caught a glimpse of Venus. Edmund, however, had seen it, but he told us that in order to do so he had been obliged to alter our course because the planet was directly in the eye of the sun. In consequence of the change of course we were now approaching Venus from the east—flanking her, so to speak—and Edmund described her appearance as that of an enormous crescent. Finally he invited us to take a look for ourselves. I shall never forget that first view! It was only a glimpse, for Edmund was nervous about meteors again, and would allow us only a moment at the peephole because he wished to be continually on the watch himself. But, brief as was the view, that vast gleaming sickle hanging in the black sky was the most tremendous thing I ever looked upon! Soon afterwards Edmund changed the course again, and then we saw her no more. We had not come upon the swarms of meteors that Edmund had expected to find lurking about the planet, and he said that he now felt safe in running into her shadow, and making a landing on her night hemisphere. You will allow me to remind you that Schiaparelli had long before found out that Venus doesn't turn on her axis once every twenty-four hours, like the earth, but keeps always the same face to the sun; the consequence being that she has perpetual day on one side and perpetual night on the other. I asked Edmund why he should not rather land on the daylight side; but he replied that his plan was safer, and that we could easily go from one side to the other whenever we chose. It didn't turn out to be so easy after all, but that is another part of the story. "I hardly expect to find any inhabitants on the night side," Edmund remarked, "for it must be fearfully cold there—too cold for life to exist, perhaps; but I have provided against that as far as we are concerned. Still, one can never tell. There may be inhabitants there, and at any rate I am going to find out. If there are none, we'll just stop long enough to take a look at things, and then the car will quickly transport us to the daylight hemisphere, where life certainly exists. By landing on the uninhabited side, you see, we shall have a chance to reconnoiter a little, and can approach the inhabitants on the other side so much the more safely." "That sounds all right enough," said Jack, "but if Venus is correctly named, I'm for getting where the inhabitants are as quick as possible." When we swung round into the shadow of the planet we got her between the sun and ourselves, and as she completely hid the sun, we now had perpetual night about the car. Out of the peephole she looked like a stupendous black circle, blacker than the sky itself, but round the rim was a beautiful ring of light. "That's her atmosphere," Edmund explained, "lighted up by the sun from behind. But, for the life of me, I cannot tell what those immense flames mean." He referred to a vast circle of many-colored spires that blazed and flickered like a burning rainbow at the inner edge of the ring of light. It was one of the most awful, and yet beautiful, sights that I had ever gazed upon. "That's something altogether outside my calculations," Edmund added. "I can't account for it at all." "Perhaps they are already celebrating our arrival with fireworks," suggested Jack, always ready to take the humorous view of everything. "That's not fire," Edmund responded earnestly. "But what it is I confess I can't imagine. We'll find out, however, for I haven't come all this distance to be scared off." And here I must try to explain a very curious thing which had puzzled our senses, though not our understanding (because Edmund had promptly explained it), throughout the voyage, and that was—levitation. On our first day out from the earth, we began to notice the remarkable ease with which we handled things, and the strange tendency we had to bump into one another because we seemed to be all the time employing more strength than was necessary and almost to be able to walk on air. Jack declared that he felt as if his head had become a toy balloon. "It's the lack of weight," said Edmund. "Every time we double our distance from the earth we lose another three quarters of our weight. If I had thought to bring along a spring dynamometer, I could have shown you, Jack, that when we were 4,000 miles above the earth's surface the 200 good pounds with which you depress the scales at home had diminished to 50, and that when we had passed about 150,000 miles into space you weighed no more than a couple of ounces. From that point on, it has been the attraction of the sun to which we have owed whatever weight we had, and the floor of the car has been toward the sun, because, at that distance from the earth, the latter ceases to exercise the master force, and the pull of the sun becomes greater than the earth's. But as we approach Venus the latter begins to restore our weight, and when we arrive on her surface we shall weigh about four fifths as much as when we started from the earth." "But I don't look as if I had lost any avoirdupois," said Jack, glancing at his round limbs. "And when you give us a fling I seem to strike pretty hard, though in other respects I confess I do feel a good deal like an angel." "Ah," said Edmund, laughing, "that's the inertia of mass. Your mass is the same, although your weight has almost disappeared. Weight depends upon the distance from the attracting body, but mass is independent of everything." "Do you mean to say that angels are massive?" "They may be as massive as they like provided they keep well away from great centers of gravitation." "But Venus is such a center—then there can't be any angels there." "I hope to find something better than angels," was Edmund's smiling reply. Now, as we drew near to Venus, the truth of Edmund's statements became apparent. We felt that our weight was returning, and our muscular activity sinking back to the normal again. We imagined that every minute we could feel our feet pressing more heavily upon the floor. Our approach was so rapid that the immense black circle grew visibly minute by minute. Soon it was so large that we could no longer see its boundaries through the peephole in the floor. "We're now within a thousand miles," said Edmund, "and must be close to the upper limits of the atmosphere. I'll have to slow down, or else we'll be burnt up by the heat of friction." He proceeded to slow down a little more rapidly than was comfortable. It was jerk after jerk, as he dropped off the power, and put on the brakes, but at last we got down to the speed of a fast express train. Soon we were so close that the surface of the planet became dimly visible, simply from the starlight. We were now settling down very cautiously, and presently we began to notice curious shafts of light which appeared to issue from the ground, as if the surface beneath us had been sprinkled with iron founderies. "Aha!" cried Edmund, "I believe there are inhabitants on this side after all. Those lights don't come from volcanoes. I'm going to make for the nearest one, and we'll soon know what they are." Accordingly we steered for one of the gleaming shafts. It was a thrilling moment, I can tell you—that when we first saw another world than ours under our feet! As we approached the light it threw a pale illumination on the ground around. Everything appeared to be perfectly flat and level. It was like dropping down at night upon a vast prairie. But the features of the landscape were indistinguishable in the gloom. Edmund boldly continued to approach until we were within a hundred feet of the shaft of light, which we could now perceive issued directly from the ground. Suddenly, with the slightest perceptible bump, we touched the soil, and the car came to rest. We had landed on Venus! "It's unquestionably frightfully cold outside," said Edmund, "and we'll now put on these things." He dragged out of one of his many lockers four suits of thick fur garments, and as many pairs of fur gloves, together with caps and shields for the face, leaving only narrow openings for the eyes. When we had got them on we looked like so many Esquimaux. Finally Edmund handed each of us a pair of small automatic pistols, telling us to put them where they would be handy in our side pockets. "Boarders all!" cried the irrepressible Jack. "Pirates, do your duty!" Our preparations being made, we opened the door. The air that rushed in almost hardened us into icicles! "It won't hurt you," said Edmund in a whisper. "It can't be down to absolute zero on account of the dense atmosphere. You'll get used to it in a few minutes. Come on." His whispering gave us a sense of imminent danger, but nevertheless we followed as he led the way straight toward the shaft of light. On nearing it we saw that it came out of an irregularly round hole in the ground. When we got yet nearer we were astonished to see rough steps which led down into the pit. The next instant we were frozen in our tracks! For a moment my heart stopped beating. Standing on the steps, just below the level of the ground, and intently watching us, with eyes as big and luminous as moons, was a creature shaped like a man, but more savage than a gorilla! About HackerNoon Book Series: We bring you the most important technical, scientific, and insightful public domain books. This book is part of the public domain. Garrett Putman Serviss (2005). A Columbus of Space. Urbana, Illinois: Project Gutenberg. Retrieved October 2022 https://www.gutenberg.org/cache/epub/8673/pg8673.html This eBook is for the use of anyone anywhere at no cost and with almost no restrictions whatsoever. You may copy it, give it away or re-use it under the terms of the Project Gutenberg License included with this eBook or online at www.gutenberg.org , located at https://www.gutenberg.org/policy/license.html .

THE PLANETARY LIMITED

Getting started with IPFS, Python, and Jupyter Notebooks And because we’re working in Python, we can take advantage of some of the nice features these bindings afford us, such as helpers functions for adding strings and dicts directly to IPFS: metadata = {"data": "about data"}cid = api.add_json(metadata)# You can also check the public gateway:print(" }".format(cid)) https://ipfs.io/ipfs/{ and then check that our data is actually available via our local peer: import jsonjson.loads(api.cat(cid)) And that’s it for now! At , we use a whole range of IPFS tools to interact with our own data, as well as the growing infrastructure we’re developing to enable secure photo backup and sharing on the distributed web. Come , and jump on the to request early access to a whole new way to control your photos. Textile check us out Textile Photos waitlist Resources A Notebook for the above code, hosted in IPFS, added with Python! The IPFS API Python module(ipfsapi)on GitHub IPFS API reference Another getting started guide A Python Notebook with all sorts of useful code snippets The corresponding blog post to go with the above Notebook

A short trip to Jupyter via the Inter-planetary File System

The Logic of Being: From Illusory Social Content to Future Planetary Ecologies

Ten terrible attempts to make the Inter Planetary File System human-friendly

Design for human and planetary health: a transdisciplinary approach to sustainability

Authors:
(1) Youn Kil Jung, Korea Astronomy and Space Science Institute, University of Science and Technology, and The KMTNet Collaboration;
(2) Cheongho Han, Department of Physics, Chungbuk National University and The KMTNet Collaboration;
(3) Andrzej Udalski, Warsaw University Observatory and The OGLE Collaboration;
(4) Andrew Gould, Korea Astronomy and Space Science Institute, Department of Astronomy, Ohio State University, Max-Planck-Institute for Astronomy and The KMTNet Collaboration;
(5) Jennifer C. Yee, Center for Astrophysics | Harvard & Smithsonian and The KMTNet Collaboration;
(6) Michael D. Albrow, University of Canterbury, Department of Physics and Astronomy;
(7) Sun-Ju Chung, Korea Astronomy and Space Science Institute and University of Science and Technology;
(8) Kyu-Ha Hwang, Korea Astronomy and Space Science Institute;
(9) Yoon-Hyun Ryu, Korea Astronomy and Space Science Institute;
(10) In-Gu Shin, Korea Astronomy and Space Science Institute;
(11) Yossi Shvartzvald, Department of Particle Physics and Astrophysics, Weizmann Institute of Science;
(12) Wei Zhu, Canadian Institute for Theoretical Astrophysics, University of Toronto;
(13) Weicheng Zang, Department of Astronomy, Tsinghua University;
(14) Sang-Mok Cha, Korea Astronomy and Space Science Institute and 2School of Space Research, Kyung Hee University;
(15) Dong-Jin Kim, Korea Astronomy and Space Science Institute;
(16) Hyoun-Woo Kim, Korea Astronomy and Space Science Institute;
(17) Seung-Lee Kim, Korea Astronomy and Space Science Institute and University of Science and Technology;
(18) Chung-Uk Lee, Korea Astronomy and Space Science Institute and University of Science and Technology;
(19) Dong-Joo Lee, Korea Astronomy and Space Science Institute;
(20) Yongseok Lee, Korea Astronomy and Space Science Institute and School of Space Research, Kyung Hee University;
(21) Byeong-Gon Park, Korea Astronomy and Space Science Institute and University of Science and Technology;
(22) Richard W. Pogge, Department of Astronomy, Ohio State University;
(23) Przemek Mroz, Warsaw University Observatory and Division of Physics, Mathematics, and Astronomy, California Institute of Technology;
(24) Michal K. Szymanski, Warsaw University Observatory;
(25) Jan Skowron, Warsaw University Observatory;
(26) Radek Poleski, Warsaw University Observatory and Department of Astronomy, Ohio State University;
(27) Igor Soszynski, Warsaw University Observatory;
(28) Pawel Pietrukowicz, Warsaw University Observatory;
(29) Szymon Kozlowski, Warsaw University Observatory;
(30) Krzystof Ulaczyk, Department of Physics, University of Warwick, Gibbet;
(31) Krzysztof A. Rybicki, Warsaw University Observatory;
(32) Patryk Iwanek, Warsaw University Observatory;
(33) Marcin Wrona, Warsaw University Observatory. Table of Links Abstract and Intro
Observation
Light Curve Analysis
Physical Parameters
Microlensing Planets in the (log s, log q) plane
Summary and Conclusions
References 5. Microlensing Planets in the (log s, log q) plane Our two survey-only microlensing planets are detected from the perturbations caused by the planetary caustics (see Figures 3 and 4). In particular, the planetary perturbation of OGLE-2018-BLG-0567 was generated by a “Hollywood” geometry (Gould 1997), in which the source size contributes strongly to, or dominates, the anomaly cross section relative to the size of the caustic. These detections prove the capability of the high-cadence surveys for detecting planets through the planetary-caustic channel. Only 24 planets are placed outside the near-resonant boundary and 18 planets among them are detected from the perturbations produced by clearly isolated planetary caustics [2]. We find that most of these planetary-caustic planets (12 planets) are found in the Hollywood events and they are located in high-cadence observational fields of the lensing surveys. This proves the capability of the Hollywood strategy of following big stars to find planets (Gould 1997). The majority of the Hollywood planets are located in the region s > 1. This is mainly due to the difference in the size of planetary caustics. For s > 1, there is one four-sided planetary caustic. For s < 1, on the other hand, there are two triangular planetary caustics and each of which size is much smaller than that of s > 1. In addition, the planetary signals from these smaller planetary caustics tends to be more significantly diminished by the finite-source effects (Gould & Gaucherel 1997). As a result, the wide-planetary caustic has a larger effective cross section and therefore higher sensitivity for finding planets. This paper is available on arxiv under CC0 1.0 DEED license. [1] https://exoplanetarchive.ipac.caltech.edu [2] The corresponding planetary-caustic events are OGLE-2005-BLG-390 (Beaulieu et al. 2006), MOAbin-1 (Bennett et al. 2012), OGLE-2006-BLG-109 (Gaudi et al. 2008; Bennett et al. 2010), OGLE2008-BLG-092 (Poleski et al. 2014), MOA-2010-BLG-353 (Rattenbury et al. 2015), MOA-2011-BLG-028 (Skowron et al. 2016), MOA-2012-BLG-006 (Poleski et al. 2017), OGLE-2012-BLG-0838 (Poleski et al. 2020), OGLE-2013-BLG-0341 (Gould et al. 2014), MOA-2013-BLG-605 (Sumi et al. 2016), OGLE-2014- BLG-1722 (Suzuki et al. 2018), OGLE-2016-BLG-0263 (Han et al. 2017), OGLE-2016-BLG-1227 (Han et al. 2020), KMT-2016-BLG-1107 (Hwang et al. 2019), OGLE-2017-BLG-0173 (Hwang et al. 2018), OGLE-2017- BLG-0373 (Skowron et al. 2018), OGLE-2018-BLG-0596 (Jung et al. 2019), and OGLE-2018-BLG-0962 (this work). Authors: (1) Youn Kil Jung, Korea Astronomy and Space Science Institute, University of Science and Technology, and The KMTNet Collaboration; (2) Cheongho Han, Department of Physics, Chungbuk National University and The KMTNet Collaboration; (3) Andrzej Udalski, Warsaw University Observatory and The OGLE Collaboration; (4) Andrew Gould, Korea Astronomy and Space Science Institute, Department of Astronomy, Ohio State University, Max-Planck-Institute for Astronomy and The KMTNet Collaboration; (5) Jennifer C. Yee, Center for Astrophysics | Harvard & Smithsonian and The KMTNet Collaboration; (6) Michael D. Albrow, University of Canterbury, Department of Physics and Astronomy; (7) Sun-Ju Chung, Korea Astronomy and Space Science Institute and University of Science and Technology; (8) Kyu-Ha Hwang, Korea Astronomy and Space Science Institute; (9) Yoon-Hyun Ryu, Korea Astronomy and Space Science Institute; (10) In-Gu Shin, Korea Astronomy and Space Science Institute; (11) Yossi Shvartzvald, Department of Particle Physics and Astrophysics, Weizmann Institute of Science; (12) Wei Zhu, Canadian Institute for Theoretical Astrophysics, University of Toronto; (13) Weicheng Zang, Department of Astronomy, Tsinghua University; (14) Sang-Mok Cha, Korea Astronomy and Space Science Institute and 2School of Space Research, Kyung Hee University; (15) Dong-Jin Kim, Korea Astronomy and Space Science Institute; (16) Hyoun-Woo Kim, Korea Astronomy and Space Science Institute; (17) Seung-Lee Kim, Korea Astronomy and Space Science Institute and University of Science and Technology; (18) Chung-Uk Lee, Korea Astronomy and Space Science Institute and University of Science and Technology; (19) Dong-Joo Lee, Korea Astronomy and Space Science Institute; (20) Yongseok Lee, Korea Astronomy and Space Science Institute and School of Space Research, Kyung Hee University; (21) Byeong-Gon Park, Korea Astronomy and Space Science Institute and University of Science and Technology; (22) Richard W. Pogge, Department of Astronomy, Ohio State University; (23) Przemek Mroz, Warsaw University Observatory and Division of Physics, Mathematics, and Astronomy, California Institute of Technology; (24) Michal K. Szymanski, Warsaw University Observatory; (25) Jan Skowron, Warsaw University Observatory; (26) Radek Poleski, Warsaw University Observatory and Department of Astronomy, Ohio State University; (27) Igor Soszynski, Warsaw University Observatory; (28) Pawel Pietrukowicz, Warsaw University Observatory; (29) Szymon Kozlowski, Warsaw University Observatory; (30) Krzystof Ulaczyk, Department of Physics, University of Warwick, Gibbet; (31) Krzysztof A. Rybicki, Warsaw University Observatory; (32) Patryk Iwanek, Warsaw University Observatory; (33) Marcin Wrona, Warsaw University Observatory. Authors: Authors: (1) Youn Kil Jung, Korea Astronomy and Space Science Institute, University of Science and Technology, and The KMTNet Collaboration; (2) Cheongho Han, Department of Physics, Chungbuk National University and The KMTNet Collaboration; (3) Andrzej Udalski, Warsaw University Observatory and The OGLE Collaboration; (4) Andrew Gould, Korea Astronomy and Space Science Institute, Department of Astronomy, Ohio State University, Max-Planck-Institute for Astronomy and The KMTNet Collaboration; (5) Jennifer C. Yee, Center for Astrophysics | Harvard & Smithsonian and The KMTNet Collaboration; (6) Michael D. Albrow, University of Canterbury, Department of Physics and Astronomy; (7) Sun-Ju Chung, Korea Astronomy and Space Science Institute and University of Science and Technology; (8) Kyu-Ha Hwang, Korea Astronomy and Space Science Institute; (9) Yoon-Hyun Ryu, Korea Astronomy and Space Science Institute; (10) In-Gu Shin, Korea Astronomy and Space Science Institute; (11) Yossi Shvartzvald, Department of Particle Physics and Astrophysics, Weizmann Institute of Science; (12) Wei Zhu, Canadian Institute for Theoretical Astrophysics, University of Toronto; (13) Weicheng Zang, Department of Astronomy, Tsinghua University; (14) Sang-Mok Cha, Korea Astronomy and Space Science Institute and 2School of Space Research, Kyung Hee University; (15) Dong-Jin Kim, Korea Astronomy and Space Science Institute; (16) Hyoun-Woo Kim, Korea Astronomy and Space Science Institute; (17) Seung-Lee Kim, Korea Astronomy and Space Science Institute and University of Science and Technology; (18) Chung-Uk Lee, Korea Astronomy and Space Science Institute and University of Science and Technology; (19) Dong-Joo Lee, Korea Astronomy and Space Science Institute; (20) Yongseok Lee, Korea Astronomy and Space Science Institute and School of Space Research, Kyung Hee University; (21) Byeong-Gon Park, Korea Astronomy and Space Science Institute and University of Science and Technology; (22) Richard W. Pogge, Department of Astronomy, Ohio State University; (23) Przemek Mroz, Warsaw University Observatory and Division of Physics, Mathematics, and Astronomy, California Institute of Technology; (24) Michal K. Szymanski, Warsaw University Observatory; (25) Jan Skowron, Warsaw University Observatory; (26) Radek Poleski, Warsaw University Observatory and Department of Astronomy, Ohio State University; (27) Igor Soszynski, Warsaw University Observatory; (28) Pawel Pietrukowicz, Warsaw University Observatory; (29) Szymon Kozlowski, Warsaw University Observatory; (30) Krzystof Ulaczyk, Department of Physics, University of Warwick, Gibbet; (31) Krzysztof A. Rybicki, Warsaw University Observatory; (32) Patryk Iwanek, Warsaw University Observatory; (33) Marcin Wrona, Warsaw University Observatory. Table of Links Abstract and Intro Observation Light Curve Analysis Physical Parameters Microlensing Planets in the (log s, log q) plane Summary and Conclusions References Abstract and Intro Abstract and Intro Observation Observation Light Curve Analysis Light Curve Analysis Physical Parameters Physical Parameters Microlensing Planets in the (log s , log q ) plane Microlensing Planets in the (log s s , log q q ) plane Summary and Conclusions Summary and Conclusions References References 5. Microlensing Planets in the (log s, log q) plane Our two survey-only microlensing planets are detected from the perturbations caused by the planetary caustics (see Figures 3 and 4). In particular, the planetary perturbation of OGLE-2018-BLG-0567 was generated by a “Hollywood” geometry (Gould 1997), in which the source size contributes strongly to, or dominates, the anomaly cross section relative to the size of the caustic. These detections prove the capability of the high-cadence surveys for detecting planets through the planetary-caustic channel. Only 24 planets are placed outside the near-resonant boundary and 18 planets among them are detected from the perturbations produced by clearly isolated planetary caustics [2]. We find that most of these planetary-caustic planets (12 planets) are found in the Hollywood events and they are located in high-cadence observational fields of the lensing surveys. This proves the capability of the Hollywood strategy of following big stars to find planets (Gould 1997). The majority of the Hollywood planets are located in the region s > 1. This is mainly due to the difference in the size of planetary caustics. For s > 1, there is one four-sided planetary caustic. For s < 1, on the other hand, there are two triangular planetary caustics and each of which size is much smaller than that of s > 1. In addition, the planetary signals from these smaller planetary caustics tends to be more significantly diminished by the finite-source effects (Gould & Gaucherel 1997). As a result, the wide-planetary caustic has a larger effective cross section and therefore higher sensitivity for finding planets. This paper is available on arxiv under CC0 1.0 DEED license. This paper is available on arxiv under CC0 1.0 DEED license. available on arxiv [1] https://exoplanetarchive.ipac.caltech.edu [2] The corresponding planetary-caustic events are OGLE-2005-BLG-390 (Beaulieu et al. 2006), MOAbin-1 (Bennett et al. 2012), OGLE-2006-BLG-109 (Gaudi et al. 2008; Bennett et al. 2010), OGLE2008-BLG-092 (Poleski et al. 2014), MOA-2010-BLG-353 (Rattenbury et al. 2015), MOA-2011-BLG-028 (Skowron et al. 2016), MOA-2012-BLG-006 (Poleski et al. 2017), OGLE-2012-BLG-0838 (Poleski et al. 2020), OGLE-2013-BLG-0341 (Gould et al. 2014), MOA-2013-BLG-605 (Sumi et al. 2016), OGLE-2014- BLG-1722 (Suzuki et al. 2018), OGLE-2016-BLG-0263 (Han et al. 2017), OGLE-2016-BLG-1227 (Han et al. 2020), KMT-2016-BLG-1107 (Hwang et al. 2019), OGLE-2017-BLG-0173 (Hwang et al. 2018), OGLE-2017- BLG-0373 (Skowron et al. 2018), OGLE-2018-BLG-0596 (Jung et al. 2019), and OGLE-2018-BLG-0962 (this work).

Two Microlensing Planets: Microlensing Planets in the (log s, log q) plane

দুটি মাইক্রোলেনসিং প্ল্যানেট: (লগ s, লগ কিউ) সমতলে মাইক্রোলেনসিং গ্রহ

Zwei Mikrolinsenplaneten: Mikrolinsenplaneten in der (log s, log q)-Ebene

Dos planetas con microlentes: planetas con microlentes en el plano (log s, log q)

Deux planètes à microlentille : planètes à microlentille dans le plan (log s, log q)

दो माइक्रोलेंसिंग ग्रह: (लॉग एस, लॉग क्यू) तल में माइक्रोलेंसिंग ग्रह

2つのマイクロレンズ惑星: (log s, log q) 平面におけるマイクロレンズ惑星

두 개의 마이크로렌즈 행성: (log s, log q) 평면의 마이크로렌즈 행성

Dois planetas de microlentes: planetas de microlentes no plano (log s, log q)

Две микролинзирующие планеты: микролинзирующие планеты в плоскости (log s, log q).

İki Mikro Mercekleme Gezegeni: (log s, log q) düzlemindeki Mikro Mercekleme Gezegenleri

Hai hành tinh vi thấu kính: Các hành tinh vi thấu kính trong mặt phẳng (log s, log q)

两个微透镜行星：（log s，log q）平面上的微透镜行星

Authors:
(1) Toshit Jain, Indian Institute of Science Bangalore, India;
(2) Varun Singh, Indian Institute of Science Bangalore, India;
(3) Vijay Kumar Boda, Indian Institute of Science Bangalore, India;
(4) Upkar Singh, Indian Institute of Science Bangalore, India;
(5) Ingrid Hotz, Indian Institute of Science Bangalore, India and Department of Science and Technology (ITN), Linköping University, Norrköping, Sweden;
(6) P. N. Vinayachandran, Indian Institute of Science Bangalore, India;
(7) Vijay Natarajan, Indian Institute of Science Bangalore, India. Table of Links Abstract and Intro
Ocean data
pyParaOcean: Architecture
pyParaOcean: Functionalities
Case study: Bay of Bengal
Conclusion
Acknowledgments and References Abstract Visual analysis is well adopted within the field of oceanography for the analysis of model simulations, detection of different phenomena and events, and tracking of dynamic processes. With increasing data sizes and the availability of multivariate dynamic data, there is a growing need for scalable and extensible tools for visualization and interactive exploration. We describe pyParaOcean, a visualization system that supports several tasks routinely used in the visual analysis of ocean data. The system is available as a plugin to Paraview and is hence able to leverage its distributed computing capabilities and its rich set of generic analysis and visualization functionalities. pyParaOcean provides modules to support different visual analysis tasks specific to ocean data, such as eddy identification and salinity movement tracking. These modules are available as Paraview filters and this seamless integration results in a system that is easy to install and use. A case study on the Bay of Bengal illustrates the utility of the system for the study of ocean phenomena and processes. 1. Introduction Understanding ocean data is paramount to predicting extreme weather events such as hurricanes and tsunamis, better understanding of planetary scale processes like global warming, and sustainably managing and preserving ocean resources and its marine life. Visualizing ocean data is challenging due to the presence of multiple fields and parameters that change with time. Ocean currents are undeniably the biggest factor that maintain the heat balance of the ocean-atmosphere system and affect the movement of minerals and salt. Mesoscale eddies, that span from tens to hundreds of kilometers in diameter and have a lifespan that can range from days to months [RR10], are ubiquitous in the oceans. They play a big role in transporting heat and mass within the oceans [McW08]. They also have a big impact on the ecology of the ocean and on the biogeochemical processes [MJD∗ 99,BNBD∗ 07]. With the strides in collection and generation of ocean data [FD06, Ros89], there is a need for tools that support effective visualization of the data, and are scalable to keep pace with the ever expanding resolutions and sizes of ocean datasets. 1.1. Related work Visualization in oceanography is a challenging area of research due to the rapidly increasing size of data, the heterogeneity and multivariate nature of the data, and the inherent complexity of the ocean phenomena. The use of general purpose analysis and visualization software such as Matlab, Tecplot, AVS, and Paraview is prevalent in the community. However, oceanographers often use tools developed specifically for ocean data, such as Ferret [Fer23], pyFerret [pyF23], and Copernicus MyOcean [myO23]. These specialized tools provide multiple functionalities and produce 2D views of the data. A few software frameworks developed within the visualization community provide 2D and 3D data visualization capabilities. COVE [GSK∗ 08] is a collaborative ocean visualization environment that supports interactive analysis of ocean models over the web. RedSeaAtlas [AGT∗ 19] supports the selection of regions in a 2D map and provides exploratory views of winds, waves, tides, chlorophyll, etc. over the Red Sea. OceanPaths [NL15] is a multivariate data visualization tool that computes pathways tracing ocean currents and supports the plotting of different high-dimensional data along the pathways. This enables the study of correlations between different oceanographic features. An oceanographer’s analysis workflow includes a few common tasks [GSK∗ 08] such as inspection of temperature and salinity distributions and vertical cross sections, compare recently measured salinity data against model data, inspect and analyze current vorticities and circulation based on flow data, and analyze extreme events. Isosurfaces and volume rendering are natural choices for visualization of 3D temperature and salinity distributions [DAN12, PBI04]. However, visualization of the dynamically changing distributions is a challenge. VAPOR [LJP∗ 19] is one of the few tools that provides efficient 3D visualization for oceanography and atmospheric science applications. The VAPOR data collection (VDC) data model supports interactive visual analysis of large data sizes on modern GPUs and commodity hardware. Xie et al. [XLWD19] and Afzal et al. [AHG∗ 19] present surveys of visual analysis methods and tools developed for ocean data. Xie et al. classify the visual analysis tasks into four categories, namely study of different environmental variables, ocean phenomena identification and tracking, discovery of patterns and correlations, and visualization of ensembles and uncertainty. Further, they identify different opportunities and unexplored areas for future work including efficient and scalable methods for data processing and management, identification of features at multiple scales, and immersive platforms. While we recognize the availability of several methods for oceanography visualization, we note that they are often standalone solutions. We aim to leverage the extensive advancement in visualization technology as implemented in Paraview while providing functionalities and views that are specific to ocean data. 1.2. Contributions We present pyParaOcean, a system for interactive exploration and visual analysis of ocean data. The system leverages the power of Paraview [AGL05] to enable scalable visualizations of data available from ocean models while supporting a multitude of tasks and functionalities that are specialized for oceanography. The visualization capabilities of pyParaOcean are available via a seamless integration into Paraview using plugins. Key features of the system include • 3D field visualization to study salinity and temperature distribution with support to display and explore dynamically evolving isovolumes. • Ocean current visualization with a support for different seeding strategies for streamlines and pathlines. • Vertical section views and parallel coordinates plot that support interactive selection and slicing of the data. • Identification and tracking of salinity movement via extraction of surface fronts. • Visualization and tracking of eddy features. • An extensible design that supports incorporation of new functionalities as filters in Paraview. We present the results of an exploration of the Bay of Bengal, performed in collaboration with an oceanographer, as a case study to demonstrate the utility of the system. This paper is available on arxiv under CC 4.0 license. Authors: (1) Toshit Jain, Indian Institute of Science Bangalore, India; (2) Varun Singh, Indian Institute of Science Bangalore, India; (3) Vijay Kumar Boda, Indian Institute of Science Bangalore, India; (4) Upkar Singh, Indian Institute of Science Bangalore, India; (5) Ingrid Hotz, Indian Institute of Science Bangalore, India and Department of Science and Technology (ITN), Linköping University, Norrköping, Sweden; (6) P. N. Vinayachandran, Indian Institute of Science Bangalore, India; (7) Vijay Natarajan, Indian Institute of Science Bangalore, India. Authors: Authors: (1) Toshit Jain, Indian Institute of Science Bangalore, India; (2) Varun Singh, Indian Institute of Science Bangalore, India; (3) Vijay Kumar Boda, Indian Institute of Science Bangalore, India; (4) Upkar Singh, Indian Institute of Science Bangalore, India; (5) Ingrid Hotz, Indian Institute of Science Bangalore, India and Department of Science and Technology (ITN), Linköping University, Norrköping, Sweden; (6) P. N. Vinayachandran, Indian Institute of Science Bangalore, India; (7) Vijay Natarajan, Indian Institute of Science Bangalore, India. Table of Links Abstract and Intro Ocean data pyParaOcean: Architecture pyParaOcean: Functionalities Case study: Bay of Bengal Conclusion Acknowledgments and References Abstract and Intro Abstract and Intro Ocean data Ocean data pyParaOcean: Architecture pyParaOcean: Architecture pyParaOcean: Functionalities pyParaOcean: Functionalities Case study: Bay of Bengal Case study: Bay of Bengal Conclusion Conclusion Acknowledgments and References Acknowledgments and References Abstract Visual analysis is well adopted within the field of oceanography for the analysis of model simulations, detection of different phenomena and events, and tracking of dynamic processes. With increasing data sizes and the availability of multivariate dynamic data, there is a growing need for scalable and extensible tools for visualization and interactive exploration. We describe pyParaOcean, a visualization system that supports several tasks routinely used in the visual analysis of ocean data. The system is available as a plugin to Paraview and is hence able to leverage its distributed computing capabilities and its rich set of generic analysis and visualization functionalities. pyParaOcean provides modules to support different visual analysis tasks specific to ocean data, such as eddy identification and salinity movement tracking. These modules are available as Paraview filters and this seamless integration results in a system that is easy to install and use. A case study on the Bay of Bengal illustrates the utility of the system for the study of ocean phenomena and processes. Visual analysis is well adopted within the field of oceanography for the analysis of model simulations, detection of different phenomena and events, and tracking of dynamic processes. With increasing data sizes and the availability of multivariate dynamic data, there is a growing need for scalable and extensible tools for visualization and interactive exploration. We describe pyParaOcean, a visualization system that supports several tasks routinely used in the visual analysis of ocean data. The system is available as a plugin to Paraview and is hence able to leverage its distributed computing capabilities and its rich set of generic analysis and visualization functionalities. pyParaOcean provides modules to support different visual analysis tasks specific to ocean data, such as eddy identification and salinity movement tracking. These modules are available as Paraview filters and this seamless integration results in a system that is easy to install and use. A case study on the Bay of Bengal illustrates the utility of the system for the study of ocean phenomena and processes. 1. Introduction Understanding ocean data is paramount to predicting extreme weather events such as hurricanes and tsunamis, better understanding of planetary scale processes like global warming, and sustainably managing and preserving ocean resources and its marine life. Visualizing ocean data is challenging due to the presence of multiple fields and parameters that change with time. Ocean currents are undeniably the biggest factor that maintain the heat balance of the ocean-atmosphere system and affect the movement of minerals and salt. Mesoscale eddies, that span from tens to hundreds of kilometers in diameter and have a lifespan that can range from days to months [RR10], are ubiquitous in the oceans. They play a big role in transporting heat and mass within the oceans [McW08]. They also have a big impact on the ecology of the ocean and on the biogeochemical processes [MJD∗ 99,BNBD∗ 07]. With the strides in collection and generation of ocean data [FD06, Ros89], there is a need for tools that support effective visualization of the data, and are scalable to keep pace with the ever expanding resolutions and sizes of ocean datasets. 1.1. Related work Visualization in oceanography is a challenging area of research due to the rapidly increasing size of data, the heterogeneity and multivariate nature of the data, and the inherent complexity of the ocean phenomena. The use of general purpose analysis and visualization software such as Matlab, Tecplot, AVS, and Paraview is prevalent in the community. However, oceanographers often use tools developed specifically for ocean data, such as Ferret [Fer23], pyFerret [pyF23], and Copernicus MyOcean [myO23]. These specialized tools provide multiple functionalities and produce 2D views of the data. A few software frameworks developed within the visualization community provide 2D and 3D data visualization capabilities. COVE [GSK∗ 08] is a collaborative ocean visualization environment that supports interactive analysis of ocean models over the web. RedSeaAtlas [AGT∗ 19] supports the selection of regions in a 2D map and provides exploratory views of winds, waves, tides, chlorophyll, etc. over the Red Sea. OceanPaths [NL15] is a multivariate data visualization tool that computes pathways tracing ocean currents and supports the plotting of different high-dimensional data along the pathways. This enables the study of correlations between different oceanographic features. An oceanographer’s analysis workflow includes a few common tasks [GSK∗ 08] such as inspection of temperature and salinity distributions and vertical cross sections, compare recently measured salinity data against model data, inspect and analyze current vorticities and circulation based on flow data, and analyze extreme events. Isosurfaces and volume rendering are natural choices for visualization of 3D temperature and salinity distributions [DAN12, PBI04]. However, visualization of the dynamically changing distributions is a challenge. VAPOR [LJP∗ 19] is one of the few tools that provides efficient 3D visualization for oceanography and atmospheric science applications. The VAPOR data collection (VDC) data model supports interactive visual analysis of large data sizes on modern GPUs and commodity hardware. Xie et al. [XLWD19] and Afzal et al. [AHG∗ 19] present surveys of visual analysis methods and tools developed for ocean data. Xie et al. classify the visual analysis tasks into four categories, namely study of different environmental variables, ocean phenomena identification and tracking, discovery of patterns and correlations, and visualization of ensembles and uncertainty. Further, they identify different opportunities and unexplored areas for future work including efficient and scalable methods for data processing and management, identification of features at multiple scales, and immersive platforms. While we recognize the availability of several methods for oceanography visualization, we note that they are often standalone solutions. We aim to leverage the extensive advancement in visualization technology as implemented in Paraview while providing functionalities and views that are specific to ocean data. 1.2. Contributions We present pyParaOcean, a system for interactive exploration and visual analysis of ocean data. The system leverages the power of Paraview [AGL05] to enable scalable visualizations of data available from ocean models while supporting a multitude of tasks and functionalities that are specialized for oceanography. The visualization capabilities of pyParaOcean are available via a seamless integration into Paraview using plugins. Key features of the system include • 3D field visualization to study salinity and temperature distribution with support to display and explore dynamically evolving isovolumes. • Ocean current visualization with a support for different seeding strategies for streamlines and pathlines. • Vertical section views and parallel coordinates plot that support interactive selection and slicing of the data. • Identification and tracking of salinity movement via extraction of surface fronts. • Visualization and tracking of eddy features. • An extensible design that supports incorporation of new functionalities as filters in Paraview. We present the results of an exploration of the Bay of Bengal, performed in collaboration with an oceanographer, as a case study to demonstrate the utility of the system. This paper is available on arxiv under CC 4.0 license. This paper is available on arxiv under CC 4.0 license. available on arxiv

pyParaOcean, A System for Visual Analysis of Ocean Data: Abstract and Intro

pyParaOcean, একটি সিস্টেম ফর ভিজ্যুয়াল অ্যানালাইসিস অফ ওশান ডেটা: অ্যাবস্ট্রাক্ট এবং ইন্ট্রো

pyParaOcean, ein System zur visuellen Analyse von Ozeandaten: Zusammenfassung und Einführung

pyParaOcean, un sistema para el análisis visual de datos oceánicos: resumen e introducción

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pyParaOcean、海洋データの視覚的分析システム: 概要と紹介

pyParaOcean, 해양 데이터의 시각적 분석 시스템: 개요 및 소개

pyParaOcean, um sistema para análise visual de dados oceânicos: resumo e introdução

pyParaOcean, Система визуального анализа океанических данных: Краткое содержание и введение

pyParaOcean, Okyanus Verilerinin Görsel Analizi İçin Bir Sistem: Özet ve Giriş

pyParaOcean, Hệ thống phân tích trực quan dữ liệu đại dương: Tóm tắt và giới thiệu

pyParaOcean，海洋数据可视化分析系统：摘要和简介

This paper is available on arxiv under CC 4.0 license.
Authors:
(1) Yici Zhong, Department of Physics, Graduate School of Science, University of Tokyo, Bunkyo-ku, Tokyo 113-0033, Japan;
(2) Kazumi Kashiyama, Research Center for the Early Universe, Graduate School of Science, University of Tokyo, Bunkyo-ku, Tokyo 113-0033, Japan and Kavli Institute for the Physics and Mathematics of the Universe (Kavli IPMU,WPI), The University of Tokyo, Chiba 277-8582, Japan;
(3) Shinsuke Takasao, Department of Earth and Space Science, Graduate School of Science, Osaka University, Toyonaka, Osaka 560-0043, Japan;
(4) Toshikazu Shigeyama, Research Center for the Early Universe (RESCEU), School of Science, The University of Tokyo, 7-3-1 Hongo, Bunkyo-ku, Tokyo 113-0033, Japan and Department of Astronomy, School of Science, The University of Tokyo, 7-3-1 Hongo, Bunkyo-ku, Tokyo 113-0033, Japan;
(5) Kotaro Fujisawa, Research Center for the Early Universe (RESCEU), School of Science, The University of Tokyo, 7-3-1 Hongo, Bunkyo-ku, Tokyo 113-0033, Japan and Department of Liberal Arts, Tokyo University of Technology, Ota-ku, Tokyo 144-0051, Japan. Table of Links Abstract and Intro Setup Result Summary and Discussion Appendix A. Dual Energy Formalism B. Convergence of Results C. Change of the Mass Loss Rate in MHD Regime References REFERENCES Briggs, G. P., Ferrario, L., Tout, C. A., Wickramasinghe, D. T., & Hurley, J. R. 2015, MNRAS, 447, 1713, doi: 10.1093/mnras/stu2539 Bryan, G. L., Norman, M. L., Stone, J. M., Cen, R., & Ostriker, J. P. 1995, Computer Physics Communications, 89, 149, doi: 10.1016/0010-4655(94)00191-4 Bucciantini, N., Thompson, T. A., Arons, J., Quataert, E., & Del Zanna, L. 2006, MNRAS, 368, 1717, doi: 10.1111/j.1365-2966.2006.10217.x Caiazzo, I., Burdge, K. B., Fuller, J., et al. 2021, Nature, 595, 39, doi: 10.1038/s41586-021-03615-y Cheng, S., Cummings, J. D., M´enard, B., & Toonen, S. 2020, ApJ, 891, 160, doi: 10.3847/1538-4357/ab733c Contopoulos, I., & Spitkovsky, A. 2006, ApJ, 643, 1139, doi: 10.1086/501161 Ferreira, J. M. 2000, MNRAS, 316, 647, doi: 10.1046/j.1365-8711.2000.03540.x Garc´ıa-Berro, E., Lor´en-Aguilar, P., Aznar-Sigu´an, G., et al. 2012, ApJ, 749, 25, doi: 10.1088/0004-637X/749/1/25 Gvaramadze, V. V., Gr¨afener, G., Langer, N., et al. 2019, Nature, 569, 684, doi: 10.1038/s41586-019-1216-1 Iben, I., J., & Tutukov, A. V. 1984, ApJS, 54, 335, doi: 10.1086/190932 Iijima, H. 2016, PhD thesis, University of Tokyo, Department of Earth and Planetary Environmental Science Jardine, M., & Collier Cameron, A. 2019, MNRAS, 482, 2853, doi: 10.1093/mnras/sty2872 Kashiyama, K., Fujisawa, K., & Shigeyama, T. 2019, ApJ, 887, 39, doi: 10.3847/1538-4357/ab4e97 Kashiyama, K., Ioka, K., & Kawanaka, N. 2011, PhRvD, 83, 023002, doi: 10.1103/PhysRevD.83.023002 Kashiyama, K., & Murase, K. 2017, ApJL, 839, L3, doi: 10.3847/2041-8213/aa68e1 Kilic, M., Kosakowski, A., Moss, A. G., Bergeron, P., & Conly, A. A. 2021, ApJL, 923, L6, doi: 10.3847/2041-8213/ac3b60 Kirsten, F., Marcote, B., Nimmo, K., et al. 2022, Nature, 602, 585, doi: 10.1038/s41586-021-04354-w Ko, T., Suzuki, H., Kashiyama, K., et al. 2023, arXiv e-prints, arXiv:2304.14669, doi: 10.48550/arXiv.2304.14669 Kremer, K., Piro, A. L., & Li, D. 2021, ApJL, 917, L11, doi: 10.3847/2041-8213/ac13a0 Lu, W., Beniamini, P., & Kumar, P. 2022, MNRAS, 510, 1867, doi: 10.1093/mnras/stab3500 Lykou, F., Parker, Q. A., Ritter, A., et al. 2022, arXiv e-prints, arXiv:2208.03946, doi: 10.48550/arXiv.2208.03946 Matt, S. P., MacGregor, K. B., Pinsonneault, M. H., & Greene, T. P. 2012, ApJL, 754, L26, doi: 10.1088/2041-8205/754/2/L26 Michel, F. C. 1969, ApJ, 158, 727, doi: 10.1086/150233 Miyoshi, T., & Kusano, K. 2005, Journal of Computational Physics, 208, 315, doi: 10.1016/j.jcp.2005.02.017 Nomoto, K., & Iben, I., J. 1985, ApJ, 297, 531, doi: 10.1086/163547 Oskinova, L. M., Gvaramadze, V. V., Gr¨afener, G., Langer, N., & Todt, H. 2020, A&A, 644, L8, doi: 10.1051/0004-6361/202039232 Parker, E. N. 1965, SSRv, 4, 666, doi: 10.1007/BF00216273 Raives, M. J., Coleman, M. S. B., & Thompson, T. A. 2023, arXiv e-prints, arXiv:2302.05462, doi: 10.48550/arXiv.2302.05462 Ritter, A., Parker, Q. 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Authors: (1) Yici Zhong, Department of Physics, Graduate School of Science, University of Tokyo, Bunkyo-ku, Tokyo 113-0033, Japan; (2) Kazumi Kashiyama, Research Center for the Early Universe, Graduate School of Science, University of Tokyo, Bunkyo-ku, Tokyo 113-0033, Japan and Kavli Institute for the Physics and Mathematics of the Universe (Kavli IPMU,WPI), The University of Tokyo, Chiba 277-8582, Japan; (3) Shinsuke Takasao, Department of Earth and Space Science, Graduate School of Science, Osaka University, Toyonaka, Osaka 560-0043, Japan; (4) Toshikazu Shigeyama, Research Center for the Early Universe (RESCEU), School of Science, The University of Tokyo, 7-3-1 Hongo, Bunkyo-ku, Tokyo 113-0033, Japan and Department of Astronomy, School of Science, The University of Tokyo, 7-3-1 Hongo, Bunkyo-ku, Tokyo 113-0033, Japan; (5) Kotaro Fujisawa, Research Center for the Early Universe (RESCEU), School of Science, The University of Tokyo, 7-3-1 Hongo, Bunkyo-ku, Tokyo 113-0033, Japan and Department of Liberal Arts, Tokyo University of Technology, Ota-ku, Tokyo 144-0051, Japan. This paper is available on arxiv under CC 4.0 license. Authors: Authors: (1) Yici Zhong, Department of Physics, Graduate School of Science, University of Tokyo, Bunkyo-ku, Tokyo 113-0033, Japan; (2) Kazumi Kashiyama, Research Center for the Early Universe, Graduate School of Science, University of Tokyo, Bunkyo-ku, Tokyo 113-0033, Japan and Kavli Institute for the Physics and Mathematics of the Universe (Kavli IPMU,WPI), The University of Tokyo, Chiba 277-8582, Japan; (3) Shinsuke Takasao, Department of Earth and Space Science, Graduate School of Science, Osaka University, Toyonaka, Osaka 560-0043, Japan; (4) Toshikazu Shigeyama, Research Center for the Early Universe (RESCEU), School of Science, The University of Tokyo, 7-3-1 Hongo, Bunkyo-ku, Tokyo 113-0033, Japan and Department of Astronomy, School of Science, The University of Tokyo, 7-3-1 Hongo, Bunkyo-ku, Tokyo 113-0033, Japan; (5) Kotaro Fujisawa, Research Center for the Early Universe (RESCEU), School of Science, The University of Tokyo, 7-3-1 Hongo, Bunkyo-ku, Tokyo 113-0033, Japan and Department of Liberal Arts, Tokyo University of Technology, Ota-ku, Tokyo 144-0051, Japan. Table of Links Abstract and Intro Abstract and Intro Setup Setup Result Result Summary and Discussion Summary and Discussion Appendix Appendix A. Dual Energy Formalism A. Dual Energy Formalism B. Convergence of Results B. Convergence of Results C. Change of the Mass Loss Rate in MHD Regime C. Change of the Mass Loss Rate in MHD Regime References References REFERENCES Briggs, G. P., Ferrario, L., Tout, C. A., Wickramasinghe, D. T., & Hurley, J. R. 2015, MNRAS, 447, 1713, doi: 10.1093/mnras/stu2539 Bryan, G. L., Norman, M. L., Stone, J. M., Cen, R., & Ostriker, J. P. 1995, Computer Physics Communications, 89, 149, doi: 10.1016/0010-4655(94)00191-4 Bucciantini, N., Thompson, T. A., Arons, J., Quataert, E., & Del Zanna, L. 2006, MNRAS, 368, 1717, doi: 10.1111/j.1365-2966.2006.10217.x Caiazzo, I., Burdge, K. B., Fuller, J., et al. 2021, Nature, 595, 39, doi: 10.1038/s41586-021-03615-y Cheng, S., Cummings, J. D., M´enard, B., & Toonen, S. 2020, ApJ, 891, 160, doi: 10.3847/1538-4357/ab733c Contopoulos, I., & Spitkovsky, A. 2006, ApJ, 643, 1139, doi: 10.1086/501161 Ferreira, J. M. 2000, MNRAS, 316, 647, doi: 10.1046/j.1365-8711.2000.03540.x Garc´ıa-Berro, E., Lor´en-Aguilar, P., Aznar-Sigu´an, G., et al. 2012, ApJ, 749, 25, doi: 10.1088/0004-637X/749/1/25 Gvaramadze, V. V., Gr¨afener, G., Langer, N., et al. 2019, Nature, 569, 684, doi: 10.1038/s41586-019-1216-1 Iben, I., J., & Tutukov, A. V. 1984, ApJS, 54, 335, doi: 10.1086/190932 Iijima, H. 2016, PhD thesis, University of Tokyo, Department of Earth and Planetary Environmental Science Jardine, M., & Collier Cameron, A. 2019, MNRAS, 482, 2853, doi: 10.1093/mnras/sty2872 Kashiyama, K., Fujisawa, K., & Shigeyama, T. 2019, ApJ, 887, 39, doi: 10.3847/1538-4357/ab4e97 Kashiyama, K., Ioka, K., & Kawanaka, N. 2011, PhRvD, 83, 023002, doi: 10.1103/PhysRevD.83.023002 Kashiyama, K., & Murase, K. 2017, ApJL, 839, L3, doi: 10.3847/2041-8213/aa68e1 Kilic, M., Kosakowski, A., Moss, A. G., Bergeron, P., & Conly, A. A. 2021, ApJL, 923, L6, doi: 10.3847/2041-8213/ac3b60 Kirsten, F., Marcote, B., Nimmo, K., et al. 2022, Nature, 602, 585, doi: 10.1038/s41586-021-04354-w Ko, T., Suzuki, H., Kashiyama, K., et al. 2023, arXiv e-prints, arXiv:2304.14669, doi: 10.48550/arXiv.2304.14669 Kremer, K., Piro, A. L., & Li, D. 2021, ApJL, 917, L11, doi: 10.3847/2041-8213/ac13a0 Lu, W., Beniamini, P., & Kumar, P. 2022, MNRAS, 510, 1867, doi: 10.1093/mnras/stab3500 Lykou, F., Parker, Q. A., Ritter, A., et al. 2022, arXiv e-prints, arXiv:2208.03946, doi: 10.48550/arXiv.2208.03946 Matt, S. P., MacGregor, K. B., Pinsonneault, M. H., & Greene, T. P. 2012, ApJL, 754, L26, doi: 10.1088/2041-8205/754/2/L26 Michel, F. C. 1969, ApJ, 158, 727, doi: 10.1086/150233 Miyoshi, T., & Kusano, K. 2005, Journal of Computational Physics, 208, 315, doi: 10.1016/j.jcp.2005.02.017 Nomoto, K., & Iben, I., J. 1985, ApJ, 297, 531, doi: 10.1086/163547 Oskinova, L. M., Gvaramadze, V. V., Gr¨afener, G., Langer, N., & Todt, H. 2020, A&A, 644, L8, doi: 10.1051/0004-6361/202039232 Parker, E. N. 1965, SSRv, 4, 666, doi: 10.1007/BF00216273 Raives, M. J., Coleman, M. S. B., & Thompson, T. A. 2023, arXiv e-prints, arXiv:2302.05462, doi: 10.48550/arXiv.2302.05462 Ritter, A., Parker, Q. 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Magnetic Wind From a Massive White Dwarf Merger: References

Originally, Bitcoin came to the fore as a potential tool for disrupting the financial system. Despite all criticisms and attacks, it has done exactly that, as evidenced by the launch of Bitcoin Spot ETFs, with a subsequent rise to all-time highs above $70,000. Yet other industries are set for disruption. Content creation has yet to transition to Web3. Think about Amazon Kindle or the mainstream media, which are still centrally owned but command huge budgets and influence. Hollywood and traditional entertainment are losing subscribers and fans, and brands like Marvel and DC are still running on old stories that were created decades ago. Ultimately, people want to release their own stories and be able to make money from their creativity without paying centralized actors. The Content Creation Industry Traditionally, it was incredibly difficult to get a book published. Even J.K Rowling was rejected by twelve different editors before finally getting published, as one of the most popular franchises of all time. She’s now worth over $1 Billion. This difficulty changed a lot with the rise of self-publishing tools, most notably Amazon Kindle and its impressive range of tools for both writing and marketing. Online sites Hackernoon offers a Web 2.5 approach that allows people to publish their views, with neat tools and light moderation. But for a pure experience, the entire network has to be user-powered with fully equitable rewards, and little to no censorship. Users should have the features to create and release content quickly, without third parties. And with multiple revenue options. Innovative Web3 ecosystems like Lightning Works (LW) do precisely this. Artists can create and release their own comics with the help of AI. LW has already released some of its own comics, aiming to start its own franchise with its own heroes, with the help of former Marvel, DC, and Disney artists and executives. It is redefining content creation as we know it, with a user-empowerment focus. This comes at a time when the power of Hollywood is waning and streaming has been shown to be a money-losing way to deliver content.  The world is ready for a new business model, and Web3 can solve this problem. Social Media vs Publishing vs Content Creation It has become a little difficult to delineate between content creation, publishing, and social media. There are new media formats coming to prominence and as users become more empowered, they take on the role of creators and publishers. The publishing industry traditionally referred to the release of books from prestigious firms, as well as the publication from mainstream media outlets (the MSM). But both of these have lost tremendous power, as faith in the MSM wanes and readers now gravitate to online formats. Social media is another form of content creation with more features made available for a variety of self-expression. However, there are many concerns about de-platforming as well as online censorship. Bluesky is a Web3 social media platform that deviated from Twitter. It’s technically an open messaging protocol - users can subscribe to the tags and groups that meet their preferences. In this way, they are effectively becoming their own moderators. Most importantly, creators are independent from platforms, being able to take content and contacts with them. The same theme is reflected in the gaming industry. Hexacore offers self publishing for games developers, with true digital ownership. It provides a hybrid monetization model with both free to play and play to own multiplayer games, and users can create their own in-game characters using AI. Meme Generation: Advanced Communication Evolved Through Web3 Memes, often misunderstood as mere internet jokes, are powerful forms of content creation that have reshaped communication. These cultural symbols harness the ability to convey complex messages and emotions swiftly and effectively. They have gotten a bad reputation due to their degenerative nature. But their power and impact cannot be denied, with huge trading volumes and massive user bases. Wall Street Memes, the Gamestop Saga, Dogecoin and more have risen from ‘mere’ meme status to cultural icons of their respective industries, ‘champions’ of the retail class of consumers, relatable to the extreme in their own right. Veme is a company that realized we still struggle to meaningfully engage communities on larger social platforms that are increasingly becoming ‘pay-to-play’. Their platform is a comprehensive communal video network that empowers creators and audiences alike. Equipped with 'Mira,' their own advanced AI model, VEME transforms how meme content is created and shared online. The AI accesses global RSS feeds, converting trending news into engaging, shareable video memes, enabling creators to respond to cultural pulses in real-time. The Future of Content Creation Will Result In Individual Empowerment Ultimately, people want to have power over their data and how they express themselves. Web3 projects offer a means for this to happen without any centralized intermediaries. The most successful projects will allow their users to create content and get out of the way. Right now, many companies and institutions will reject these Web3 ecosystems much like they rejected J.K Rowling - because there is no ‘market fit’. Yet this is a huge mistake. Content creation and distribution are being completely revised on a planetary scale, with many new concepts such as the tokenized lore of Alien Worlds. The public is crying out for authentic self-expression. They will find a way to express themselves creatively using the most efficient means possible - even if they have to fall a few times along the way. Originally, Bitcoin came to the fore as a potential tool for disrupting the financial system. Despite all criticisms and attacks, it has done exactly that, as evidenced by the launch of Bitcoin Spot ETFs, with a subsequent rise to all-time highs above $70,000. Originally, Bitcoin came to the fore as a potential tool for disrupting the financial system. Despite all criticisms and attacks, it has done exactly that, as evidenced by the launch of Bitcoin Spot ETFs , with a subsequent rise to all-time highs above $70,000. Bitcoin Spot ETFs Bitcoin Spot ETFs Yet other industries are set for disruption. Content creation has yet to transition to Web3. Think about Amazon Kindle or the mainstream media, which are still centrally owned but command huge budgets and influence. Hollywood and traditional entertainment are losing subscribers and fans, and brands like Marvel and DC are still running on old stories that were created decades ago. Ultimately, people want to release their own stories and be able to make money from their creativity without paying centralized actors. The Content Creation Industry Traditionally, it was incredibly difficult to get a book published. Even J.K Rowling was rejected by twelve different editors before finally getting published, as one of the most popular franchises of all time. She’s now worth over $1 Billion. rejected by twelve different editors rejected by twelve twelve different editors This difficulty changed a lot with the rise of self-publishing tools, most notably Amazon Kindle and its impressive range of tools for both writing and marketing. Online sites Hackernoon offers a Web 2.5 approach that allows people to publish their views, with neat tools and light moderation. But for a pure experience, the entire network has to be user-powered with fully equitable rewards, and little to no censorship. Users should have the features to create and release content quickly, without third parties. And with multiple revenue options. Innovative Web3 ecosystems like Lightning Works (LW) do precisely this. Artists can create and release their own comics with the help of AI. LW has already released some of its own comics, aiming to start its own franchise with its own heroes, with the help of former Marvel, DC, and Disney artists and executives. It is redefining content creation as we know it, with a user-empowerment focus. This comes at a time when the power of Hollywood is waning and streaming has been shown to be a money-losing way to deliver content.  The world is ready for a new business model, and Web3 can solve this problem. money-losing money-losing Social Media vs Publishing vs Content Creation It has become a little difficult to delineate between content creation, publishing, and social media. There are new media formats coming to prominence and as users become more empowered, they take on the role of creators and publishers. The publishing industry traditionally referred to the release of books from prestigious firms, as well as the publication from mainstream media outlets (the MSM). But both of these have lost tremendous power, as faith in the MSM wanes and readers now gravitate to online formats. Social media is another form of content creation with more features made available for a variety of self-expression. However, there are many concerns about de-platforming as well as online censorship. Bluesky is a Web3 social media platform that deviated from Twitter. It’s technically an open messaging protocol - users can subscribe to the tags and groups that meet their preferences. In this way, they are effectively becoming their own moderators. Most importantly, creators are independent from platforms, being able to take content and contacts with them. The same theme is reflected in the gaming industry. Hexacore offers self publishing for games developers, with true digital ownership. It provides a hybrid monetization model with both free to play and play to own multiplayer games, and users can create their own in-game characters using AI. Meme Generation: Advanced Communication Evolved Through Web3 Memes, often misunderstood as mere internet jokes, are powerful forms of content creation that have reshaped communication. These cultural symbols harness the ability to convey complex messages and emotions swiftly and effectively. They have gotten a bad reputation due to their degenerative nature. But their power and impact cannot be denied, with huge trading volumes and massive user bases. huge trading volumes huge trading volumes Wall Street Memes, the Gamestop Saga, Dogecoin and more have risen from ‘mere’ meme status to cultural icons of their respective industries, ‘champions’ of the retail class of consumers, relatable to the extreme in their own right. Veme is a company that realized we still struggle to meaningfully engage communities on larger social platforms that are increasingly becoming ‘pay-to-play’. Their platform is a comprehensive communal video network that empowers creators and audiences alike. Equipped with 'Mira,' their own advanced AI model, VEME transforms how meme content is created and shared online. The AI accesses global RSS feeds, converting trending news into engaging, shareable video memes, enabling creators to respond to cultural pulses in real-time. The Future of Content Creation Will Result In Individual Empowerment Ultimately, people want to have power over their data and how they express themselves. Web3 projects offer a means for this to happen without any centralized intermediaries. The most successful projects will allow their users to create content and get out of the way. Right now, many companies and institutions will reject these Web3 ecosystems much like they rejected J.K Rowling - because there is no ‘market fit’. Yet this is a huge mistake. Content creation and distribution are being completely revised on a planetary scale, with many new concepts such as the tokenized lore of Alien Worlds. The public is crying out for authentic self-expression. They will find a way to express themselves creatively using the most efficient means possible - even if they have to fall a few times along the way.

Embracing Change: The Evolution of Content Creation in the Web3 Era

A time is coming when your thoughts will be the only activity you need to get things done. Have you ever been so caught up with work, you don't want to move a muscle? You are not willing to use your voice because you feel the ideas will escape once you do. So, what do you do when you suddenly wish your favorite songs were playing at that moment, but you feel too lazy to pick up your phone or call Siri's attention to turn on your playlist? If only your thoughts could make the orders, right? Here, you are thinking, "Siri, play me 'Easy on Me' by Adele" and seconds later the sound fills your workspace. Then you think, "Nope, too low. Siri, increase the volume to 10", and the volume gets adjusted to suit what’s on your mind perfectly. Your brain alone processes commands without any effort from your mouth. I guess that can be seen as a grand breakthrough in the history of neuroscience—or probably not! Let's find out what this means for the world collectively. What Exactly is Neurocomputing? Neurocomputing is a branch of neuroscience that deals with the examination of brain patterns and activities. It is a subfield of cognitive neuroscience that scientifically studies the biological mechanisms and reactions of the brain to different experiences. The term applies to the process of reading, analyzing, and interpreting brain activities by utilizing brain sensors and an imaging framework to examine how our brain reacts in response to different emotions. This is usually through the use of a Brain-Computer Interface Device. The framework, in this case, is called the "triad,” a 3-step process of emotion-valuation, sensory-motor, and meaning-knowledge evaluation. With the introduction of Al, neuroscientists hit a new milestone with brain activity studies. The Rise of Neurocomputing Would you have ever imagined that one day, the content of your thoughts could be read by devices? Science fiction? Sure! Why not? We see a lot of that. But reality? That's almost impossible (or so we thought). Lie detectors were the most mind readers, but they can never detect what your thoughts are word by word. However, technology always seems to awe us as time progresses because the technology we once thought only existed in movies is right here! The use of brainwave-controlled devices to read minds began with the invention of Electro Encephalogram (EEG) in the 1900s. History has it that the German psychiatrist, Hans Berger, created the in neurosurgery. first EEG brain recording These devices, fitted with sensors, were used mostly to monitor and record a patient's brain activity. When placed on your scalp, the sensors pick up electrical signals produced by the brain, which can be interpreted. Around 2008, consumer-focused EEG became commercialized for public use. and —both tech companies—were among the early players in this scene as they released EEG headsets with the promise to create mind-controlled video games. NeuroSky Emotive Furthermore, it began being tested in other areas besides video games, like how it could be used to control your phone or other activities by companies like and . iBrain Muse Relief from Brain-Computer Interfaces Technology Innovations and advanced companies like Meta and Neuralink notched it up with their research into Brain-Computer Interfaces (BCIs) - a technology that can pick thoughts directly from brain neurons and translate them into words. This technology uses AI algorithms to read brain activity and decode emotions into words. Between 2017 and 2019, Meta began funding . As of March 2022, the funded Nature Neuroscience, UCSF researchers achieved brain-to-text decoding with an average error rate as low as 3% when it was tested with vocabularies of up to 300 words—a huge advancement from previous studies. this technology research into At the same time, Elon Musk's Neuralink is already making a good deal of progress with its flexible ultra-thin threads that can be implanted directly into the brain, enabling the carrier to control their gadgets/devices with their thoughts. This is already being tested on paraplegics. The technology has been very much welcomed by paralytic patients who need to gain a good level of control over their lives again. Neuralink has already begun testing the brain threads on paraplegics. Case Study of Neurocomputing Although this technological concept sounds somewhat new, neurocomputing has been in the research and development stage for years, and test-flight gadgets are already being produced. The possibilities of mind reading and brainwave-controlled gadgets are endless. Scientists continue to look into ways to integrate them into our lives, experimenting across various sectors with the possible use of non-invasive EEG devices and BCIs. Many of these experiments are often procedures aimed at helping the physically and mentally disabled to communicate their needs and gain some control over their lives. The world is not new to cases of patients who can not speak due to sicknesses, paralysis, stroke, or just being born that way. So when, for the first time in history, researchers at the GrapheneX-UTS Human-centric Artificial Intelligence Centre, University of Technology Sydney, invented a portable non-invasive device that could translate thoughts into words, it was seen as a breakthrough in neurocomputing. Breakthrough at the GrapheneX-UTS Human-centric Artificial Intelligence Centre: At the time, though, the accuracy was questionable, but with the initial goal achieved, it would only take more years of developing it to increase its accuracy rating. We already find Meta and Neuralink taking up this task with BCIs and electron threads. Evolving neurocomputing also makes smooth communication possible between humans and machines, be it our gadgets, robots, or prosthetic arms. The history of neurocomputing and brain-controlled devices left a remarkable mark in the FIFA 2014 World Cup when, for the first time, the symbolic kick-off event for the tournament was led and completed by a paraplegic man using an advanced assisted mobility technology—a brain-controlled exoskeleton. The FIFA 2014 World Cup Kick-Off Event: This technology, by , a collaborative invention of over 100 scientists from around the world, made use of a set of non-invasive electrodes to read the brain signals from the paraplegic and transmit them to the lightweight exoskeleton triggering movements that helped the man complete the kick-off successfully. The Walk Again Project In the same year of the FIFA World Cup kick-off event, the director of the Center for Neuromodulation, Ohio State University, Dr. Ali Rezai, performed a on 26-year-old quadriplegic Ian Burkhart. Paralyzed Ian Burkhart Regained Mobility: life-changing surgery The surgery involved implanting a tiny 4 x 4 mm microchip into Burkhart's motor cortex, used alongside an electrical sleeve and purpose-made algorithms. This allowed the sensors to trigger his thoughts to control his hands and fingers while bypassing his damaged spinal cord. It was a success. This is not the only successful brain implant in the history of neurocomputing; a man paralyzed from the shoulders down has also been able to regain control of his paralyzed muscles by bypassing the injured spinal cord with the into his motor cortex. implantation of two aspirin-sized 96-channel electrode arrays EEG devices and BCIs are greatly contributing to improved quality of life for disabled people. Other Notable Strides: But we can't say that brain-controlled and mind-reading devices are only for the sick and disabled. These devices could also be used to carry out other tasks/activities for the good of everyone: BBC and This Place teamed up to create a mind-reading headset to enable its user to control the with their thoughts—goodbye to remote controls. BBC iPlayer A team led by an Associate Professor at the KU-KIST Graduate School of Converging Science and Technology, Korea University, . Suk-Won Hwang, developed E-Glasses This prototype eyeglass is made up of flexible electrode sensors located between the ears and eyes of the wearer. First, the electrodes consist of an EEG to monitor the brain's electrical activity and an ElectroOculogram (EOG) to track eye movements and transmit both from the glasses to a device for processing and interpretation. This glass can be used to monitor the mental health of the wearer, help them control games with their eyes, and turn on and off the sunglasses mode when the wearer needs it. Nissan and NASA are working together to build a self-driving robot car technology called that can read, monitor, and measure a driver's brain activity to know if he/she is alert to drive or not. Mind Sense In an exciting twist of things, in 2013, NASA came up with the crazy idea of using . Together with scientists from the University of Essex, they launched a project to control a virtual spaceship with the mind. BCIs to control planetary rovers A competition was held in 2016 by neuroscientists at the University of Florida, a competition that had pilot flying their drones to the finish line by using their minds. Brain Drone Race And the list goes on and on. But like every other technology and thing that exists, there will always be pros and cons to consider. The Ethical Considerations of Neurocomputing Neurocomputing is a technology that is already transforming lives, especially for paraplegics, who, in many cases, have been able to get robotic body parts that can be controlled with their minds or bypass spinal cord injuries to stimulate their bodies into motion through brain neuron implants. People who couldn't talk can now communicate their feelings and what they want/need and interact through mind-reading gadgets. For everyone else abled people, organizations, and companies that wish to apply these gadgets in their daily lives or their various sectors, it is very much achievable. It can bring "ease" into certain activities and, perhaps, create a more quiet world. However, the implantation of invasive BCIs into the brain involves a surgical procedure that is almost too risky to be considered. The brain is a fragile organ; damage to it can lead to mental abnormalities or even brain death. As such, the risk of brain implants makes this technology far-fetched for fully functional humans. Paraplegics, on the other hand, can wager these procedures because of the quest to have a better quality of life. A delicate situation, but if that is what it takes for them not to be stuck in a static world at the mercy of others, it is worth the risky shot. This is why BCIs by companies like Neuralink and Meta, although envisioned to cater to all and sundry, are more appealing to the paralytic section of the world at the moment. Because of these concerns, scientists are looking back into non-invasive methods of mind reading. Last year, researchers at the , University of Technology Sydney, invented a portable, non-invasive cap-like device that could translate thoughts into words when placed on the head. GrapheneX-UTS Human-centric Artificial Intelligence Centre Additionally, scientists from the University of Texas, Austin, developed to translate the thoughts in one's brain into actual speech by monitoring the brain's activity involving the use of fMRI and Al language models. a non-invasive technique The accuracy of these techniques was average. However, with the intended goal achieved, it would only take more years of development to increase its accuracy. Still, no one wants to walk around carrying a headpiece with cords sticking out, and neither can they carry fMRI machines all day. Hence, there is a need for less obvious, non-intrusive devices or less risky invasive BCIs. While the world can be swamped by Brainwave-controlled devices that read our minds, it poses serious concerns. One day, like every other day, we'll be carrying out activities with silent thoughts all in our heads, but this is the sad part: organizations would be able to read, monitor, store, access, and use these thoughts when needed. As tragic as this sounds, it is already in progress. The thoughts in our brain are currently our only inaccessible assets, our privacy safe, our most intimate thoughts, and our personal identity—no one should be able to access our minds. Data Privacy: But with the recent discoveries and technologies in neuroscience, this intrinsic privacy may be breached sooner than we know, leaving us truly vulnerable to Big Tech companies and organizations. If we lose control of our minds, if any company can spy into our thoughts, what else do we have left of ourselves? Just like we have on the internet, companies would be able to buy and access our brain data for targeted marketing. The first appeal for every product starts with the brain. You may not be able to say it, but you can think it accurately. Imagine advertisers having that exact information just as we feel it; then, they will be able to market their products in a practically irresistible way. Neurocomputing and mind-reading devices would make brain data available on a massive scale, and this is also very detrimental to us. Think about it; aside from compelling advertising, how safe are you? The brain is where all your secrets lie: your passwords, location, investments, amount of money you own, where you saved your assets, etc. A brain data hack would mean a loss too great to bear. The argument of some neuroscientists that the potential for misuse of neurocomputing and mind reading is so great that there needs to be a revamp of the human rights laws to protect us all is valid. Because this technology has what it takes to interfere with our most basic rights, the current laws are not fully equipped to salvage the situation; we need a new "jurisprudence of the mind" for our protection. So, in all, our biggest challenge is privacy and safety! What's the future? A quiet world. Maybe what we need? Or maybe not. Elon Musk and his company, Neuralink, have been at the forefront, pushing the concept of neurocomputing beyond the idea of it being the help for paraplegics only. For Musk, it would take conceptual interactions to a whole new level where words and conversations don't have to be verbalized, just thought. He calls it "consensual telepathy,” a realm where your speech becomes completely unnecessary. You can walk into a room with people conversing but not conversing because their thoughts are flying invisibly between them. Reading that now, it does sound uncanny. What becomes of our speech? Oh! I know what you are thinking, "there would never be a day when our speech isn't needed,” and of course, that's somewhat true. But come to think of it, before the advent of mobile phones, would there have been a day we thought we'd be so glued to these gadgets we'd rarely appreciate physical communication and rather be embedded in virtual conversations? I don't think so. When all you need is your thoughts to perform the most basic activities like ordering a coffee from a cafe, asking your friend to pass you the popcorn at a movie, communicating a proposal to your boss, conversing verbally on a date, etc., you may slowly lose touch of actual words. Almost the same way, we are slowly losing touch with writing on paper because we'd rather type into our computers, tablets, or phones. Well, there's no denying the fact that it sounds pretty interesting, too. You'd never have to say you don't know how to express yourself because your mind will do all the expressing for you where words would have escaped you. The concept of your feelings will flow just as you feel them, and no matter how disgruntled they are, your receiver will get the exact message with the fear, excitement, contempt, and all the fleeting emotions - conveyed just as it is. Also, the advancement of this technology would eliminate the language barrier. Whatever we think can be communicated directly to the recipient in whatever language desired. What neurocomputing proposes for the future is both unsettling and intriguing, but we really can't stop technology from evolving, and neither can we stop the future. We only hope that measures are instituted to mitigate the cons while we hope for the best.

From Science Fiction to Reality: The Promise of Neurocomputing and Brain-Computer Interfaces (BCIs)

কল্পবিজ্ঞান থেকে বাস্তবে: নিউরোকম্পিউটিং এবং ব্রেন-কম্পিউটার ইন্টারফেসের প্রতিশ্রুতি (BCIs)

Von der Science-Fiction zur Realität: Das Versprechen von Neurocomputing und Brain-Computer-Interfaces (BCIs)

De la ciencia ficción a la realidad: la promesa de la neurocomputación y las interfaces cerebro-computadora (BCI)

De la science-fiction à la réalité : la promesse de la neuroinformatique et des interfaces cerveau-ordinateur (BCI)

विज्ञान कथा से वास्तविकता तक: न्यूरोकंप्यूटिंग और मस्तिष्क-कंप्यूटर इंटरफेस (बीसीआई) का वादा

サイエンスフィクションから現実へ: ニューロコンピューティングと脳コンピュータインターフェース (BCI) の可能性

SF에서 현실로: 신경컴퓨팅과 뇌-컴퓨터 인터페이스(BCI)의 전망

Da ficção científica à realidade: a promessa da neurocomputação e das interfaces cérebro-computador (BCIs)

От научной фантастики к реальности: перспективы нейрокомпьютеров и интерфейсов «мозг-компьютер» (BCI)

Bilim Kurgudan Gerçeğe: Nörobilgisayar ve Beyin-Bilgisayar Arayüzlerinin (BCI) Vaadi

Từ khoa học viễn tưởng đến hiện thực: Lời hứa về giao diện máy tính thần kinh và não-máy tính (BCI)

从科幻到现实：神经计算和脑机接口 (BCI) 的前景

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