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Planet42

planet42

The Great Size of Jupiter

* * Achievement unlocked: With more than ‘4 billion’ in total votes -- almost half the population of earth voted for startups! JUST KIDDING! Some companies had a to accumulating their votes. unique approach In 2021, decided to host to highlight the backbone of the future - tech startups! for the first time in forever (make sure you sing it in Anna’s voice), HackerNoon.com Startups of The Year More than 44,000 startups were nominated all across the globe, spanning over 4,553 cities. That’s.Just.Spiffy! To see who is a winner in each respective city, visit and pick a city. The name at the top of the list is the winner. (Compromised awards are under review.) startups.hackernoon.com The will announce the winners per region in their respective cities. Startups Winners Announcement Series We’d like to take a moment here and thank every single person who cast a vote and every single company, both nominated and not nominated yet this year. Furthermore, we thank you for existing and opening more opportunities for the wonders of the future to come. Even if you don’t win anything today, you’ve won something much more valuable - our hearts <3 Okay, sorry for the long introduction. Below are all the Startups Winners: Startups of the Year (SOTY) in Africa Johannesburg, South Africa With more than 900 votes cast, #SOTY calls.... MiBRAND Thank you for connecting businesses and consumers, great job! Lagos, Nigeria With 836 votes in the bag, let’s give it up for... Goodtalent Thanks for helping tech companies build great engineering teams. Cape Town, South Africa Want to learn more about finance and use that knowledge to make better financial decisions? Look no further. Introducing winner of Startups of The Year, Cape Town: Revix With 527 votes cast, it seems like a lot of people have more money in their pockets thanks to . Revix Mahé, Seychelles With around 515 votes cast, #SOTY summons... DAOLaunch Thank you for bridging the gap between investors and startups. Lusaka And the winner for #SOTY in Lusaka is... ComGrow Thanks to them, people here are getting closer to the reality of the digitization of village banking. Nairobi, Kenya With 252 votes cast, UTU came out top as the Startup of The Year. Thanks for building the trust infrastructure of the internet to help businesses and consumers engage and transact in a more reliable way. Yaoundé Accounting for more than 73% of total votes, CamPay won this award fair and square. Thank you for making sending and receiving payments easier between online merchants. Abuja, Nigeria A proud winner in the prestigious capital of Nigeria, Elesaro deserves all the plaudits it gets. is a suite crowdfunding protocol built on BSC, Reward, Equity, Lending & NFT Marketplace. Congratulations! Elesaro Dar Es Salaam, Tanzania Jamii Africa is the name that will always be engraved on the #SOTY trophy. As a mobile micro-health insurance, Jamii Africa has done a great job for the health sector in Tanzania. Kigali, Rwanda Another #SOTY medal in the bag for none other than …wait for it… BAG Innovation BAG Innovation applies Gamification to offer real-time access to experience-based learning for University students in East Africa. Everybody loves playing games, but using games to learn in school is on another level. Gauteng, South Africa And the award goes to... Planet42 Thanks for democratising mobility by enabling people ignored by banks to get access to a personal vehicle through a car subscription service. Once again, congratulations! Port Harcourt, Nigeria Cryptocurrency is the present and the future, as we’ve all come to know. FLITBASE makes these digital assets more accessible to everyone. #SOTY is proud to add you to our Hall of Fame. Cairo, Egypt With 18 votes won out of the 91 cast, it seems there was fierce competition. Congratulations to... SubsBase for winning Startups of The Year. SubsBase allows businesses to manage their subscribers, automate recurring billings, set pricing plans, and monitor subscription KPIs. Tunis, Tunisia Come one, come all! Witness the greatness of yet another wonderful startup in the #SOTY. Thank you... VYND for providing a fully integrated digital platform to help venue owners better serve their customers and grow their businesses. Stellenbosch, South Africa BankTech connects clients to a payment network where it provides a convenient interface to meet various payments needs. You’ve won #SOTY proudly! Pretoria #SOTY acknowledges... Grays Pharmaceuticals Thank you for all you do. Lekki, Nigeria Middletrust provides reliable escrow services in Africa. Congratulations on winning a #SOTY medal. Addis Ababa Thank you... Hello Solar for consistently accelerating sustainable energy solutions, especially for remote communities. With half of the votes cast, you beat the odds. Accra, Ghana UT Bank Ghana provides various commercial banking services to individuals and companies in Ghana. We cannot emphasize enough the importance of financial services to humankind. #SOTY is proud of all you do. Gîza, Egypt Big congratulations to... HOVO for winning this award. Your on-demand mobile app for ordering trucks is truly appreciated! Goma, Democratic Republic of Congo Congratulations for coming out on top of #SOTY, SillonBlue Technologies As an ICT Consulting and SaaS company, SillonBlue Technologies focuses on software and mobile app development, and data collection. Yaba, Nigeria With more than half of the votes cast, this nominee conquered undisputedly. Let’s give it up for... Kuda a no-fee full-service digital bank making banking affordable for all Africans on the planet. Morocco City Almes provides infrastructure and logistics services. Congratulations on earning a #SOTY medal. Dakar ShopMeAway provides families and businesses with new ways to shop around the world with reduced shipping costs. You deserve the plaudits you’ve received! Casablanca Sheaply provides crowd shipping and crowd shopping solutions. This reduces cost and improves efficiency on shipping and shopping. Congratulations on winning a #SOTY medal. Nguru, Nigeria Accounting for 88% of the votes, TradeBuza wins #SOTY almost flawlessly. TradeBuza is a tech-enabled commodities sourcing platform for commodities aggregators and out-grower schemes. Ikeja, Nigeria PropertyPro Nigeria is now pronounced Startup of the Year in Ikeja. Let’s admit, who doesn’t appreciate a platform built to search for real estate properties? Ibadan, Nigeria No Bank, No Problem! (That’s probably not their motto, by the way) Shield Finders is a fintech and financial service provider to the unbanked. Congratulation on winning most of the votes! 6 October City, Egypt Wuilt is a website builder where you can create your own Arabic website in under 5 minutes. Thank you for making this technology accessible to people. One #SOTY medal for you! Algiers The only nominee who outvoted all others, please give it up for... Yassir Thank you for providing convenient transport services using your app. Enugu In an area that usually suffers from inconsistent electricity, Greenage comes to the rescue with their green cape and spandex suit. Greenage Technologies is a Nigerian startup solving electricity problems in Nigeria using solar energy technology. Congrats, Greenage. Abeokuta, Nigeria A government organization creating opportunities for entrepreneurs and the unemployed - no one deserves the title Startup of The Year better than Ogun Innovate Congratulations! Ariana And the award goes to... E-Stores Factory a web platform that helps rent and manage e-shops for enterprises seeking to sell online. Thank you for making the (not a typo) more friendly! e-cosystem Benin City Health really is wealth. MOBicure provides mobile technology solutions for Africa's biggest health problems. Thank you for all you do. From #SOTY with love <3 Centurion GameZBoost offers white label gaming platforms, including online desktop solutions, fully responsive mobile and social platforms. Thank you for making the world a more fun place! Gaborone Augmenta Cyber Security provides services in cyber security, safe data storage, SCADA security, SAP Security, etc. Congratulations on winning 10/10 of the votes. You rock! Garki There can never be enough medical platforms in the world. Congratulations to... Wella Health an operator of a healthcare technology company intended to provide treatments and medicines for malaria. Thank you for all you do! Lilongwe Yellow is a digital platform enabling informal merchants in Africa. #SOTY welcomes you to its hall of fame. Make yourself at home ;) Luanda Access to finance is important for any company or sector to succeed. And no other company deserves the title Startup of The Year more than Deya the first Angolan and PALOP crowdfunding platform that aims to increase access to financing for social impact causes and entrepreneurs. . 10/10 will recommend Mombasa Life can be hard, and so a little humor helps ease these hardships. Congratulations to this political satire puppet show, The XYZ Show for winning #SOTY. Thanks for putting smiles on our faces. Port Louis Town Bet you’ve never heard of a Smartcup. Thanks to Intellicup that exists now, and therefore earns this startup a #SOTY badge.  Intellicup is a unique high-speed beverage dispensing solution with integrated smart technology. While this cup won’t be able to wake you up in the morning, you have to agree that it’s still pretty impressive. Rabat Atlan Space is a startup building AI to autonomously pilot any fixed-wing drone, to monitor and take measures over very large areas. You deserve the #SOTY medal. Réunion Imagine having the power to do ultrasound scans on your handheld device. OSCULT by Oscadi is a handheld ultrasound imaging device interfaced with the Apple iPad. Congratulations on making it into the #SOTY! Somerset West Winning the award fair and square is Sticitt a cashless payment platform that is also aimed at teaching learners at school the basics of finance. The future of the world would be in good hands when our children know how to adequately manage finances. Thank you for saving the world in advance. Thika Flowers make the world a beautiful place to live in. Wilmar Flowers exports summer flowers grown by small and medium-sized farmers from Kenya. Kudos for making the world beautiful, #SOTY is honored to have you in our Hall of Fame. Kampala, Uganda Yo-Waste Limited is an African startup that provides waste, recycling and “smart city” solutions to businesses and governments. Your #SOTY gold medal shines as much as you do <3 Harare, Zimbabwe The world is becoming more and more digital every day. Thanks to companies like Golix that provide services of digital currencies for people in Africa, the digitization of the world is becoming more robust. Freetown Easy Solar is a distribution company making energy, durable goods and financial services affordable and accessible through pay-as-you-go tech. Thumbs up! Kicukiro FOODLINE specializes in non-genetically-modified grocery farming and production lines. Winner Winner Chicken Dinner! #SOTY Goma, Democratic Republic of Congo Startups Nuru is a renewable and environmental company that specializes in the fields of storage micro-grids and solar energy. After racking up all the votes, #SOTY honors you. Abidjan, Côte d'Ivoire Digitech provides a fully integrated and cloud-based InsurTech platform to incumbent insurance companies. You are awesome! Durban Security can never really be enough. We’d like to honor Blue Security the title Startup of The Year, for specializing in the installation and monitoring of intruder detection systems, and in providing armed response services. Ikoyi And the Startup of The year goes to... Winich Farms an Agritech Startup leveraging tech to connect rural farmers to Finance & Market, thus, increasing productivity and cutting post-harvest loss. You rock! Lomé The last recipient of #SOTY in Africa calls for... Gozem a transport technology platform for Francophone West and Central Africa. Thank you for providing a platform for transportation. We are honored to have you! *Winners missing from this list will be added accordingly. More Information If you’re a winner, please answer ! If you’re a reader, participant, just a curious individual, consider answering one of our interviews . this interview here Read the FAQs about or . Startups here here To see all of the winners you may visit , pick any city and view the name that appears at the top. this site If you’re interested in partnering with us, we invite you to look through some of these or reach out to our business department. unique sponsorship options Perhaps creating your very own tickles your fancy or maybe you have a whole new idea for how we can partner! writing contest Thank you to all of our sponsors! We truly appreciate your contribution to the tech world and thus the future! The Startups Awards are sponsored by: , , , , , , , , , , Blockster Brex FreeCodeCamp LaunchDarkly Coil Udacity Udemy Vercel Asia Pacific Transgender Network Bybit Everscale Network This post was written and edited by Kien Dao and Joshua Omale. If you have any questions or concerns or would like to report a discrepancy please email ellen@hackernoon.com.

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Table of Links Abstract and 1. Introduction 2. Methods 2.1. Modeling Panspermia and Terraformation 2.2. Identifying the Presence of Terraformed Planets and 2.3. Software and Availability 3. Results 3.1. Panspermia can increase the correlation between planets’ compositions and positions 3.2. Likely terraformed planets can be identified from clustering 4. Summary and Discussion 5. Acknowledgements and References APPENDIX A. Appendix 2.2. Identifying the Presence of Terraformed Planets 2.2.1. Summary We hypothesize that the process of panspermia and terraformation in our model will lead to a population of planets with anomalously high positive correlations between their spatial locations and compositions, compared to random permutations of these planets’ compositions. We quantify this using the Mantel test—a statistical test common in ecological science (Sec. 2.2.2). By clustering on the planet compositions, we can begin to pin down clusters of planets driving these correlations (Sec. 2.2.3). From these initial clusters, we select those localized in space (via their interquartile range, IQR), because we hypothesize that life would not only change the distribution of planetary compositions, but would also do so in a relatively compact portion of the galaxy. We further select clusters which, when removed, cause a decrease in the Mantel coefficient of the residual space of planets (Sec. 2.2.4). Finally, we attempt to evaluate how well our clusters reflect the presence of truly terraformed planets (Sec. 2.2.5). 2.2.2. Mantel Test The Mantel test is a measure of correlation between two distance matrices. The resulting value is called the Mantel coefficient, and is reported alongside a p-value calculated from an approximate permutation test (indicating the proportion of randomly permuted distance matrices which have correlations greater or equal to the correlation between the non-permuted distance matrices). Simply put, the p-value indicates how unlikely this correlation is compared to random permutations of the data. We wrote the Mantel test in Julia, with the algorithm and code adapted from Python’s scikit-bio (The scikit-bio development team 2020; Rideout et al. 2023). Here we used the Mantel test to measure the Pearson correlation between a distance matrix of all planet positions, and a distance matrix of all planet compositions. For each Mantel coefficient calculation, the p-value was generated using 99 permutations with a 2-sided alternative hypothesis. This is approximately equal to 2.5σ confidence. Because the p-value quantifies how anomalous an observed composition/position association is, given the assumptions of the model that correlations should only occur from panspermia and terraformation, we treat the p-value as one measure of confidence in the space containing a biosignature. To get an idea of how sensitive the Mantel coefficient corresponding to a 2.5σ detection is, we plotted how it varies based on number of planets observed (Fig. A3). We find that the sensitivity of the Mantel coefficient to number of planets observed decreases exponentially, and 1000 planets seems like a reasonable choice to reflect the balance of the challenge of realistically observing planets, with the need for those planets to exhibit potentially small correlations in composition-position space. The exact shape of this plot will vary by model parameters, but is especially dependent on the distribution of planet compositions and positions (e.g., planets being evenly distributed in composition or position space, vs. extremely heterogeneous). 2.2.3. Clustering We clustered planets in each iteration of the simulation based only on their compositions, using the DBSCAN algorithm implemented in R (Hahsler et al. 2019). Briefly, compared to other clustering algorithms, DBSCAN does not require the number of clusters to be predefined, can identify clusters of varying shapes and sizes based on the density of data points in the feature space, and separates points as belonging to clusters or noise. Arguments were chosen based on advice in the documentation, with minPts = 11 (the dimensionality of the data + 1), and eps was chosen dynamically at each iteration based on the location of the elbow in the k-nearest neighbor distance plot. Because the location of the elbow is not always obvious, we used the R implementation of the Kneedle algorithm (Satopaa et al. 2011), with sensitivity parameter = 1, empirically determined based on visual examination of the elbow placement on the nearest neighbor curves (Fig. A4). Note that the sensitivity should be adjusted to the specific data being analyzed, and in our case the data changes at each time step. This results in the Kneedle sensitivity being appropriate for only part of the time steps in our simulation. We chose to focus on the early steps of the simulation, but the sensitivity should be adjusted if finding the curves’ elbows in later time steps. DBSCAN classifies each point (planet) as either being part of a particular cluster, or noise (meaning it does not meet the criteria to fall into a cluster based on our chosen arguments). 2.2.4. Selecting clusters We first sought to select clusters for their likelihood of containing terraformed planets, without the aid of ground truth labels (i.e., without using our knowledge of which planets were truly terraformed in the model). We selected them by measuring their spatial spread, and by analyzing how the Mantel coefficient of the residual space of planets changes when removing clusters of planets. We created a threshold for the spatial spread of the planets in the clusters by taking the average of the interquartile range (IQR, where the middle 50% of planets fall) of all planets across each of the x, y, z dimensions, 2.2.5. Evaluating clustering We evaluated selected clusters meeting our criteria (IQR ≤ 25.2 ∧ MC ≥ 0) for how well they identified terraformed/non-terraformed planets, based on the true labels of each planet throughout our simulation. At each iteration, for each selected cluster, we calculated the ratio of planets in the cluster which were terraformed (true positives, TP) and non-terraformed (false positives, FP), as well as the ratio of planets outside the cluster which were non-terraformed (true negatives, TN) and terraformed (false negatives, FN) (Fig. A13). For example, if 100 of 1000 planets are terraformed, and a single selected cluster is identified with 80 planets, only 75 of which are terraformed, then the ratios for each metric in this cluster are: TP = 75/80, FP = 5/80, TN = 895/920, FN = 25/920. To simplify how this information is conveyed, we report the summary statistics of sensitivity, specificity, and accuracy. • Sensitivity is the proportion of all terraformed planets correctly selected by the cluster, TP/(TP+FN). This is 75/(75 + 25) in our example. • Specificity is the proportion of all non-terraformed planets correctly not selected by the cluster, TN/(TN+FP). This is 895/(895 + 5) in our example. • Accuracy is the proportion of all planets correctly classified, TP+TN/(TP+FP+TN+FN). This is (75 + 895)/1000 in our example. We believe a reliable biosignature must minimize false positives (i.e., must not misclassify non-terraformed planets), even at the expense of producing false negatives (i.e., missing terraformed planets). We thus consider our evaluation to be successful in validating our approach if specificity is high, even if sensitivity is low. 2.3. Software and Availability The code necessary to run the simulations and analyses is available on Github at https://github.com/ hbsmith/SmithSinapayen2024. Simulations were built in Julia, and analyses were carried out in Julia, Python, and R. Authors:
(1) Harrison B. Smith, Earth-Life Science Institute, Tokyo Institute of Technology, Ookayama, Meguro-ku, Tokyo, Japan, and Blue Marble Space Institute of Science, Seattle, Washington, USA (hbs@elsi.jp);
(2) Lana Sinapayen, Sony Computer Science Laboratories, Kyoto, Japan and National Institute for Basic Biology, Okazaki, Japan (lana.sinapayen@gmail.com). This paper is available on arxiv under CC BY-NC-ND 4.0 Deed license. [6] Though the extent we chose for an IQR threshold is arbitrary, it reflects the relative size of our model space and the presumption that looking for life that is still relatively spatially localized is of greater interest than looking for life which has already spread over the galaxy (the latter implying there might be other easier ways to look for life). This choice, like others, could be modified depending on other assumptions or objectives. Table of Links Abstract and 1. Introduction Abstract and 1. Introduction 2. Methods 2.1. Modeling Panspermia and Terraformation 2.1. Modeling Panspermia and Terraformation 2.2. Identifying the Presence of Terraformed Planets and 2.3. Software and Availability 2.2. Identifying the Presence of Terraformed Planets and 2.3. Software and Availability 3. Results 3.1. Panspermia can increase the correlation between planets’ compositions and positions 3.1. Panspermia can increase the correlation between planets’ compositions and positions 3.2. Likely terraformed planets can be identified from clustering 3.2. Likely terraformed planets can be identified from clustering 4. Summary and Discussion 4. Summary and Discussion 5. Acknowledgements and References 5. Acknowledgements and References APPENDIX APPENDIX A. Appendix A. Appendix 2.2. Identifying the Presence of Terraformed Planets 2.2.1. Summary 2.2.1. Summary We hypothesize that the process of panspermia and terraformation in our model will lead to a population of planets with anomalously high positive correlations between their spatial locations and compositions, compared to random permutations of these planets’ compositions. We quantify this using the Mantel test—a statistical test common in ecological science (Sec. 2.2.2). By clustering on the planet compositions, we can begin to pin down clusters of planets driving these correlations (Sec. 2.2.3). From these initial clusters, we select those localized in space (via their interquartile range, IQR), because we hypothesize that life would not only change the distribution of planetary compositions, but would also do so in a relatively compact portion of the galaxy. We further select clusters which, when removed, cause a decrease in the Mantel coefficient of the residual space of planets (Sec. 2.2.4). Finally, we attempt to evaluate how well our clusters reflect the presence of truly terraformed planets (Sec. 2.2.5). 2.2.2. Mantel Test 2.2.2. Mantel Test The Mantel test is a measure of correlation between two distance matrices. The resulting value is called the Mantel coefficient, and is reported alongside a p-value calculated from an approximate permutation test (indicating the proportion of randomly permuted distance matrices which have correlations greater or equal to the correlation between the non-permuted distance matrices). Simply put, the p-value indicates how unlikely this correlation is compared to random permutations of the data. We wrote the Mantel test in Julia, with the algorithm and code adapted from Python’s scikit-bio (The scikit-bio development team 2020; Rideout et al. 2023). Here we used the Mantel test to measure the Pearson correlation between a distance matrix of all planet positions, and a distance matrix of all planet compositions. For each Mantel coefficient calculation, the p-value was generated using 99 permutations with a 2-sided alternative hypothesis. This is approximately equal to 2.5σ confidence. Because the p-value quantifies how anomalous an observed composition/position association is, given the assumptions of the model that correlations should only occur from panspermia and terraformation, we treat the p-value as one measure of confidence in the space containing a biosignature. To get an idea of how sensitive the Mantel coefficient corresponding to a 2.5σ detection is, we plotted how it varies based on number of planets observed (Fig. A3). We find that the sensitivity of the Mantel coefficient to number of planets observed decreases exponentially, and 1000 planets seems like a reasonable choice to reflect the balance of the challenge of realistically observing planets, with the need for those planets to exhibit potentially small correlations in composition-position space. The exact shape of this plot will vary by model parameters, but is especially dependent on the distribution of planet compositions and positions (e.g., planets being evenly distributed in composition or position space, vs. extremely heterogeneous). 2.2.3. Clustering 2.2.3. Clustering We clustered planets in each iteration of the simulation based only on their compositions, using the DBSCAN algorithm implemented in R (Hahsler et al. 2019). Briefly, compared to other clustering algorithms, DBSCAN does not require the number of clusters to be predefined, can identify clusters of varying shapes and sizes based on the density of data points in the feature space, and separates points as belonging to clusters or noise. Arguments were chosen based on advice in the documentation, with minPts = 11 (the dimensionality of the data + 1), and eps was chosen dynamically at each iteration based on the location of the elbow in the k-nearest neighbor distance plot. Because the location of the elbow is not always obvious, we used the R implementation of the Kneedle algorithm (Satopaa et al. 2011), with sensitivity parameter = 1, empirically determined based on visual examination of the elbow placement on the nearest neighbor curves (Fig. A4). Note that the sensitivity should be adjusted to the specific data being analyzed, and in our case the data changes at each time step. This results in the Kneedle sensitivity being appropriate for only part of the time steps in our simulation. We chose to focus on the early steps of the simulation, but the sensitivity should be adjusted if finding the curves’ elbows in later time steps. DBSCAN classifies each point (planet) as either being part of a particular cluster, or noise (meaning it does not meet the criteria to fall into a cluster based on our chosen arguments). 2.2.4. Selecting clusters 2.2.4. Selecting clusters We first sought to select clusters for their likelihood of containing terraformed planets, without the aid of ground truth labels (i.e., without using our knowledge of which planets were truly terraformed in the model). We selected them by measuring their spatial spread, and by analyzing how the Mantel coefficient of the residual space of planets changes when removing clusters of planets. We created a threshold for the spatial spread of the planets in the clusters by taking the average of the interquartile range (IQR, where the middle 50% of planets fall) of all planets across each of the x, y, z dimensions, 2.2.5. Evaluating clustering 2.2.5. Evaluating clustering We evaluated selected clusters meeting our criteria (IQR ≤ 25.2 ∧ MC ≥ 0) for how well they identified terraformed/non-terraformed planets, based on the true labels of each planet throughout our simulation. At each iteration, for each selected cluster, we calculated the ratio of planets in the cluster which were terraformed (true positives, TP) and non-terraformed (false positives, FP), as well as the ratio of planets outside the cluster which were non-terraformed (true negatives, TN) and terraformed (false negatives, FN) (Fig. A13). For example, if 100 of 1000 planets are terraformed, and a single selected cluster is identified with 80 planets, only 75 of which are terraformed, then the ratios for each metric in this cluster are: TP = 75/80, FP = 5/80, TN = 895/920, FN = 25/920. To simplify how this information is conveyed, we report the summary statistics of sensitivity, specificity, and accuracy. • Sensitivity is the proportion of all terraformed planets correctly selected by the cluster, TP/(TP+FN). This is 75/(75 + 25) in our example. • Specificity is the proportion of all non-terraformed planets correctly not selected by the cluster, TN/(TN+FP). This is 895/(895 + 5) in our example. • Accuracy is the proportion of all planets correctly classified, TP+TN/(TP+FP+TN+FN). This is (75 + 895)/1000 in our example. We believe a reliable biosignature must minimize false positives (i.e., must not misclassify non-terraformed planets), even at the expense of producing false negatives (i.e., missing terraformed planets). We thus consider our evaluation to be successful in validating our approach if specificity is high, even if sensitivity is low. 2.3. Software and Availability The code necessary to run the simulations and analyses is available on Github at https://github.com/ hbsmith/SmithSinapayen2024. Simulations were built in Julia, and analyses were carried out in Julia, Python, and R. Authors: (1) Harrison B. Smith, Earth-Life Science Institute, Tokyo Institute of Technology, Ookayama, Meguro-ku, Tokyo, Japan, and Blue Marble Space Institute of Science, Seattle, Washington, USA (hbs@elsi.jp); (2) Lana Sinapayen, Sony Computer Science Laboratories, Kyoto, Japan and National Institute for Basic Biology, Okazaki, Japan (lana.sinapayen@gmail.com). Authors: Authors: (1) Harrison B. Smith, Earth-Life Science Institute, Tokyo Institute of Technology, Ookayama, Meguro-ku, Tokyo, Japan, and Blue Marble Space Institute of Science, Seattle, Washington, USA ( hbs@elsi.jp ); hbs@elsi.jp (2) Lana Sinapayen, Sony Computer Science Laboratories, Kyoto, Japan and National Institute for Basic Biology, Okazaki, Japan ( lana.sinapayen@gmail.com ). lana.sinapayen@gmail.com This paper is available on arxiv under CC BY-NC-ND 4.0 Deed license. This paper is available on arxiv under CC BY-NC-ND 4.0 Deed license. available on arxiv [6] Though the extent we chose for an IQR threshold is arbitrary, it reflects the relative size of our model space and the presumption that looking for life that is still relatively spatially localized is of greater interest than looking for life which has already spread over the galaxy (the latter implying there might be other easier ways to look for life). This choice, like others, could be modified depending on other assumptions or objectives.

A Biosignature Based on Modeling Panspermia and Terraformation: Identifying Terraformed Planets

It can appear that the world at large is facing a litany of irresolvable issues. Cost of living crises, natural disasters, 40-year inflation highs, huge interest rates, unaffordable rent, the Ukraine war, AI-based employment fears, privacy intrusions, viruses, increasing disease rates, declining social security funds, online censorship, and more. Yet all of this can be easily simplified into ONE, critical issue: FINANCE. It is through finance that the government and other actors are empowered to make (secret) decisions that are clearly detrimental to those who were fooled into supporting them. Money printing is the source of problems, and printed money is mainly used to buy government treasury bonds, propping up a fraudulent system. Closely tied in with financial control are KYC procedures, which have proven increasingly invasive and with very little justification. There is no intrinsic reason that sensitive information should be uploaded just for making payments, as this treats people like criminals before any suggestion of wrongdoing. Bitcoin swiftly addresses all of this. A Brief BTC History On the Bitcoin Genesis Block were imprinted the words “The Times 03/Jan/2009. Chancellor on brink of second bailout for banks.”. This was a clear reference to the fact that Bitcoin was needed as an alternative to the fiat system. Satoshi Nakamoto laid the groundwork for an ongoing financial revolution with a very coherent message. Since 2009, little has changed. If anything, the use case for Bitcoin is even more relevant, and central banks have increased their powers.  We are still in a position where we need a globally recognized alternative to printed fiat money to help world citizens. I previously wrote about the importance of a global constitution and one world nation, which is the only viable path forward. In the meantime, the MSM spent a solid 12+ years making up false narratives about Bitcoin. They said it was a Ponzi scheme. They said it used up too much energy. They said it would die off within a few years. They said it was used to launder money by ‘terrorists’, an often used and ill-defined term. And they never retracted a single one of their statements. They consistently made such statements while propping up a system with remarkable similarities to a Ponzi scheme, which is used to launch wars and surveillance operations, through a highly fraudulent banking system that has a proven track record of billion-dollar money laundering. Why Bitcoin For Planetary Sovereignty? Aside from attacks that were designed specifically to discredit Bitcoin on false premises, there were, at one time, legitimate concerns. Many cited the fact that Bitcoin’s PoW consensus mechanism was slow, high-cost, and inefficient. Yet all these concerns have been dealt with through numerous L2s such as Rootstock, Stacks, and Lightning Network. Rootstock

Stacks

Lightning Network



EVM Compatible

Yes

No

No



Micro Payments

Yes

Yes

Yes



Type

Ethereum Sidechain

Independent Blockchain

State Channel



Mining

Merged Mining

PoX

NA



Native Token

RBTC

STX

NA With the possible exception of Monero, Bitcoin is the only cryptocurrency that is truly decentralized in terms of its servers and its founders. Nobody knows who founded Bitcoin and there has even been a server launched into outer space. It has the highest adoption rates and is the most well-known. Of course, it also has the largest market cap and trade volume. Bitcoin is one of the few crypto movements that can be said to be purely grassroots and people-powered, with no initial investment, no marketing, and no vested interests. It’s why world governments and central banks hate it so much - there are no founders or investors to harass and target. It’s a truly anti-fragile technology that gets stronger the more it is attacked. Bitcoin Adoption Levels Bitcoin adoption levels are through the roof and have been helped hugely by irresponsible government spending, lockdowns, privacy intrusions, and frustrating social policies. It is becoming popular both in countries with large numbers of unbanked as well as in developed countries with draconian regulatory procedures. Remember, we are still in the early days of Bitcoin adoption and it has much more room for growth. The globe at large is slowly, if reluctantly, waking up to the fact that fiat-based governments act in a way that is indistinguishable from the threats they say they are protecting us from. Thankfully, this trend of alertness is accelerating and pushing people towards Bitcoin. The following are some inspiring adoption facts relevant to Bitcoin: The government of El Salvador has adopted Bitcoin as a legal tender and made huge profits doing so, despite much criticism. The Central African Republic has done the same. Small towns in South Africa have integrated Bitcoin as an accepted means of payment. Other areas include Bitcoin Beach in El Salvador.


Special Economic Zones (SEVs) such as Prospera in Honduras have a 5% tax rate and are based on decentralization and bitcoin-based capital.


Social media sites like Substack and Twitter (X) have integrated Bitcoin’s Lightning Network as a means of payment. Paxful also accepts Lightning Network payments, as does McDonalds’ and Walmart. In terms of on-chain metrics, active wallet addresses are nearing all-time highs, and the price is widely expected to hit $100,000 by 2025. A Bitcoin ETF was recently approved by the SEC. At the time of writing, there are over 32,000 Bitcoin ATMs in the US alone. Attitude is Everything An uplifting idiom that is often heard among BTC proponents is to “stay humble, stack satoshis”. This is the needed attitude to have, not mindless profit-taking driven by 100x returns and a mindless meme frenzy. It’s about financial equality and the creation of a new economy built on trust, transparency, and liberty, the polar opposite of the existing fiat ecosystem. With L2s like Rootstock, LW, and Stacks rendering moot most prior criticisms of Bitcoin, we are all set to take back the financial economy through the only crypto that has ever mattered: Bitcoin Business owners should be encouraged, across the world, to do their part and accept BTC for payment. Not as a means of taking profits on Bitcoin holding, but so it becomes an accepted norm for payment transactions. This will lead to liberated financial markets, known as KYC-free Bitcoin Circular Economies. Despite decades of propaganda, the truth is that Bitcoin is the PERFECT solution to a broken financial system and the only thing needed is usage and adoption. It’s low-cost, scalable, fast, and iconic. It’s also more than capable of handling large transaction volumes and will help to alleviate a world under siege by inept politicians and corrupt central banks. The rate of Bitcoin adoption across the globe might be the best metric we have to measure individual liberties. It can appear that the world at large is facing a litany of irresolvable issues. Cost of living crises, natural disasters, 40-year inflation highs , huge interest rates, unaffordable rent, the Ukraine war, AI-based employment fears, privacy intrusions, viruses, increasing disease rates, declining social security funds, online censorship, and more. 40-year inflation highs Yet all of this can be easily simplified into ONE, critical issue: FINANCE. It is through finance that the government and other actors are empowered to make (secret) decisions that are clearly detrimental to those who were fooled into supporting them. Money printing is the source of problems, and printed money is mainly used to buy government treasury bonds, propping up a fraudulent system. Closely tied in with financial control are KYC procedures, which have proven increasingly invasive and with very little justification. There is no intrinsic reason that sensitive information should be uploaded just for making payments, as this treats people like criminals before any suggestion of wrongdoing. Bitcoin swiftly addresses all of this. Closely tied in with financial control are KYC procedures, which have proven increasingly invasive and with very little justification. There is no intrinsic reason that sensitive information should be uploaded just for making payments, as this treats people like criminals before any suggestion of wrongdoing. Bitcoin swiftly addresses all of this. A Brief BTC History A Brief BTC History On the Bitcoin Genesis Block were imprinted the words “The Times 03/Jan/2009. Chancellor on brink of second bailout for banks.”. This was a clear reference to the fact that Bitcoin was needed as an alternative to the fiat system. Satoshi Nakamoto laid the groundwork for an ongoing financial revolution with a very coherent message. “The Times 03/Jan/2009. Chancellor on brink of second bailout for banks.”. Since 2009, little has changed. If anything, the use case for Bitcoin is even more relevant, and central banks have increased their powers.  We are still in a position where we need a globally recognized alternative to printed fiat money to help world citizens. I previously wrote about the importance of a global constitution and one world nation, which is the only viable path forward. Bitcoin the importance of a global constitution In the meantime, the MSM spent a solid 12+ years making up false narratives about Bitcoin. They said it was a Ponzi scheme. They said it used up too much energy. They said it would die off within a few years. They said it was used to launder money by ‘terrorists’, an often used and ill-defined term. And they never retracted a single one of their statements. a single one They consistently made such statements while propping up a system with remarkable similarities to a Ponzi scheme, which is used to launch wars and surveillance operations, through a highly fraudulent banking system that has a proven track record of billion-dollar money laundering. proven billion-dollar money laundering. Why Bitcoin For Planetary Sovereignty? Why Bitcoin For Planetary Sovereignty? Aside from attacks that were designed specifically to discredit Bitcoin on false premises, there were, at one time, legitimate concerns. Many cited the fact that Bitcoin’s PoW consensus mechanism was slow, high-cost, and inefficient. Yet all these concerns have been dealt with through numerous L2s such as Rootstock, Stacks, and Lightning Network. Rootstock

Stacks

Lightning Network



EVM Compatible

Yes

No

No



Micro Payments

Yes

Yes

Yes



Type

Ethereum Sidechain

Independent Blockchain

State Channel



Mining

Merged Mining

PoX

NA



Native Token

RBTC

STX

NA Rootstock

Stacks

Lightning Network EVM Compatible

Yes

No

No Micro Payments

Yes

Yes

Yes Type

Ethereum Sidechain

Independent Blockchain

State Channel Mining

Merged Mining

PoX

NA Native Token

RBTC

STX

NA Rootstock Stacks Lightning Network Rootstock Rootstock Stacks Stacks Lightning Network Lightning Network EVM Compatible Yes No No EVM Compatible EVM Compatible Yes Yes No No No No Micro Payments Yes Yes Yes Micro Payments Micro Payments Yes Yes Yes Yes Yes Yes Type Ethereum Sidechain Independent Blockchain State Channel Type Type Ethereum Sidechain Ethereum Sidechain Independent Blockchain Independent Blockchain State Channel State Channel Mining Merged Mining PoX NA Mining Mining Merged Mining Merged Mining PoX PoX NA NA Native Token RBTC STX NA Native Token Native Token RBTC RBTC STX STX NA NA With the possible exception of Monero, Bitcoin is the only cryptocurrency that is truly decentralized in terms of its servers and its founders. Nobody knows who founded Bitcoin and there has even been a server launched into outer space. It has the highest adoption rates and is the most well-known. Of course, it also has the largest market cap and trade volume. Bitcoin is one of the few crypto movements that can be said to be purely grassroots and people-powered, with no initial investment, no marketing, and no vested interests. It’s why world governments and central banks hate it so much - there are no founders or investors to harass and target. It’s a truly anti-fragile technology that gets stronger the more it is attacked. Bitcoin Adoption Levels Bitcoin Adoption Levels Bitcoin adoption levels are through the roof and have been helped hugely by irresponsible government spending, lockdowns, privacy intrusions, and frustrating social policies. It is becoming popular both in countries with large numbers of unbanked as well as in developed countries with draconian regulatory procedures. Remember, we are still in the early days of Bitcoin adoption and it has much more room for growth. The globe at large is slowly, if reluctantly, waking up to the fact that fiat-based governments act in a way that is indistinguishable from the threats they say they are protecting us from. Thankfully, this trend of alertness is accelerating and pushing people towards Bitcoin. The following are some inspiring adoption facts relevant to Bitcoin: The government of El Salvador has adopted Bitcoin as a legal tender and made huge profits doing so, despite much criticism. The Central African Republic has done the same. The government of El Salvador has adopted Bitcoin as a legal tender and made huge profits doing so, despite much criticism. The Central African Republic has done the same. Bitcoin as a legal tender Bitcoin as a legal tender Small towns in South Africa have integrated Bitcoin as an accepted means of payment. Other areas include Bitcoin Beach in El Salvador. Special Economic Zones (SEVs) such as Prospera in Honduras have a 5% tax rate and are based on decentralization and bitcoin-based capital. Social media sites like Substack and Twitter (X) have integrated Bitcoin’s Lightning Network as a means of payment. Paxful also accepts Lightning Network payments, as does McDonalds’ and Walmart. Small towns in South Africa have integrated Bitcoin as an accepted means of payment. Other areas include Bitcoin Beach in El Salvador. Small towns in South Africa have integrated Bitcoin as an accepted means of payment. Other areas include Bitcoin Beach in El Salvador. integrated Bitcoin integrated Bitcoin Special Economic Zones (SEVs) such as Prospera in Honduras have a 5% tax rate and are based on decentralization and bitcoin-based capital. Special Economic Zones (SEVs) such as Prospera in Honduras have a 5% tax rate and are based on decentralization and bitcoin-based capital. Prospera in Honduras Prospera in Honduras Social media sites like Substack and Twitter (X) have integrated Bitcoin’s Lightning Network as a means of payment. Paxful also accepts Lightning Network payments, as does McDonalds’ and Walmart. Social media sites like Substack and Twitter (X) have integrated Bitcoin’s Lightning Network as a means of payment. Paxful also accepts Lightning Network payments, as does McDonalds’ and Walmart. In terms of on-chain metrics, active wallet addresses are nearing all-time highs, and the price is widely expected to hit $100,000 by 2025 . A Bitcoin ETF was recently approved by the SEC. At the time of writing, there are over 32,000 Bitcoin ATMs in the US alone. $100,000 by 2025 $100,000 by 2025 Attitude is Everything Attitude is Everything An uplifting idiom that is often heard among BTC proponents is to “stay humble, stack satoshis” . This is the needed attitude to have, not mindless profit-taking driven by 100x returns and a mindless meme frenzy. It’s about financial equality and the creation of a new economy built on trust, transparency, and liberty, the polar opposite of the existing fiat ecosystem. BTC “stay humble, stack satoshis” With L2s like Rootstock, LW, and Stacks rendering moot most prior criticisms of Bitcoin, we are all set to take back the financial economy through the only crypto that has ever mattered: Bitcoin With L2s like Rootstock, LW, and Stacks rendering moot most prior criticisms of Bitcoin, we are all set to take back the financial economy through the only crypto that has ever mattered: Bitcoin Business owners should be encouraged, across the world, to do their part and accept BTC for payment. Not as a means of taking profits on Bitcoin holding, but so it becomes an accepted norm for payment transactions. This will lead to liberated financial markets, known as KYC-free Bitcoin Circular Economies . KYC-free Bitcoin Circular Economies KYC-free Bitcoin Circular Economies Despite decades of propaganda, the truth is that Bitcoin is the PERFECT solution to a broken financial system and the only thing needed is usage and adoption. It’s low-cost, scalable, fast, and iconic. It’s also more than capable of handling large transaction volumes and will help to alleviate a world under siege by inept politicians and corrupt central banks. The rate of Bitcoin adoption across the globe might be the best metric we have to measure individual liberties.

Bitcoin Adoption & Planetary Sovereignty - One And The Same?

বিটকয়েন গ্রহণ এবং গ্রহের সার্বভৌমত্ব - এক এবং একই?

Bitcoin-Einführung und planetare Souveränität – ein und dasselbe?

Adopción de Bitcoin y soberanía planetaria: ¿uno y el mismo?

Adoption du Bitcoin et souveraineté planétaire : une seule et même chose ?

बिटकॉइन अपनाना और ग्रहीय संप्रभुता - एक ही बात?

ビットコインの採用と惑星の主権は同じもの？

비트코인 채택과 행성 주권 - 하나이고 같은가?

Adoção do Bitcoin e Soberania Planetária - A Mesma?

Принятие биткойнов и планетарный суверенитет – одно и то же?

Bitcoin'in Benimsenmesi ve Gezegensel Egemenlik - Bir Ve Aynı mı?

Việc áp dụng Bitcoin và chủ quyền hành tinh - Một và giống nhau?

比特币的采用和行星主权——是一回事吗？

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 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) 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

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