GAIA

gaia

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

Physical Properties of KIC 9851944: Conclusion, Data Availability, Acknowledgments, and References

Colliding Magnetospheres in The Young High-Eccentricity Binary DQ Tau:Acknowledgments and References

This paper is available on arxiv under CC 4.0 license.
Authors:
(1) Konstantin V. Getman, Department of Astronomy & Astrophysics, Pennsylvania State University;
(2) Agnes Kospal, Konkoly Observatory, Research Centre for Astronomy and Earth Sciences, E¨otv¨os Lor´and Research Network (ELKH), MTA Centre of
Excellence, Max Planck Institute for Astronomy, and ELTE E¨otv¨os Lor´and University, Institute of Physics;
(3) Nicole Arulanantham, Space Telescope Science Institute;
(4) Dmitry A. Semenov, Konkoly Observatory, Research Centre for Astronomy and Earth Sciences;
(5) Grigorii V. Smirnov-Pinchukov, Konkoly Observatory, Research Centre for Astronomy and Earth Sciences;
(6) Sierk E. van Terwisga, Konkoly Observatory, Research Centre for Astronomy and Earth Sciences. Table of Links Abstract and Intro
X-ray Observations and Data Extraction
Flare Analyses
Comparison with X-ray Flares from Young Stars
Discussion
Conclusions
Acknowledgments and References ABSTRACT DQ Tau is a unique young high-eccentricity binary system that exhibits regular magnetic reconnection flares and pulsed accretion near periastron. We conducted NuSTAR, Swift, and Chandra observations during the July 30, 2022 periastron to characterize X-ray, near-ultraviolet (NUV), and optical flaring emissions. Our findings confirm the presence of X-ray super-flares accompanied by substantial NUV and optical flares, consistent with previous discoveries of periastron flares in 2010 and 2021. These observations, supported by new evidence, strongly establish the magnetosphere collision mechanism as the primary driver of magnetic energy release during DQ Tau’s periastron flares. The energetics of the observed X-ray super-flares remain consistent across the three periastrons, indicating recurring energy sources during each passage, surpassing the capabilities of single stars. The observed flaring across multiple bands supports the Adams et al. model for magnetosphere interaction in eccentric binaries. Evidence from modeling and past and current observations suggests that both the mm/X-ray periastron flares and tentatively, the magnetic reconnection-related components of the optical/NUV emissions, conform to the classical solar/stellar non-thermal thick-target model, except for the distinctive magnetic energy source. However, our NuSTAR observations suffered from high background levels, hindering the detection of anticipated non-thermal hard X-rays. Furthermore, we report serendipitous discovery of X-ray super-flares occurring away from periastron, potentially associated with interacting magnetospheres. The current study is part of a broader multi-wavelength campaign, which is planned to investigate the influence of DQ Tau’s stellar radiation on gas-phase ion chemistry within its circumbinary disk. Keywords: Pre-main sequence stars (1290) — Spectroscopic binary stars (1557) — X-ray stars (1823) — Stellar magnetic fields (1610) — Optical flares (1166) — Ultraviolet transient sources (1854) —- Stellar x-ray flares (1637) — Solar x-ray flares (1816) — Solar flares (1496) — Stellar flares (1603) — Protoplanetary disks (1300) 1. INTRODUCTION DQ Tau is a nearby (D = 195 pc; Gaia Collaboration et al. 2023), non-eclipsing, double-lined spectro scopic binary system, consisting of two pre-main sequence (PMS) stars of equal mass (0.6 M⊙) and equal radius (2 R⊙) (Mathieu et al. 1997; Czekala et al. 2016; Pouilly et al. 2023). These stars exhibit spectral types within the range of M0 to K7. The rotational periods of the primary and secondary components are 3 days (K´osp´al et al. 2018) and 4.5 days (Pouilly et al. in prep.), respectively. The orbital period measures 15.8 days. DQ Tau boasts a highly eccentric orbit (e ∼ 0.6) and displays an exceptionally small periastron separation, measuring only about 8 −10 stellar radii (Mathieu et al. 1997; Czekala et al. 2016; Pouilly et al. 2023). Furthermore, the binary components of DQ Tau harbor relatively strong surface magnetic fields, estimated at around 2.5 kG, which give rise to formidable magnetospheres (Pouilly et al. 2023, Pouilly et al. in prep.). Surrounding DQ Tau is a protoplanetary disk of average size (≤ 100 au), complete with a small 0.3 au cavity (Czekala et al. 2016; K´osp´al et al. 2018; Ballering & Eisner 2019). Large optical and UV brightenings primarily occur at orbital phase (Φ = 0.8 − 1.2), and they are mainly attributed to the pulsed accretion of disk material onto the binary components (Tofflemire et al. 2017; K´osp´al et al. 2018; Muzerolle et al. 2019; Fiorellino et al. 2022). However, far-UV (FUV) observations of DQ Tau with the Cosmic Origins Spectrograph onboard HST (HST-COS) showed no correlation between the orbital phase of the binary and the C IV flux, a tracer of mass accretion rate, indicating that some component of the behavior is stochastic (Ardila et al. 2015). The system exhibits powerful mm/X-ray flares coinciding with periastron passage, attributed to collisions between the magnetospheres of the binary components. The evidence supporting the magnetsophere collision hypothesis includes the recurrence of synchrotron mmband flaring during 4 periastron encounters (Salter et al. 2008, 2010), the recurrence of soft X-ray flaring in 2 periastron encounters (Getman et al. 2011, 2022a), the timing and energy relationships between the mm and X-ray flares, and the consistency observed between the flare loop size and binary separation (Salter et al. 2010; Getman et al. 2011). Several other young binary systems with high eccentricities have been reported to exhibit enhanced levels of either X-ray, optical/mm, or radio emissions near their periastron passages. Notable examples include ϵ Lupi (Das et al. 2023), a collective study of four binaries (Parenago 523, RX J1622.7-2325 Nw, UZ Tau E, and HD 152404) conducted by Getman et al. (2016), UZ Tau E (K´osp´al et al. 2011), and V773 Tau A (Massi et al. 2008; Adams et al. 2011). In these systems, magnetosphere collision has been proposed as a primary mechanism responsible for generating the magnetic reconnection energy that drives these events. Modelling studies have shown that PMS X-rays have strong impact on disk ionization and chemistry (Glassgold et al. 2000; Alexander et al. 2014). But most studies assume continuous irradiation without considering the high-amplitude variations in flux and spectrum due to super-flares. A few time-dependent calculations show that disk ionization may respond to sudden large Xray flares (Rab et al. 2017; Waggoner & Cleeves 2022). This may already have been seen. One empirical report of ionization variability has emerged: the H13CO+ abundance of IM Lup’s disk jumped up and down by a factor of 2.5 over months (Cleeves et al. 2017). However, since no concurrent X-ray observations were conducted, the exact cause cannot be definitively ascribed to X-ray flaring. The occurrence of large X-ray flares in young stars is relatively rare and unpredictable, displaying a stochastic nature (Getman & Feigelson 2021). However, the presence of predictable X-ray super-flares and accretion outbursts in close proximity to periastron passage makes DQ Tau an extraordinary laboratory for investigating the influence of stellar radiation on the gas-phase ion chemistry within its disk. To achieve this, we conducted a single X-ray observation using the NuSTAR telescope, along with multiple short-duration observations using the Swift telescope in the X-ray, UV, and optical wavelengths. These observations were strategically timed near a specific periastron passage of DQ Tau, taking place in July-August 2022. Additionally, we captured multiple snapshots of the non-periastron portion of DQ Tau’s orbit using the Chandra X-ray telescope. However, we encountered unfavorable weather conditions that limited our ALMA observations to a single short session near periastron. The results from this ALMA observation will be presented in a forthcoming paper. Meanwhile, building upon the X-ray/UV/optical data acquired in 2022 and the previously obtained X-ray/mm data (Salter et al. 2010; Getman et al. 2011, 2022a), our current study is dedicated to further investigating the origins and energetic properties of X-ray flares, along with their corresponding near-ultraviolet (NUV) and optical flare counterparts, observed within the remarkable young binary system DQ Tau. The structure of the paper is outlined as follows: Section 2 provides a detailed description of the data reduction and reduction procedures employed for X-ray, UV, and optical analyses. In Section 3, we present the detection of flares and examine their spectral properties. Section 4 offers a comparison between the X-ray periastron flares observed in DQ Tau and super-flares observed in numerous other PMS stars. Finally, Section 5 delves into a discussion surrounding the origin and energetics of the X-ray flares, as well as their associated NUV and optical counterparts. This paper is available on arxiv under CC 4.0 license. Authors: (1) Konstantin V. Getman, Department of Astronomy & Astrophysics, Pennsylvania State University; (2) Agnes Kospal, Konkoly Observatory, Research Centre for Astronomy and Earth Sciences, E¨otv¨os Lor´and Research Network (ELKH), MTA Centre of Excellence, Max Planck Institute for Astronomy, and ELTE E¨otv¨os Lor´and University, Institute of Physics; (3) Nicole Arulanantham, Space Telescope Science Institute; (4) Dmitry A. Semenov, Konkoly Observatory, Research Centre for Astronomy and Earth Sciences; (5) Grigorii V. Smirnov-Pinchukov, Konkoly Observatory, Research Centre for Astronomy and Earth Sciences; (6) Sierk E. van Terwisga, Konkoly Observatory, Research Centre for Astronomy and Earth Sciences. This paper is available on arxiv under CC 4.0 license. Authors: Authors: (1) Konstantin V. Getman, Department of Astronomy & Astrophysics, Pennsylvania State University; (2) Agnes Kospal, Konkoly Observatory, Research Centre for Astronomy and Earth Sciences, E¨otv¨os Lor´and Research Network (ELKH), MTA Centre of Excellence, Max Planck Institute for Astronomy, and ELTE E¨otv¨os Lor´and University, Institute of Physics; (3) Nicole Arulanantham, Space Telescope Science Institute; (4) Dmitry A. Semenov, Konkoly Observatory, Research Centre for Astronomy and Earth Sciences; (5) Grigorii V. Smirnov-Pinchukov, Konkoly Observatory, Research Centre for Astronomy and Earth Sciences; (6) Sierk E. van Terwisga, Konkoly Observatory, Research Centre for Astronomy and Earth Sciences. Table of Links Abstract and Intro X-ray Observations and Data Extraction Flare Analyses Comparison with X-ray Flares from Young Stars Discussion Conclusions Acknowledgments and References Abstract and Intro Abstract and Intro X-ray Observations and Data Extraction X-ray Observations and Data Extraction Flare Analyses Flare Analyses Comparison with X-ray Flares from Young Stars Comparison with X-ray Flares from Young Stars Discussion Discussion Conclusions Conclusions Acknowledgments and References Acknowledgments and References ABSTRACT DQ Tau is a unique young high-eccentricity binary system that exhibits regular magnetic reconnection flares and pulsed accretion near periastron. We conducted NuSTAR, Swift, and Chandra observations during the July 30, 2022 periastron to characterize X-ray, near-ultraviolet (NUV), and optical flaring emissions. Our findings confirm the presence of X-ray super-flares accompanied by substantial NUV and optical flares, consistent with previous discoveries of periastron flares in 2010 and 2021. These observations, supported by new evidence, strongly establish the magnetosphere collision mechanism as the primary driver of magnetic energy release during DQ Tau’s periastron flares. The energetics of the observed X-ray super-flares remain consistent across the three periastrons, indicating recurring energy sources during each passage, surpassing the capabilities of single stars. The observed flaring across multiple bands supports the Adams et al. model for magnetosphere interaction in eccentric binaries. Evidence from modeling and past and current observations suggests that both the mm/X-ray periastron flares and tentatively, the magnetic reconnection-related components of the optical/NUV emissions, conform to the classical solar/stellar non-thermal thick-target model, except for the distinctive magnetic energy source. However, our N u STAR observations suffered from high background levels, hindering the detection of anticipated non-thermal hard X-rays. Furthermore, we report serendipitous discovery of X-ray super-flares occurring away from periastron, potentially associated with interacting magnetospheres. The current study is part of a broader multi-wavelength campaign, which is planned to investigate the influence of DQ Tau’s stellar radiation on gas-phase ion chemistry within its circumbinary disk. u Keywords : Pre-main sequence stars (1290) — Spectroscopic binary stars (1557) — X-ray stars (1823) — Stellar magnetic fields (1610) — Optical flares (1166) — Ultraviolet transient sources (1854) —- Stellar x-ray flares (1637) — Solar x-ray flares (1816) — Solar flares (1496) — Stellar flares (1603) — Protoplanetary disks (1300) Keywords 1. INTRODUCTION DQ Tau is a nearby (D = 195 pc; Gaia Collaboration et al. 2023), non-eclipsing, double-lined spectro scopic binary system, consisting of two pre-main sequence (PMS) stars of equal mass (0.6 M⊙) and equal radius (2 R⊙) (Mathieu et al. 1997; Czekala et al. 2016; Pouilly et al. 2023). These stars exhibit spectral types within the range of M0 to K7. The rotational periods of the primary and secondary components are 3 days (K´osp´al et al. 2018) and 4.5 days (Pouilly et al. in prep.), respectively. The orbital period measures 15.8 days. DQ Tau boasts a highly eccentric orbit (e ∼ 0.6) and displays an exceptionally small periastron separation, measuring only about 8 −10 stellar radii (Mathieu et al. 1997; Czekala et al. 2016; Pouilly et al. 2023). Furthermore, the binary components of DQ Tau harbor relatively strong surface magnetic fields, estimated at around 2.5 kG, which give rise to formidable magnetospheres (Pouilly et al. 2023, Pouilly et al. in prep.). Surrounding DQ Tau is a protoplanetary disk of average size (≤ 100 au), complete with a small 0.3 au cavity (Czekala et al. 2016; K´osp´al et al. 2018; Ballering & Eisner 2019). Large optical and UV brightenings primarily occur at orbital phase (Φ = 0.8 − 1.2), and they are mainly attributed to the pulsed accretion of disk material onto the binary components (Tofflemire et al. 2017; K´osp´al et al. 2018; Muzerolle et al. 2019; Fiorellino et al. 2022). However, far-UV (FUV) observations of DQ Tau with the Cosmic Origins Spectrograph onboard HST (HST-COS) showed no correlation between the orbital phase of the binary and the C IV flux, a tracer of mass accretion rate, indicating that some component of the behavior is stochastic (Ardila et al. 2015). The system exhibits powerful mm/X-ray flares coinciding with periastron passage, attributed to collisions between the magnetospheres of the binary components. The evidence supporting the magnetsophere collision hypothesis includes the recurrence of synchrotron mmband flaring during 4 periastron encounters (Salter et al. 2008, 2010), the recurrence of soft X-ray flaring in 2 periastron encounters (Getman et al. 2011, 2022a), the timing and energy relationships between the mm and X-ray flares, and the consistency observed between the flare loop size and binary separation (Salter et al. 2010; Getman et al. 2011). Several other young binary systems with high eccentricities have been reported to exhibit enhanced levels of either X-ray, optical/mm, or radio emissions near their periastron passages. Notable examples include ϵ Lupi (Das et al. 2023), a collective study of four binaries (Parenago 523, RX J1622.7-2325 Nw, UZ Tau E, and HD 152404) conducted by Getman et al. (2016), UZ Tau E (K´osp´al et al. 2011), and V773 Tau A (Massi et al. 2008; Adams et al. 2011). In these systems, magnetosphere collision has been proposed as a primary mechanism responsible for generating the magnetic reconnection energy that drives these events. Modelling studies have shown that PMS X-rays have strong impact on disk ionization and chemistry (Glassgold et al. 2000; Alexander et al. 2014). But most studies assume continuous irradiation without considering the high-amplitude variations in flux and spectrum due to super-flares. A few time-dependent calculations show that disk ionization may respond to sudden large Xray flares (Rab et al. 2017; Waggoner & Cleeves 2022). This may already have been seen. One empirical report of ionization variability has emerged: the H13CO+ abundance of IM Lup’s disk jumped up and down by a factor of 2.5 over months (Cleeves et al. 2017). However, since no concurrent X-ray observations were conducted, the exact cause cannot be definitively ascribed to X-ray flaring. The occurrence of large X-ray flares in young stars is relatively rare and unpredictable, displaying a stochastic nature (Getman & Feigelson 2021). However, the presence of predictable X-ray super-flares and accretion outbursts in close proximity to periastron passage makes DQ Tau an extraordinary laboratory for investigating the influence of stellar radiation on the gas-phase ion chemistry within its disk. To achieve this, we conducted a single X-ray observation using the N u STAR telescope, along with multiple short-duration observations using the Swift telescope in the X-ray, UV, and optical wavelengths. These observations were strategically timed near a specific periastron passage of DQ Tau, taking place in July-August 2022. Additionally, we captured multiple snapshots of the non-periastron portion of DQ Tau’s orbit using the Chandra X-ray telescope. However, we encountered unfavorable weather conditions that limited our ALMA observations to a single short session near periastron. The results from this ALMA observation will be presented in a forthcoming paper. u Meanwhile, building upon the X-ray/UV/optical data acquired in 2022 and the previously obtained X-ray/mm data (Salter et al. 2010; Getman et al. 2011, 2022a), our current study is dedicated to further investigating the origins and energetic properties of X-ray flares, along with their corresponding near-ultraviolet (NUV) and optical flare counterparts, observed within the remarkable young binary system DQ Tau. The structure of the paper is outlined as follows: Section 2 provides a detailed description of the data reduction and reduction procedures employed for X-ray, UV, and optical analyses. In Section 3, we present the detection of flares and examine their spectral properties. Section 4 offers a comparison between the X-ray periastron flares observed in DQ Tau and super-flares observed in numerous other PMS stars. Finally, Section 5 delves into a discussion surrounding the origin and energetics of the X-ray flares, as well as their associated NUV and optical counterparts.

Colliding Magnetospheres in The Young High-Eccentricity Binary DQ Tau: Abstract and Intro

Ping Ping Ping That is the sound of my phone alerting me to overnight snowfall at the various Hokkaido ski resorts I monitor. While this sound brings me immense joy in January and February, in March, it brings only FOMO. I decamped from Hokkaido in early March for the past few ski seasons. My recent experience taught me that Mother Nature turns on the heat circa March 1st. I’m a primadonna skier who only likes the driest and deepest pow. However, this season, Gaia changed up big time. There was a brutal warm spell in February that rekt the snow back. The cold weather only returned towards the end of the month. But frigid temperatures came back in March, accompanied by 10 to 30cm dumps of freshie pow pow every night. Hence, the reason why my phone was blowing up. Sitting in various South East Asian hot and humid countries throughout March, I kept foolishly checking the app and ruing my decision to leave the slopes. The April thaw finally occurred in earnest, and with it, the end to my FOMO. As readers know, my ski experiences act as metaphors for my macro and crypto trading book. I previously wrote that the cessation of the US Bank Term Funding Program (BTFP) on March 12th would cause a global market rout. The BTFP was cancelled, but a vicious sell-off in crypto specifically did not occur. Bitcoin broke $70,000 decisively and topped out around $74,000. Solana kept pumping alongside various doggie and kitty meme coins. My timing was wrong, but like the ski season, the unexpected favorable March conditions will not be repeated in April. While I love winter, summer brings joy as well. The onset of northern hemispheric summer brings sporting bliss as I reorient time towards playing tennis, surfing, and kiteboarding. Summer will usher in a renewed gusher of fiat liquidity due to the policies of the US Federal Reserve (Fed) and Treasury. I will briefly outline my mental map on how and why April will experience extreme weakness in risky asset markets. For those intrepid enough to short crypto, the macro setup is favorable. While I will not outright short the market, I have closed in profit several shitcoin and memecoin trading positions. From now until May 1st, I will be in a no-trade zone. I hope to return in May with dry powder ready to deploy to position myself for the bull market to begin in earnest. Tricksters The Bank Term Funding Program (BTFP) ended a few weeks ago, but no US, non-Too-Big-to-Fail (TBTF) banks have subsequently faced any real stress. That is because high priests of fugazi finance have a bag of tricks they will use to surreptitiously print money in order to bail out the financial system. I will peek behind the curtain and explain how they are expanding the USD fiat money supply, which will underpin the general rise of crypto and stonks until the end of the year. While the end result is always money printing, the journey is not without periods where liquidity growth slows, providing a negative catalyst for risk markets. By going through the bag of tricks and estimating when the rabbit will be pulled from the hat, we can guestimate when there will be periods where the free market is allowed to operate. The Discount Window The Fed and most other central banks operate a facility known as the discount window. Banks and other covered financial institutions who are in need of funds can pledge eligible securities to the Fed in exchange for cash. By and large, the discount window, for now, only accepts US Treasuries (UST) and mortgage-backed securities (MBS). Assume that a bank is fucked because a bunch of Pierce & Pierce boomer muppets runs it. The bank holds a UST that was worth $100 when purchased but is currently worth $80. The bank is in need of cash to satisfy deposit outflows. Rather than declaring bankruptcy, the dogshit insolvent bank can tap the discount window. The bank swaps the $80 UST for $80 of dolla dolla bills because under the current rules the bank receives the market value of pledged securities. To deprecate the BTFP and remove the associated negative stigma without increasing the risk of bank failures, the Fed and US Treasury now encourage troubled banks to tap the discount window instead. However, under the current collateral terms, the discount window is not as attractive as the recently expired BTFP. Let’s go back to our example above to understand why. Remember that the UST’s value declined from $100 to $80, which means the bank has an unrealized loss of $20. Initially the $100 of UST was funded with $100 of deposits. But now the UST is worth $80; therefore, the bank would be short $20 if all the depositors fled. Under the BTFP rules, the bank receives par for underwater USTs. That means a UST worth $80, when delivered to the Fed, is swapped for $100 of cash. This restores the solvency of the bank. But the discount window only gives $80 for a UST worth $80. The $20 loss is still there, and the bank remains insolvent. Given that the Fed can unilaterally change the collateral rules to equalize the treatment of assets by the BTFP and discount window, by greenlighting the use of the discount window by the insolvent banking system, the Fed continued the stealth banking bailout. Therefore, the Fed has essentially solved the BTFP problem; the entire UST and MBS balance sheet of the insolvent US banking system (I estimate at $4 trillion) will be supported when needed by money printed to finance loans through the discount window. This is why I believe the markets haven’t forced any non-TBTF banks into bankruptcy post-March 12th, when the BTFP ended. Bank Capital Requirements Banks are often called upon to finance governments who offer bonds at yields less than nominal GDP. But why would private for-profit entities buy something that features a negative real yield? They do it because the banking regulators allow banks to purchase government bonds with little to no money down. When the banks, who hold an insufficient capital cushion against their government bond portfolio, inevitably blow up because inflation appears and bond prices fall as yields rise, the Fed allows them to use the discount window in the manner described above. As a result, banks would rather buy and hold government bonds than lend to businesses and individuals in need of capital. When you or I buy anything using borrowed money, we must pledge collateral or equity against potential losses. That is prudent risk management. But the rules are different if you are a vampire squid zombie bank. After the 2008 Global Financial Crisis (GFC), the world’s banking regulators attempted to force banks globally to hold more capital, thus creating a more robust and resilient global banking system. The system of rules that codified these changes are called Basel III. The problem with Basel III is that government bonds are not treated as riskless. Banks must put a small amount of capital behind their gargantuan portfolio of sovereign bonds. These capital requirements have proven problematic during times of stress. During the COVID March 2020 market crash, the Fed decreed that banks could hold USTs with no collateral backing. This allowed banks to step in and warehouse trillions of dollars worth of USTs in a riskless fashion … at least in terms of their accounting treatment. When the crisis abated, the supplemental leverage ratio (SLR) exemption for USTs was reinstated. Predictably, as UST prices fell due to inflation, banks went bust due to an insufficient capital cushion. The Fed rode to the rescue with the BTFP and now the discount window, but that only covers losses from the last crisis. How can banks step up and slurp down more bonds at the current unattractively high prices? The US banking system loudly proclaimed in November 2023 that due to Basel III forcing them to hold more capital against their government bond portfolios, Bad Gurl Yellen could not stuff them with more bonds. Therefore, something had to give because the US government has no other natural buyers of its debt at these negative real yields. Below is the polite way the banks phrased their precarious situation. Demand for US Treasuries may have softened among several traditional buyers. Bank security portfolio assets have been declining since last year, with bank holdings of Treasuries down $154 billion compared to one year ago. Source: Report to the Secretary of the Treasury from the Treasury Borrowing Advisory Committee Again, the Fed – led by Powell – saved the day. Out of nowhere, at a recent , Powell proclaimed that banks would not be subject to higher capital requirements. Remember that many politicians called for banks to hold more capital so that the regional banking crisis of 2023 would not repeat itself. Obviously, the banks lobbied hard to nullify these higher capital requirements. They had a good argument –  if you, Bad Gurl Yellen, want us to buy dogshit government bonds, then we can only do it profitably with infinite leverage. Banks around the world run every flavour of government; the US is no different. US Senate Banking hearing The icing on the cake was a recent letter from the International Swaps Dealer Association (ISDA) advocating for an exemption of USTs from the SLR I spoke about earlier. In essence, banks can only hold USTs in the trillions of dollars needed to finance the US government deficit on a go-forward basis if they are required to put no money down. I expect as the US Treasury ramps up debt issuance, the ISDA proposal will be accepted. This excellent chart from clearly shows how wasteful the US Government is, as evidenced by the record-high deficit. The two recent periods where deficit spending was higher were due to the 2008 GFC and the boomer-led COVID lockdowns. The US economy is growing, but the government is spending money like it's an economic depression. Bianco Research Taken together, the relaxation of capital requirements and a likely future exemption of USTs from the SLR are a covert way of money printing. The Fed doesn’t print the money, rather the banking system creates the credit money out of thin air and purchases the bonds which then appear on their balance sheet. As always, the goal is to ensure that government bond yields do not rise to a level above the nominal GDP growth rate. As long as real rates remain negative, stonks, crypto, gold, etc., will continue advancing in fiat currency terms. Bad Gurl Yellen My essay “ ” spoke in depth about how the US Treasury, led by Bad Gurl Yellen, increased the issuance of short-term Treasury bills (T-bills) in an effort to drain the trillions of dollars locked in the Fed’s Reverse Repo Program (RRP). As expected, the RRP decline coincided with a rip higher in stonks, bonds, and crypto. But now that the RRP is down to $400 billion, the market is wondering what the next source of fiat liquidity will be that bolsters asset prices. Don’t you worry, Yellen ain’t done yet, shout ‘bout to booty drop. Bad Gurl RRP Balance (white) vs. Bitcoin (yellow) The flow of fiat funds I will discuss focuses on US tax payments, the Fed’s Quantitative Tightening (QT) program, and the Treasury General Account (TGA). The timeline in question is from April 15th (the day tax payments are due for the 2023 tax year) to May 1st. Let me provide a quick guide on their positive or negative impact on liquidity to help you understand the implications of these three things. remove liquidity from the system. That is because payers must remove cash from the financial system by selling securities for example, in order to pay their taxes. Analysts expect tax payments for the 2023 tax year to be on the high side because of the large amounts of interest income received and a solid performance in the stock market. Tax Payments removes liquidity from the system. As of March 2022, the Fed allows roughly $95 billion worth of UST and MBS to mature without reinvesting the proceeds. This causes the Fed’s balance sheet to fall, which we all know reduces dollar liquidity. However, we are not concerned about the absolute level of the Fed’s balance sheet but the pace at which it declines. Analysts, like Joe Kalish of Ned Davis Research, expect the Fed to reduce the pace of QT by $30 billion per month at its May 1st meeting. The reduction in the pace of QT is positive for dollar liquidity as the Fed’s balance sheet rate of decline slows. QT When the balance rises, it removes liquidity from the system, but when it falls, it adds liquidity to the system. When the Treasury receives tax payments, the TGA balance rises. I expect the TGA balance to swell well above the current ~$750 billion level as tax payments are processed on April 15th. This is dollar liquidity negative. Don’t forget it's an election year. Yellen’s job is to get her boss, US President , reelected. That means she must do all she can to juice the stock market to make voters feel rich and ascribe this great outcome to the slow “genius” of Bidenomics. When the RRP balances finally go to zero, Yellen will spend down the TGA, releasing, most likely, an additional $1 trillion of liquidity into the system, which will pump markets. TGA Jeo Boden The precarious period for risky assets is April 15th to May 1st. This is when tax payments remove liquidity from the system, QT rumbles on at the current elevated pace, and Yellen has yet to start running down the TGA. After May 1st, the pace of QT declines, and Yellen gets busy cashing checks to jack up asset prices. If you are a trader looking for an opportune time to put on a cheeky short position, the month of April is the perfect time to do so. After May 1st, it’s back to regular programming … asset inflation sponsored by Fed and US Treasury financial shenanigans. Bitcoin Halving The Bitcoin block reward is forecast to halve on April 20th. This is seen as a bullish catalyst for crypto markets. I agree that it will pump prices in the medium term; however, the price action directly before and after could be negative. The narrative of the halving being positive for crypto prices is well entrenched. When most market participants agree on a certain outcome, the opposite usually occurs. That is why I believe Bitcoin and crypto prices in general will slump around the halving. Given that the halving occurs at a time when dollar liquidity is tighter than usual, it will add propellant to a raging firesale of crypto assets. The timing of the halving adds further weight to my decision to abstain from trading until May. To date I took full profit on these positions, MEW, SOL, and NMT. The proceeds were placed into and staked to earn that phat yield. Before Ethena, I would have held USDT or USDC and earned nothing while Tether and Circle captured the entire T-bill yield. Ethena’s USDe Could the market defy my bearish inclinations and continue higher? Fuck yeah. I’m perennially long as fuck crypto, so I welcome being wrong. Do I really want to babysit my most speculative shitcoin positions while I’m two-stepping at Token2049 Dubai? Hell no. Therefore, I dump. There is no need to be upset. If the dollar liquidity scenarios I discussed above come true, I will have that much more confidence to ape into all manner of dogshit. If I miss a few percentage points of gains but definitely avoid losses for my portfolio and lifestyle, that is an acceptable outcome. With that, I bid you adieu. Please remember to put your dancing shoes on, and I will see you in Dubai for a celebration of the crypto bull market.

Heatwave

তাপপ্রবাহ

Hitzewelle

Ola de calor

Vague De Chaleur

हीटवेव

熱波

폭염

Onda de calor

Волна тепла

Sıcak hava dalgası

Đợt nắng nóng

热浪

, an industrial partner with the University of California, Berkeley (“Berkeley”) FHL Vive Center, today announced that the partnership has led to the launch of , a new decentralized AI infrastructure project. ByteTrade Lab GaiaNet GaiaNet is a decentralized network that provides secure, censorship-resistant, and monetizable AI agents that incorporate each individual’s proprietary knowledge and skills while preserving privacy. Instead of setting up centralized servers, GaiaNet is building a distributed network of edge-computing nodes controlled by individuals and businesses, to host fine-tuned AI models, based on the node operator’s proprietary domain knowledge and expertise. Each GiaiaNet node is a digital twin of a real-world expert or personality, such as a university teaching assistant, a high school teacher, a crypto trader, or a customer service agent, performing skilled knowledge tasks on behalf of its creator or operator. GaiaNet boldly challenges the centralized industry giants that have dominated the AI lifecycle, from data collection to model training and fine-tuning. GaiaNet recognizes the advancement of edge AI research at Berkeley, particularly at the FHL Vive Center where it drives the adoption of small language models for offering interactive and educational AI teaching assistant services to the broad student community. GaiaNet envisions that its decentralized infrastructure will help to onboard more educational content and more educators in a decentralized fashion, and spread the use of AI teaching and learning applications outside the elite higher-education institutions to professional development and professional services markets. “I am honored to collaborate with Berkeley in our shared mission to revolutionize learning through decentralized AI. GaiaNet is not just a network; it's a paradigm shift towards a more secure, censorship-resistant future while preserving privacy and autonomy”, stated Shashank Sripada， Co-founder of GaiaNet. “GaiaNet is also committed to simplicity, ensuring that individuals and businesses can easily set up their own nodes and fine-tune their AI models with their proprietary knowledge. Through GaiaNet's intuitive interface and streamlined processes, accessing cutting-edge AI technology has never been easier”. As an esteemed academic institution, UC Berkeley Vive Center is primed to leverage its expertise to openly support the advancement of decentralized AI, especially with its partner ByteTrade to explore the technologies behind GaiaNet. This collaboration exemplifies the University's dedication to staying at the forefront of the most significant challenges and innovations in Artificial Intelligence. About GaiaNet Gaianet stands as a trailblazer in decentralized AI technology, dedicated to reshaping the tech industry with a focus on user privacy, transparency, and control. Our cutting-edge open-source infrastructure empowers users by ensuring privacy and censorship resistance in daily AI activities through a dynamic network of peer-to-peer edge nodes. This framework fosters the creation and collaboration of innovative AI business ecosystems, benefiting both private data holders and developers. Gaianet aims to revolutionize the user experience with AI chatbots, seamlessly introducing transformative changes while preserving the intuitive technology and satisfaction currently existing in the Web2 era. | | Website Github Twitter About ByteTrade Lab is inventing the infrastructure to decentralize the internet application and protocol layer for developers and users, ushering in a new internet paradigm that achieves the full Web 3.0 value proposition. ByteTrade’s innovative Web 3.0 Operating System-Terminus OS, running atop a network of decentralized personal servers protected by personal private keys, will build a new decentralized internet to empower users in controlling their own data and services. The company is backed by Susquehanna International Group (SIG)’s Asia Venture Capital Fund, and leading institutional investors including INCE Capital, BAI Capital, Sky9 Capital, BlueRun, and PWC with a $50mil USD A round financing. ByteTrade Lab | Website Twitter About UC Berkeley FHL Vive Center Connecting the world of individuals and businesses in a fully decentralized and trustless fashion has generated tremendous excitement to develop new solutions in the blockchain and DeFi space. Berkeley FHL Vive Center aims to support the long-term growth of decentralized technologies and applications by offering our expertise to create new education and degree programs for motivated students; promote cross-disciplinary research to address urgent technology bottlenecks and provide a Berkeley platform for academic and industrial partners to collaborate. Together, we can shape our society in a digital world that is more immersive, more connected, and more fair. Website This story was distributed as a release by BTCWire under HackerNoon’s Business Blogging Program. Learn more about the program here: https://business.hackernoon.com/

ByteTrade Lab and UC Berkeley Partner to Explore the Next Generation of Decentralized AI

বাইটট্রেড ল্যাব এবং UC বার্কলে অংশীদার বিকেন্দ্রীভূত AI এর পরবর্তী প্রজন্মের অন্বেষণ করতে

ByteTrade Lab und UC Berkeley arbeiten zusammen, um die nächste Generation dezentraler KI zu erforschen

ByteTrade Lab y UC Berkeley se asocian para explorar la próxima generación de IA descentralizada

ByteTrade Lab et UC Berkeley s'associent pour explorer la prochaine génération d'IA décentralisée

बाइटट्रेड लैब और यूसी बर्कले ने विकेंद्रीकृत एआई की अगली पीढ़ी का पता लगाने के लिए साझेदारी की

ByteTrade Lab とカリフォルニア大学バークレー校が次世代の分散型 AI の探索で提携

ByteTrade Lab과 UC Berkeley, 차세대 분산 AI 탐색을 위해 파트너십 체결

ByteTrade Lab e UC Berkeley fazem parceria para explorar a próxima geração de IA descentralizada

ByteTrade Lab и Калифорнийский университет в Беркли сотрудничают в изучении следующего поколения децентрализованного искусственного интеллекта

ByteTrade Lab ve UC Berkeley, Yeni Nesil Merkezi Olmayan Yapay Zekayı Keşfetmek İçin İşbirliği Yapıyor

Phòng thí nghiệm ByteTrade và UC Berkeley hợp tác để khám phá thế hệ tiếp theo của AI phi tập trung

ByteTrade Lab 与加州大学伯克利分校合作探索下一代去中心化人工智能

This paper is under CC 4.0 license. available on arxiv Authors: (1) Prajwal Niraula, Department of Earth, Atmospheric and Planetary Sciences; (2) Julien de Wit, Department of Earth, Atmospheric and Planetary Sciences; (3) Benjamin V. Rackham, Department of Earth, Atmospheric and Planetary Sciences; (4) Elsa Ducrot, Astrobiology Research Unit, University of Li`ege; (5) Artem Burdanov, Department of Earth, Atmospheric and Planetary Sciences; (6) Ian J. M. Crossfield, Kansas University Department of Physics and Astronomy; (7) Valerie Van Grootel´, Space Sciences, Technologies and Astrophysics Research (STAR) Institute, University of Li`ege; (8) Catriona Murray, 5Cavendish Laboratory; (9) Lionel J. Garcia, Astrobiology Research Unit, University of Li`ege; (10) Roi Alonso, Instituto de Astrof´ısica de Canarias & Dpto. de Astrof´ısica, Universidad de La Laguna; (11) Corey Beard, Department of Physics & Astronomy, The University of California; (12) Yilen Gomez Maqueo Chew, Instituto de Astronom´ıa, Universidad Nacional Aut´onoma de M´exico, Ciudad Universitaria; (13) Laetitia Delrez, Astrobiology Research Unit, University of Li`ege, Space Sciences, Technologies and Astrophysics Research (STAR) Institute, University of Li`ege & 0Observatoire de lUniversit´e de Gen`eve; (14) Brice-Olivier Demory, University of Bern, Center for Space and Habitability; (15) Benjamin J. Fulton, NASA Exoplanet Science Institute/Caltech-IPAC; (16) Michael Gillon, Astrobiology Research Unit, University of Li`ege; (17) Maximilian N. Gunther, Department of Physics, and Kavli Institute for Astrophysics and Space Research, Massachusetts Institute of Technology; (18) Andrew W. Howard, California Institute of Technology; (19) Howard Issacson, Department of Astronomy, University of California Berkeley; (20) Emmanuel Jehin, Space Sciences, Technologies and Astrophysics Research (STAR) Institute, University of Li`ege; (21) Peter P. Pedersen, Cavendish Laboratory; (22) Francisco J. Pozuelos, Astrobiology Research Unit, University of Li`ege & Space Sciences, Technologies and Astrophysics Research (STAR) Institute, University of Li`ege; (23) Didier Queloz, Cavendish Laboratory; (24) Rafael Rebolo-Lopez, Instituto de Astrof´ısica de Canarias & Dpto. de Astrof´ısica, Universidad de La Laguna'; (25) Sairam Lalitha, School of Physics & Astronomy, University of Birmingham; (26) Daniel Sebastian, Astrobiology Research Unit, University of Li`ege (27) Samantha Thompson, Cavendish Laboratory; (28) Amaury H.M.J. Triaud, School of Physics & Astronomy, University of Birmingham. Table of Links Abstract & Introduction Observation Analysis and Validation Future Prospects & References 4. FUTURE PROSPECTS The search for transiting planets around small stars has been motivated in large part by their potential for atmospheric characterization. Owing to the size and proximity of its host, K2-315b is thus one of the few known terrestrial exoplanets possibly amenable for atmospheric characterization in the next two decades. In order to quantify and contextualize its prospects for atmospheric study, we followed the same approach as for TRAPPIST-1 in Gillon et al. (2016) (see de Wit & Seager 2013), focusing here on all known terrestrial planets. We selected terrestrial planets as planets with a reported radius below 1.6 R⊕ in the NASA Exoplanet Archive[4] (Rogers 2015; Fulton et al. 2017). We thus derive the amplitude of the planets’ signals in transmission as: where Rp is the planetary radius, R∗ is the stellar radius, and heff is the effective atmospheric height, µ is the atmospheric mean molecular mass, T is the atmospheric temperature and g is the local gravity. We assume heff to cover seven atmospheric scale heights, µ the atmospheric mean molecular mass to be 20 amu, and the atmospheric temperature to be the equilibrium temperature for a Bond albedo of 0. For the planets with missing masses, we estimated g using the model of Chen & Kipping (2017). The signal amplitudes are reported in Figure 7 together with the SNR relative to TRAPPIST-1 b’s, calculated by scaling the signal amplitude with the hosts’ brightness in J band. We find that K2-315b fares closely to the outer planets of TRAPPIST-1 in terms of potential for atmospheric exploration with JWST— its warmer and thus larger atmosphere compensating for its larger star. In fact, its relative SNR for transmission spectroscopy is half those of TRAPPIST-1 f–h, meaning that assessing the presence of a µ ∼ 20 atmosphere around the planet would require of the order of 40 transits—four times the ∼10 transits required for a similar assessment for TRAPPIST-1 f–h (Lustig-Yaeger et al. 2019). K2-315b is thus at the very edge of JWST’s capability for atmospheric characterization, mostly due to its “large” host star. The derivation above allows us to rank planets in terms of relative potential for atmospheric characterization, assuming a similar atmospheric scenario. In practice, a significant difference in atmospheric mean molecular mass, surface pressure, and/or cloud/haze altitude will strongly affect the actual potential of a planet for characterization (Lustig-Yaeger et al. 2019). For example, in some cases clouds could render the characterization of the favorable TRAPPIST-1 e difficult even with the generation of instruments following the JWST (i.e., LUVOIR, Pidhorodetska et al. 2020). With an estimated radial velocity semi-amplitude of 1.3 m s−1 (assuming a mass comparable to that of Earth), the planet could be accessible for mass measurements using modern ultra-precise radial velocity instruments. Such possibilities and a ranking amongst the 10 best-suited Earth-sized planets for atmospheric study, EPIC 249631677 b will therefore play an important role in the upcoming era of comparative exoplanetology for terrestrial worlds. It will surely be a prime target for the generation of observatories to follow JWST and bring the field fully into this new era. This project makes use of publicly available K2 data. P.N. would like to acknowledge funding for Kerr Fellowship and Elliot Fellowship at MIT. J.d.W. and MIT gratefully acknowledge financial support from the Heising-Simons Foundation, Dr. and Mrs. Colin Masson and Dr. Peter A. Gilman for Artemis, the first telescope of the SPECULOOS network situated in Tenerife, Spain. B.V.R. thanks the Heising-Simons Foundation for support. V.V.G. is a F.R.S.-FNRS Research Associate. M.G. and E.J. are F.R.S.-FNRS Senior Research Associates. This work was also partially supported by a grant from the Simons Foundation (PI Queloz, grant number 327127), and funding from the European Research Council under the European Union’s Seventh Framework Programme (FP/2007-2013) ERC Grant Agreement Number 336480, from the ARC grant for Concerted Research Actions financed by the Wallonia-Brussels Federation, from the Balzan Prize Foundation, from F.R.S-FNRS (Research Project ID T010920F), from the European Research Council (ERC) under the European Unions Horizon 2020 research and innovation programme (grant agreement n◦ 803193/BEBOP), and from a Leverhulme Trust Research Project Grant n◦ RPG-2018-418. 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π Earth: a 3.14-day Earth-sized Planet from K2's Kitchen Served Warm: Future Prospects & References

This paper is under CC 4.0 license. available on arxiv Authors: (1) Prajwal Niraula, Department of Earth, Atmospheric and Planetary Sciences; (2) Julien de Wit, Department of Earth, Atmospheric and Planetary Sciences; (3) Benjamin V. Rackham, Department of Earth, Atmospheric and Planetary Sciences; (4) Elsa Ducrot, Astrobiology Research Unit, University of Li`ege; (5) Artem Burdanov, Department of Earth, Atmospheric and Planetary Sciences; (6) Ian J. M. Crossfield, Kansas University Department of Physics and Astronomy; (7) Valerie Van Grootel´, Space Sciences, Technologies and Astrophysics Research (STAR) Institute, University of Li`ege; (8) Catriona Murray, 5Cavendish Laboratory; (9) Lionel J. Garcia, Astrobiology Research Unit, University of Li`ege; (10) Roi Alonso, Instituto de Astrof´ısica de Canarias & Dpto. de Astrof´ısica, Universidad de La Laguna; (11) Corey Beard, Department of Physics & Astronomy, The University of California; (12) Yilen Gomez Maqueo Chew, Instituto de Astronom´ıa, Universidad Nacional Aut´onoma de M´exico, Ciudad Universitaria; (13) Laetitia Delrez, Astrobiology Research Unit, University of Li`ege, Space Sciences, Technologies and Astrophysics Research (STAR) Institute, University of Li`ege & 0Observatoire de lUniversit´e de Gen`eve; (14) Brice-Olivier Demory, University of Bern, Center for Space and Habitability; (15) Benjamin J. Fulton, NASA Exoplanet Science Institute/Caltech-IPAC; (16) Michael Gillon, Astrobiology Research Unit, University of Li`ege; (17) Maximilian N. Gunther, Department of Physics, and Kavli Institute for Astrophysics and Space Research, Massachusetts Institute of Technology; (18) Andrew W. Howard, California Institute of Technology; (19) Howard Issacson, Department of Astronomy, University of California Berkeley; (20) Emmanuel Jehin, Space Sciences, Technologies and Astrophysics Research (STAR) Institute, University of Li`ege; (21) Peter P. Pedersen, Cavendish Laboratory; (22) Francisco J. Pozuelos, Astrobiology Research Unit, University of Li`ege & Space Sciences, Technologies and Astrophysics Research (STAR) Institute, University of Li`ege; (23) Didier Queloz, Cavendish Laboratory; (24) Rafael Rebolo-Lopez, Instituto de Astrof´ısica de Canarias & Dpto. de Astrof´ısica, Universidad de La Laguna'; (25) Sairam Lalitha, School of Physics & Astronomy, University of Birmingham; (26) Daniel Sebastian, Astrobiology Research Unit, University of Li`ege (27) Samantha Thompson, Cavendish Laboratory; (28) Amaury H.M.J. Triaud, School of Physics & Astronomy, University of Birmingham. Table of Links Abstract & Introduction Observation Analysis and Validation Future Prospects & References 3. ANALYSIS AND VALIDATION 3.1. Stellar Host Characterization 3.1.1. Semi-empirical Stellar Parameters We constructed the spectral energy distribution (SED) of EPIC 249631677 using photometric magnitudes from Gaia (GBP and GRP ; Gaia Collaboration et al. 2018) and the AllWISE source catalog (J, H, Ks, W1, W2, and W3; Cutri et al. 2013). The corresponding fluxes for these magnitudes are tabulated on VizieR (Ochsenbein et al. 2000) and shown in Figure 5 and Table 1. The parallax of EPIC 249631677 is π = 17.61 ± 0.09 mas, which yields a distance of 56.8 ± 0.3 pc (Gaia Collaboration et al. 2018; Stassun & Torres 2018). We then derived the stellar luminosity L∗ by integrating over the SED, which yielded L∗ = 0.0041 ± 0.0001L . Two independent methods were applied to obtain stellar mass. First, we used the empirical M∗−MKs relation (applying the metallicity obtained in Section 3.1.2) from Mann et al. (2019) to obtain M∗ = 0.1721 ± 0.0044M . We also applied stellar evolution modeling, using the models presented in Fernandes et al. (2019), using as a constraint the luminosity inferred above and the metallicity derived in Sect. 3.1.2). We considered the stellar age to be >1 Gyr in the absence of signs of youth, such as presence of prominent flares (Ilin et al. 2019, see Section 3.1.3). We obtained with this method M∗ = 0.176 ± 0.004 M . This uncertainty reflects the error propagation on the stellar luminosity and metallicity, but also the uncertainty associated with the input physics of the stellar models. We combined these two mass estimates as in Van Grootel et al. (2018) to obtain M∗ = 0.174±0.004M as our best estimate for the stellar mass of EPIC 249631677. Given its proximity, we expect minimal extinction (Av) for the target; the SED fitting analysis described in Section 3.2.1 similarly constrains it to be 0.02 at 3σ confidence and we adopt that upper limit here. Finally, we note that given its luminosity, mass, and Gaia colors this star is likely to be fully convective (Jao et al. 2018; Rabus et al. 2019). Due to the absence of a strong constraint on the stellar density from the transits, we further obtained stellar radius, surface gravity, effective temperature and density from our evolutionary models. Table 1 summarizes the results from this analysis, along with other properties of the star. Our values are consistent with those listed in the TESS Input Catalog (Stassun et al. 2019), and we adopt them for the remainder of this analysis. 3.1.2. Reconaissance Spectroscopy To confirm EPIC 249631677’s stellar properties and better characterize the system, we acquired an optical spectrum using Keck/HIRES (Vogt et al. 1994) on UT 30 May 2020. The observation took place in 0.6 00 effective seeing and using the C2 decker without the HIRES iodine gas cell, giving an effective resolution of λ/∆λ ≈ 55, 000 from 3600 ˚A to 7990 ˚A. We exposed for 1800 s and obtained SNR of roughly 23 per pixel. Data reduction followed the standard approach of the California Planet Search consortium (Howard et al. 2010). We used our Keck/HIRES radial velocity and Gaia DR2 data to estimate the 3D galactic (UV W) space velocity using the online kinematics calculator[2] of Rodriguez (2016). Following Chubak et al. (2012), our Keck/HIRES spectrum gives a barycentric radial velocity of 6.25±0.17 km s−1 . With the Gaia-derived coordinates, proper motion, and distance listed in Table 1, we find (U, V, W) values of (−17.02, −9.06, +33.66) km s−1 , indicating a likely membership in the Milky Way’s thin disk (Bensby et al. 2014). Using the SpecMatch-Empirical algorithm (Yee et al. 2017), we derive from our HIRES spectrum stellar parameters of Teff = 3195 ± 70 K, R∗ = 0.23 ± 0.10R , and [Fe/H]= −0.24 ± 0.09, consistent with the values tabulated in Table 1. The three best-matching stars in the SpecMatch-Empirical template library are GJ 15B, GJ 447, and GJ 725B, which have spectral types of M3.5V, M4V, and M3.5V, respectively. Given the close match between the spectra of these stars and our target (see Fig. 4), we therefore classify EPIC 249631677 as an M dwarf with subclass 3.5±0.5. We see no evidence of emission line cores at Hα, consistent with our determination that our target is not a young star. We see no evidence of spectral broadening compared to these three stars (which all have v sin i < 2.5 km s−1 ; Reiners et al. 2012), so we set an upper limit on EPIC 249631677’s projected rotational velocity of < 5 km s−1 , comparable to the spectral resolution of HIRES. 3.1.3. Stellar Variability The long-term variations apparent in the everest light curve (Figure 1) are not evident in light curves from other reduction pipelines (e.g., K2SFF). These variations likely arise from systematics and are not reliable for estimating the stellar rotation period (Esselstein et al. 2018). Similarly, no flares are apparent either in the K2 or SPECULOOS data. Flare rates peak for ∼M3.5 stars in TESS data (G¨unther et al. 2020). However, given the long integration time of 29.4 minutes as well as a need for data processing which corrects for the saw-tooth pattern, flare signals, unless very prominent, are expected to be difficult to detect in K2 long cadence data. 3.2. Vetting In order to produce a transit depth on the level of 0.2% in the light curve of the primary target, a background eclipsing binary producing eclipses with depths of 25% to 50% would have to be 5.25 to 6.0 mag fainter than the target, respectively. Qualitatively, the odds of EPIC 249631677 hosting a planet are higher than the odds of such magnitude contrast eclipsing binary being present within the SPECULOOS aperture, given occurrence rates of M-dwarf planets (Dressing & Charbonneau 2013; Mulders et al. 2015; Hardegree-Ullman et al. 2019). A stringent quantitative constraint can be placed using the ingress/egress duration (T12/T34) compared to the total transit duration (T14) (Seager & Mall´enOrnelas 2003, Equation 21). Such a test yields an upper limit on the relative radius of the transiting body. By assuming equal effective surface temperatures, the lower magnitude limit ∆m (corresponding to a flux difference ∆F) for a blended binary mimicking a signal of depth δ is given by: Using the posterior for the transit fit (See Section 3.3), we find for EPIC 249631677 that such a background object can be fainter at most by 1.73 mag at the 3σ level. Fortunately, EPIC 249631677 has a significant proper motion, ∼140 mas yr−1 , which allows us to investigate the presence of background sources at its current sky position. We looked at archival imaging of EPIC 246331677 going back to 1953[3] . A POSS I plate from 1953 is the publicly available oldest image of EPIC 249631677, and it does not show any background source at the current position of the target as shown in Figure 6. The plate is sensitive to objects at least 3.5 magnitudes fainter than the target. Similarly, the Hubble Guide Star Catalogue (GSC), with a limiting magnitude of 20 (Lasker et al. 1990), does not show any background source. While POSS II would go the deepest in terms of limiting magnitude (20.8, Reid et al. 1991), the star has moved appreciably closer to its current location, precluding a definitive measurement from this image. Overall, using archival images we can rule out the possibility of the transit signal originating from background star at a high level of confidence. 3.2.1. Binarity of the Host Star Despite the lack of background sources, the host star could produce a false-positive transit signal if it were a grazing eclipsing binary or a hierarchical eclipsing binary. We investigated the evidence for host star binarity using the isochrones software package (Morton 2015), which performs isochrone fitting in the context of the MESA (Paxton et al. 2011, 2013, 2015) Isochrones and Stellar Tracks database (Dotter 2016; Choi et al. 2016). Single-star and binary evolutionary models are available within isochrones, and the inference is performed via the nested sampling algorithm MULTINEST (Feroz et al. 2009) (as implemented in the PyMultiNest software package (Buchner et al. 2014)), which allows for direct comparisons of the Bayesian evidence ln Z. We tested both single-star and binary models using the priors on photometric magnitudes and stellar distance described in Section 3.1.1. The inferred properties from the single-star model fit are consistent with those given in Table 1 at the 2σ level. The ln Z for the single-star model is −213.86±0.04, whereas the ln Z for the binary model is −229.6 ± 0.2. According to Kass & Raftery (1995), the corresponding Bayes factor of 16 indicates “decisive” evidence in favor of the single-star model. We also examined our Keck/HIRES spectrum for secondary lines that would indicate the presence of another star following the approach of Kolbl et al. (2015). We found no evidence of additional lines down to the method’s standard sensitivity limit of ∆V = 5 mag for ∆v > 10 km s−1 , consistent with EPIC 249631677 being a single, isolated star. We therefore conclude that the available data strongly support EPIC 246331677 being a single star. 3.2.2. Photometric Tests We performed a series of tests on the photometric data to rule out false-positive scenarios. First, we performed an even-odd test on the target using K2 photometry. The even and odd transits are consistent with one another in transit depth to within 1σ. We also looked for secondary eclipses in the phase-folded light curve and found none to be present. Note that since we observe consistent signals in both the K2 and SPECULOOS data sets, we can rule out the signal originating from systematics. The transit depth in SPECULOOS observations with I+z filter, which is redder than Kepler bandpass, are consistent to K2 transit depths within 1σ level, keeping up with the expectation of the achromatic nature of planetary transit. Furthermore, a massive companion, such as a faint white dwarf, can be ruled out using the ellipsoidal variation, which puts a 3σ upper limit on the mass of any companions at the given orbital period of the transit signal as ∼100 MJup (Morris 1985; Niraula et al. 2018). From the transit fit, we can rule out a grazing eclipse originating from a larger transiting object (i.e. ≥ 2R⊕) at >3σ confidence. Together, these tests rule out the object at 3.14 days being a massive companion. 3.3. Transit Fitting We used the refined estimates of the host properties together with a joint analysis of the K2 and SPECULOOS light curves to derive the planetary properties. In order to calculate the transit model, we used batman (Kreidberg 2015). We simultaneously model both the K2 observation as well as the ground-based observations with 21 parameters in a Monte Carlo Markov Chain (MCMC) framework using the emcee package (ForemanMackey et al. 2013). We use a Gaussian prior on the scaled semi-major axis of the orbit a/R∗ of N (25.72, 0.27), derived using Eq. 30 from Winn (2010) along with the stellar density of 32.6 ± 1.0 g cm−3 (see Section 3.1.1) and orbital period of 3.1443 days from the TLS search. As for the limb darkening, we use the non-informative q1, q2 parameterization of the quadratic limb-darkening law as suggested by Kipping (2013). We fixed the eccentricity to 0, given that the expected time of circularization is 50 Myr (assuming a quality factor Qp ∼ 500, Goldreich & Soter 1966; Patra et al. 2017), which is at least an order of magnitude smaller than the estimated age of the system. For K2 data, we supersample the transits by a factor of 15 in batman to take into account the effect of non-negligible integration time. As for the ground-based data, we use second-order polynomials to detrend against the observables airmass and FWHM. We ran the MCMC for 50,000 steps with 150 walkers performing a combined fit of K2 and SPECULOOS — (1) This work. (2) Huber et al. (2016). (3) Stassun et al. (2019). (4) Cutri et al. (2003). (5) Gaia Collaboration et al. (2018). (6) Cutri et al. (2013). (7) This work, evolutionary model analysis. (8) This work, Keck/HIRES analysis. (9) This work, SED analysis. References data, and use the last half of the run to build the parameter posteriors. We assessed the convergence of walkers using the suggested autocorrelation test for emcee. The resulting median values from the fit with 1σ deviation are reported in Table 2, while the best-fit transit models are shown in Figure 2 and Figure 3. [2] http://kinematics.bdnyc.org/query [3] http://stdatu.stsci.edu/cgi-bin/dss form

π Earth: a 3.14-day Earth-sized Planet from K2's Kitchen Served Warm: Analysis and Validation

Having taken the world by storm last year with its mind-blowing technology that generates text and images on command, OpenAI is looking ahead to create its next updated version of the software. However, the company could face stiff competition as major tech companies make headway in catching up and producing their own version of the . The question on everyone’s minds now is, will Meta create its own improved version of ChatGPT? In a recent , Meta said, “We're excited to announce that Llama 2, our open-source large language model, is now free and available for research and commercial use. This release offers a unique opportunity for developers while reflecting our commitment to open source, cross-collaboration, and innovation!” Without a doubt, Meta has its eyes set on overtaking ChatGPT as the next LLM to take the world by storm with significant improvements and capabilities. The next few months will determine whether Meta achieves this lofty goal. But a lot more is happening on the AI front. As noted, with the support of the Saudi Data and Artificial Intelligence Authority (SDAIA) and the National Technology Development Program (NTDP), the GAIA generative AI accelerator is bolstering startups specialized in generative AI. Their aim is to enhance these startups and expedite their market entry. To date, GAIA has organized four AI Hackathons. Over 7,000 AI enthusiasts and developers have participated, resulting in the creation of 185 prototypes. The program has been backed with a budget of $30 million, targeting the empowerment of 300 generative AI startups. That’s not an insignificant number. In July 2023, GAIA's accelerator initiative introduced its inaugural batch, consisting of 15 startups. This initiative is backed by a robust investment fund valued at $160 million, with a goal to invest in 120 early-stage companies. Notably, GAIA's model utilizes generative AI techniques to monitor the progression of these startups automatically. GAIA's foundation is aligned with the ambitions of SDAIA and NTDP, which aim to solidify Saudi Arabia’s position as a forefront player in AI technology development. Furthermore, GAIA is dedicated to strengthening the AI ecosystem in the , which it believes can be achieved by introducing programs tailored for the entrepreneurial sector and technology startups and by drawing AI-centric businesses to the Kingdom. In other AI news, this time dealing with ethics, Mustafa Suleyman, co-founder of Google DeepMind, recently expressed his concerns about the ethical use of Nvidia's AI chips in an interview with the Financial Times. He emphasized that the US should permit the sale of Nvidia's AI chips solely to those customers who commit to using the technology ethically. Suleyman believes the US has a responsibility to set and enforce global standards when it comes to the utilization of AI. This would mean that companies interested in acquiring such technologies should, at the very least, adhere to the ethical guidelines and commitments made by premier AI firms to the US administration. Earlier in July, several prominent AI entities, including OpenAI, Alphabet, and Meta Platforms, had voluntarily pledged to the White House their commitment to ensure the safer deployment of AI technologies. As reported by Reuters, part of these voluntary commitments involved the introduction of initiatives like watermarking . This measure, among others, is seen as a step towards making AI technology more transparent and accountable, thereby ensuring that users can differentiate between human and AI-generated content. Suleyman's call to action underlines the urgency of establishing a global framework for AI's ethical use, considering the rapidly growing influence and capabilities of the technology. These concerns are highly relevant as AI is developing quickly around the globe. Technology heavyweight China's inaugural public AI chatbot, ERNIE, designed to filter out sensitive subjects in alignment with the Communist Party's directives, including events like the Tiananmen Square incident. Earlier this month, Beijing introduced fresh guidelines for AI developers in China. These regulations strike a balance by ensuring governmental oversight on disseminated information while still allowing Chinese developers to remain competitive against global counterparts such as Microsoft and OpenAI. Baidu isn’t the only company introducing new AI tools. Google has expanded its portfolio by to enterprise customers. These tools, powered by advanced AI, can now be accessed for a monthly fee of US $30 per user. This move, under the umbrella of Alphabet, capitalizes on the rising popularity and demand for AI technologies seen throughout the year. Google’s pricing strategy aligns with that of its major competitor, Microsoft, which offers "Copilot,” an AI-enhanced office software suite. It also comes with a similar price tag and includes widely-used applications like Teams and Outlook. Google's decision to delve deeper into generative AI investments is a strategic move to remain competitive. The company is ramping up its efforts, especially after the impactful launch of OpenAI’s ChatGPT, which received backing from Microsoft. signifies its determination to keep pace with rapid innovations and changing market dynamics – a necessary move if it wants to remain relevant in the years to come. generative AI technology announcement this article Middle East-North Africa (MENA) region content generated by AI Baidu just unveiled offering its AI-driven tools Google's intensified focus on AI

Will Meta Create Its Own ChatGPT and Other News in the World of AI

In a , we covered how the rise of BRC-20 memecoins on the Bitcoin ordinal standard was breathing new life into the crypto ecosystem. Now we're here to take a more network-agnostic view on memecoins, showing you some projects worth looking at, the history of some more prominent memes/coins, and why market conditions notwithstanding, memecoins are maintaining resilient communities and competitive market caps. previous article Memecoin Up and Comers  - July 2023 - PREZ is a unique spin on Pepe - a charitable frog with the drive of a presidential candidate. The project presents itself as a utility meme coin through its novel and turnkey digital merchandising system and like Hope of Life, an organization that renders humanitarian aid to children, elderly, and disabled in Guatemala. The token has outperformed the market, seeing a gain of over 37% at the time of this writing, and gained a die-hard community in the process. Prez is tradeable via and through - a vote of confidence from one of the largest exchanges in the world, and especially in the US. The Dog Days Are Over! Prez ($PREZ) commitment to donate a portion of proceeds to pro-crypto governmental candidates and charitable organizations Uniswap Coinbase wallet - If you missed the first boat on $PEPE, PEPE 2.0 is your second chance to capitalize on the pepe wave - this time with a yellow pepe instead of a green one. You can poke fun at the blatant derivative nature of the token but it is up 51.5% on the 7-day chart, with very liquid markets on Uniswap. Pepe 2.0 ($PEPE2.0) - Wall Street Memes’ $WSM token on its first day on presale, shooting up to surpass $13.1 million over the next month. Wall Street Memes has over one million followers across five social media platforms, signifying a well-established, supportive community and a potentially bright future for the token. Wall Street Memes ($WSM) secured over $300,000 - Wojak Token is a meme coin that represents a creative extension for the , known for its popularity across some social media circles, especially among cryptocurrency and finance enthusiasts (“Wokajians”). They currently have over on Twitter. Wojak ($WOJ) Wojak meme 65k followers - Samoyedcoin isn’t strictly new but is one of the longest-standing memecoins born out of the Solana ecosystem. Created to promote, educate and support Solana, the coin is a derivative of the wave of dog-related tokens that hit the market in 2021. Samoyed is a fantastic example of the influence dog coins have in onboarding new market participants, marketing their underlying blockchain, and infiltrating modern-day culture. Samoyedcoin ($SAMO) The History of Frogs and Dogs Dogecoin ($DOGE) is one of, if not, the original memecoin - and has little need for a further introduction. It owes its genesis to a joke - created by Billy Markus and Jackson Palmer, software engineers at IBM and Adobe respectively, who decided to create an ironic “payment system” to make fun of cryptocurrency speculation. However, it didn’t take long for the joke to be on them. It was introduced on December 6, 2013, and ironically gained a sudden and tremendous amount of traction and popularity in Reddit communities, reaching a peak market capitalization of over $85 billion on May 5, 2021. Multiple derivatives of the “doge” have been created in it’s image, namely: Shiba Inu ($SHIB), Floki Inu ($FLOKI), and Babydoge ($BABYDOGE). [a] Pepe is a cartoon character and created by cartoonist Matt Furie. Designed as a green with a body, Pepe originated in Furie's 2005 comic ,  in a series of blog posts on in 2005. The character became an Internet meme when his popularity steadily grew across websites such as , , and in 2008. By 2015, he had become one of the most popular memes used on 4chan and . Internet meme anthropomorphic frog humanoid Boy's Club Myspace Myspace Gaia Online 4chan Tumblr The coin, $PEPE, launched in mid-April 2023 and is currently the #69 cryptocurrency (hehe) according to CMC at the time of this writing. PEPE’s describes the token as the “most memeable memecoin in existence,” adding that the “dogs have had their day.” Since then, others have followed suit, similarly giving rise to a plethora of frog tokens hoping to ride the coattails of its success. Some of these coins include , , , , , , and . official Twitter account Prez Pepe McPepe’s PepeAI Saudi Pepe Trans Pepe BOB Token JIM token Memecoins really gained traction after “meme stocks” such as GameStop ( ) and AMC Entertainment ( ) saw their prices pump by as much as 100-fold in a few months during late 2020 by a Reddit community called WallStreetBets. The crypto community quickly followed suit. In January 2021, a Reddit group joked about pumping up the price of DOGE to create a crypto equivalent of GME. That idea gained momentum, accompanying the influence of Tesla CEO Elon Musk’s tweets, and the price of DOGE rallied. In a matter of only five days, Dogecoin had increased by 2,000% — reaching a new all-time high of $0.73. GME AMC Derivative coins often accrue value through retail FOMO - the fear of missing out on becoming overnight millionaires, creating a positive feedback loop of meme rallies. Meme coins are heavily community-driven tokens. Sans any fundamental economic or business use-cases, their prices are heavily influenced by social media and online sentiment. Hype and FOMO often work together to bring communities together in what has been a bizarre social experiment showcasing the power of decentralized but systemized coordination, and the allure of a quick payday. A recent trend has been meme coins emerging as utility meme coins. One example is Pawthereum ($PAWTH), which uses a small tax on each transaction to help animal charities, raising hundreds of thousands of dollars in the process. Another trend, like ($PREZ), has been raising money for political contributions in a fun and anonymous manner. Prez Pepe Ultimately, the coins themselves mirror the high-thrills, volatility-seeking, degen nature of the investors who load up on them. While some coins are likely to rise and fall back into obscurity, human nature won’t. Amusement, the hankering for wagers, and the pursuit of quick thrills are not going away anytime soon - and on the contrary will likely intensify in the face of technological and social progress that offer us more of what we want, delivered in a shorter amount of time. Crypto fund DFG founder James Wo, has famously said that “[memecoins] are huge parts of the crypto trading landscape, whether we like it or not”. We embrace it, or we hate it. Either way, memecoins are here to stay.

Are The Doge Days Really Over?

Initial Coin Offerings (ICO) have been a popular way to fundraise projects in the crypto market, but that changed with the advent of regulations. Since then, Initial Exchange Offering (IEO) and Initial DEX Offering (IDO) have entered the market. But with the rise of blockchain games or GameFi, the latest buzz in the town is Initial Game Offering (IGO). We will look at the top 3 things you need to know about Initial Game Offerings in this article. So, without further ado, let's dive straight into it. What is IGO? Much like ICOs and IEOs, IGO is also a fundraising event for crypto gaming projects where participants get assets needed to play the game. Some IGOs also offer in-game rewards. However, it depends on a participant's investment. Simply put, that allows investors to invest in a gaming project at its early development stage. What this fundraising method does is that it lowers the barrier to entry for retail investors by enabling them to get their hands on the in-game assets and tokens before they are made available to the public. IGO is a crowdfunding approach for crypto games While the crypto game project gets the funding directly from its audience, investors get lucrative in-game assets and tokens at a considerable discount before the public sale. A significant benefit of IGOs is that it is open to all investors. The growing interest and popularity of this fundraising type have encouraged tremendous growth in the blockchain gaming space. For instance, Binance's centralized fundraising platform Binance Launchpad was the one behind the launch of the most notable gaming project Axie Infinity. A Look into Launchpads IGOs are organized through specialized platforms known as launchpad platforms. The platform you chose is crucial for the success of an IGO. This means that the platform history, success rate, amount of money raised, and time taken to achieve the funding target must be analyzed. Currently, we are at Listing.Help work with several launchpads that are hosting IGOs: 1 — GameFi was one of the first launchpads to introduce the concept of IGOs. It has four investment tiers, but only one offers guaranteed allocation. One needs a minimum of one lottery ticket, which is equivalent to 20 GAFI tokens. KABY Pool and Deathroad IGO are two popular offerings on the platform. 2 — Binance NFT is another one where IGOs grant access to exclusive in-game assets. The platform uses a subscription system to give all users an equal opportunity to participate. To ensure fairness, NFTs are allocated via public and verifiable algorithmic selection. 3 — A popular IGO launchpad Seedify Fund is governed by a DAO. As for participating in Seedify IGOs, you need between 250 and 100,000 Seedify (SFUND) tokens. The platform has nine tiers. The first one is a lottery tier, while guaranteed allocation starts from tier 2. So far, Seedify has crowdfunded Cyber Trade, Heros Chained, MetaStrike, Penguin Karts, Space, Misfits, Supernova, and other gaming projects. 4 — Enjinstarter is another popular one that has a unique approach to IGO. The ecosystem reserves 75% of IGO tokens for guaranteed allocations, which are then split into three tiers. It operates on a first-come, first-served basis, and investors can participate even with a small holding of at least 1,250 EJS tokens. Age of Tanks, Attack Wagon, Ecia, Gaia Everworld, and PathDAO, among other games, have been crowdfunded on Enjinstarter. 5 — Gamestarter, which has crowdfunded BitHotel, Crypto Fight Club, Dark Frontiers, Demole, and others, allow gaming projects to sell their NFTs or tokens to raise funds. It also has plans to expand beyond the crypto gaming space, as, in the future, Gamestarter will also support INO (Initial NFT Offering). Mechanics of IGO Buying an IGO is a chance to invest in a gaming project early. To participate in such an event, you must purchase the launchpad's native coin and lock it for a certain period of time. These tokens are locked in a pool, and based on the algorithm, the investors would receive either the project tokens or the NFTs required to play the game. In some cases, these tokens and NFTs can be traded outside of the gaming ecosystem on DEXs and NFT marketplaces. Different launchpads have different setups for an IGO, but the typical process involves: Connect your wallet to the launchpad. Select a tier that reflects the value of the investment. Identifying an IGO you want to invest in. It is also better to check whether the launchpad provides guaranteed allocation or not. To qualify for these IGOs, you can apply for Whitelist by going to relevant Launchpad's website, connecting your wallet, and staking the native token. Some platforms also require you to complete KYC. Once you have joined the pool, you can apply for the Whitelist. Raffles are another way launchpads assign assets to investors. To apply for the lottery, go to the launchpad website and ensure you're accessing the correct URL address. Connect your wallet and then join the Lottery by clicking on the button. On selecting the IGO, you'll be all set to participate in the raffle for the upcoming projects. The Crucial Ingredient: Community For an IGO to be successful, the crypto game needs to have a vibrant and strong community rooting for them. A community is usually formed and maintained via popular social media platforms such as Discord, Telegram, and Twitter. In the crypto industry, communities are instrumental in shaping how projects develop and operate. To build a thriving community, a project needs to start with potential members who identify with its envision. The project's focus needs to be on its purpose and members. Members should be involved in every step of the project and empowered through acknowledgment, feedback, and rewards. The beauty of crypto communities is that they are spread worldwide and united by the same idea and purpose. The support of a community ensures the long-term success of a project. Conclusion Crypto gaming projects are already experiencing tremendous growth and a rise in revenue. And IGO is an important part of this success. Although, GameFi help crypto adoption a lot. The recent Chainplay showed that 75% of respondents came to crypto through GameFI. And I think, as crypto goes mainstream and decentralized gaming combined with NFTs gain traction, some established blockchain games have received multimillion-dollar valuations. research The blockchain gaming industry is relatively new but fast-growing. Ultimately, with GameFi on the rise, IGOs can emerge as a viable solution for crypto gaming projects, which are already becoming a mainstay in the industry.

Top 3 Things You Need to Know About Initial Game Offerings (IGOs)

The Odyssey: Book XI

The Odyssey, by Homer and translated by Samuel Butler is part of HackerNoon’s Book Blog Post series. You can jump to any chapter in this book . Book VII: RECEPTION OF ULYSSES AT THE PALACE OF KING ALCINOUS here BOOK VII. RECEPTION OF ULYSSES AT THE PALACE OF KING ALCINOUS. Thus, then, did Ulysses wait and pray; but the girl drove on to the town. When she reached her father’s house she drew up at the gateway, and her brothers—comely as the gods—gathered round her, took the mules out of the waggon, and carried the clothes into the house, while she went to her own room, where an old servant, Eurymedusa of Apeira, lit the fire for her. This old woman had been brought by sea from Apeira, and had been chosen as a prize for Alcinous because he was king over the Phaeacians, and the people obeyed him as though he were a god. She had been nurse to Nausicaa, and had now lit the fire for her, and brought her supper for her into her own room. [57] Presently Ulysses got up to go towards the town; and Minerva shed a thick mist all round him to hide him in case any of the proud Phaeacians who met him should be rude to him, or ask him who he was. Then, as he was just entering the town, she came towards him in the likeness of a little girl carrying a pitcher. She stood right in front of him, and Ulysses said: “My dear, will you be so kind as to show me the house of king Alcinous? I am an unfortunate foreigner in distress, and do not know one in your town and country.” Then Minerva said, “Yes, father stranger, I will show you the house you want, for Alcinous lives quite close to my own father. I will go before you and show the way, but say not a word as you go, and do not look at any man, nor ask him questions; for the people here cannot abide strangers, and do not like men who come from some other place. They are a sea-faring folk, and sail the seas by the grace of Neptune in ships that glide along like thought, or as a bird in the air.” On this she led the way, and Ulysses followed in her steps; but not one of the Phaeacians could see him as he passed through the city in the midst of them; for the great goddess Minerva in her good will towards him had hidden him in a thick cloud of darkness. He admired their harbours, ships, places of assembly, and the lofty walls of the city, which, with the palisade on top of them, were very striking, and when they reached the king’s house Minerva said: “This is the house, father stranger, which you would have me show you. You will find a number of great people sitting at table, but do not be afraid; go straight in, for the bolder a man is the more likely he is to carry his point, even though he is a stranger. First find the queen. Her name is Arete, and she comes of the same family as her husband Alcinous. They both descend originally from Neptune, who was father to Nausithous by Periboea, a woman of great beauty. Periboea was the youngest daughter of Eurymedon, who at one time reigned over the giants, but he ruined his ill-fated people and lost his own life to boot. “Neptune, however, lay with his daughter, and she had a son by him, the great Nausithous, who reigned over the Phaeacians. Nausithous had two sons Rhexenor and Alcinous; Apollo killed the first of them while he was still a bridegroom and without male issue; but he left a daughter Arete, whom Alcinous married, and honours as no other woman is honoured of all those that keep house along with their husbands. [58] “Thus she both was, and still is, respected beyond measure by her children, by Alcinous himself, and by the whole people, who look upon her as a goddess, and greet her whenever she goes about the city, for she is a thoroughly good woman both in head and heart, and when any women are friends of hers, she will help their husbands also to settle their disputes. If you can gain her good will, you may have every hope of seeing your friends again, and getting safely back to your home and country.” Then Minerva left Scheria and went away over the sea. She went to Marathon and to the spacious streets of Athens, where she entered the abode of Erechtheus; but Ulysses went on to the house of Alcinous, and he pondered much as he paused a while before reaching the threshold of bronze, for the splendour of the palace was like that of the sun or moon. The walls on either side were of bronze from end to end, and the cornice was of blue enamel. The doors were gold, and hung on pillars of silver that rose from a floor of bronze, while the lintel was silver and the hook of the door was of gold. [59] On either side there stood gold and silver mastiffs which Vulcan, with his consummate skill, had fashioned expressly to keep watch over the palace of king Alcinous; so they were immortal and could never grow old. Seats were ranged all along the wall, here and there from one end to the other, with coverings of fine woven work which the women of the house had made. Here the chief persons of the Phaeacians used to sit and eat and drink, for there was abundance at all seasons; and there were golden figures of young men with lighted torches in their hands, raised on pedestals, to give light by night to those who were at table. There are fifty maid servants in the house, some of whom are always grinding rich yellow grain at the mill, while others work at the loom, or sit and spin, and their shuttles go backwards and forwards like the fluttering of aspen leaves, while the linen is so closely woven that it will turn oil. As the Phaeacians are the best sailors in the world, so their women excel all others in weaving, for Minerva has taught them all manner of useful arts, and they are very intelligent. [60] Outside the gate of the outer court there is a large garden of about four acres with a wall all round it. It is full of beautiful trees—pears, pomegranates, and the most delicious apples. There are luscious figs also, and olives in full growth. The fruits never rot nor fail all the year round, neither winter nor summer, for the air is so soft that a new crop ripens before the old has dropped. Pear grows on pear, apple on apple, and fig on fig, and so also with the grapes, for there is an excellent vineyard: on the level ground of a part of this, the grapes are being made into raisins; in another part they are being gathered; some are being trodden in the wine tubs, others further on have shed their blossom and are beginning to show fruit, others again are just changing colour. In the furthest part of the ground there are beautifully arranged beds of flowers that are in bloom all the year round. Two streams go through it, the one turned in ducts throughout the whole garden, while the other is carried under the ground of the outer court to the house itself, and the town’s people draw water from it. Such, then, were the splendours with which the gods had endowed the house of king Alcinous. So here Ulysses stood for a while and looked about him, but when he had looked long enough he crossed the threshold and went within the precincts of the house. There he found all the chief people among the Phaeacians making their drink offerings to Mercury, which they always did the last thing before going away for the night. He went straight through the court, still hidden by the cloak of darkness in which Minerva had enveloped him, till he reached Arete and King Alcinous; then he laid his hands upon the knees of the queen, and at that moment the miraculous darkness fell away from him and he became visible. Every one was speechless with surprise at seeing a man there, but Ulysses began at once with his petition. [61] “Queen Arete,” he exclaimed, “daughter of great Rhexenor, in my distress I humbly pray you, as also your husband and these your guests (whom may heaven prosper with long life and happiness, and may they leave their possessions to their children, and all the honours conferred upon them by the state) to help me home to my own country as soon as possible; for I have been long in trouble and away from my friends.” Then he sat down on the hearth among the ashes and they all held their peace, till presently the old hero Echeneus, who was an excellent speaker and an elder among the Phaeacians, plainly and in all honesty addressed them thus: “Alcinous,” said he, “it is not creditable to you that a stranger should be seen sitting among the ashes of your hearth; every one is waiting to hear what you are about to say; tell him, then, to rise and take a seat on a stool inlaid with silver, and bid your servants mix some wine and water that we may make a drink offering to Jove the lord of thunder, who takes all well disposed suppliants under his protection; and let the housekeeper give him some supper, of whatever there may be in the house.” When Alcinous heard this he took Ulysses by the hand, raised him from the hearth, and bade him take the seat of Laodamas, who had been sitting beside him, and was his favourite son. A maid servant then brought him water in a beautiful golden ewer and poured it into a silver basin for him to wash his hands, and she drew a clean table beside him; an upper servant brought him bread and offered him many good things of what there was in the house, and Ulysses ate and drank. Then Alcinous said to one of the servants, “Pontonous, mix a cup of wine and hand it round that we may make drink-offerings to Jove the lord of thunder, who is the protector of all well-disposed suppliants.” Pontonous then mixed wine and water, and handed it round after giving every man his drink-offering. When they had made their offerings, and had drunk each as much as he was minded, Alcinous said: “Aldermen and town councillors of the Phaeacians, hear my words. You have had your supper, so now go home to bed. To-morrow morning I shall invite a still larger number of aldermen, and will give a sacrificial banquet in honour of our guest; we can then discuss the question of his escort, and consider how we may at once send him back rejoicing to his own country without trouble or inconvenience to himself, no matter how distant it may be. We must see that he comes to no harm while on his homeward journey, but when he is once at home he will have to take the luck he was born with for better or worse like other people. It is possible, however, that the stranger is one of the immortals who has come down from heaven to visit us; but in this case the gods are departing from their usual practice, for hitherto they have made themselves perfectly clear to us when we have been offering them hecatombs. They come and sit at our feasts just like one of our selves, and if any solitary wayfarer happens to stumble upon some one or other of them, they affect no concealment, for we are as near of kin to the gods as the Cyclopes and the savage giants are.” [62] Then Ulysses said: “Pray, Alcinous, do not take any such notion into your head. I have nothing of the immortal about me, neither in body nor mind, and most resemble those among you who are the most afflicted. Indeed, were I to tell you all that heaven has seen fit to lay upon me, you would say that I was still worse off than they are. Nevertheless, let me sup in spite of sorrow, for an empty stomach is a very importunate thing, and thrusts itself on a man’s notice no matter how dire is his distress. I am in great trouble, yet it insists that I shall eat and drink, bids me lay aside all memory of my sorrows and dwell only on the due replenishing of itself. As for yourselves, do as you propose, and at break of day set about helping me to get home. I shall be content to die if I may first once more behold my property, my bondsmen, and all the greatness of my house.” [63] Thus did he speak. Every one approved his saying, and agreed that he should have his escort inasmuch as he had spoken reasonably. Then when they had made their drink offerings, and had drunk each as much as he was minded they went home to bed every man in his own abode, leaving Ulysses in the cloister with Arete and Alcinous while the servants were taking the things away after supper. Arete was the first to speak, for she recognised the shirt, cloak, and good clothes that Ulysses was wearing, as the work of herself and of her maids; so she said, “Stranger, before we go any further, there is a question I should like to ask you. Who, and whence are you, and who gave you those clothes? Did you not say you had come here from beyond the sea?” And Ulysses answered, “It would be a long story Madam, were I to relate in full the tale of my misfortunes, for the hand of heaven has been laid heavy upon me; but as regards your question, there is an island far away in the sea which is called ‘the Ogygian.’ Here dwells the cunning and powerful goddess Calypso, daughter of Atlas. She lives by herself far from all neighbours human or divine. Fortune, however, brought me to her hearth all desolate and alone, for Jove struck my ship with his thunderbolts, and broke it up in mid-ocean. My brave comrades were drowned every man of them, but I stuck to the keel and was carried hither and thither for the space of nine days, till at last during the darkness of the tenth night the gods brought me to the Ogygian island where the great goddess Calypso lives. She took me in and treated me with the utmost kindness; indeed she wanted to make me immortal that I might never grow old, but she could not persuade me to let her do so. “I stayed with Calypso seven years straight on end, and watered the good clothes she gave me with my tears during the whole time; but at last when the eighth year came round she bade me depart of her own free will, either because Jove had told her she must, or because she had changed her mind. She sent me from her island on a raft, which she provisioned with abundance of bread and wine. Moreover she gave me good stout clothing, and sent me a wind that blew both warm and fair. Days seven and ten did I sail over the sea, and on the eighteenth I caught sight of the first outlines of the mountains upon your coast—and glad indeed was I to set eyes upon them. Nevertheless there was still much trouble in store for me, for at this point Neptune would let me go no further, and raised a great storm against me; the sea was so terribly high that I could no longer keep to my raft, which went to pieces under the fury of the gale, and I had to swim for it, till wind and current brought me to your shores. “There I tried to land, but could not, for it was a bad place and the waves dashed me against the rocks, so I again took to the sea and swam on till I came to a river that seemed the most likely landing place, for there were no rocks and it was sheltered from the wind. Here, then, I got out of the water and gathered my senses together again. Night was coming on, so I left the river, and went into a thicket, where I covered myself all over with leaves, and presently heaven sent me off into a very deep sleep. Sick and sorry as I was I slept among the leaves all night, and through the next day till afternoon, when I woke as the sun was westering, and saw your daughter’s maid servants playing upon the beach, and your daughter among them looking like a goddess. I besought her aid, and she proved to be of an excellent disposition, much more so than could be expected from so young a person—for young people are apt to be thoughtless. She gave me plenty of bread and wine, and when she had had me washed in the river she also gave me the clothes in which you see me. Now, therefore, though it has pained me to do so, I have told you the whole truth.” Then Alcinous said, “Stranger, it was very wrong of my daughter not to bring you on at once to my house along with the maids, seeing that she was the first person whose aid you asked.” “Pray do not scold her,” replied Ulysses; “she is not to blame. She did tell me to follow along with the maids, but I was ashamed and afraid, for I thought you might perhaps be displeased if you saw me. Every human being is sometimes a little suspicious and irritable.” “Stranger,” replied Alcinous, “I am not the kind of man to get angry about nothing; it is always better to be reasonable; but by Father Jove, Minerva, and Apollo, now that I see what kind of person you are, and how much you think as I do, I wish you would stay here, marry my daughter, and become my son-in-law. If you will stay I will give you a house and an estate, but no one (heaven forbid) shall keep you here against your own wish, and that you may be sure of this I will attend tomorrow to the matter of your escort. You can sleep during the whole voyage if you like, and the men shall sail you over smooth waters either to your own home, or wherever you please, even though it be a long way further off than Euboea, which those of my people who saw it when they took yellow-haired Rhadamanthus to see Tityus the son of Gaia, tell me is the furthest of any place—and yet they did the whole voyage in a single day without distressing themselves, and came back again afterwards. You will thus see how much my ships excel all others, and what magnificent oarsmen my sailors are.” [64] Then was Ulysses glad and prayed aloud saying, “Father Jove, grant that Alcinous may do all as he has said, for so he will win an imperishable name among mankind, and at the same time I shall return to my country.” Thus did they converse. Then Arete told her maids to set a bed in the room that was in the gatehouse, and make it with good red rugs, and to spread coverlets on the top of them with woollen cloaks for Ulysses to wear. The maids thereon went out with torches in their hands, and when they had made the bed they came up to Ulysses and said, “Rise, sir stranger, and come with us for your bed is ready,” and glad indeed was he to go to his rest. So Ulysses slept in a bed placed in a room over the echoing gateway; but Alcinous lay in the inner part of the house, with the queen his wife by his side. About HackerNoon Book Series: We bring you the most important technical, scientific, and insightful public domain books. This book is part of the public domain. Urbana, Illinois: Project Gutenberg. Retrieved April 2022 from Homer, 1999. The Odyssey. https://www.gutenberg.org/cache/epub/1727/pg1727-images.html#chap07 This eBook is for the use of anyone anywhere at no cost and with almost no restrictions whatsoever. You may copy it, give it away or re-use it under the terms of the Project Gutenberg License included with this eBook or online at , located at . www.gutenberg.org https://www.gutenberg.org/policy/license.html Photo by on Black Iris Visuals Unsplash

The Odyssey: Book VII

Top Software Development Companies 2022 That Are Growing Fast

The Cosmos SDK had an overhaul to enter the IBC world. This is the story of the architecture and engineering approach to this overhaul. The is live, and we are close to seeing this code live on the . Using Stargate, different sovereign blockchains are already transacting with one another in a multi-chain testnet. Stargate release Cosmos Hub The -once- vision of an internet of blockchains is now a reality. As you may be aware, Regen Network took responsibility for maintaining the . Regen Network was responsible for leading the SDK architecture for the migration to Protobuf, and worked closely with the larger community to engineer the Stargate release. Since Stargate is released now, this is a good time to share more about the technical side of the new Cosmos SDK, including the design principles underpinning the new release, the paradigm of evolutionary schema based development, and the performance increases that the refactoring to Protobuf brings to the Cosmos SDK. Cosmos SDK and stewarded the non-IBC parts of the Stargate release Let’s begin with the big picture. The Stargate v0.40 release of the Cosmos SDK resulted from many teams working in collaboration for almost 10 months. This release took time due to the intersection of three large pieces creating the interconnected software: v0.34, Inter Blockchain Communication (IBC), and the Cosmos SDK. Each codebase brings its own complexity. Bringing the three together in the v0.40 Stargate release brings IBC to the world, running on the most secure state machines possible, with a flexible application development framework. This was the work of a whole community. As a community, we conducted thorough code reviews and many testnet, which decreases release time, but ensures the safety and integrity of the release. Tendermint Core Combining with for a long-running, interoperable distributed system design: semantic versioning evolutionary schema engineering A major design principle around the architecture of the refactored Cosmos SDK is in service to long-running, interoperable distributed systems. Defining stable interfaces for long-running distributed systems must be effectively executed before interesting features can be built and adopted and see large-scale usage. The first elements of executing this vision in the Stargate release are the SDK upgrade module and the upgrade daemon Cosmovisor. Long-running chains need upgrade support. The second major element in the new Stargate SDK was the refactoring of the SDK to Protobuf. Protobuf brings a transformational upgrade in performance and improved UX for clients. However, what drove the architectural decision was an understanding of the importance of evolutionary schema design for a long-running distributed system. A core goal of this engineering paradigm is to try not to break existing functionality when you add new functionality. There are two main ways we accomplish this goal of resisting breaking changes for client developers. One is simple good hygiene and refraining from arbitrary renaming of fields. The other is the use of tools that check for breaking changes in order to ensure architecture and engineering is done in a way that avoids these breaking changes whenever possible. Here is a quick example of what an evolutionary schema approach to software engineering looks like. You will quickly see why it is so important for our goal of stability for client interfaces in service to a long-running, interoperable distributed system. Proto messages have field numbers. This makes it possible to add new fields to a schema and delete unused fields without causing breaking changes for downstream clients. When depreciation occurs, we simply deprecate the whole field and its number, and add a new field with a new number for new functionality. This ensures that clients do not arbitrarily break. For instance, if you were to build a form with the following fields: 1- Name, 2- Date of Birth, 3 — Country, using amino it would be very easy to simply replace 2 — Date of birth with 2- Birthday. This breaks all downstream clients because computers just do what you tell them to. Protobuf makes it easy to check for these sorts of breaking changes and easy to deprecate field 2 if you no longer want to collect Date of Birth information. Instead of clobbering field 2 via renaming, instead, you create a new field 4 — “Account Balance,’’ to add new functionality in a way that downstream clients don’t break, but the update is reflected. This is an essential attribute in creating a stable interface for long-running distributed systems, and Protobuf has the tooling to make developing in this paradigm easy for developers. The tooling for checking and returning an error if changes are breaking is called . Buf allows developers to easily ensure that changes are backward compatible. The term for the process outlined above is called schema evolution. Buf It is important to note that in the evolution of the Cosmos SDK, or any other software, breaking changes will still have to be made. However, we want to reserve breaking changes for very important upgrades, while working hard at the client level to avoid breaking changes whenever possible. We now have the concept of evolutionary schema design under our belts, and understand why it is important for long-running distributed systems like the Cosmos Hub, and other blockchains running on the Cosmos SDK. Let’s explore the concept of Semantic Versioning and it’s importance and relationship to evolutionary schema-based engineering. is a paradigm that dictates how to version software releases. The basic idea is to have consistency in indicating breaking changes to an API in a common way. Implied within it is an engineering paradigm, in which breaking changes are postponed or minimized. For instance, you don’t want to push a software version 2.0 (denoting a large breaking change to your api) just because you can. Instead, you want to focus on a 1.1 release, and then a 1.1.1 after that, in which changes, as much as possible, are not breaking the core API. In the case of the Cosmos SDK, in order to embrace this Semantic Versioning concept, it is very important to apply the evolutionary schema paradigm described above. If you are not careful, Semantic versioning can lead developers to stop worrying about breaking changes as long as they are appropriately named, which is a nightmare for client developers and what we need to avoid in the ecosystem. Instead of being aggressive with breaking changes, we want to postpone large breaking changes as long as possible. The fusion of evolutionary schema with semantic versioning ensures we have discipline about naming breaking changes, while also striving to avoid those breaking changes whenever possible. Semantic Versioning This combination of Semantic versioning for the state machine, and evolutionary schema design for the client interface, is what will make the Cosmos SDK the right mix of stable, customizable, modular, and extensible. These are the attributes needed by developers to ensure that sovereignty AND interoperability, the two core concepts of Cosmos’s blockchain paradigm, are both achieved. 0.40 proto files were released with a beta tag, which means that we may still make some breaking changes, as needed. This is in service to ensure a stable long-running distributed system as the outcome as we march as a community towards SDK 1.0. Regen Network will do everything we can to avoid breaking change, but we are also aware that the battle testing happening in testnets and main nets around the ecosystem could uncover issues that need to be addressed with a schema-breaking change. In short, Protobuf was adopted by the Cosmos Community because it makes it easier to do a better job of something that is already very hard and important: striving to provide stable clients interfaces for as long as possible. Protobuf also brings large performance upgrades due to its use of code generation. This allows more transactions per second using the Tendermint Consensus engine, increasing the performance of a Cosmos SDK. Stargate upgrade tutorials and guides The Stargate upgrade is finally around the corner for every project that uses the Cosmos SDK. Let’s examine how the upgrade will take part. In order to use the IBC module, be up-to-date with the latest Cosmos SDK version, and benefit from the latest feature it is recommended to upgrade to the newest version. As stated above, the most notable upgrades are ProtoBufs, Light Clients, IBC, State synchronization, and relayers. We have prepared a range of documents and specifications that you can dive deeper in order to understand the changes coming to the Cosmos SDK. On February 18th, 6 am UTC the Cosmoshub-3 will halt and all full node operators and validators are required to upgrade. Please see the following documents on how this will take effect, how you can prepare, and what to do when the day arrives. Hub migration for validators Guidance for full node operators You might want to update your applications for the Stargate upgrade. The following tutorial should guide you on how to set up a local development environment to work with and test your application functionality. How to create a local testnet (Gaia v4.0) and frontend send and receive transactions If you have a working blockchain that uses the Cosmos SDK, @lukeitsbrian has created an example case on how to upgrade your module from a previous Cosmos SDK module to the next generation Tendermint v0.41.0 How to migrate from launchpad (Tendermint v0.37) to Stargate (Tendermint v0.41) If you want to start a new application with the stargate version, check the blog tutorial on how to create a blockchain application in minutes with starport. Write an application with starport on stargate (Tendermint v0.41), blog tutorial If you are interested in more documentation around IBC Written with the support of and the Tendermint Team. Aaron Craelius Previously published here

What Came Along with the Stargate Release: Cosmos SDK v0.40+

Interesting times, we live in. Scrolling through social media can be a stark reminder of harsh realities. It's easy to get lost in the noise and challenges of being a person in the world today. Maybe you've resorted to self-soothing by eating cheap fries and acting like a couch potato, maybe more often than you like to admit. Well, I'm here to tell you health problems you incur in the future (as a result of your pandemic coping mechanisms) could leave a bigger hole in your pocket than Elon's left in the crypto community. When you're ready to start focusing on your fitness again, you're likely to faced with another challenge: information overload. There are so many conversations around the topics health and wellness, and that's how it should be: health and wellness are extremely broad concepts. And there's no one-size-fits-all. To help you define what wellness means for , I'll be sharing The Seven Scope Framework for approaching your personal wellness in a holistic and customised way. you When doctors talk about being healthy, they do not mean not being sick. Health is beyond the physical; it extends to the social, physical, and mental well-being of an individual. It should be the goal of everyone to achieve good health. Wellness is living a lifestyle that is centered on being healthy. For example; a clean diet, mindfulness, meditation, exercise, and regular drinking of water are components of wellness. Think of wellness as everything you can do to achieve and maintain good health. When Did People Start Practising Wellness? Human beings have always sought out ways to improve their health from the days of the Greek philosophers to date. In 1950, an American physician by the name of Halbert Dunn coined the word, "wellness" by integrating wellbeing and fitness. Subsequently, in 1990 an American sports physician by the name of Kenneth.H.Cooper released his book on wellness titled . Aerobics Program For Total Well Being In his book, he emphasized the fact that in exercise for maintaining good health. In his words: wellness is a lifestyle, and consistency is important "Exercise is a journey, not a destination. It must be continued for the rest of your life. We do not stop exercising because we grow old - we grow old because we stop exercising." These days, social media has provided a good platform for health workers, physical trainers, and nutritionists to educate people on how to achieve and maintain good health. Some websites and applications are designed to help people understand exactly what wellness means. If you search Product Hunt right now, you'll find a plethora of apps aiming to help users understand the concept of Wellness in more effective ways; , , and to name but a few. The Wellness App Wellnest Buddy What is the Seven Scope Framework for Wellness? The scope of wellness is quite broad: there are many aspects to maintaining a healthy lifestyle. In the seven scope classification, wellness is divided into seven components: Spiritual, Physical, Mental, Environmental, Career, Intellectual and Emotional components. The Seven Scopes and 21 Apps to Help You Attain Them Each component has its own significance and unique contribution to sustaining a sense of wellness, in varying ways for each individual. The is concerned with maintaining internal peace and harmony by surrendering to a force or purpose greater and bigger than yourself, on an individual level. The concept of spiritual wellness is quite controversial, but there is a clear correlation between faith, happiness, and good health. Apps like , , and are used to maintain spiritual wellness. Spiritual Scope of Wellness Gaia ConZentrate Spirit Junkie The involves taking care of your body and maintaining an amount of physical activity that is required for good health, but not enough to cause fatigue. The basic components of the physical scope of wellness are diet, rest, and exercise. , , and are great apps for keeping fit and healthy. Physical Scope of Wellness MyFitnessPal 10K Runner 30 Days Exercise at Home is concerned with how well you react to stress, how you feel about yourself, and how you interact with people. Maintaining mental wellness may involve meditation, engaging in hobbies, volunteering, and self-expression. , , and are apps that you can use to improve your mental health and strengthen your mind. The Mental Scope of Wellness Moodfit Happify Shine involves trying to understand your environment, protect your surroundings and contribute positively to the development of the area in which you live. , , and are mobile apps that will help you contribute positively to the preservation of our planet. The Environmental Scope of Wellness #climate Ecoviate Farmstand is engaging in work that is in line with your interests and personal values, as well as providing satisfaction for the employee. , , and are great apps for career growth and wellness. The Career Scope of Wellness VantageFit Elevate Endomondo involves having a positive mindset towards acquiring knowledge and being open-minded. , and provide opportunities to learn from the best teachers and acquire knowledge. The Intellectual Scope of Wellness TED Talks Coursera LinkedIn Learning is related to that of mental wellness. It involves self-awareness and self-acceptance, as well as the ability to adapt to stress. , and are three apps that can support you if you're looking to work towards greater self-acceptance and practice self love. The Emotional Scope of Wellness Sanvello HeadSpace TalkSpace How Can We Achieve Complete Wellness? The scope of wellness is broad: it is most likely that any given individual would be lacking in some areas of wellness. However, it is possible to improve one's state of wellness by being intentional about one's health. The journey to improving wellness is a marathon, not a sprint. Gradual consistent efforts will pay off in the long run, but they will require patience and discipline. If you're serious about increasing your sense of what wellness means, the following four tips will be helpful for you. Have a set goal in mind. As a medical student, I have realized that people who have set health goals usually achieve better health in the long run. In my opinion, if weight loss is the goal, write it down. If you want to feel better or get a job that you love, include your goal in your Notes app. Mobile applications like MyFitnessPal, Mindful, Rise, and Nike + Training can help you achieve your fitness goals. After documenting your goal, work towards it consistently. You may have a few bad days, but there will be many good days. Tell your friends and family. Accountability is very important; having someone to remind you when you are slipping up is key. Tell your friends that you have decided to eat healthier and their eye rolls when you reach for the fries will be what you need to stay in check. Ask your family to remind you to go to the gym or meditate and watch your consistency grow. Get enough rest. Fatigue and sleep deprivation are linked with stress, unhealthy eating, and angry outbursts. If you want to improve your physical and mental wellness, get the required seven to eight hours of solid sleep. You can sneak in naps from time to time so that you feel energized and ready to kick the ball. Avoid risky unhealthy behaviors. Habits such as excessive drinking, smoking, drug use, and having multiple sexual partners are not going to improve your wellness. These habits are linked with diseases, accidents, mental illness, and a shorter life span. For improved wellness, avoid risky unhealthy behaviors. Find your tribe: In the area where you live, there are people like you committed to achieving their wellness goals. Find them and watch yourself grow. Healthy Minds, Healthy Bodies: The Possibility When wellness is discussed, the focus is usually on physical wellness and fitness. Beyond the toned body and ripped abs, you deserve to be happy and feel in tune with your job, home, and environment. It may seem overwhelming, having to achieve all your goals in the seven scope framework of wellness, but you are more than capable of achieving anything that you set your mind to. And getting support from today's smartest apps in never a bad idea. Having a healthy mind and body is possible; with effort and consistency, you can achieve your goal.

The 7 Scopes of Wellness and 21 Apps to Help You Attain Them

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