Systematic reanalysis of KMTNet microlensing events, paper I: Updates of the photometry pipeline and a new planet candidate

Author:

Yang HongjingORCID,Yee Jennifer C1ORCID,Hwang Kyu-Ha2,Qian QiyueORCID,Bond Ian A3,Gould Andrew45,Hu ZhechengORCID,Zhang JiyuanORCID,Mao ShudeORCID,Zhu WeiORCID,Albrow Michael D6ORCID,Chung Sun-Ju2,Kim Seung-Lee27,Park Byeong-Gon27,Han Cheongho8,Jung Youn Kil2,Ryu Yoon-Hyun2,Shin In-Gu1,Shvartzvald Yossi9,Cha Sang-Mok210ORCID,Kim Dong-Jin2,Kim Hyoun-Woo2,Lee Chung-Uk2,Lee Dong-Joo2,Lee Yongseok210,Pogge Richard W24,Zang WeichengORCID,Abe Fumio11,Barry Richard12,Bennett David P1213,Bhattacharya Aparna1213,Donachie Martin14,Fujii Hirosane15,Fukui Akihiko1617,Hirao Yuki15,Itow Yoshitaka1115,Kirikawa Rintaro15,Kondo Iona15,Koshimoto Naoki1819,Silva Stela Ishitani1220,Li Man Cheung Alex14,Matsubara Yutaka11,Muraki Yasushi11,Suzuki Daisuke21,Tristram Paul J22,Yonehara Atsunori23,Ranc Clément24,Miyazaki Shota15,Olmschenk Greg12,Rattenbury Nicholas J14,Satoh Yuki15,Shoji Hikaru15,Sumi Takahiro15,Tanaka Yuzuru15,Yamawaki Tsubasa15

Affiliation:

1. Center for Astrophysics | Harvard & Smithsonian 60 Garden St. , Cambridge, MA 02138 , USA

2. Korea Astronomy and Space Science Institute , Daejon 34055 , South Korea

3. Institute of Natural and Mathematical Sciences, Massey University , Auckland 0745 , New Zealand

4. Max-Planck-Institute for Astronomy , Königstuhl 17, D-69117 Heidelberg , Germany

5. Department of Astronomy, Ohio State University , 140 W. 18th Avenue, Columbus, OH 43210 , USA

6. Department of Physics and Astronomy, University of Canterbury , Private Bag 4800, Christchurch 8020 , New Zealand

7. University of Science and Technology, Korea, (UST) , 217 Gajeong-ro Yuseong-gu, Daejeon 34113 , South Korea

8. Department of Physics, Chungbuk National University , Cheongju 28644 , South Korea

9. Department of Particle Physics and Astrophysics, Weizmann Institute of Science , Rehovot 76100 , Israel

10. School of Space Research, Kyung Hee University , Yongin, Kyeonggi 17104 , South Korea

11. Institute for Space-Earth Environmental Research, Nagoya University , Nagoya 464-8601 , Japan

12. Code 667, NASA Goddard Space Flight Center , Greenbelt, MD 20771 , USA

13. Department of Astronomy, University of Maryland , College Park, MD 20742 , USA

14. Department of Physics, University of Auckland , Private Bag 92019, Auckland , New Zealand

15. Department of Earth and Space Science, Graduate School of Science, Osaka University , Toyonaka, Osaka 560-0043 , Japan

16. Department of Earth and Planetary Science, Graduate School of Science, The University of Tokyo , 7-3-1 Hongo, Bunkyo-ku, Tokyo 113-0033 , Japan

17. Instituto de Astrofísica de Canarias , Vía Láctea s/n, E-38205 La Laguna, Tenerife , Spain

18. Department of Astronomy, Graduate School of Science, The University of Tokyo , 7-3-1 Hongo, Bunkyo-ku, Tokyo 113-0033 , Japan

19. National Astronomical Observatory of Japan , 2-21-1 Osawa, Mitaka, Tokyo 181-8588 , Japan

20. Department of Physics, The Catholic University of America , Washington, DC 20064 , USA

21. Institute of Space and Astronautical Science, Japan Aerospace Exploration Agency , 3-1-1 Yoshinodai, Chuo, Sagamihara, Kanagawa, 252-5210 , Japan

22. University of Canterbury Mt. John Observatory , PO Box 56, Lake Tekapo 8770 , New Zealand

23. Department of Physics, Faculty of Science, Kyoto Sangyo University , 603-8555 Kyoto , Japan

24. Sorbonne Université, CNRS, Institut d’Astrophysique de Paris, IAP , F-75014 Paris , France

Abstract

ABSTRACT In this work, we update and develop algorithms for KMTNet tender-love care (TLC) photometry in order to create a new, mostly automated, TLC pipeline. We then start a project to systematically apply the new TLC pipeline to the historic KMTNet microlensing events, and search for buried planetary signals. We report the discovery of such a planet candidate in the microlensing event MOA-2019-BLG-421/KMT-2019-BLG-2991. The anomalous signal can be explained by either a planet around the lens star or the orbital motion of the source star. For the planetary interpretation, despite many degenerate solutions, the planet is most likely to be a Jovian planet orbiting an M or K dwarf, which is a typical microlensing planet. The discovery proves that the project can indeed increase the sensitivity of historic events and find previously undiscovered signals.

Funder

KASI

National Natural Science Foundation of China

NSF

Publisher

Oxford University Press (OUP)

Subject

Space and Planetary Science,Astronomy and Astrophysics

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