Microlensing Events: A Closer Look at Stars
Discover how microlensing reveals hidden stars through unusual light patterns.
Cheongho Han, Andrzej Udalski, Ian A. Bond, Chung-Uk Lee, Andrew Gould, Michael D. Albrow, Sun-Ju Chung, Kyu-Ha Hwang, Youn Kil Jung, Yoon-Hyun Ryu, Yossi Shvartzvald, In-Gu Shin, Jennifer C. Yee, Hongjing Yang, Weicheng Zang, Sang-Mok Cha, Doeon Kim, Dong-Jin Kim, Seung-Lee Kim, Dong-Joo Lee, Yongseok Lee, Byeong-Gon Park, Richard W. Pogge, Przemek Mróz, Michał K. Szymański, Jan Skowron, Radosław Poleski, Igor Soszyński, Paweł Pietrukowicz, Szymon Kozłowski, Krzysztof A. Rybicki, Patryk Iwanek, Krzysztof Ulaczyk, Marcin Wrona, Mariusz Gromadzki, Mateusz J. Mróz, Fumio Abe, Richard Barry, David P. Bennett, Aparna Bhattacharya, Hirosame Fujii, Akihiko Fukui, Ryusei Hamada, Yuki Hirao, Stela Ishitani Silva, Yoshitaka Itow, Rintaro Kirikawa, Naoki Koshimoto, Yutaka Matsubara, Shota Miyazaki, Yasushi Muraki, Greg Olmschenk, Clément Ranc, Nicholas J. Rattenbury, Yuki Satoh, Takahiro Sumi, Daisuke Suzuki, Mio Tomoyoshi, Paul J. Tristram, Aikaterini Vandorou, Hibiki Yama, Kansuke Yamashita
― 4 min read
Table of Contents
Microlensing is a fun way to observe hidden stars by looking for the light they bend. Imagine someone is holding a magnifying glass to a distant star. When another star passes in front of it, it can act like that magnifying glass, making the distant star appear brighter. This is what scientists call microlensing.
KMTNet and Others
The Players:The Korea Microlensing Telescope Network (KMTNet) is a group that uses wide-field telescopes to keep an eye on the sky. They have three telescopes in the Southern Hemisphere, and they send the data they collect back to Korea almost in real-time. They’re like the sky's watchdogs, always looking for light shows!
The Events
We’re interested in three specific microlensing events: KMT-2021-BLG-0284, KMT-2022-BLG-2480, and KMT-2024-BLG-0412. Think of these as three different light shows happening out there in space, each with its own style and quirks.
KMT-2021-BLG-0284: The Show Begins
KMT-2021-BLG-0284 was a real star of the show. It caught the attention of the KMTNet team back in April 2021. This event had some wild light patterns that made it tough to explain with the usual models.
When scientists looked closer, they noticed multiple spikes in brightness. It was as if the stars were giving a thumbs-up to the audience! After some brainstorming, they came up with a new model to explain what they saw. This turned out to show that the event involved two stars, likely both M dwarf stars - that’s science lingo for small, cool stars.
KMT-2022-BLG-2480: The Sequel
Just like a blockbuster movie, KMT-2022-BLG-2480 had its premiere soon after in 2022. This time, the event kept the audience on the edge of their seats, showing four major spikes in brightness during its run.
When scientists tried to make sense of it, they realized that their old model didn't quite fit anymore. After some tweaking and adjustments, they found that adding in an extra source star made everything click into place. The event was made up of two sources, with the primary one being a tricky early K-type Star mixed with an M dwarf friend.
KMT-2024-BLG-0412: The Grand Finale
The final act, KMT-2024-BLG-0412, made its appearance in 2024 with a bang. The KMTNet team caught it early on, and once again, things got complex.
What made this event so interesting was the way the light curve shaped up, showing both sharp rises and mysterious bumps. Despite the chaos, the scientists were able to use their newly developed model to figure out what was happening. They discovered that the event featured two stars again, one heavier than the other and likely situated in the bulge of our galaxy.
Anomalies
The Mystery ofNow, what’s an anomaly, you ask? Good question! An anomaly is basically a sneaky surprise in the data that leads scientists to scratch their heads.
In these events, the light curves weren’t smooth sailing. They had ups and downs that simply couldn’t be explained by the usual models, which led scientists to believe that there were more stars involved than initially thought.
The Science Behind the Madness
The scientists used something called Bayesian analysis, which sounds fancy but is just a method to predict outcomes based on previous data. This helped them determine the mass and distance of the different stars involved.
What They Found
After lots of note-taking, data crunching, and model fitting, the scientists found that KMT-2021-BLG-0284 and KMT-2024-BLG-0412 were likely systems with two M dwarf stars. Meanwhile, KMT-2022-BLG-2480 featured a K-type star alongside its M dwarf buddy.
Chances are good that the two systems with M dwarfs were hanging out in the bulge of our galaxy, while the K-type star was more of a free spirit, floating around in the disk.
Why Do We Care?
Why should we get excited about this? Well, studying these events helps astronomers learn about star formation, the nature of galaxies, and the overall behavior of gravity in the universe. These events are like clues in a cosmic scavenger hunt, helping us understand our place in the vastness of space.
Conclusion: The Takeaway
The adventures of KMT-2021-BLG-0284, KMT-2022-BLG-2480, and KMT-2024-BLG-0412 show us just how lively the universe can be. The KMTNet team continues to uncover exciting light shows across the sky, reminding us that there's always more to discover and explore out there, one anomaly at a time. And remember, if you ever find yourself in the night sky wondering about those twinkling stars, just think: they might be putting on their own microlensing show for us!
Title: KMT-2021-BLG-0284, KMT-2022-BLG-2480, and KMT-2024-BLG-0412: Three microlensing events involving two lens masses and two source stars
Abstract: We carried out a project involving the systematic analysis of microlensing data from the Korea Microlensing Telescope Network survey. The aim of this project is to identify lensing events with complex anomaly features that are difficult to explain using standard binary-lens or binary-source models. Our investigation reveals that the light curves of microlensing events KMT-2021-BLG-0284, KMT-2022-BLG-2480, and KMT-2024-BLG-0412 display highly complex patterns with three or more anomaly features. These features cannot be adequately explained by a binary-lens (2L1S) model alone. However, the 2L1S model can effectively describe certain segments of the light curve. By incorporating an additional source into the modeling, we identified a comprehensive model that accounts for all the observed anomaly features. Bayesian analysis, based on constraints provided by lensing observables, indicates that the lenses of KMT-2021-BLG-0284 and KMT-2024-BLG-0412 are binary systems composed of M dwarfs. For KMT-2022-BLG-2480, the primary lens is an early K-type main-sequence star with an M dwarf companion. The lenses of KMT-2021-BLG-0284 and KMT-2024-BLG-0412 are likely located in the bulge, whereas the lens of KMT-2022-BLG-2480 is more likely situated in the disk. In all events, the binary stars of the sources have similar magnitudes due to a detection bias favoring binary source events with a relatively bright secondary source star, which increases detection efficiency.
Authors: Cheongho Han, Andrzej Udalski, Ian A. Bond, Chung-Uk Lee, Andrew Gould, Michael D. Albrow, Sun-Ju Chung, Kyu-Ha Hwang, Youn Kil Jung, Yoon-Hyun Ryu, Yossi Shvartzvald, In-Gu Shin, Jennifer C. Yee, Hongjing Yang, Weicheng Zang, Sang-Mok Cha, Doeon Kim, Dong-Jin Kim, Seung-Lee Kim, Dong-Joo Lee, Yongseok Lee, Byeong-Gon Park, Richard W. Pogge, Przemek Mróz, Michał K. Szymański, Jan Skowron, Radosław Poleski, Igor Soszyński, Paweł Pietrukowicz, Szymon Kozłowski, Krzysztof A. Rybicki, Patryk Iwanek, Krzysztof Ulaczyk, Marcin Wrona, Mariusz Gromadzki, Mateusz J. Mróz, Fumio Abe, Richard Barry, David P. Bennett, Aparna Bhattacharya, Hirosame Fujii, Akihiko Fukui, Ryusei Hamada, Yuki Hirao, Stela Ishitani Silva, Yoshitaka Itow, Rintaro Kirikawa, Naoki Koshimoto, Yutaka Matsubara, Shota Miyazaki, Yasushi Muraki, Greg Olmschenk, Clément Ranc, Nicholas J. Rattenbury, Yuki Satoh, Takahiro Sumi, Daisuke Suzuki, Mio Tomoyoshi, Paul J. Tristram, Aikaterini Vandorou, Hibiki Yama, Kansuke Yamashita
Last Update: 2024-11-13 00:00:00
Language: English
Source URL: https://arxiv.org/abs/2411.09096
Source PDF: https://arxiv.org/pdf/2411.09096
Licence: https://creativecommons.org/licenses/by/4.0/
Changes: This summary was created with assistance from AI and may have inaccuracies. For accurate information, please refer to the original source documents linked here.
Thank you to arxiv for use of its open access interoperability.