2025A&A...702A..53H

Query : 2025A&A...702A..53H

2025A&A...702A..53H - Astronomy and Astrophysics, volume 702A53 (2025/10-1)

Four binary microlenses with directly measured masses.

HAN C., UDALSKI A., LEE C.-U., BOND I.A., ALBROW M.D., CHUNG S.-J., GOULD A., JUNG Y.K., HWANG K.-H., RYU Y.-H., SHVARTZVALD Y., SHIN I.-G., YEE J.C., ZANG W., YANG H., CHA S.-M., KIM D., KIM D.-J., KIM S.-L., LEE D.-J., LEE Y., PARK B.-G., POGGE R.W., MROZ P., SZYMANSKI M.K., SKOWRON J., POLESKI R., SOSZYNSKI I., PIETRUKOWICZ P., KOZLOWSKI S., RYBICKI K.A., IWANEK P., ULACZYK K., WRONA M., GROMADZKI M., MROZ M.J., JAROSZYNSKI M., KIRAGA M., ABE F., BENNETT D.P., BHATTACHARYA A., FUKUI A., HAMADA R., ISHITANI SILVA S., HIRAO Y., KOSHIMOTO N., MATSUBARA Y., MIYAZAKI S., MURAKI Y., NAGAI T., NUNOTA K., OLMSCHENK G., RANC C., RATTENBURY N.J., SATOH Y., SUMI T., SUZUKI D., TERRY S.K., TRISTRAM P.J., VANDOROU A. and YAMA H.

Abstract (from CDS):

Aims. We investigated binary-lens events from the 2022-2024 microlensing surveys, aiming to identify events suitable for lens mass measurements. We focused on two key light curve features: distinct caustic spikes with resolved crossings for measuring the angular Einstein radius (θE), and long durations enabling microlens-parallax (πE) measurements. Four events met these criteria: KMT-2022-BLG-1479, KMT-2023-BLG-0932, OGLE-2024-BLG-0142, and KMT-2024-BLG-1309.
Methods. We estimated the angular Einstein radius by combining the normalized source radius measured by modeling the resolved caustic spikes with the angular source radius derived from the source color and magnitude. Additionally, we determined the microlens parallax through light curve modeling, taking higher-order effects caused by the orbital motions of Earth and the binary lens into consideration.
Results. With measurements of the event timescale, angular Einstein radius, and microlens parallax, we uniquely determined the mass and distance of the lens. For the events KMT-2022-BLG-1479, KMT-2023-BLG-0932, and KMT-2024-BLG-1309, both components of the binary lens have masses lower than that of the Sun, consistent with M-type dwarfs, which are the most common type of lenses in Galactic microlensing events. These lenses are relatively nearby, with distances of ≲2.5 kpc, indicating their location within the Galactic disk. In contrast, for OGLE-2024-BLG-0142, the primary lens component has a mass similar to that of the Sun, while the companion lens component has about half the mass of the primary. This lens system is situated at a greater distance, roughly 4.5 kpc.

Abstract Copyright: © The Authors 2025

Journal keyword(s): gravitational lensing: micro

Simbad objects: 23

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Number of rows : 23
N Identifier Otype ICRS (J2000)
RA 		ICRS (J2000)
DEC 		Mag U Mag B Mag V Mag R Mag I Sp type #ref
1850 - 2026 		#notes
1 OGLE-2011-BLG-0417 * 17 34 33.11 -27 06 39.3           ~ 17 0
2 KMT-2016-BLG-2052 ev 17 41 19.500 -27 40 19.67           ~ 2 0
3 OGLE-2003-BUL-267 * 17 42 28.86 -23 27 15.3           ~ 4 0
4 OGLE-2014-BLG-1050 BD? 17 45 07.83 -22 54 20.0           ~ 8 0
5 MOA 2009-BLG-16 * 17 50 32.080 -34 21 10.06           ~ 5 0
6 OGLE-2016-BLG-0168 * 17 50 49.89 -31 45 30.1           ~ 6 0
7 MOA 2015-BLG-20 * 17 52 52.780 -32 29 08.91           ~ 4 0
8 EROS BLG 2000 5 * 17 53 11.43 -30 55 34.4           K3III 37 0
9 KMT-2022-BLG-1479 Lev 17 53 23.690 -28 06 34.20           ~ 1 0
10 OGLE-2016-BLG-0156 * 17 56 36.63 -31 04 40.7           ~ 3 0
11 OGLE-2007-BLG-050 * 17 58 19.39 -28 38 59.0           ~ 11 0
12 OGLE-2017-BLG-1038 * 17 58 36.5542846897 -27 18 58.325343982           ~ 3 0
13 KMT-2018-BLG-2336 Lev 17 59 01.630 -28 13 42.20           ~ 3 0
14 KMT-2023-BLG-2430 Lev 18 00 35.680 -29 13 23.95           ~ 3 0
15 MOA 2009-BLG-174 * 18 02 07.70 -31 25 26.4           FV 12 0
16 KMT-2024-BLG-1309 Lev 18 04 10.720 -28 10 53.62           ~ 1 0
17 OGLE-2009-BLG-020 * 18 04 20.960 -29 31 08.96           ~ 12 0
18 2MASS J18083825-3003386 ** 18 08 38.2563956550 -30 03 38.728877436         15.711 ~ 3 0
19 KMT-2023-BLG-2849 Lev 18 09 16.970 -30 36 47.00           ~ 3 0
20 MOA 2011-BLG-90 * 18 10 29.850 -26 38 43.03           ~ 13 0
21 KMT-2024-BLG-0813 Lev 18 10 34.710 -27 46 37.20           ~ 1 0
22 MOA 2016-BLG-339 * 18 12 49.0702747824 -27 00 45.565682832           ~ 12 0
23 KMT-2023-BLG-0932 Lev 18 15 11.730 -25 04 31.19           ~ 1 0

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