Light curve of microlensing MOA-2019-BLG-008L Virtual Observatory Resource

Authors

1. Bachelet E.
2. Tsapras Y.
3. Gould A.
4. Street R.A.
5. Bennett D.P.,Hundertmark M.P.G.
6. Bozza V.
7. Bramich D.M.
8. Cassan A.
9. Dominik M.
10. Horne K.,Mao S.
11. Saha A.
12. Wambsganss J.
13. Zang W.
14. Abe F.
15. Barry R.
16. Bennett D.P.,Bhattacharya A.
17. Bond I.A.
18. Fukui A.
19. Fujii H.
20. Hirao Y.
21. Itow Y.,Kirikawa R.
22. Kondo I.
23. Koshimoto N.
24. Matsubara Y.
25. Matsumoto S.,Miyazaki S.
26. Muraki Y.
27. Olmschenk G.
28. Ranc C.
29. Okamura A.
30. Rattenbury N.J.,Satoh Y.
31. Sumi T.
32. Suzuki D.
33. Silva S.I.
34. Toda T.
35. Tristram P..J.,Vandorou A.
36. Yama H.
37. Albrow M.D.
38. Chung S.-J.
39. Han C.
40. Hwang K.-H.,Jung Y.K.
41. Ryu Y.-H.
42. Shin I.-G.
43. Shvartzvald Y.
44. Yee J.C.
45. Cha S.-M.,Kim D.-J.
46. Kim S.-L.
47. Lee C.-U.
48. Lee D.-J.
49. Lee Y.
50. Park B.-G.
51. Pogge R.W.,Udalski A.
52. Mroz P.
53. Poleski R.
54. Skowron J.
55. Szymanski M.K.
56. Soszynski I.,Pietrukowicz P.
57. Kozlowski S.
58. Ulaczyk K.
59. Rybicki K.A.
60. Iwanek P.,Wrona M.
61. Gromadzki M.
62. The ROME/REA Collaboration
63. The MOA Collaboration,The KMTNet Collaboration
64. The OGLE Collaboration

Published by

CDS

Abstract

We report on the observations, analysis and interpretation of the microlensing event MOA-2019-BLG-008. The observed anomaly in the photometric light curve is best described through a binary lens model. In this model, the source did not cross caustics and no finite-source effects were observed. Therefore, the angular Einstein ring radius {theta}E cannot be measured from the light curve alone. However, the large event duration, tE~80days, allows a precise measurement of the microlensing parallax {pi}E. In addition to the constraints on the angular radius {theta}* and the apparent brightness Is of the source, we employ the Besancon and GalMod galactic models to estimate the physical properties of the lens. We find excellent agreement between the predictions of the two galactic models: the companion is likely a resident of the brown dwarf desert with a mass Mp~30MJup, and the host is a main-sequence dwarf star. The lens lies along the line of sight to the Galactic bulge, at a distance of <~4kpc. We estimate that in about 10 yr the lens and source will be separated by ~55mas, and it will be possible to confirm the exact nature of the lensing system by using high-resolution imaging from ground- or space-based observatories.

Keywords

1. gravitational-lensing
2. brown-dwarfs
3. exoplanets
4. infrared-photometry
5. visible-astronomy
6. photometry

Bibliographic source Bibcode

2022AJ....164...75B

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https://cdsarc.cds.unistra.fr/viz-bin/cat/J/AJ/164/75

IVOA Identifier IVOID

ivo://CDS.VizieR/J/AJ/164/75

Document Object Identifer DOI

doi:10.26093/cds/vizier.51640075

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http://vizieridia.saao.ac.za/viz-bin/VizieR-2?-source=J/AJ/164/75

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