MOA-2019-BLG-008Lb: A New Microlensing Detection of an Object at the Planet/Brown Dwarf Boundary

MOA-2019-BLG-008Lb: A New Microlensing Detection of an Object at the Planet/Brown Dwarf Boundary
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DOI：
10.3847/1538-3881/ac78ed
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发表时间：
2022-05
期刊：
The Astronomical Journal
影响因子：
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通讯作者：
E. Bachelet;Y. Tsapras;A. Gould;R. Street;D. Bennett;M. Hundertmark;V. Bozza;D. Bramich;A. Cassan;M. Dominik;K. Horne;S. Mao;A. Saha;J. Wambsganss;W. Zang;F. Abe;R. Barry;D. Bennett;A. Bhattacharya;I. Bond;A. Fukui;H. Fujii;Y. Hirao;Y. Itow;R. Kirikawa;I. Kondo;N. Koshimoto;Y. Matsubara;Sho Matsumoto;S. Miyazaki;Y. Muraki;G. Olmschenk;C. Ranc;A. Okamura;N. Rattenbury;Y. Satoh;T. Sumi;D. Suzuki;S. I. Silva;T. Toda;P. Tristram;A. Vandorou;H. Yama;M. Albrow;S. Chung;C. Han;K. Hwang;Y. Jung;Y. Ryu;I. Shin;Y. Shvartzvald;J. Yee;S. Cha;Dong-Jin Kim;Seung-Lee Kim;Chung-Uk Lee;Dong-Joo Lee;Yongseok Lee;B.-G. Park;R. Pogge;A. Udalski;P. Mróz;R. Poleski;J. Skowron;M. Szymański;I. Soszyński;P. Pietrukowicz;S. Kozłowski;K. Ulaczyk;K. Rybicki;P. Iwanek;M. Wrona;M. Gromadzki
E. Bachelet;Y. Tsapras;A. Gould;R. Street;D. Bennett;M. Hundertmark;V. Bozza;D. Bramich;A. Cassan;M. Dominik;K. Horne;S. Mao;A. Saha;J. Wambsganss;W. Zang;F. Abe;R. Barry;D. Bennett;A. Bhattacharya;I. Bond;A. Fukui;H. Fujii;Y. Hirao;Y. Itow;R. Kirikawa;I. Kondo;N. Koshimoto;Y. Matsubara;Sho Matsumoto;S. Miyazaki;Y. Muraki;G. Olmschenk;C. Ranc;A. Okamura;N. Rattenbury;Y. Satoh;T. Sumi;D. Suzuki;S. I. Silva;T. Toda;P. Tristram;A. Vandorou;H. Yama;M. Albrow;S. Chung;C. Han;K. Hwang;Y. Jung;Y. Ryu;I. Shin;Y. Shvartzvald;J. Yee;S. Cha;Dong-Jin Kim;Seung-Lee Kim;Chung-Uk Lee;Dong-Joo Lee;Yongseok Lee;B.-G. Park;R. Pogge;A. Udalski;P. Mróz;R. Poleski;J. Skowron;M. Szymański;I. Soszyński;P. Pietrukowicz;S. Kozłowski;K. Ulaczyk;K. Rybicki;P. Iwanek;M. Wrona;M. Gromadzki
中科院分区：
其他
文献类型：
--
作者：
E. Bachelet;Y. Tsapras;A. Gould;R. Street;D. Bennett;M. Hundertmark;V. Bozza;D. Bramich;A. Cassan;M. Dominik;K. Horne;S. Mao;A. Saha;J. Wambsganss;W. Zang;F. Abe;R. Barry;D. Bennett;A. Bhattacharya;I. Bond;A. Fukui;H. Fujii;Y. Hirao;Y. Itow;R. Kirikawa;I. Kondo;N. Koshimoto;Y. Matsubara;Sho Matsumoto;S. Miyazaki;Y. Muraki;G. Olmschenk;C. Ranc;A. Okamura;N. Rattenbury;Y. Satoh;T. Sumi;D. Suzuki;S. I. Silva;T. Toda;P. Tristram;A. Vandorou;H. Yama;M. Albrow;S. Chung;C. Han;K. Hwang;Y. Jung;Y. Ryu;I. Shin;Y. Shvartzvald;J. Yee;S. Cha;Dong-Jin Kim;Seung-Lee Kim;Chung-Uk Lee;Dong-Joo Lee;Yongseok Lee;B.-G. Park;R. Pogge;A. Udalski;P. Mróz;R. Poleski;J. Skowron;M. Szymański;I. Soszyński;P. Pietrukowicz;S. Kozłowski;K. Ulaczyk;K. Rybicki;P. Iwanek;M. Wrona;M. Gromadzki

文献摘要

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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 θ E cannot be measured from the light curve alone. However, the large event duration, t E ∼ 80 days, allows a precise measurement of the microlensing parallax π E. In addition to the constraints on the angular radius θ * and the apparent brightness I s of the source, we employ the Besançon 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 M p ∼ 30 M Jup, 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 ≤4 kpc. We estimate that in about 10 yr the lens and source will be separated by ∼55 mas, 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.