dc.contributor.author |
Han, C |
en |
dc.contributor.author |
Lee, C-U |
en |
dc.contributor.author |
Udalski, A |
en |
dc.contributor.author |
Gould, A |
en |
dc.contributor.author |
Bond, IA |
en |
dc.contributor.author |
Bozza, V |
en |
dc.contributor.author |
Albrow, MD |
en |
dc.contributor.author |
Chung, S-J |
en |
dc.contributor.author |
Hwang, K-H |
en |
dc.contributor.author |
Jung, YK |
en |
dc.contributor.author |
Ryu, Y-H |
en |
dc.contributor.author |
Shin, I-G |
en |
dc.contributor.author |
Shvartzvald, Y |
en |
dc.contributor.author |
Yee, JC |
en |
dc.contributor.author |
Zang, W |
en |
dc.contributor.author |
Cha, S-M |
en |
dc.contributor.author |
Kim, D-J |
en |
dc.contributor.author |
Kim, H-W |
en |
dc.contributor.author |
Kim, S-L |
en |
dc.contributor.author |
Lee, D-J |
en |
dc.contributor.author |
Lee, Y |
en |
dc.contributor.author |
Park, B-G |
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dc.contributor.author |
Pogge, RW |
en |
dc.contributor.author |
Jee, MJ |
en |
dc.contributor.author |
Kim, D |
en |
dc.contributor.author |
Mróz, P |
en |
dc.contributor.author |
Szymański, MK |
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dc.contributor.author |
Skowron, J |
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dc.contributor.author |
Poleski, R |
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dc.contributor.author |
Soszyński, I |
en |
dc.contributor.author |
Pietrukowicz, P |
en |
dc.contributor.author |
Kozłowski, S |
en |
dc.contributor.author |
Ulaczyk, K |
en |
dc.contributor.author |
Rybicki, KA |
en |
dc.contributor.author |
Iwanek, P |
en |
dc.contributor.author |
Wrona, M |
en |
dc.contributor.author |
Abe, F |
en |
dc.contributor.author |
Barry, R |
en |
dc.contributor.author |
Bennett, DP |
en |
dc.contributor.author |
Bhattacharya, A |
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dc.contributor.author |
Donachie, M |
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dc.contributor.author |
Fujii, H |
en |
dc.contributor.author |
Fukui, A |
en |
dc.contributor.author |
Itow, Y |
en |
dc.contributor.author |
Hirao, Y |
en |
dc.contributor.author |
Kamei, Y |
en |
dc.contributor.author |
Kondo, I |
en |
dc.contributor.author |
Koshimoto, N |
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dc.contributor.author |
Li, MCA |
en |
dc.contributor.author |
Matsubara, Y |
en |
dc.contributor.author |
Muraki, Y |
en |
dc.contributor.author |
Miyazaki, S |
en |
dc.contributor.author |
Nagakane, M |
en |
dc.contributor.author |
Ranc, C |
en |
dc.contributor.author |
Rattenbury, Nicholas |
en |
dc.contributor.author |
Satoh, Y |
en |
dc.contributor.author |
Shoji, H |
en |
dc.contributor.author |
Suematsu, H |
en |
dc.contributor.author |
Sullivan, DJ |
en |
dc.contributor.author |
Sumi, T |
en |
dc.contributor.author |
Suzuki, D |
en |
dc.contributor.author |
Tristram, PJ |
en |
dc.contributor.author |
Yamakawa, T |
en |
dc.contributor.author |
Yamawaki, T |
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dc.contributor.author |
Yonehara, A |
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dc.date.accessioned |
2020-01-10T03:10:09Z |
en |
dc.date.issued |
2019-10-24 |
en |
dc.identifier.citation |
Arxiv (1910.10974v1). 24 Oct 2019. 9 pages |
en |
dc.identifier.uri |
http://hdl.handle.net/2292/49495 |
en |
dc.description.abstract |
Short-timescale microlensing events are likely to be produced by substellar brown dwarfs (BDs), but it is difficult to securely identify BD lenses based on only event timescales $t_{\rm E}$ because short-timescale events can also be produced by stellar lenses with high relative lens-source proper motions. In this paper, we report three strong candidate BD-lens events found from the search for lensing events not only with short timescales ($t_{\rm E} \lesssim 6~{\rm days}$) but also with very small angular Einstein radii ($\theta_{\rm E}\lesssim 0.05~{\rm mas}$) among the events that have been found in the 2016--2019 observing seasons. These events include MOA-2017-BLG-147, MOA-2017-BLG-241, and MOA-2019-BLG-256, in which the first two events are produced by single lenses and the last event is produced by a binary lens. From the Bayesian analysis conducted with the combined $t_{\rm E}$ and $\theta_{\rm E}$ constraint, it is estimated that the lens masses of the individual events are $0.051^{+0.100}_{-0.027}~M_\odot$, $0.044^{+0.090}_{-0.023}~M_\odot$, and $0.046^{+0.067}_{-0.023}~M_\odot/0.038^{+0.056}_{-0.019}~M_\odot$ and the probability of the lens mass smaller than the lower limit of stars is $\sim 80\%$ for all events. We point out that routine lens mass measurements of short time-scale lensing events require survey-mode space-based observations. |
en |
dc.relation.ispartof |
Arxiv |
en |
dc.rights |
Items in ResearchSpace are protected by copyright, with all rights reserved, unless otherwise indicated. Previously published items are made available in accordance with the copyright policy of the publisher. |
en |
dc.rights.uri |
https://researchspace.auckland.ac.nz/docs/uoa-docs/rights.htm |
en |
dc.rights.uri |
https://arxiv.org/licenses/nonexclusive-distrib/1.0/license.html |
en |
dc.subject |
astro-ph.SR |
en |
dc.subject |
astro-ph.SR |
en |
dc.subject |
astro-ph.EP |
en |
dc.title |
Candidate Brown-dwarf Microlensing Events with Very Short Timescales and Small Angular Einstein Radii |
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dc.type |
Report |
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dc.rights.holder |
Copyright: The authors |
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pubs.author-url |
http://arxiv.org/abs/1910.10974v1 |
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dc.rights.accessrights |
http://purl.org/eprint/accessRights/OpenAccess |
en |
pubs.subtype |
Working Paper |
en |
pubs.elements-id |
785094 |
en |
pubs.org-id |
Science |
en |
pubs.org-id |
Physics |
en |
pubs.arxiv-id |
1910.10974 |
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pubs.number |
1910.10974v1 |
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pubs.record-created-at-source-date |
2020-01-13 |
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