J/AJ/162/17 KMTNet, MOA and OGLE light curve of KMT-2019-BLG-0371 (Kim+, 2021)
KMT-2019-BLG-0371 and the limits of Bayesian analysis.
Kim Y.H., Chung S.-J., Yee J.C., Udalski A., Bond I.A., Jung Y.K.,
Gould A., Albrow M.D., Han C., Hwang K.-H., Ryu Y.-H., Shin I.-G.,
Shvartzvald Y., Zang W., Cha S.-M., Kim D.-J., Kim H.-W., Kim S.-L.,
Lee C.-U., Lee D.-J., Lee Y., Park B.-G., Pogge R.W.,
(the Kmtnet Collaboration), Poleski R., Mroz P., Skowron J.,
Szymanski M.K., Soszynski I., Pietrukowicz P., Kozlowski S., Ulaczyk K.,
Rybicki K.A., Iwanek P., Wrona M., Gromadzki M., (the Ogle Collaboration),
Abe F., Barry R., Bennett D.P., Bhattacharya A., Donachie M., Fujii H.,
Fukui A., Itow Y., Hirao Y., Kirikawa R., Kondo I., Koshimoto N.,
Matsubara Y., Muraki Y., Miyazaki S., Ranc C., Rattenbury N.J., Satoh Y.,
Shoji H., Sumi T., Suzuki D., Tristram P.J., Tanaka Y., Yamawaki T.,
Yonehara A., (the Moa Collaboration)
<Astron. J., 162, 17-17 (2021)>
=2021AJ....162...17K 2021AJ....162...17K (SIMBAD/NED BibCode)
ADC_Keywords: Gravitational lensing; Photometry, RI
Keywords: Binary lens microlensing
Abstract:
We show that the perturbation at the peak of the light curve of
microlensing event KMT-2019-BLG-0371 is explained by a model with a
mass ratio between the host star and planet of q∼0.08. Due to the
short event duration (tE∼6.5days), the secondary object in this
system could potentially be a massive giant planet. A Bayesian
analysis shows that the system most likely consists of a host star
with a mass Mh=0.09-0.05+0.14Msun and a massive giant planet
with a mass Mp=7.70-3.90+11.34MJup. However, the
interpretation of the secondary as a planet (i.e., as having
Mp<13MJup) rests entirely on the Bayesian analysis. Motivated by
this event, we conduct an investigation to determine which constraints
meaningfully affect Bayesian analyses for microlensing events. We find
that the masses inferred from such a Bayesian analysis are determined
almost entirely by the measured value of θE and are relatively
insensitive to other factors such as the direction of the event (l,
b), the lens-source relative proper motion µrel, or the specific
Galactic model prior.
Description:
The microlensing event KMT-2019-BLG-0371 was first discovered on 2019
April 15 by the alert system of the Korea Microlensing Telescope
Network (KMTNet). KMTNet uses three identical ground-based telescopes
located at the Cerro Tololo Inter-American Observatory in Chile
(KMTC), South African Astronomical Observatory in South Africa (KMTS),
and Siding Spring Observatory in Australia (KMTA). The event was
detected in two KMTNet fields; BLG01 and BLG41.
The event was also detected by the Optical Gravitational Lensing
Experiment (OGLE) by the 1.3m Warsaw telescope at the Las Campanas
Observatory in Chile.
Moreover, the event was found by the Microlensing Observations in
Astrophysics (MOA).
Objects:
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RA (2000) DE Designation(s)
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17 53 32.14 -31 33 18.08 KMT-2019-BLG-0371 = EWS 2019-BLG-505
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File Summary:
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FileName Lrecl Records Explanations
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ReadMe 80 . This file
fig1.dat 36 14103 Light curve of KMT-2019-BLG-0371
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See also:
J/A+A/549/A147 : Abundances of microlensed bulge dwarf stars V. (Bensby+, 2013)
J/AJ/159/116 : I-band light curves of OGLE-2015-BLG-1771Lb (Zhang+, 2020)
J/AJ/159/256 : Light curve of OGLE-2018-BLG-0677 (Herrera-Martin+, 2020)
J/AJ/159/261 : LC of microlensing event OGLE-2012-BLG-0838 (Poleski+, 2020)
J/AJ/160/148 : RI LC microlensing event OGLE-2018-BLG-1269Lb (Jung+, 2020)
J/AJ/160/255 : KMTNet & OGLE I photometry of KMT-2019-BLG-0842 (Jung+, 2020)
Byte-by-byte Description of file: fig1.dat
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Bytes Format Units Label Explanations
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1- 6 A6 --- Tel Telescope identifier; KMTNet, MOA or OGLE
8- 8 A1 --- Filt Filter used; R or I
10- 19 F10.5 d HJD [7435/8931] Heliocentric Julian Date; HJD-2450000
21- 28 F8.5 mag mag [14.66/21.51] Apparent magnitude in Filter
30- 36 F7.5 mag e_mag [0.009/3.2] Uncertainty in mag
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History:
From electronic version of the journal
(End) Prepared by [AAS], Coralie Fix [CDS], 08-Nov-2021