J/AJ/164/118 VRI light curve of MOA 2020-BLG-135 (Ishitani Silva+, 2022)
MOA-2020-BLG-135Lb; A New Neptune-class Planet for the Extended MOA-II Exoplanet
Microlens Statistical Analysis.
Ishitani Silva S., Ranc C., Bennett D.P., Bond I.A., Zang W., Abe F.,
Barry R.K., Bhattacharya A., Fujii H., Fukui A., Hirao Y., Itow Y.,
Kirikawa R., Kondo I., Koshimoto N., Matsubara Y., Matsumoto S.,
Miyazaki S., Muraki Y., Olmschenk G., Okamura A., Rattenbury N.J., Satoh Y.,
Sumi T., Suzuki D., Toda T., Tristram P.J., Vandorou A., Yama H., Petric A.,
Burdullis T., Fouque P., Mao S., Penny M.T., Zhu W., Rau G.,
Leading authors, The MOA Collaboration, The CFHT Microlensing Collaboration
<Astron. J., 164, 118 (2022)>
=2022AJ....164..118I 2022AJ....164..118I
ADC_Keywords: Gravitational lensing; Exoplanets; Photometry, VRI
Keywords: Gravitational microlensing ; Gravitational microlensing exoplanet
detection ; Binary lens microlensing ; Exoplanet detection
methods ; Exoplanets ; Exoplanet systems ; Exoplanet astronomy
Abstract:
We report the light-curve analysis for the event MOA-2020-BLG-135,
which leads to the discovery of a new Neptune-class planet,
MOA-2020-BLG-135Lb. With a derived mass ratio of
q=1.52-0.31+0.39x10-4 and separation s∼1, the planet lies
exactly at the break and likely peak of the exoplanet mass-ratio
function derived by the Microlensing Observations in Astrophysics
(MOA) Collaboration. We estimate the properties of the lens system
based on a Galactic model and considering two different Bayesian
priors: one assuming that all stars have an equal planet-hosting
probability and the other that planets are more likely to orbit
more-massive stars. With a uniform host mass prior, we predict that
the lens system is likely to be a planet of mass
mp=11.3-6.9+19.2M⊕ and a host star of mass
M*=0.23-0.14+0.39M☉, located at a distance
DL=7.9-1.0+1.0kpc. With a prior that holds that planet
occurrence scales in proportion to the host-star mass, the estimated
lens system properties are mp=25-15+22M⊕,
M*=0.53-0.32+0.42M☉, and DL=8.3-1.0+0.9kpc. This
planet qualifies for inclusion in the extended MOA-II exoplanet
microlens sample.
Description:
The Microlensing Observations in Astrophysics (MOA) observations were
performed using the purpose-built 1.8m wide-field MOA telescope
located at Mount John Observatory, New Zealand, and the observations
of the field "gb5" were taken with a 15minute cadence using the
MOA-Red filter. The MOA-Red filter corresponds to a customized
wide-band similar to a sum of the Kron-Cousins R and I bands, from 600
to 900nm.
The Canada-France-Hawaii Telescope (CFHT), located near the summit of
Maunakea in Hawaii, United States, also observed the event in the
Sloan Digital Sky Survey i-band filter.
Objects:
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RA (2000) DE Designation(s)
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17 53 41.64 -29 48 27.2 MOA-2020-BLG-135 = KMT-2020-BLG-0579
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File Summary:
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FileName Lrecl Records Explanations
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ReadMe 80 . This file
cfhti.dat 46 51 CFHT-i band data
moa2r.dat 46 14270 MOA-Red band data
moa2v.dat 46 499 MOA-V band data
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See also:
J/ApJS/101/117 : UBVRIJHKLMNQ photometry in Taurus-Auriga (Kenyon+ 1995)
J/A+A/533/A134 : Abundances of microlensed stars in the Bulge (Bensby+, 2011)
J/other/Nat/481.167 : 2002-2007 PLANET microlensing events (Assan+, 2012)
J/ApJ/778/150 : Microlensing events toward the Bulge from MOA-II (Sumi+, 2013)
J/AJ/158/13 : The first 300 stars observed by the GPIES (Nielsen+, 2019)
J/ApJS/254/39 : Exoplanet candidates from TESS first 2yr obs (Guerrero+, 2021)
Byte-by-byte Description of file: cfhti.dat moa2[rv].dat
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Bytes Format Units Label Explanations
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1- 10 F10.5 d HJD Heliocentric Julian Date of observation; HJD-2450000
12- 18 F7.4 mag mag Magnitude; Zpt=21
20- 25 F6.4 mag e_mag Uncertainty in mag
27- 36 F10.4 --- flux Flux in band
38- 46 F9.4 --- e_flux Uncertainty in flux
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History:
From electronic version of the journal
(End) Prepared by [AAS], Coralie Fix [CDS], 21-Nov-2022