J/AJ/167/154 OGLE-2014-BLG-0221Lb VRI light curve (Kirikawa+, 2024)
OGLE-2014-BLG-0221Lb: A Jupiter Mass Ratio Companion Orbiting Either a Late-
type Star or a Stellar Remnant
Kirikawa R., Sumi T., Bennett D.P., Suzuki D., Koshimoto N., Miyazaki S.,
Bond I.A., Udalski A., Rattenbury N.J. (The Leading Authors), Abe F.,
Barry R., Bhattacharya A., Fujii H., Fukui A., Hamada R., Hirao Y.,
Ishitani Silva S., Itow Y., Matsubara Y., Muraki Y., Olmschenk G., Ranc C.,
Satoh Y.K., Tomoyoshi M., Tristram P.J., Vandorou A., Yama H.,
Yamashita K. (The MOA Collaboration), Mroz P., Poleski R., Skowron J.,
Szymanski M.K., Soszynski I., Pietrukowicz P., Kozlowski S., Ulaczyk K.,
Mroz M.J. (The OGLE Collaboration)
<Astron. J., 164, 154 (2024)>
=2024AJ....167..154K 2024AJ....167..154K
ADC_Keywords: Exoplanets; Stars, late-type; Photometry, VRI
Keywords: Gravitational microlensing; Exoplanets; Stellar remnants
Abstract:
We present the analysis of the microlensing event OGLE-2014-BLG-0221,
a planetary candidate event discovered in 2014. The photometric light
curve is best described by a binary-lens single-source model. Our
light-curve modeling finds two degenerate models, with event
timescales of tE∼70days and ∼110days. These timescales are relatively
long, indicating that the discovered system would possess a
substantial mass. The two models are similar in their planetary
parameters with a Jupiter mass ratio of q∼10-3 and a separation of
s∼1.1. Bayesian inference is used to estimate the physical parameters
of the lens, revealing that the shorter timescale model predicts 65%
and 25% probabilities of a late-type star and white dwarf host,
respectively, while the longer timescale model favors a black hole
host with a probability ranging from 60% to 95%, under the assumption
that stars and stellar remnants have equal probabilities of hosting
companions with planetary mass ratios. If the lens is a remnant, this
would be the second planet found by microlensing around a stellar
remnant. The current separation between the source and lens stars is
41-139mas depending on the models. This indicates the event is now
ready for high-angular-resolution follow-up observations to rule out
either of the models. If precise astrometric measurements are
conducted in multiple bands, the centroid shift due to the color
difference between the source and lens would be detected in the
luminous lens scenario.
Description:
The OGLE group conducted the observations with their 1.3m Warsaw
telescope at the Las Campanas Observatory in Chile. Data were obtained
mostly in the standard Kron-Cousins I band and occasionally in the
standard Johnson V band in order to extract color information of the
source star.
The event was also independently discovered by the Microlensing
Observations in Astrophysics (MOA) collaboration as a part of the
MOA-I I survey on 2014 March 9 and designated as MOA-2014-BLG-069. The
MOA group uses their 1.8m MOA-I I telescope and 2.2deg2 wide
field-of-view camera, MOA-cam3, at the Mount John Observatory in New
Zealand. Data were obtained in the designated MOA-Red band, equivalent
to a combined band of the standard Cousins R and I. MOA also
occasionally observes in the Johnson V band.
Object:
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RA (ICRS) DE Designation(s)
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18 01 12.90 -27 25 36.3 OGLE-2014-BLG-0221Lb = NAME OGLE-2014-BLG-0221Lb
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File Summary:
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FileName Lrecl Records Explanations
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ReadMe 80 . This file
fig1.dat 34 10520 The light curve of OGLE-2014-BLG-0221
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See also:
II/323 : OGLE-III Bulge Photometric Catalog (Szymanski+ 2011)
J/ApJS/101/117 : UBVRIJHKLMNQ photometry in Taurus-Auriga (Kenyon+ 1995)
J/A+A/529/A75 : Limb-darkening coefficients (Claret+, 2011)
J/A+A/533/A134 : Abundances of microlensed stars in the Bulge (Bensby+, 2011)
J/A+A/587/A61 : BlackCAT, stellar-mass BH X-ray trans. (Corral-Santana+, 2016)
J/ApJS/244/29 : Microlensing events toward the Galactic bulge (Mroz+, 2019)
J/AJ/161/54 : VRI photometry of MOA 2009-BLG-319 (Terry+, 2021)
J/A+A/664/A159 : Radial velocities of Galactic SB1s (Mahy+, 2022)
J/other/NatAs/6.1085 : Light curve for VFTS 243 (Shenar+, 2022)
J/AJ/166/6 : GaiaDR34373465352415301632 abundances (Chakrabarti+, 2023)
Byte-by-byte Description of file: fig1.dat
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Bytes Format Units Label Explanations
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1- 7 A7 --- Filt Filter used; I, MOA_Red or V
9- 19 F11.6 d HJD [5266/8743] Heliocentric Julian Date, JD-2450000
21- 27 F7.1 --- Flux [-2858/8418] Observed flux
29- 34 F6.1 --- e_Flux [1/1752] Uncertainty in Flux
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History:
From electronic version of the journal
(End) Prepared by [AAS], Coralie Fix [CDS], 21-May-2024