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Peer-reviewedCC BY 4.0The Astronomical Journal

OGLE-2012-BLG-0563: Relative Proper Motion Constraint from Keck Follow-up Finds the Correct Lens

  • Aparna Bhattacharya1,2
  • David P. Bennett1,2
  • Jean Philippe Beaulieu3,4
  • Ian A. Bond5
  • Kansuke Nunota6,7
  • Jessica R. Lu8
  • Joshua W. Blackman9
  • Clément Ranc3
  • Natalia Rektsini3
  • Aikaterini Vandorou1,2
  • Sean K. Terry1,2
  • Jean Baptiste Marquette3
2 more authors
  • Andrew A. Cole4
  • Akihiko Fukui6,10
10 affiliations
  1. 1Code 667
  2. 2University of Maryland
  3. 3Institut d’Astrophysique de Paris
  4. 4University of Tasmania
  5. 5Massey University
  6. 6The University of Tokyo
  7. 7National Astronomical Observatory of Japan
  8. 8University of California Berkeley
  9. 9Physikalisches Institut
  10. 10Instituto de Astrofísica de Canarias (IAC)
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Abstract

We present Keck/NIRC2 adaptive optics imaging results of planetary microlensing event OGLE-2012-BLG-0563. We find that the OGLE-2012-BLG-0563L planetary system consists of a 1.12 ± 0.09 M Jup planet orbiting a 0.81 ± 0.04 M ⊙ host star at a distance of 5.49 ± 0.56 kpc from the Sun. This event has a lens-source separation of 23.28 ± 0.48 mas, which is the smallest lens-source separation measured to date with Keck AO data. We find that the incorrect solution—which identifies the northeast (NE) star as the source star—is favored if one only considers the discovery paper, the A. Fukui et al. (2015) solution, or an unconstrained model. However, by performing an image-constrained light-curve model fit using the relative proper-motion direction constraint from the Keck follow-up data, we demonstrate that the correct solution identifies the NE star as the lens star. The discrepancy in the unconstrained models is driven by systematics in the Faulkes Telescope South (FTS) and ​​​Microlensing Observations in Astrophysics (MOA) B and C data, alongside the impact of the relative proper-motion direction constraints. This outcome offers two important lessons for future Roman data analysis: (1) thoroughly verify systematics across all passbands and identify the precise origin of χ ² differences, and (2) utilize image-constrained light-curve modeling incorporating relative proper-motion direction constraints to identify the correct lens.

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Cite

BibTeXRIS
BibTeX
@article{bhattacharya2026ogle2012blg0563,
  title = {{OGLE-2012-BLG-0563: Relative Proper Motion Constraint from Keck Follow-up Finds the Correct Lens}},
  author = {Aparna Bhattacharya and David P. Bennett and Jean Philippe Beaulieu and Ian A. Bond and Kansuke Nunota and Jessica R. Lu and Joshua W. Blackman and Clément Ranc and Natalia Rektsini and Aikaterini Vandorou and Sean K. Terry and Jean Baptiste Marquette and Andrew A. Cole and Akihiko Fukui},
  journal = {The Astronomical Journal},
  year = {2026},
  month = nov,
  doi = {10.3847/1538-3881/aeb01f},
  url = {https://iopscience.iop.org/article/10.3847/1538-3881/aeb01f},
  note = {CC BY 4.0},
}
RIS
TY  - JOUR
TI  - OGLE-2012-BLG-0563: Relative Proper Motion Constraint from Keck Follow-up Finds the Correct Lens
AU  - Aparna Bhattacharya
AU  - David P. Bennett
AU  - Jean Philippe Beaulieu
AU  - Ian A. Bond
AU  - Kansuke Nunota
AU  - Jessica R. Lu
AU  - Joshua W. Blackman
AU  - Clément Ranc
AU  - Natalia Rektsini
AU  - Aikaterini Vandorou
AU  - Sean K. Terry
AU  - Jean Baptiste Marquette
AU  - Andrew A. Cole
AU  - Akihiko Fukui
PY  - 2026
DA  - 2026/11/03
JO  - The Astronomical Journal
DO  - 10.3847/1538-3881/aeb01f
UR  - https://iopscience.iop.org/article/10.3847/1538-3881/aeb01f
AB  - We present Keck/NIRC2 adaptive optics imaging results of planetary microlensing event OGLE-2012-BLG-0563. We find that the OGLE-2012-BLG-0563L planetary system consists of a 1.12 ± 0.09 M Jup planet orbiting a 0.81 ± 0.04 M ⊙ host star at a distance of 5.49 ± 0.56 kpc from the Sun. This event has a lens-source separation of 23.28 ± 0.48 mas, which is the smallest lens-source separation measured to date with Keck AO data. We find that the incorrect solution—which identifies the northeast (NE) star as the source star—is favored if one only considers the discovery paper, the A. Fukui et al. (2015) solution, or an unconstrained model. However, by performing an image-constrained light-curve model fit using the relative proper-motion direction constraint from the Keck follow-up data, we demonstrate that the correct solution identifies the NE star as the lens star. The discrepancy in the unconstrained models is driven by systematics in the Faulkes Telescope South (FTS) and ​​​Microlensing Observations in Astrophysics (MOA) B and C data, alongside the impact of the relative proper-motion direction constraints. This outcome offers two important lessons for future Roman data analysis: (1) thoroughly verify systematics across all passbands and identify the precise origin of χ ² differences, and (2) utilize image-constrained light-curve modeling incorporating relative proper-motion direction constraints to identify the correct lens.
SN  - 0004-6256
SN  - 1538-3881
ER  -