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Peer-reviewedCC BY 4.0The Astronomical Journal

You Shall Not Pass (Without Modeling): High-resolution Analysis of KMT-2019-BLG-0253 using MORIA

  • T. Dex Bhadra1
  • Sean K. Terry1,2
  • David P. Bennett1,2
  • Aparna Bhattacharya1,2
  • Ian A. Bond3
  • Jon Hulberg2,4,5
  • Stela Ishitani Silva2,6
  • Przemek Mróz7
  • Aikaterini Vandorou1,2
7 affiliations
  1. 1University of Maryland
  2. 2NASA Goddard Space Flight Center
  3. 3Massey University
  4. 4Catholic University of America
  5. 5Center for Research and Exploration in Space Science and Technology
  6. 6IPAC
  7. 7University of Warsaw
Open at sourcePDFDOICite

Abstract

We present the Microlensing Object high-Resolution Imaging Analysis pipeline, or MORIA . This is an automated procedure to reduce high-resolution Hubble Space Telescope (HST) images of microlensing targets, build empirical point-spread function (PSF) models from the data, and perform simultaneous multistar PSF fitting to blended sources, lenses, and neighbor stars. We have developed and tested this pipeline using HST observations of the microlensing event KMT-2019-BLG-0253, which shows clear evidence of three highly blended stars in HST. Under our assumed source and lens identification, we determine a host mass of M host = 0.65 ± 0.04 M ⊙ . We have reduced the number of possible solutions for this target by a factor of 2, with the remaining solution subject to the well-known close/wide degeneracy. We determine a planet mass of m p = 7.18 ± 0.40 M ⊕ (close) or m p = 9.48 ± 1.13 M ⊕ (wide), and distance to the lens system of D L = 2.64 ± 0.22 kpc. This target lies within the upcoming Roman Telescope Galactic Bulge Time Domain Survey (GBTDS) field. Future analysis of the Roman data for this event can confirm or reject the initial source and lens identifications presented in this work. Finally, this work demonstrates the importance of using an automated high-resolution imaging tool to inform lightcurve modeling for microlensing planets found during the GBTDS.

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Cite

BibTeXRIS
BibTeX
@article{bhadra2026shall,
  title = {{You Shall Not Pass (Without Modeling): High-resolution Analysis of KMT-2019-BLG-0253 using MORIA}},
  author = {T. Dex Bhadra and Sean K. Terry and David P. Bennett and Aparna Bhattacharya and Ian A. Bond and Jon Hulberg and Stela Ishitani Silva and Przemek Mróz and Aikaterini Vandorou},
  journal = {The Astronomical Journal},
  year = {2026},
  month = oct,
  doi = {10.3847/1538-3881/aead98},
  url = {https://iopscience.iop.org/article/10.3847/1538-3881/aead98},
  note = {CC BY 4.0},
}
RIS
TY  - JOUR
TI  - You Shall Not Pass (Without Modeling): High-resolution Analysis of KMT-2019-BLG-0253 using MORIA
AU  - T. Dex Bhadra
AU  - Sean K. Terry
AU  - David P. Bennett
AU  - Aparna Bhattacharya
AU  - Ian A. Bond
AU  - Jon Hulberg
AU  - Stela Ishitani Silva
AU  - Przemek Mróz
AU  - Aikaterini Vandorou
PY  - 2026
DA  - 2026/10/26
JO  - The Astronomical Journal
DO  - 10.3847/1538-3881/aead98
UR  - https://iopscience.iop.org/article/10.3847/1538-3881/aead98
AB  - We present the Microlensing Object high-Resolution Imaging Analysis pipeline, or MORIA . This is an automated procedure to reduce high-resolution Hubble Space Telescope (HST) images of microlensing targets, build empirical point-spread function (PSF) models from the data, and perform simultaneous multistar PSF fitting to blended sources, lenses, and neighbor stars. We have developed and tested this pipeline using HST observations of the microlensing event KMT-2019-BLG-0253, which shows clear evidence of three highly blended stars in HST. Under our assumed source and lens identification, we determine a host mass of M host = 0.65 ± 0.04 M ⊙ . We have reduced the number of possible solutions for this target by a factor of 2, with the remaining solution subject to the well-known close/wide degeneracy. We determine a planet mass of m p = 7.18 ± 0.40 M ⊕ (close) or m p = 9.48 ± 1.13 M ⊕ (wide), and distance to the lens system of D L = 2.64 ± 0.22 kpc. This target lies within the upcoming Roman Telescope Galactic Bulge Time Domain Survey (GBTDS) field. Future analysis of the Roman data for this event can confirm or reject the initial source and lens identifications presented in this work. Finally, this work demonstrates the importance of using an automated high-resolution imaging tool to inform lightcurve modeling for microlensing planets found during the GBTDS.
SN  - 0004-6256
SN  - 1538-3881
ER  -