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| OGLE-2007-BLG-349L | |
|---|---|
| Name | OGLE-2007-BLG-349L |
| Epoch | J2000 |
| Constellation | Sagittarius |
| Type | Main sequence (M-dwarf) |
| Apparent magnitude | ~? |
| Distance | ~8 kpc (Galactic bulge) |
OGLE-2007-BLG-349L is a low-mass stellar object identified as the host of a microlensing event discovered by the Optical Gravitational Lensing Experiment. The detection was reported through collaborations involving the Microlensing Follow-Up Network, the Hubble Space Telescope, and ground-based observatories, linking observational programs such as the European Southern Observatory and the Las Campanas Observatory. The system lies toward the direction of the Galactic bulge, in the constellation Sagittarius, and was inferred from a gravitational microlensing light curve rather than direct imaging.
The event was first detected by the Optical Gravitational Lensing Experiment survey and announced alongside alerts from the Microlensing Observations in Astrophysics collaboration, with follow-up by the Probing Lensing Anomalies NETwork and observations coordinated with the Hubble Space Telescope and the Very Large Telescope. Analysis involved teams affiliated with institutions such as the Max Planck Institute for Astronomy, the California Institute of Technology, the Harvard–Smithsonian Center for Astrophysics, and the Korean Astronomy and Space Science Institute. The discovery combined photometric data from facilities including the CTIO 1.3 m telescope, the OGLE telescope at Las Campanas Observatory, and the Wise Observatory.
The host was characterized as a low-mass star consistent with an M-dwarf classification, with mass estimates derived from microlensing model degeneracies comparable to masses typical of objects catalogued by the Henry Draper Catalogue and surveyed by the Two Micron All Sky Survey. Distance estimates placed the system near the Galactic center region, comparable to sources in the OGLE-III and OGLE-IV surveys. Stellar parameters relied on comparisons to stellar models from groups such as the Baraffe models and databases maintained by the Gaia mission and the Sloan Digital Sky Survey for color–magnitude calibration. Reddening and extinction corrections used maps produced by the OGLE team and methods employed in analyses by the Pan-STARRS consortium.
Modeling of the microlensing light curve indicated the presence of at least one planetary companion, analogous in some analyses to systems catalogued in the Extrasolar Planets Encyclopaedia and compared to planets discovered by the Kepler space telescope and the Spitzer Space Telescope. The inferred planet(s) had mass ratios and projected separations that were discussed alongside known planets in surveys by the Harvard Exoplanet Archive and the NASA Exoplanet Archive. Proposed configurations included both single-planet and circumbinary interpretations, with comparison to circumbinary planets such as those found by the Kepler mission and to wide-orbit planets characterized by the Gemini Planet Imager. Measurements drew on techniques developed in studies by the OGLE group and by microlensing analysis teams at the University of Auckland and the University of Notre Dame.
The event's light curve exhibited anomalies that required complex modeling similar to methods applied in analyses by researchers at the University of California, Berkeley, the University of Tokyo, and the University of Cambridge. Bayesian inference and Markov Chain Monte Carlo techniques from groups at the Harvard–Smithsonian Center for Astrophysics and the Institute of Astronomy, Cambridge were used to explore lens mass, distance, and lens–source relative proper motion. High-resolution imaging from the Hubble Space Telescope and adaptive optics from the Keck Observatory and the Very Large Telescope helped constrain lens flux in follow-up studies comparable to approaches used by teams at the Carnegie Institution for Science. Degeneracies in the microlensing solutions invoked comparisons with known degeneracy cases discussed in literature from the Max Planck Institute for Astronomy and the Princeton University microlensing groups.
Proposed planetary architectures were evaluated using n-body integration techniques and stability criteria employed by dynamical groups at the University of Cambridge, the University of Arizona, and the Jet Propulsion Laboratory. Simulations considered resonant interactions and long-term stability analogous to analyses of circumbinary systems studied by the Kepler team and dynamical studies from the Institute for Advanced Study. Constraints on semi-major axes and eccentricities used frameworks developed by researchers at the University of California, Santa Cruz and the University of Tokyo to assess whether configurations resembled those of known multi-body systems published by the International Astronomical Union symposia and reviewed in the literature by the American Astronomical Society.
The event contributed to statistical studies of planet occurrence toward the Galactic bulge and to the census of planets around low-mass hosts compiled by the NASA Exoplanet Science Institute and the European Space Agency. It informed population synthesis models produced by groups at the Max Planck Institute for Astronomy and the University of Cambridge, and influenced target selection strategies for missions such as the Roman Space Telescope and follow-up surveys planned by the ESO and the Korea Astronomy and Space Science Institute. The case highlighted methodological links between microlensing teams at the OGLE project, the MOA collaboration, and space-based observers at the Hubble Space Telescope, reinforcing the role of microlensing in probing planetary demographics beyond the reach of techniques used by the Kepler and TESS missions.
Category:Stars Category:Exoplanet hosts Category:Microlensing events