Year: 2025
Type: article
Abstract: We present the analysis of OGLE-2014-BLG-1760, a planetary system in the galactic bulge. We combine Keck Adaptive Optics follow-up observations in K-band with re-reduced light-curve data to confirm the source and lens star identifications and stellar types. The re-reduced Microlensing Observations in Astrophysics data set had an important impact on the light-curve model. We find the Einstein ring crossing time of the event to be ∼2.5 days shorter than previous fits, which increases the planetary mass-ratio and decreases the source angular size by a factor of 0.25. Our OSIRIS images obtained 6 yr after the peak of the event show a source-lens separation of 54.20 ± 0.23 mas, which leads to a relative proper motion of μ rel = 9.14 ± 0.05 mas yr−1 and is larger than the previous light-curve-only models. Our analysis shows that the event consists of a Jupiter-mass planet of M p = 0.931 ± 0.117 M Jup orbiting a K-dwarf star of M * = 0.803 ± 0.097 M ⊙ with a K-magnitude of K L = 18.30 ± 0.05, located in the galactic bulge or bar. We also attempt to constrain the source properties using the source angular size θ * and K-magnitude. Our results favor the scenario of the source being a younger star in the galactic disk, behind the galactic bulge, but future multicolor observations are needed to constrain the source and thus the lens properties.
Source: The Astronomical Journal
Institutions: Centre National de la Recherche Scientifique, University of Tasmania, Institut d'Astrophysique de Paris, Sorbonne Université, The University of Osaka, Goddard Space Flight Center, University of Maryland, College Park, California Institute of Technology, Infrared Processing and Analysis Center, Massey University, University of Warsaw, University of Bern, Université de Bordeaux, Laboratoire d'Astrophysique de Bordeaux
Language: English
Subfield: Astronomy and Astrophysics
Field: Physics and Astronomy
Domain: Physical Sciences
Open Access status: gold
Estimated APC paid: $4,499
Awards: IN DECEMBER 2015 WE WERE INFORMED OF THE WFIRST SCIENCE INVESTIGATION TEAM SELECTIONS AND OF THE FUNDING FOR THE WIRST SCIENCE INVESTIGATION TEAMS. UNFORTUNATELY THE FUNDING FOR THE WFIRST EXOPLANET MICROLENSING PROGRAM WAS NOT SUFFICIENT TO DEVELOP ALL THE TOOLS NEEDED TO EXECUTE THIS PROGRAM. BECAUSE OF THIS THE PI SUBMITTED A REQUEST TO THE NASA PROGRAM OFFICER DR. DOMINIC BENFORD TO CHANGE THE FOCUS OF THIS WFIRST PREPARATORY SCIENCE GRANT AND DR. BENFORD APPROVED THIS REQUEST. THE NEW FOCUS INCLUDES THE DEVELOPMENT OF THE WFIRST EXOPLANET MICROLENSING SURVEY PHOTOMETRY/ASTROMETRY PIPELINE ALGORITHMS AND THE DEVELOPMENT OF ADVANCED LIGHT CURVE MODELING AND DATA ANALYSIS METHODS. IT ALSO INCLUDES THE STUDY OF MICROLENSING EVENTS LOCATED IN THE CANDIDATE WFIRST EXOPLANET MICROLENSING SURVEY FIELDS TO DETERMINE IF NEW DIFFICULTIES MIGHT ARISE WITH THE WFIRST EXOPLANET MASS MEASUREMENT METHODS DUE TO THE LOW LATITUDES OF THE WFIRST MICROLENSING FIELDS., G5477955166, demographics of planets close to their birth place & their occurrence in the disk and the bar of our Galaxy., G7796512131
OpenAlex ID: W4413874267