OGLE-2003-BLG-262: Finite-Source Effects from a Point-Mass Lens

By Jaiyul Yoo, D. DePoy, A. Gal-yam, B. Gaudi, A. Gould, C. Han, Y. Lipkin, D. Maoz, E. Park, R. Pogge and 14 more. 2003

289 citations recorded by the source corpus.

We analyze OGLE-2003-BLG-262, a relatively short (tE = 12.5 ± 0.1 day) microlensing event generated by a point-mass lens transiting the face of a K giant source in the Galactic bulge. We use the resulting finite-source effects to measure the angular Einstein radius, θE = 195 ± 17 μas, and so constrain the lens mass to the FWHM interval 0.08 < M/M☉ < 0.54. The lens-source relative proper motion is μrel = 27 ± 2 km s-1 kpc-1. Both values are typical of what is expected for lenses detected toward the bulge. Despite the short duration of the event, we detect marginal evidence for a "parallax asymmetry" but argue that this is more likely to be induced by acceleration of the source, a binary lens, or possibly by statistical fluctuations. Although OGLE-2003-BLG-262 is only the second published event to date in which the lens transits the source, such events will become more common with the new OGLE-III survey in place. We therefore give a detailed account of the analysis of this event to facilitate the study of future events of this type.

Subfields: Astronomy and Astrophysics, Instrumentation

View Paper: https://www.semanticscholar.org/paper/fd8a1eb75dccde35bc37e18e9348eef323686447

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Citations in the corpus

MOA-2009-BLG-387Lb: a massive planet orbiting an M dwarf (2011, background): “The Microlensing Follow Up Network (μFUN; Yoo et al. 2004) followed the event from Chile (1.3 m SMARTS telescope at CTIO) (V, I and H band data), South Africa (0.35 m telescope at Bronberg observatory), New Zealand (0.40 m and 0.35 m telescopes at Auckland Observatory (AO) and Farm Cove (FCO)…”
Microlensing Surveys for Exoplanets (2012, background): “The extinction toward the source can be estimated by comparison to nearby red giant clump stars (Yoo et al. 2004, Bennett et al. 2010), which have a known and essentially constant luminosity and intrinsic color (Paczyński & Stanek 1998).”
A COLD NEPTUNE-MASS PLANET OGLE-2007-BLG-368Lb: Cold neptunes are common (2009, methodology): “Following Yoo et al. (2004b), the dereddened source color and brightness (V -”
Microlens OGLE-2005-BLG-169 Implies That Cool Neptune-like Planets Are Common (2006, unknown): “We first determine the angular source radius θ∗ using the standard approach (Yoo et al. 2004a), finding θ∗ = 0.44 ± 0.04µas.”
Predictions of the WFIRST Microlensing Survey. I. Bound Planet Detection Rates (2018, unknown): “This is important to consider, because, in addition to the requirement of sampling the planetary perturbation, the cadence must be chosen to also sample any finite source effects, which can be used to measure the angular Einstein radius (e.g., Nemiroff & Wickramasinghe 1994; Yoo et al. 2004).”
FREQUENCY OF SOLAR-LIKE SYSTEMS AND OF ICE AND GAS GIANTS BEYOND THE SNOW LINE FROM HIGH-MAGNIFICATION MICROLENSING EVENTS IN 2005–2008 (2010, methodology): “…the procedure of Gaudi et al. (2002) and adopt ρ = θ∗/(µtyptE), where θ∗ is determined from the instrumental color-magnitude diagram in the standard way (Yoo et al. 2004), tE is the measured Einstein timescale, and µtyp = 4 mas yr −1 is the typical source-lens proper motion toward the Galactic…”