OGLE-2016-BLG-0263Lb: Microlensing Detection of a Very Low-mass Binary Companion through a Repeating Event Channel
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Citations
OGLE-2015-BLG-1459L: The Challenges of Exo-Moon Microlensing
OGLE-2015-BLG-1459L: The Challenges of Exo-Moon Microlensing.
OGLE-2018-BLG-0567Lb and OGLE-2018-BLG-0962Lb: Two Microlensing Planets through Planetary-Caustic Channel
Systematic KMTNet Planetary Anomaly Search. I. OGLE-2019-BLG-1053Lb, a Buried Terrestrial Planet
An Ice Giant Exoplanet Interpretation of the Anomaly in Microlensing Event OGLE-2011-BLG-0173
References
Discovering Planetary Systems through Gravitational Microlenses
Reddening and extinction toward the galactic bulge from ogle-iii: the inner milky way's rv ∼ 2.5 extinction curve*
Planet formation around stars of various masses : the snow line and the frequency of giant planets
Real-time difference imaging analysis of moa galactic bulge observations during 2000
Extending the MACHO Search to approximately 10 6 M sub sun
Related Papers (5)
Ogle-2003-blg-262: finite-source effects from a point-mass lens
Reddening and extinction toward the galactic bulge from ogle-iii: the inner milky way's rv ∼ 2.5 extinction curve*
Chemical evolution of the Galactic bulge as traced by microlensed dwarf and subgiant stars - V. Evidence for a wide age distribution and a complex MDF
Frequently Asked Questions (14)
Q2. What are the future works in "Ogle-2016-blg-0263lb: microlensing detection of a very low-mass binary companion through a repeating event channel" ?
The repeating-event channel is also important in future space-based microlensing surveys, such as WFIRST, from which many free-floating planet candidates are expected to be detected.
Q3. How many planets are detected by high-cadence surveys?
Under the assumption of power-law distributions of host-planet separations, Han (2007) estimated that planets detectable by high-cadence surveys through the repeating channel will comprise ∼3%–4% of all planets.
Q4. Why do space-based lensing observations not observe the bulge field continuously?
Due to the time-window limit set by the orbits of satellites, space-based lensing observations will not observe the bulge field continuously.
Q5. What is the scientific significance of the repeating-event channel?
The scientific importance of the repeating-event channel is that the range of planets and brown dwarfs (BDs) detectable by microlensing is expanded.
Q6. What is the advantage of high-cadence surveys?
Another important advantage of high-cadence surveys is that they open an additional channel of detecting very low-mass companions.
Q7. How do the authors model the light curve of a BS event?
Since the light curve of a BS event varies smoothly with the changes of the lensing parameters, the authors search for the best-fit parameters by 2c minimization using a downhill approach.
Q8. What is the q–s parameter for the repeating-event channel?
The repeating-event channel is also important in future space-based microlensing surveys, such as WFIRST, from which many free-floating planet candidates are expected to be detected.
Q9. What are the two dotted circles around the individual caustics?
The two dotted circles around the individual caustics represent the Einstein rings corresponding to the masses of the individual BL components with radii r q1 11 1 2= +[ ( )] and r q q12 1 2= +[ ( )] .
Q10. Why do the authors characterize the source star for the sake of completeness?
Although one cannot determine Eq for OGLE-2016-BLG-0263 because the source did not cross caustics and thus the light curve is not affected by finite-source effects, the authors characterize the source star for the sake of completeness.
Q11. What is the normalization factor used to make the 2c per degree of freedom?
Following the usual procedure described in Yee et al. (2012), the authors normalize the error bars byk , 10 2 min 2 1 2s s s= +( ) ( )where 0s is the error bar estimated from the photometry pipeline, mins is a term used to adjust error bars for consistency with the scatter of the data set, and k is a normalization factor used to make the 2c per degree of freedom unity.
Q12. What is the first case of a BS event?
The first case is a binary-source (BS) event in which the double peaks are produced when the lens passes close to both components of the source separately, one after another (Griest & Hu 1992; Sazhin & Cherepashchuk 1994; Han & Gould 1997).
Q13. What is the effect of the lens binarity on the light curve of a BL?
Unlike the case of a BS event, the light curve of a BL event cannot be described by the superposition of the two light curves involved with the individual lens components because the lens binarity induces a region of discontinuous lensing magnifications, i.e., caustics.
Q14. What is the basic description of the light curve of a BS event?
For the basic description of the light curve of a BS event, therefore, one needs six lensing parameters, including t0,1, t0,2, u0,1, u0,2, tE, and qF (Hwang et al. 2013).