Discovery of a Jupiter/Saturn Analog with Gravitational Microlensing

Gaudi, B. Scott; Bennett, D. P.; Udalski, A.; Gould, Andrew; Christie, Grant; Maoz, Dan; Dong, Subo; McCormick, J.; Szymański, M. K.; Tristram, P. J.; Nikolaev, Sergei; Paczyński, B.; Kubiak, M.; Pietrzyński, G.; Soszyński, I.; Szewczyk, O.; Ulaczyk, K.; Wyrzykowski, Ł.; DePoy, D. L.; Han, Cheongho; Kaspi, S.; Lee, Chung-Uk; Mallia, F.; Natusch, T.; Pogge, Richard W.; Park, B.-G.; Abe, F.; Bond, I. A.; Botzler, C. S.; Fukui, A.; Hearnshaw, John; Itow, Y.; Kamiya, K.; Korpela, A.; Kilmartin, P. M.; Lin, Wei; Masuda, K.; Matsubara, Y.; Motomura, M.; Muraki, Y.; Nakamura, Satoko; Okumura, Teppei; Ohnishi, Kouhei; Rattenbury, N. J.; Sako, T.; Saito, To.; Sato, Shuji; Skuljan, L.; Sullivan, D. J.; Sumi, T.; Sweatman, W. L.; Yock, P. C. M.; Albrow, M. D.; Allan, A.; Beaulieu, J. P.; Burgdorf, M.; Cook, K. H.; Coutures, C.; Dominik, M.; Dieters, S.; Fouqué, P.; Greenhill, J.; Horne, K.; Steele, I. A.; Tsapras, Y.; Chaboyer, Brian; Crocker, Alison F.; Stephan, F.; Macintosh, Bruce

doi:10.1126/science.1151947

Cited by 331 publications

(246 citation statements)

References 34 publications

Supporting

Mentioning

243

Contrasting

Order By: Relevance

“…Understanding the reasons for the discrepancies for this event will help to improve the characterisation of microlensing systems, which have already been detected or will be detected with the K2, WFIRST and Euclid space missions. In the coming years, using future ESO facilities such as ESPRESSO at VLT, or HIRES at E-ELT, it will be possible to perform such measurements on planetary systems detected by microlensing such as OGLE-2006-BLG-109 (Gaudi et al 2008) and OGLE-2012-BLG-0026 , once it has been confirmed via high angular resolution observation that there is no strong contamination by a blend, for example, thanks to high angular resolution observations. Note that, during the referee process on this letter, Yee et al (2015) published RV measurements on another microlensing event revealing an orbit consistent with the prediction from the light-curve analysis.…”

Section: Discussionmentioning

confidence: 99%

The first radial velocity measurements of a microlensing event: no evidence for the predicted binary

Boisse

Santerne

Beaulieu

et al. 2015

A&A

Self Cite

View full text Add to dashboard Cite

The gravitational microlensing technique allows the discovery of exoplanets around stars distributed in the disk of the galaxy towards the bulge. The alignment of two stars that led to the discovery is unique over the timescale of a human life, however, and cannot be re-observed. Moreover, the target host is often very faint and located in a crowded region. These difficulties hamper and often make impossible the follow up of the target and study of its possible companions. A radial-velocity curve was predicted for the binary system, OGLE-2011-BLG-0417, discovered and characterised from a microlensing event. We used the UVES spectrograph mounted at the VLT, ESO to derive precise radial-velocity measurements of OGLE-2011-BLG-0417. To gather high-precision radial velocities on faint targets of microlensing events, we proposed to use the source star as a reference to measure the lens radial velocities. We obtained ten radial velocities on the putative V = 18 lens with a dispersion of ∼100 m s −1 , spread over one year. Our measurements do not confirm the microlensing prediction for this binary system. The most likely scenario is that the putative V = 18 mag lens is actually a blend and not the primary lens which is 2 mag fainter. Further observations and analyses are needed to understand the microlensing observation and infer on the nature and characteristics of the lens itself.

show abstract

Section: Discussionmentioning

confidence: 99%

The first radial velocity measurements of a microlensing event: no evidence for the predicted binary

Boisse

Santerne

Beaulieu

et al. 2015

A&A

Self Cite

View full text Add to dashboard Cite

show abstract

“…• Simulation 1 -two giant planets with initial orbital parameters to emulate the OGLE-06-109L system (Gaudi et al 2008). 500 planetary embryos and planetesimals with total mass 10 M ⊕ were distributed between 0.3 AU < a < 5.2 AU and with e < 0.02.…”

Section: Simulation Setup and Resultsmentioning

confidence: 99%

Forming short-period earth-like planets via a collision-merger scenario

Jin¹,

Ji²,

Tinney³

2010

Proc. IAU

View full text Add to dashboard Cite

show abstract

“…In addition, there are a comparable number of events that required including limb darkening in their analysis (such as MACHO Alert 95−30), but for which a sufficiently accurate limb-darkening measurement was not (and often could not be) performed. These include two other single-lens events (Yee et al 2009;Batista et al 2009), as well as all ten published planetary microlensing events, in which a star with a planet acted as the lens (Bond et al 2004;Udalski et al 2005;Beaulieu et al 2006;Gould et al 2006;Gaudi et al 2008;Bennett et al 2008;Dong et al 2009;Sumi et al 2010;Janczak et al 2010).…”

Section: Introductionmentioning

confidence: 99%

OGLE 2008–BLG–290: an accurate measurement of the limb darkening of a galactic bulge K Giant spatially resolved by microlensing

Fouqué

Heyrovsky

Dong

et al. 2010

A&A

Self Cite

View full text Add to dashboard Cite

Context. Not only is gravitational microlensing a successful tool for discovering distant exoplanets, but it also enables characterization of the lens and source stars involved in the lensing event.Aims. In high-magnification events, the lens caustic may cross over the source disk, which allows determination of the angular size of the source and measurement of its limb darkening. Methods. When such extended-source effects appear close to maximum magnification, the resulting light curve differs from the characteristic Paczyński point-source curve. The exact shape of the light curve close to the peak depends on the limb darkening of the source. Dense photometric coverage permits measurement of the respective limb-darkening coefficients.Results. In the case of the microlensing event OGLE 2008-BLG-290, the K giant source star reached a peak magnification at about 100. Thirteen different telescopes have covered this event in eight different photometric bands. Subsequent light-curve analysis yielded measurements of linear limb-darkening coefficients of the source in six photometric bands. The best-measured coefficients lead to an estimate of the source effective temperature of about 4700 +100 −200 K. However, the photometric estimate from colour-magnitude diagrams favours a cooler temperature of 4200 ± 100 K. Conclusions. Because the limb-darkening measurements, at least in the CTIO/SMARTS2 V s -and I s -bands, are among the most accurate obtained, the above disagreement needs to be understood. A solution is proposed, which may apply to previous events where such a discrepancy also appeared.

show abstract

Discovery of a Jupiter/Saturn Analog with Gravitational Microlensing

Cited by 331 publications

References 34 publications

The first radial velocity measurements of a microlensing event: no evidence for the predicted binary

The first radial velocity measurements of a microlensing event: no evidence for the predicted binary

Forming short-period earth-like planets via a collision-merger scenario

OGLE 2008–BLG–290: an accurate measurement of the limb darkening of a galactic bulge K Giant spatially resolved by microlensing

Contact Info

Product

Resources

About