OGLE 2003-BLG-235/MOA 2003-BLG-53: A Planetary Microlensing Event

Bond, I. A.; Udalski, A.; Jaroszyński, M.; Rattenbury, N. J.; Paczyński, B.; Soszyński, I.; Wyrzykowski, Ł.; Szymański, M. K.; Kubiak, M.; Szewczyk, O.; Zebrun, K.; Pietrzyński, G.; Abe, F.; Bennett, D. P.; Eguchi, S.; Furuta, Y.; Hearnshaw, John; Kamiya, K.; Kilmartin, P. M.; Kurata, Yoshimasa; Masuda, K.; Matsubara, Y.; Muraki, Y.; Noda, S.; Okajima, Kazuhisa; Sako, T.; Sekiguchi, T.; Sullivan, D. J.; Sumi, T.; Tristram, P. J.; Yanagisawa, Takufumi; Yock, P. C. M.

doi:10.1086/420928

Cited by 351 publications

(236 citation statements)

References 31 publications

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“…This can be quantified by simulating planetary light curves with different values of q and v (where v is the angle of source motion with respect to the lens axis) but the remaining parameters are fixed to the values for the three known microlensing planets. We find that the probability of detecting a q < 4-7 £ 10 23 planet, like the first two microlens planets 13,14 , is ,50 times larger than the probability of detecting a q ¼ 7.6 £ 10 25 planet like OGLE-2005-BLG-390Lb. This suggests that, at the orbital separations probed by microlensing, sub-Neptune-mass planets are significantly more common than large gas giants around the most common stars in our Galaxy.…”

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confidence: 71%

“…The PLANET collaboration 12 maintains the high sampling rate required to detect low-mass planets while monitoring the most promising of the .500 microlensing events discovered annually by the OGLE collaboration, as well as events discovered by MOA. A decade of pioneering microlensing searches has resulted in the recent detections of two Jupiter-mass extrasolar planets 13,14 with orbital separations of a few AU by the combined observations of the OGLE, MOA, MicroFUN and PLANET collaborations. The absence of perturbations to stellar microlensing events can be used to constrain the presence of planetary lens companions.…”

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confidence: 99%

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Discovery of a cool planet of 5.5 Earth masses through gravitational microlensing

Beaulieu¹,

Bennett²,

Fouqué³

et al. 2006

Nature

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544

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In the favoured core-accretion model of formation of planetary systems, solid planetesimals accumulate to build up planetary cores, which then accrete nebular gas if they are sufficiently massive. Around M-dwarf stars (the most common stars in our Galaxy), this model favours the formation of Earth-mass (M % ) to Neptune-mass planets with orbital radii of 1 to 10 astronomical units (AU), which is consistent with the small number of gas giant planets known to orbit M-dwarf host stars 1-4 . More than 170 extrasolar planets have been discovered with a wide range of masses and orbital periods, but planets of Neptune's mass or less have not hitherto been detected at separations of more than 0.15 AU from normal stars. Here we report the discovery of a 5.5 15.5 22.7 M % planetary companion at a separation of 2.6 11.5 20.6 AU from a 0.22 10.21 20.11 M ( M-dwarf star, where M ( refers to a solar mass. (We propose to name it OGLE-2005-BLG-390Lb, indicating a planetary mass companion to the lens star of the microlensing event.) The mass is lower than that of GJ876d (ref. 5), although the error bars overlap. Our detection suggests that such cool, sub-Neptune-mass planets may be more common than gas giant planets, as predicted by the core accretion theory.Gravitational microlensing events can reveal extrasolar planets orbiting the foreground lens stars if the light curves are measured frequently enough to characterize planetary light curve deviations with features lasting a few hours 6-9 . Microlensing is most sensitive to planets in Earth-to-Jupiter-like orbits with semi-major axes in the range 1-5 AU. The sensitivity of the microlensing method to lowmass planets is restricted by the finite angular size of the source stars 10,11 , limiting detections to planets of a few M % for giant source stars, but allowing the detection of planets as small as 0.1M % for main-sequence source stars in the Galactic Bulge. The PLANET collaboration 12 maintains the high sampling rate required to detect low-mass planets while monitoring the most promising of the .500 microlensing events discovered annually by the OGLE collaboration, as well as events discovered by MOA. A decade of pioneering microlensing searches has resulted in the recent detections of two Jupiter-mass extrasolar planets 13,14 with orbital separations of a few AU by the combined observations of the OGLE, MOA, MicroFUN and PLANET collaborations. The absence of perturbations to stellar microlensing events can be used to constrain the presence of planetary lens companions. With large samples of events, upper LETTERS 1 PLANET/RoboNet Collaboration

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mentioning

confidence: 71%

mentioning

confidence: 99%

Discovery of a cool planet of 5.5 Earth masses through gravitational microlensing

Beaulieu¹,

Bennett²,

Fouqué³

et al. 2006

Nature

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544

350

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“…At larger separations, microlensing surveys similarly probe the frequency of planets as a function of their mass. That technique has detected four putative planets that are probably orbiting M dwarfs : OGLE235-MOA53b (m p ∼ 2.6 M Jup - Bond et al 2004;Bennett et al 2006), OGLE-05-071Lb (m p = 0.9 M Jup - Udalski et al 2005), OGLE-05-390Lb (m p = 0.017 M Jup - Beaulieu et al 2006), and OGLE-05-169Lb (m p = 0.04 M Jup - Gould et al 2006). Two of these four planets very likely have masses below 0.1 M Jup .…”

Section: Introductionmentioning

confidence: 99%

The HARPS search for southern extra-solar planets

Bonfils¹,

Mayor

Delfosse

et al. 2007

A&A

252

257

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AstrophysicsThe HARPS search for southern extra-solar planets X. A m sin i = 11 M ⊕ planet around the nearby spotted M dwarf GJ 674 , ABSTRACTContext. How planet properties depend on stellar mass is a key diagnostic of planetary formation mechanisms. Aims. This motivates planet searches around stars that are significantly more massive or less massive than the Sun, and in particular our radial velocity search for planets around very low-mass stars. Methods. As part of that program, we obtained measurements of GJ 674, an M 2.5 dwarf at d = 4.5 pc. These measurements have dispersion much in excess of their internal errors. An intensive observing campaign demonstrates that the excess dispersion is due to two superimposed coherent signals, with periods of 4.69 and 35 days. Results. These data are described well by a 2-planet Keplerian model where each planet has a ∼11 M ⊕ minimum mass. A careful analysis of the (low-level) magnetic activity of GJ 674, however, demonstrates that the 35-day period coincides with the stellar rotation period. This signal therefore originates in a spot inhomogeneity modulated by stellar rotation. The 4.69-day signal, on the other hand, is caused by a bona-fide planet, GJ 674b. Conclusions. Its detection adds to the growing number of Neptune-mass planets around M-dwarfs and reinforces the emerging conclusion that this mass domain is much more populated than the Jovian mass range. We discuss the metallicity distributions of M dwarf with and without planets and find a low 11% probability that they are drawn from the same parent distribution. Moreover, we find tentative evidence that the host star metallicity correlates with the total mass of their planetary system.

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“…This has been done already for several microlensing events where the system is composed of a star and a gaseous planet (Bond et al 2004;Bennett et al 2006;Udalski et al 2005;Dong et al 2009;Gaudi et al 2008;Janczak et al 2010). We observed MOA-2007-BLG-192 in JHK using adaptive optics on the VLT while it was still amplified by a factor of 1.23 and again when the microlensing was over.…”

Section: Introductionmentioning

confidence: 84%

A frozen super-Earth orbiting a star at the bottom of the main sequence

Kubas

Beaulieu

Bennett

et al. 2012

A&A

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Context. Microlensing is a unique method to probe low mass exoplanets beyond the snow line. However, the scientific potential of the new microlensing planet discovery is often unfulfilled due to lack of knowledge of the properties of the lens and source stars. The discovery light curve of the super Earth MOA-2007-BLG-192Lb suffers from significant degeneracies that limit what can be inferred about its physical properties. Aims. High resolution adaptive optics images allow us to solve this problem by resolving the microlensing target from all unrelated background stars, yielding the unique determination of magnified source and lens fluxes. This estimation permits the solution of our microlens model for the mass of the planet and its host and their physical projected separation. Methods. We observed the microlensing event MOA-2007-BLG-192 at high angular resolution in JHKs with the NACO adaptive optics system on the VLT while the object was still amplified by a factor 1.23 and then at baseline 18 months later. We analyzed and calibrated the NACO photometry in the standard 2MASS system in order to accurately constrain the source and the lens star fluxes. Results. We detect light from the host star of MOA-2007-BLG-192Lb, which significantly reduces the uncertainties in its characteristics as compared to earlier analyses. We find that MOA-2007-BLG-192L

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OGLE 2003-BLG-235/MOA 2003-BLG-53: A Planetary Microlensing Event

Cited by 351 publications

References 31 publications

Discovery of a cool planet of 5.5 Earth masses through gravitational microlensing

Discovery of a cool planet of 5.5 Earth masses through gravitational microlensing

The HARPS search for southern extra-solar planets

A frozen super-Earth orbiting a star at the bottom of the main sequence

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