SUB-SATURN PLANET MOA-2008-BLG-310Lb: LIKELY TO BE IN THE GALACTIC BULGE

Janczak, J.; Fukui, A.; Dong, Subo; Monard, L. A. G.; Kozłowski, S.; Gould, Andrew; Beaulieu, J. P.; Kubas, D.; Marquette, J. B.; Sumi, T.; Bond, I. A.; Bennett, D. P.; Abe, F.; Furusawa, K.; Hearnshaw, John; Hosaka, S.; Itow, Y.; Kamiya, K.; Korpela, A.; Kilmartin, P. M.; Lin, Wei; Ling, C. H.; Makita, S.; Masuda, K.; Matsubara, Y.; Miyake, N.; Muraki, Y.; Nagaya, M.; Nagayama, Takahiro; Nishimoto, K.; Ohnishi, Kouhei; Perrott, Y. C.; Rattenbury, N. J.; Sako, T.; Saito, To.; Skuljan, L.; Sullivan, D. J.; Sweatman, W. L.; Tristram, P. J.; Yock, P. C. M.; An, J.; Christie, Grant; Chung, Sun Ju; DePoy, D. L.; Gaudi, B. Scott; Han, Cheongho; Lee, Chung-Uk; Mallia, F.; Natusch, T.; Park, B. G.; Pogge, Richard W.; Anguita, T.; Novati, S. Calchi; Dominik, M.; Jørgensen, U. G.; Masi, G.; Mathiasen, M.; Batista, V.; Brillant, S.; Cassan, A.; Cole, A. A.; Corrales, E.; Coutures, C.; Dieters, S.; Fouqué, P.; Greenhill, J.

doi:10.1088/0004-637x/711/2/731

Cited by 119 publications

(117 citation statements)

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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: 83%

“…As in our previous analysis of planetary microlensing event MOA-2008-BLG-310Lb (Janczak et al 2010), we extract the photometry of NACO images using Starfinder (Diolaiti et al 2000). This tool is tailor suited to perform photometry of AO images of crowded fields.…”

Section: Photometric Analysismentioning

confidence: 99%

“…It is necessary to use the intermediate step of IRSF observations because we have too few stars in common between 2MASS and NACO. Such ladder has been used already and described in the appendix of (Janczak et al 2010). The three JHKs color systems are very close.…”

Section: Building a Calibration Laddermentioning

confidence: 99%

“…This can be done by directly measuring the light coming from the lens and measuring the lens and source relative proper motion (Bennett et al , 2007Gaudi et al 2008;Dong et al 2009;Janczak et al 2010) An extrasolar planet with a best-fit mass ratio of q ∼ 2 ×10 −4 was discovered in the microlensing event MOA 2007-BLG-192 (Bennett et al 2008 found by the MOA collaboration toward the Galactic bulge, (J2000: RA, Dec) = (18:08:03.8, −27:09:00).…”

Section: Introductionmentioning

confidence: 99%

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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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Section: Introductionmentioning

confidence: 83%

Section: Photometric Analysismentioning

confidence: 99%

Section: Building a Calibration Laddermentioning

confidence: 99%

Section: Introductionmentioning

confidence: 99%

See 2 more Smart Citations

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

Kubas

Beaulieu

Bennett

et al. 2012

A&A

Self Cite

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“…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

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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.

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Realisation of a fully‐deterministic microlensing observing strategy for inferring planet populations

et al. 2010

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Within less than 15 years, the count of known planets orbiting stars other than the Sun has risen from none to more than 400 with detections arising from four successfully applied techniques: Doppler-wobbles, planetary transits, gravitational microlensing, and direct imaging. While the hunt for twin Earths is on, a statistically well-defined sample of the population of planets in all their variety is required for probing models of planet formation and orbital evolution so that the origin of planets that harbour life, like and including ours, can be understood. Given the different characteristics of the detection techniques, a complete picture can only arise from a combination of their respective results. Microlensing observations are well-suited to reveal statistical properties of the population of planets orbiting stars in either the Galactic disk or bulge from microlensing observations, but a mandatory requirement is the adoption of strictly-deterministic criteria for selecting targets and identifying signals. Here, we describe a fully-deterministic strategy realised by means of the ARTEMiS (Automated Robotic Terrestrial Exoplanet Microlensing Search) system at the Danish 1.54-m telescope at ESO La Silla between June and August 2008 as part of the MiNDSTEp (Microlensing Network for the Detection of Small Terrestrial Exoplanets) campaign, making use of immediate feedback on suspected anomalies recognized by the SIGNAL-MEN anomaly detector. We demonstrate for the first time the feasibility of such an approach, and thereby the readiness for studying planet populations down to Earth mass and even below, with ground-based observations. While the quality of the real-time photometry is a crucial factor on the efficiency of the campaign, an impairment of the target selection by data of bad quality can be successfully avoided. With a smaller slew time, smaller dead time, and higher through-put, modern robotic telescopes could significantly outperform the 1.54-m Danish, whereas lucky-imaging cameras could set new standards for high-precision follow-up monitoring of microlensing events.

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SUB-SATURN PLANET MOA-2008-BLG-310Lb: LIKELY TO BE IN THE GALACTIC BULGE

Cited by 119 publications

References 36 publications

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

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

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

Realisation of a fully‐deterministic microlensing observing strategy for inferring planet populations

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