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The PLANET microlensing follow-up network: results and prospects for the detection of extra-solar planets

Citation

Dominik, M and Albrow, MD and Beaulieu, JP and Caldwell, JAR and DePoy, DL and Gaudi, BS and Gould, A and Greenhill, JG and Hill, KM and Kane, S and Martin, R and Menzies, J and Naber, RM and Pel, JW and Pogge, RW and Pollard, KR and Sackett, PD and Sahu, KC and Vermaak, P and Watson, RD and Williams, A, The PLANET microlensing follow-up network: results and prospects for the detection of extra-solar planets, Planetary and Space Science, 50, (3) pp. 299-307. ISSN 0032-0633 (2002) [Refereed Article]

DOI: doi:10.1016/S0032-0633(01)00126-X

Abstract

Among various techniques to search for extra-solar planets, microlensing has some unique characteristics. Contrary to all other methods which favour nearby objects, microlensing is sensitive to planets around stars at distances of several kpc. These stars act as gravitational lenses leading to a brightening of observed luminous source stars. The lens stars that are tested for the presence of planets are not generally seen themselves. The largest sensitivity is obtained for planets at orbital separations of 1-10 AU offering the view on an extremely interesting range with regard to our own solar system and in particular to the position of Jupiter. The microlensing signal of a jupiter-mass planet lasts typically a few days. This means that a planet reveals its existence by producing a short signal at its quasi-instantaneous position, so that planets can be detected without the need to observe a significant fraction of the orbital period. Relying on the microlensing alerts issued by several survey groups that observe ∼ 10 7 stars in the Galactic bulge. PLANET (Probing Lensing Anomalies NETwork) performs precise and frequent measurements on ongoing microlensing events in order to detect deviations from a light curve produced by a single point-like object. These measurements allow constraints to be put on the abundance of planets. From 42 well-sampled events between 1995 and 1999, we infer that less than 1/3 of M-dwarfs in the Galactic bulge have jupiter-mass companions at separations between 1 and 4 AU from their parent star, and that < 45% have 3-jupiter-mass companions between 1 and 7 AU. © 2002 Elsevier Science Ltd. All rights reserved.

Item Details

Item Type:Refereed Article
Research Division:Physical Sciences
Research Group:Astronomical and Space Sciences
Research Field:Galactic Astronomy
Objective Division:Expanding Knowledge
Objective Group:Expanding Knowledge
Objective Field:Expanding Knowledge in the Physical Sciences
Author:Greenhill, JG (Dr John Greenhill)
Author:Hill, KM (Dr Kym Hill)
Author:Watson, RD (Dr Bob Watson)
ID Code:24014
Year Published:2002
Web of Science® Times Cited:26
Deposited By:Physics
Deposited On:2002-08-01
Last Modified:2011-08-02
Downloads:0

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