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Limits on additional planetary companions to OGLE 2005-BLG-390L

Citation

Kubas, D and Cassan, A and Dominik, M and Bennett, DP and Wambsganss, J and Brillant, S and Beaulieu, JP and Albrow, MD and Batista, V and Bode, M and Bramich, DM and Burgdorf, M and Caldwell, JAR and Calitz, H and Cook, KH and Coutures, C and Dieters, S and Dominis Prester, D and Donatowicz, J and Fouque, P and Greenhill, JG and Hill, KM and Hoffman, M and Horne, K and Jorgensen, UG and Kains, N and Kane, S and Marquette, JB and Martin, R and Meintjes, P and Menzies, J and Pollard, KR and Sahu, KC and Snodgrass, C and Steele, I and Tsapras, Y and Vinter, C and Williams, A and Woller, K and Zub, M, Limits on additional planetary companions to OGLE 2005-BLG-390L, Astronomy and Astrophysics, 483, (1) pp. 317-324. ISSN 0004-6361 (2008) [Refereed Article]


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Copyright Statement

Copyright © 2008 EDP Sciences

Official URL: http://www.edpsciences.org/

DOI: doi:10.1051/0004-6361:20077449

Abstract

Aims. We investigate constraints on additional planets orbiting the distant M-dwarf star OGLE 2005-BLG-390L, around which photometric microlensing data has revealed the existence of the sub-Neptune-mass planet OGLE 2005–BLG–390Lb. We specifically aim to study potential Jovian companions and compare our findings with predictions from core-accretion and disc-instability models of planet formation. We also obtain an estimate of the detection probability for sub-Neptune mass planets similar to OGLE 2005–BLG–390Lb using a simplified simulation of a microlensing experiment. Methods. We compute the efficiency of our photometric data for detecting additional planets around OGLE 2005-BLG-390L, as a function of the microlensing model parameters and convert it into a function of the orbital axis and planet mass by means of an adopted model of the Milky Way. Results. We find that more than 50% of potential planets with a mass in excess of 1 MJ between 1.1 and 2.3 AU around OGLE 2005-BLG-390Lwould have revealed their existence, whereas for gas giants above 3 MJ in orbits between 1.5 and 2.2 AU, the detection efficiency reaches 70%; however, no such companion was observed. Our photometric microlensing data therefore do not contradict the existence of gas giant planets at any separation orbiting OGLE 2005-BLG-390L. Furthermore we find a detection probability for an OGLE 2005–BLG–390Lb-like planet of around 2−5%. In agreement with current planet formation theories, this quantitatively supports the prediction that sub-Neptune mass planets are common around low-mass stars.

Item Details

Item Type:Refereed Article
Research Division:Physical Sciences
Research Group:Astronomical and Space Sciences
Research Field:Stellar Astronomy and Planetary Systems
Objective Division:Expanding Knowledge
Objective Group:Expanding Knowledge
Objective Field:Expanding Knowledge in the Physical Sciences
UTAS Author:Dieters, S (Dr Stefan Dieters)
UTAS Author:Greenhill, JG (Dr John Greenhill)
UTAS Author:Hill, KM (Dr Kym Hill)
ID Code:52306
Year Published:2008
Web of Science® Times Cited:22
Deposited By:Physics
Deposited On:2008-06-18
Last Modified:2011-03-22
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