1. Limits on additional planetary companions to OGLE-2005-BLG-390L
- Author
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Kubas, Daniel, Cassan, Arnaud, Dominik, Martin, Bennett, Dave P., Wambsganss, Joachim, Beaulieu, Jean-Philippe, Albrow, Michael D., Batista, Virginie, Bode, M., Bramich, Daniel M., Brillant, Stéphane, Burgdorf, M., Caldwell, John A. R., Calitz, Hannes, Cook, Kem H., Coutures, Christian, Dieters, Stefan, Dominis Prester, Dijana, Donatowicz, Jadzia, Fouqué, Pascal, Greenhill, John, Hill, Kym, Hoffman, Matie, Horne, Keith, Jø rgensen, Uffe G., Kains, Noe, Kane, Stephen, Marquette, Jean-Baptiste, Martin, Ralph, Meintjes, Pieter, Menzies, John, Pollard, Karen R., Sahu, Kailash C., Snodgrass, C., Steele, I., Tsapras, Y., Vinter, Christian, Williams, Andrew, Woller, Kristian, and Zub, Marta
- Subjects
Astrophysics::Solar and Stellar Astrophysics ,Astrophysics::Cosmology and Extragalactic Astrophysics ,Astrophysics::Earth and Planetary Astrophysics ,techniques microlensing ,exoplanets individual OGLE-2005-BLG-390Lb ,stars M-dwarfs ,stars K-dwarfs ,Astrophysics::Galaxy Astrophysics - Abstract
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. 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. We find that more than 50 % of potential planets with a mass in excess of 1 M_J between 1.1 and 2.3 AU around OGLE-2005-BLG-390L would have revealed their existence, whereas for gas giants above 3 M_J 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.
- Published
- 2008