Discovery of a Cool Planet of 5.5 Earth Masses Through Gravitational Microlensing

J. -P. Beaulieu; D. P. Bennett; P. Fouque; A. Williams; M. Dominik; U. G. Jorgensen; D. Kubas; A. Cassan; C. Coutures; J. Greenhill; K. Hill; J. Menzies; P. D. Sackett; M. Albrow; S. Brillant; J. A. R. Caldwell; J. J. Calitz; K. H. Cook; E. Corrales; M. Desort; S. Dieters; D. Dominis; J. Donatowicz; M. Hoffman; S. Kane; J. -B. Marquette; R. Martin; P. Meintjes; K. Pollard; K. Sahu; C. Vinter; J. Wambsganss; K. Woller; K. Horne; I. Steele; D. Bramich; M. Burgdorf; C. Snodgrass; M. Bode; A. Udalski; M. Szymanski; M. Kubiak; T. Wieckowski; G. Pietrzynski; I. Soszynski; O. Szewczyk; L. Wyrzykowski; B. Paczynski; the MOA Collaboration

doi:10.1038/nature04441

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arXiv · astro-ph/0601563

Discovery of a Cool Planet of 5.5 Earth Masses Through Gravitational Microlensing

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Abstract

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 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. 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 (+5.5/-2.7) M_earth planetary companion at a separation of 2.6 (+1.5/-0.6) AU from a 0.22 (+0.21/-0.11) M_solar M-dwarf star. (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, 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.

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J. -P. Beaulieu, D. P. Bennett, P. Fouque, A. Williams, M. Dominik, U. G. Jorgensen, D. Kubas, A. Cassan, C. Coutures, J. Greenhill, K. Hill, J. Menzies, P. D. Sackett, M. Albrow, S. Brillant, J. A. R. Caldwell, J. J. Calitz, K. H. Cook, E. Corrales, M. Desort, S. Dieters, D. Dominis, J. Donatowicz, M. Hoffman, S. Kane, J. -B. Marquette, R. Martin, P. Meintjes, K. Pollard, K. Sahu, C. Vinter, J. Wambsganss, K. Woller, K. Horne, I. Steele, D. Bramich, M. Burgdorf, C. Snodgrass, M. Bode, A. Udalski, M. Szymanski, M. Kubiak, T. Wieckowski, G. Pietrzynski, I. Soszynski, O. Szewczyk, L. Wyrzykowski, B. Paczynski, the MOA Collaboration. 2006-01-25. Discovery of a Cool Planet of 5.5 Earth Masses Through Gravitational Microlensing. https://doi.org/10.1038/nature04441

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