Discovery of a cool planet of 5.5 Earth masses through gravitational microlensing

  • Nature volume 439, pages 437440 (26 January 2006)
  • doi:10.1038/nature04441
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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 (M) 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 stars1,2,3,4. 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 M planetary companion at a separation of au from a M M-dwarf star, where M refers to a solar mass. (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 (ref. 5), 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.


Gravitational microlensing events can reveal extrasolar planets orbiting the foreground lens stars if the light curves are measured frequently enough to characterize planetary light curve deviations with features lasting a few hours6,7,8,9. Microlensing is most sensitive to planets in Earth-to-Jupiter-like orbits with semi-major axes in the range 1–5 au. The sensitivity of the microlensing method to low-mass planets is restricted by the finite angular size of the source stars10,11, limiting detections to planets of a few M for giant source stars, but allowing the detection of planets as small as 0.1M for main-sequence source stars in the Galactic Bulge. The PLANET collaboration12 maintains the high sampling rate required to detect low-mass planets while monitoring the most promising of the >500 microlensing events discovered annually by the OGLE collaboration, as well as events discovered by MOA. A decade of pioneering microlensing searches has resulted in the recent detections of two Jupiter-mass extrasolar planets13,14 with orbital separations of a few au by the combined observations of the OGLE, MOA, MicroFUN and PLANET collaborations. The absence of perturbations to stellar microlensing events can be used to constrain the presence of planetary lens companions. With large samples of events, upper limits on the frequency of Jupiter-mass planets have been placed over an orbital range of 1–10 au, down to M planets15,16,17 for the most common stars of our galaxy.

On 11 July 2005, the OGLE Early Warning System18announced the microlensing event OGLE-2005-BLG-390 (right ascension α = 17 h 54 min 19.2 s, declination δ = -30° 22′ 38″, J2000) with a relatively bright clump giant as a source star. Subsequently, PLANET, OGLE and MOA monitored it with their different telescopes. After peaking at a maximum magnification of Amax = 3.0 on 31 July 2005, a short-duration deviation from a single lens light curve was detected on 9 August 2005 by PLANET. As described below, this deviation was due to a low-mass planet orbiting the lens star.

From analysis of colour-magnitude diagrams, we derive the following reddening-corrected colours and magnitudes for the source star: (V - I)0 = 0.85, I0 = 14.25 and (V - K)0 = 1.9. We used the surface brightness relation20 linking the emerging flux per solid angle of a light-emitting body to its colour, calibrated by interferometric observations, to derive an angular radius of 5.25 ± 0.73 µas, which corresponds to a source radius of 9.6 ± 1.3R (where R is the radius of the Sun) if the source star is at a distance of 8.5 kpc. The source star colours indicate that it is a 5,200 K giant, which corresponds to a G4 III spectral type.

Figure 1 shows our photometric data for microlensing event OGLE-2005-BLG-390 and the best planetary binary lens model. The best-fit model has χ2 = 562.26 for 650 data points, seven lens parameters, and 12 flux normalization parameters, for a total of 631 degrees of freedom. Model length parameters in Table 1 are expressed in units of the Einstein ring radius RE (typically 2 au for a Galactic Bulge system), the size of the ring image that would be seen in the case of perfect lens–source alignment. In modelling the light curve, we adopted linear limb darkening laws21 with ΓI = 0.538 and ΓR = 0.626, appropriate for this G4 III giant source star, to describe the centre-to-limb variation of the intensity profile in the I and R bands. Four different binary lens modelling codes were used to confirm that the model we present is the only acceptable model for the observed light curve. The best alternative model is one with a large-flux-ratio binary source with a single lens, which has gross features that are similar to a planetary microlensing event22. However, as shown in Fig. 1, this model fails to account for the PLANET-Perth, PLANET-Danish and OGLE measurements near the end of the planetary deviation, and it is formally excluded by Δχ2 = 46.25 with one less model parameter.

Figure 1: The observed light curve of the OGLE-2005-BLG-390 microlensing event and best-fit model plotted as a function of time.
Figure 1

Error bars are 1σ. The data set consists of 650 data points from PLANET Danish (ESO La Silla, red points), PLANET Perth (blue), PLANET Canopus (Hobart, cyan), RoboNet Faulkes North (Hawaii, green), OGLE (Las Campanas, black), MOA (Mt John Observatory, brown). This photometric monitoring was done in the I band (with the exception of the Faulkes R-band data and the MOA custom red passband) and real-time data reduction was performed with the different OGLE, PLANET and MOA data reduction pipelines. Danish and Perth data were finally reduced by the image subtraction technique19 with the OGLE pipeline. The top left inset shows the OGLE light curve extending over the previous 4 years, whereas the top right one shows a zoom of the planetary deviation, covering a time interval of 1.5 days. The solid curve is the best binary lens model described in the text with q = 7.6 ± 0.7 × 10-5, and a projected separation of d = 1.610 ± 0.008RE. The dashed grey curve is the best binary source model that is rejected by the data, and the dashed orange line is the best single lens model.

Table 1: Microlensing fit parameters

The planet is designated OGLE-2005-BLG-390Lb, where the ‘Lb’ suffix indicates the secondary component of the lens system with a planetary mass ratio. The microlensing fit only directly determines the planet–star mass ratio, q = 7.6 ± 0.7 × 10-5, and the projected planet–star separation, d = 1.610 ± 0.008RE. Although the planet and star masses are not directly determined for planetary microlensing events, we can derive their probability densities. We have performed a bayesian analysis23 employing the Galactic models and mass functions described in refs 11 and 23. We averaged over the distances and velocities of the lens and source stars, subject to the constraints due to the angular diameter of the source and the measured parameters given in Table 1. This analysis gives a 95% probability that the planetary host star is a main-sequence star, a 4% probability that it is a white dwarf, and a probability of <1% that it is a neutron star or black hole. The host star and planet parameter probability densities for a main sequence lens star are shown in Fig. 2 for the Galactic model used in ref. 23. The medians of the lens parameter probability distributions yield a companion mass of and an orbital separation of au from the M lens star, which is located at a distance of DL = 6.6 ± 1.0 kpc. These error bars indicate the central 68% confidence interval. These median parameters imply that the planet receives radiation from its host star that is only 0.1% of the radiation that the Earth receives from the Sun, so the probable surface temperature of the planet is 50 K, similar to the temperatures of Neptune and Pluto.

Figure 2: Bayesian probability densities for the properties of the planet and its host star.
Figure 2

a, The masses of the lens star and its planet (M* and Mp respectively), b, their distance from the observer (DL), c, the three-dimensional separation or semi-major axis a of an assumed circular planetary orbit; and d, the orbital period Ω of the planet. (In a, Mref refers to M on the upper x axis and M on the lower x axis.) The bold, curved line in each panel is the cumulative distribution, with the percentiles listed on the right. The dashed vertical lines indicate the medians, and the shading indicates the central 68.3% confidence intervals, while dots and arrows on the abscissa mark the expectation value and standard deviation. All estimates follow from a bayesian analysis assuming a standard model for the disk and bulge population of the Milky Way, the stellar mass function of ref. 23, and a gaussian prior distribution for DS = 1.05 ± 0.25RGC (where RGC = 7.62 ± 0.32 kpc for the Galactic Centre distance). The medians of these distributions yield a M planetary companion at a separation of au from a M Galactic Bulge M-dwarf at a distance of 6.6 ± 1.0 kpc from the Sun. The median planetary period is years. The logarithmic means of these probability distributions (which obey Kepler's third law) are a separation of 2.9 au, a period of 10.4 years, and masses of 0.22M and 5.5M for the star and planet, respectively. In each plot, the independent variable for the probability density is listed within square brackets. The distribution of the planet–star mass ratio was taken to be independent of the stellar mass, and a uniform prior distribution was assumed for the planet–star separation distribution.

The parameters of this event are near the limits of microlensing planet detectability for a giant source star. The separation of d = 1.61 is near the outer edge of the so-called lensing zone7, which has the highest planet detection probability, and the planet's mass is about a factor of two above the detection limit set by the finite size of the source star. Planets with q > 10-3 and d ≈ 1 are much easier to detect, and so it may be that the parameters of OGLE-2005-BLG-390Lb represent a more common type of planet. This can be quantified by simulating planetary light curves with different values of q and θ (where θ is the angle of source motion with respect to the lens axis) but the remaining parameters are fixed to the values for the three known microlensing planets. We find that the probability of detecting a q ≈ 4–7 × 10-3 planet, like the first two microlens planets13,14, is 50 times larger than the probability of detecting a q = 7.6 × 10-5 planet like OGLE-2005-BLG-390Lb. This suggests that, at the orbital separations probed by microlensing, sub-Neptune-mass planets are significantly more common than large gas giants around the most common stars in our Galaxy. Similarly, the first detection of a sub-Neptune-mass planet at the outer edge of the ‘lensing zone’ provides a hint that these sub-Neptune-mass planets may tend to reside in orbits with semi-major axes a > 2 au.

The core-accretion model of planet formation predicts that rocky/icy 5–15M planets orbiting their host stars at 1–10 au are much more common than Jupiter-mass planets, and this prediction is consistent with the small fraction of M-dwarfs with planets detected by radial velocities3,5 and with previous limits from microlensing15. Our discovery of such a low-mass planet by gravitational microlensing lends further support to this model, but more detections of similar and lower-mass planets over a wide range of orbits are clearly needed. Planets with separations of 0.1 au will be detected routinely by the radial velocity method or space observations of planetary transits in the coming years24,25,26,27, but the best chance to increase our understanding of such planets over orbits of 1–10 au in the next 5–10 years is by future interferometer programs28 and more advanced microlensing surveys11,29,30.


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PLANET is grateful to the observatories that support our science (the European Southern Observatory, Canopus, Perth; and the South African Astronomical Observatory, Boyden, Faulkes North) and to the ESO team in La Silla for their help in maintaining and operating the Danish telescope. Support for the PLANET project was provided by CNRS, NASA, the NSF, the LLNL/NNSA/DOE, PNP, PICS France-Australia, D. Warren, the DFG, IDA and the SNF. RoboNet is funded by the UK PPARC and the FTN was supported by the Dill Faulkes Educational Trust. Support for the OGLE project, conducted at Las Campanas Observatory (operated by the Carnegie Institution of Washington), was provided by the Polish Ministry of Science, the Foundation for Polish Science, the NSF and NASA. The MOA collaboration is supported by MEXT and JSPS of Japan, and the Marsden Fund of New Zealand.

Author information


  1. PLANET/RoboNet Collaboration (http://planet.iap.fr and http://www.astro.livjm.ac.uk/RoboNet/)

    • J.-P. Beaulieu
    • , D. P. Bennett
    • , P. Fouqué
    • , A. Williams
    • , M. Dominik
    • , U. G. Jørgensen
    • , 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. M. Bramich
    • , M. Burgdorf
    • , C. Snodgrass
    •  & M. Bode
  2. OGLE Collaboration (http://ogle.astrouw.edu.pl)

    • A. Udalski
    • , M. K. Szymański
    • , M. Kubiak
    • , T. Wiȩckowski
    • , G. Pietrzyński
    • , I. Soszyński
    • , O. Szewczyk
    • , Ł. Wyrzykowski
    •  & B. Paczyński
  3. MOA Collaboration (http://www.physics.auckland.ac.nz/moa)

    • D. P. Bennett
    • , F. Abe
    • , I. A. Bond
    • , T. R. Britton
    • , A. C. Gilmore
    • , J. B. Hearnshaw
    • , Y. Itow
    • , K. Kamiya
    • , P. M. Kilmartin
    • , A. V. Korpela
    • , K. Masuda
    • , Y. Matsubara
    • , M. Motomura
    • , Y. Muraki
    • , S. Nakamura
    • , C. Okada
    • , K. Ohnishi
    • , N. J. Rattenbury
    • , T. Sako
    • , S. Sato
    • , M. Sasaki
    • , T. Sekiguchi
    • , D. J. Sullivan
    • , P. J. Tristram
    • , P. C. M. Yock
    •  & T. Yoshioka
  4. Institut d'Astrophysique de Paris, CNRS, Université Pierre et Marie Curie UMR7095, 98bis Boulevard Arago, 75014 Paris, France

    • J.-P. Beaulieu
    • , A. Cassan
    • , E. Corrales
    • , M. Desort
    •  & J.-B. Marquette
  5. University of Notre Dame, Department of Physics, Notre Dame, Indiana 46556-5670, USA

    • D. P. Bennett
  6. Observatoire Midi-Pyrénées, Laboratoire d'Astrophysique, UMR 5572, Université Paul Sabatier—Toulouse 3, 14 avenue Edouard Belin, 31400 Toulouse, France

    • P. Fouqué
  7. Perth Observatory, Walnut Road, Bickley, Perth, WA 6076, Australia

    • A. Williams
    •  & R. Martin
  8. Scottish Universities Physics Alliance, University of St Andrews, School of Physics and Astronomy, North Haugh, St Andrews KY16 9SS, UK

    • M. Dominik
    • , K. Horne
    •  & D. M. Bramich
  9. Niels Bohr Institutet, Astronomisk Observatorium, Juliane Maries Vej 30, 2100 København Ø, Denmark

    • U. G. Jørgensen
    • , C. Vinter
    •  & K. Woller
  10. European Southern Observatory, Casilla 19001, Santiago 19, Chile

    • D. Kubas
    •  & S. Brillant
  11. CEA DAPNIA/SPP Saclay, 91191 Gif-sur-Yvette cedex, France

    • C. Coutures
  12. University of Tasmania, School of Mathematics and Physics, Private Bag 37, Hobart, TAS 7001, Australia

    • J. Greenhill
    • , K. Hill
    •  & S. Dieters
  13. South African Astronomical Observatory, PO Box 9, Observatory 7935, South Africa

    • J. Menzies
  14. Research School of Astronomy and Astrophysics, Australian National University, Mt Stromlo Observatory, Weston Creek, ACT 2611, Australia

    • P. D. Sackett
  15. University of Canterbury, Department of Physics and Astronomy, Private Bag 4800, Christchurch 8020, New Zealand

    • M. Albrow
    • , K. Pollard
    • , T. R. Britton
    • , A. C. Gilmore
    • , J. B. Hearnshaw
    •  & P. M. Kilmartin
  16. McDonald Observatory, 16120 St Hwy Spur 78 #2, Fort Davis, Texas 79734, USA

    • J. A. R. Caldwell
  17. Boyden Observatory, University of the Free State, Department of Physics, PO Box 339, Bloemfontein 9300, South Africa

    • J. J. Calitz
    •  & P. Meintjes
  18. Lawrence Livermore National Laboratory, IGPP, PO Box 808, Livermore, California 94551, USA

    • K. H. Cook
  19. Universität Potsdam, Institut für Physik, Am Neuen Palais 10, 14469 Potsdam, Astrophysikalisches Institut Potsdam, An der Sternwarte 16, D-14482, Potsdam, Germany

    • D. Dominis
    •  & M. Hoffman
  20. Technische Universität Wien, Wiedner Hauptstrasse 8 / 020 B.A. 1040 Wien, Austria

    • J. Donatowicz
  21. Department of Astronomy, University of Florida, 211 Bryant Space Science Center, Gainesville, Florida 32611-2055, USA

    • S. Kane
  22. Space Telescope Science Institute, 3700 San Martin Drive, Baltimore, Maryland 21218, USA

    • K. Sahu
  23. Astronomisches Rechen-Institut (ARI), Zentrum für Astronomie, Universität Heidelberg, Mönchhofstrasse 12–14, 69120 Heidelberg, Germany

    • J. Wambsganss
  24. Astrophysics Research Institute, Liverpool John Moores University, Twelve Quays House, Egerton Wharf, Birkenhead CH41 1LD, UK

    • I. Steele
    • , D. M. Bramich
    • , M. Burgdorf
    •  & M. Bode
  25. Astronomy and Planetary Science Division, Department of Physics, Queen's University Belfast, Belfast, UK

    • C. Snodgrass
  26. Obserwatorium Astronomiczne Uniwersytetu Warszawskiego, Aleje Ujazdowskie 4, 00-478 Warszawa, Poland

    • A. Udalski
    • , M. K. Szymański
    • , M. Kubiak
    • , T. Wiȩckowski
    • , G. Pietrzyński
    • , I. Soszyński
    • , O. Szewczyk
    •  & Ł. Wyrzykowski
  27. Universidad de Concepcion, Departamento de Fisica, Casilla 160–C, Concepcion, Chile

    • G. Pietrzyński
    •  & I. Soszyński
  28. Jodrell Bank Observatory, The University of Manchester, Macclesfield, Cheshire SK11 9DL, UK

    • Ł. Wyrzykowski
    •  & N. J. Rattenbury
  29. Princeton University Observatory, Peyton Hall, Princeton, New Jersey 08544, USA

    • B. Paczyński
  30. Solar-Terrestrial Environment Laboratory, Nagoya University, Nagoya 464-860, Japan

    • F. Abe
    • , Y. Itow
    • , K. Kamiya
    • , K. Masuda
    • , Y. Matsubara
    • , M. Motomura
    • , Y. Muraki
    • , S. Nakamura
    • , C. Okada
    • , T. Sako
    • , M. Sasaki
    • , T. Sekiguchi
    •  & T. Yoshioka
  31. Institute for Information and Mathematical Sciences, Massey University, Private Bag 102-904, Auckland, New Zealand

    • I. A. Bond
  32. Department of Physics, University of Auckland, Private Bag 92019, Auckland, New Zealand

    • T. R. Britton
    • , P. J. Tristram
    •  & P. C. M. Yock
  33. School of Chemical and Physical Sciences, Victoria University, PO Box 600, Wellington, New Zealand

    • A. V. Korpela
    •  & D. J. Sullivan
  34. Nagano National College of Technology, Nagano 381-8550, Japan

    • K. Ohnishi
  35. Department of Astrophysics, Faculty of Science, Nagoya University, Nagoya 464-860, Japan

    • S. Sato


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  73. Search for T. Yoshioka in:

Competing interests

The photometric data set is available at planet.iap.fr and ogle.astrouw.edu.pl Reprints and permissions information is available at npg.nature.com/reprintsandpermissions. The authors declare no competing financial interests.

Corresponding author

Correspondence to J.-P. Beaulieu.


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