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! Year of discovery ! Year of discovery
|- |-
| ] <ref name="Bennett2008"/> || 0.01 || 0.66 || || || || 2008 | ] <ref name="Bennett2008"/> || 0.01 || 0.66 || || || || 2008
|- |-
| ] <ref name="Dong2009b"/> || 0.9 || 0.85 || || || || 2008 | ] <ref name="Dong2009b"/> || 0.9 || 0.85 || || || || 2008
|- |-
| ] || 2.4 || 1.0 || || || || 2012 | ] || 2.4 || 1.0 || || || || 2012
|- |-
| ] <ref name="Janczak2010"/> || 0.23 || 1.25 || || || || 2009 | ] <ref name="Janczak2010"/> || 0.23 || 1.25 || || || || 2009
|- |-
| ] <ref name="Batista2011"/> || 2.6 || 1.8 || 1970 || || || 2011 | ] <ref name="Batista2011"/> || 2.6 || 1.8 || 1970 || || || 2011
|- |-
| ] <ref name="Miyake2011"/> || 0.157 || 2.0 || || || || 2010 | ] <ref name="Miyake2011"/> || 0.157 || 2.0 || || || || 2010
|- |-
| ] <ref name="Beaulieu2006"/> || 0.017 || 2.1 || 3500 || || || 2005 | ] <ref name="Beaulieu2006"/> || 0.017 || 2.1 || 3500 || || || 2005
|- bgcolor="#ffffb0" |- bgcolor="#ffffb0"
| ] <ref name="Gaudi2008"/> || 0.727 || 2.3 || 1790 || || 64 || 2008 | ] <ref name="Gaudi2008"/> || 0.727 || 2.3 || 1790 || || 64 || 2008
|- |-
| ] <ref name="Gould2006"/> || 0.04 || 2.8 || 3300 || || || 2005 | ] <ref name="Gould2006"/> || 0.04 || 2.8 || 3300 || || || 2005
|- |-
| ] <ref name="Muraki2011"/> || 0.0327 || 3.2 || 2780 || || || 2010 | ] <ref name="Muraki2011"/> || 0.0327 || 3.2 || 2780 || || || 2010
|- |-
| ] <ref name="Sumi2010"/> || 0.0694 || 3.3 || || || || 2008 | ] <ref name="Sumi2010"/> || 0.0694 || 3.3 || || || || 2008
|- |-
| ] <ref name="dong2009a"/> || 3.5 || 3.6 || ~ 3600 || || || 2005 | ] <ref name="dong2009a"/> || 3.5 || 3.6 || ~ 3600 || || || 2005
|- bgcolor="#ffffb0" |- bgcolor="#ffffb0"
| ] <ref name="Gaudi2008"/> || 0.271 || 4.5 || 4931 || 0.15 || 64 || 2008 | ] <ref name="Gaudi2008"/> || 0.271 || 4.5 || 4931 || 0.15 || 64 || 2008
|- |-
| ] <ref name="bennett2006"/> || 2.6 || 5.1 || || || || 2004 | ] <ref name="bennett2006"/> || 2.6 || 5.1 || || || || 2004
|- |-
| ] || 3.7 || 8.3 || || || || 2012 | ] || 3.7 || 8.3 || || || || 2012
|- |-
| MOA-2010-BLG477L b<ref></ref> || 1.5 || 2±1 || || || || 2012 | MOA-2010-BLG477L b<ref></ref> || 1.5 || 2±1 || || || || 2012
Line 58: Line 58:
| ] || 5±2.5 || 4±1.6 || || || || 2013 | ] || 5±2.5 || 4±1.6 || || || || 2013
|- |-
| ] || 0.03 ± 0.0075 || 0.92 <ref>http://iopscience.iop.org/0004-637X/779/2/91/article</ref> || || || || 2013 | ] || 0.03 ± 0.0075 || 0.92 <ref>http://iopscience.iop.org/0004-637X/779/2/91/article</ref> || || || || 2013
|-
| ] || 5±2.5 || 4±1.6 || || || || 2013
|-
| ]<ref>http://arxiv.org/abs/1312.3951</ref>|| ~4 or 0.055 || Free-floating or ~1 || || || || 2013
|} |}


Revision as of 15:50, 17 December 2013

This article needs to be updated. Please help update this article to reflect recent events or newly available information. (March 2013)

This is the list of 19 extrasolar planets detected by microlensing, sorted by projected separations. To find planets using that method, the background star is temporarily magnified by a foreground star because of the gravity that bends light. If the foreground star has a planet, the light from background star would be slightly brighter than the star with no planet. Studying the brightness difference of background star between the foreground star with planets and foreground star with no planets, then mass can be estimated. The projected separation can be determined from how much the light bended.

The most massive planet detected by microlensing is MOA-bin-1b, which masses 3.7 MJ; the least massive is MOA-2007-BLG-192Lb, which masses 0.01 MJ or 3.3 M⊕. The widest separation between a planet and a star is MOA-bin-1b, which is 8.3 AU; the shortest separation is MOA-2007-BLG-192Lb, which is 0.66 AU.

There are 2 members of the multi-planet systems.

Yellow rows denote the members of the multi-planet system

Planet Mass (MJ) Projected separation (AU) Period (d) Eccentricity Inclination (°) Year of discovery
MOA-2007-BLG-192L b 0.01 0.66 2008
MOA-2007-BLG-400L b 0.9 0.85 2008
MOA-2011-BLG-293L b 2.4 1.0 2012
MOA-2008-BLG-310L b 0.23 1.25 2009
MOA-2009-BLG-387L b 2.6 1.8 1970 2011
MOA-2009-BLG-319 b 0.157 2.0 2010
OGLE-2005-BLG-390L b 0.017 2.1 3500 2005
OGLE-2006-BLG-109L b 0.727 2.3 1790 64 2008
OGLE-2005-BLG-169L b 0.04 2.8 3300 2005
MOA-2009-BLG-266L b 0.0327 3.2 2780 2010
OGLE-2007-BLG-368L b 0.0694 3.3 2008
OGLE-2005-BLG-071L b 3.5 3.6 ~ 3600 2005
OGLE-2006-BLG-109L c 0.271 4.5 4931 0.15 64 2008
OGLE-2003-BLG-235Lb 2.6 5.1 2004
MOA-bin-1 b 3.7 8.3 2012
MOA-2010-BLG477L b 1.5 2±1 2012
OGLE-2011-BLG-0251 b 0.53±0.21 2.72±0.75 or 1.5±0.5 2012/2013
OGLE-2012-BLG-0406L b 2.73±0.43 3.45±0.26 2013
OGLE-2012-BLG-0358L b 1.9±0.2 0.87 2013
MOA-2008-BLG-379 b 5±2.5 4±1.6 2013
MOA-2010-BLG-328L b 0.03 ± 0.0075 0.92 2013
MOA-2008-BLG-379 b 5±2.5 4±1.6 2013
MOA-2011-BLG-262 b ~4 or 0.055 Free-floating or ~1 2013

References

  1. Bennett, D. P.; et al. (2008). "A Low-Mass Planet with a Possible Sub-Stellar-Mass Host in Microlensing Event MOA-2007-BLG-192". The Astrophysical Journal. 684 (1): 663–683. arXiv:0806.0025. Bibcode:2008ApJ...684..663B. doi:10.1086/589940.
  2. Dong, Subo; et al. (2009). "Microlensing Event MOA-2007-BLG-400: Exhuming the Buried Signature of a Cool, Jovian-Mass Planet". The Astrophysical Journal. 698 (2): 1826–1837. arXiv:0809.2997. Bibcode:2009ApJ...698.1826D. doi:10.1088/0004-637X/698/2/1826.
  3. Janczak, Julia; et al. (2010). "Sub-Saturn Planet MOA-2008-BLG-310Lb: Likely To Be In The Galactic Bulge". The Astrophysical Journal. 711 (2): 731. arXiv:0908.0529. Bibcode:2010ApJ...711..731J. doi:10.1088/0004-637X/711/2/731.
  4. Batista, Virginie; et al. (2011). "MOA-2009-BLG-387Lb: A massive planet orbiting an M dwarf". Astronomy and Astrophysics. 529. arXiv:1102.0558. Bibcode:2011yCat..35299102B. doi:10.1051/0004-6361/201016111.
  5. Miyake, N.; et al. (2011). "A Sub-Saturn Mass Planet, MOA-2009-BLG-319Lb" (PDF). The Astrophysical Journal. 728 (2). article number 120. arXiv:1010.1809. Bibcode:2011ApJ...728..120M. doi:10.1088/0004-637X/728/2/120.
  6. Beaulieu, J.-P.; et al. (2006). "Discovery of a cool planet of 5.5 Earth masses through gravitational microlensing". Nature. 439 (7075): 437–440. arXiv:astro-ph/0601563. Bibcode:2006Natur.439..437B. doi:10.1038/nature04441. PMID 16437108. {{cite journal}}: Unknown parameter |month= ignored (help)
  7. ^ Gaudi; et al. (2008). "Discovery of a Jupiter/Saturn Analog with Gravitational Microlensing". Science. 319 (5865): 927–930. arXiv:0802.1920. Bibcode:2008Sci...319..927G. doi:10.1126/science.1151947. PMID 18276883.
  8. Gould, A.; et al. (2006). "Microlens OGLE-2005-BLG-169 Implies That Cool Neptune-like Planets Are Common". The Astrophysical Journal Letters. 644 (1): L37 – L40. arXiv:astro-ph/0603276. Bibcode:2006ApJ...644L..37G. doi:10.1086/505421.
  9. Muraki, Y.; et al. (2011). "Discovery and Mass Measurements of a Cold, 10 Earth Mass Planet and Its Host Star". The Astrophysical Journal. 741 (1). 22. arXiv:1106.2160. Bibcode:2011ApJ...741...22M. doi:10.1088/0004-637X/741/1/22.
  10. Sumi, T.; et al. (2010). "A Cold Neptune-Mass Planet OGLE-2007-BLG-368Lb: Cold Neptunes Are Common". The Astrophysical Journal. 710 (2): 1641–1653. arXiv:0912.1171. Bibcode:2010ApJ...710.1641S. doi:10.1088/0004-637X/710/2/1641.
  11. Dong, Subo; et al. (2009). "OGLE-2005-BLG-071Lb, the Most Massive M Dwarf Planetary Companion?". The Astrophysical Journal. 695 (2): 970–987. arXiv:0804.1354. Bibcode:2009ApJ...695..970D. doi:10.1088/0004-637X/695/2/970.
  12. Bennett, David P.; et al. (2006). "Identification of the OGLE-2003-BLG-235/MOA-2003-BLG-53 Planetary Host Star". The Astrophysical Journal Letters. 647 (2): L171 – L174. arXiv:astro-ph/0606038. Bibcode:2006ApJ...647L.171B. doi:10.1086/507585.
  13. MOA 2010-BLG-477Lb: constraining the mass of a microlensing planet from microlensing parallax, orbital motion and detection of blended light
  14. http://iopscience.iop.org/0004-637X/779/2/91/article
  15. http://arxiv.org/abs/1312.3951

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