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Revision as of 13:49, 25 January 2012 editMadkat25 (talk | contribs)59 edits updated all planets to date, added MOA-2011-BLG-293Lb and MOA-2009-BLG-266Lb to planet list. added period, inclination and eccentricity to table. updated starting text to match← Previous edit Revision as of 20:06, 1 May 2012 edit undoPlanetStar (talk | contribs)Autopatrolled, Extended confirmed users21,134 edits add MOA-bin-1bNext edit →
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This is the '''list of 14 ] ]''', 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. This is the '''list of 15 ] ]''', 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 ], which masses 3.5 M<sub>J</sub>; the least massive is ], which masses 0.01 M<sub>J</sub> or 3.3 M<sub>⊕</sub>. The widest separation between a planet and a star is ], which is 5.1 AU; the shortest separation is MOA-2007-BLG-192Lb, which is 0.66 AU. The most massive planet detected by microlensing is ], which masses 3.7 M<sub>J</sub>; the least massive is ], which masses 0.01 M<sub>J</sub> or 3.3 M<sub>⊕</sub>. 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. There are 2 members of the multi-planet systems.
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|- |-
| ] <ref name="Dong2009b"/> || 0.9 || 0.85 || || || || 2008 | ] <ref name="Dong2009b"/> || 0.9 || 0.85 || || || || 2008
⚫ |-
⚫ | ] || 2.4 || 1.0 || || || || 2012
|- |-
| ] <ref name="Janczak2010"/> || 0.23 || 1.25 || || || || 2009 | ] <ref name="Janczak2010"/> || 0.23 || 1.25 || || || || 2009
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| ] <ref name="Batista2011"/> || 2.6 || 1.8 || 1970 || || || 2011 | ] <ref name="Batista2011"/> || 2.6 || 1.8 || 1970 || || || 2011
|- |-
| ] <ref name="Miyake2011"/> || 0.157 || 2 || || || || 2010 | ] <ref name="Miyake2011"/> || 0.157 || 2.0 || || || || 2010
|-
| ] <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
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| ] <ref name="Gould2006"/> || 0.04 || 2.8 || 3300 || || || 2005 | ] <ref name="Gould2006"/> || 0.04 || 2.8 || 3300 || || || 2005
|- |-
| ] <ref name="Beaulieu2006"/> || 0.017 || 2.1 || 3500 || || || 2005 | ] || 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
⚫ |-
⚫ | ] <ref name="bennett2006"/> || 2.6 || 5.1 || || || || 2004
|- 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
|- |-
| ] || 0.0327 || 3.2 || 2780 || || || 2010 | ] <ref name="bennett2006"/> || 2.6 || 5.1 || || || || 2004
|- |-
| ] || 2.4 || 1 || || || || 2012 | ] || 3.7 || 8.3 || || || || 2012
|} |}


Revision as of 20:06, 1 May 2012

This is the list of 15 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-192Lb 0.01 0.66 2008
MOA-2007-BLG-400Lb 0.9 0.85 2008
MOA-2011-BLG-293Lb 2.4 1.0 2012
MOA-2008-BLG-310Lb 0.23 1.25 2009
MOA-2009-BLG-387Lb 2.6 1.8 1970 2011
MOA-2009-BLG-319b 0.157 2.0 2010
OGLE-2005-BLG-390Lb 0.017 2.1 3500 2005
OGLE-2006-BLG-109Lb 0.727 2.3 1790 64 2008
OGLE-2005-BLG-169Lb 0.04 2.8 3300 2005
MOA-2009-BLG-266Lb 0.0327 3.2 2780 2010
OGLE-2007-BLG-368Lb 0.0694 3.3 2008
OGLE-2005-BLG-071Lb 3.5 3.6 ~ 3600 2005
OGLE-2006-BLG-109Lc 0.271 4.5 4931 0.15 64 2008
OGLE-2003-BLG-235Lb 2.6 5.1 2004
MOA-bin-1b 3.7 8.3 2012

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. 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.
  10. Dong, Subo; et al. (2009). "OGLE-2005-BLG-071Lb, the Most Massive M Dwarf Planetary Companion?". The Astrophysical Journal. 695 (2): 970–987. Bibcode:2009ApJ...695..970D. doi:10.1088/0004-637X/695/2/970.
  11. 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.

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