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Discovery and mass measurements of a cold, 10 earth mass planet and its host star


Muraki, Y and Han, C and Bennett, DP and Suzuki, D and Monard, LAG and Street, R and Jorgensen, UG and Kundurthy, P and Skowron, J and Becker, AC and Albrow, MD and Fouque, P and Heyrovsky, D and Barry, RK and Beaulieu, JP and Wellnitz, DD and Bond, IA and Sumi, T and Dong, S and Gaudi, BS and Bramich, M and Dominik, M and Abe, F and Botzler, CS and Freeman, M and Fukui, A and Furusawa, K and Hayashi, F and Hearnshaw, JB and Hosaka, S and Itow, Y and Kamiya, K and Korpela, AV and Kilmartin, PM and Lin, W and Ling, CH and Makita, S and Masuda, K and Matsubara, Y and Miyake, N and Nishimoto, K and Ohnishi, K and Perrott, YC and Rattenbury, NJ and Saito, T and Skuljan, L and Sullivan, DJ and Sweatman, WL and Tristram, PJ and Wada, K and Yock, PCM and Christie, GW and DePoy, DL and Gorbikov, E and Gould, A and Kaspi, S and Lee, CU and Mallia, F and Maoz, D and McCormick, J and Moorhouse, D and Natusch, T and Park, BG and Pogge, RW and Polishook, D and Shporer, A and Thornley, G and Yee, JC and Allan, A and Browne, P and Horne, K and Kains, N and Snodgrass, C and Steele, I and Tsapras, Y and Batista, V and Bennett, CS and Brillant, S and Caldwell, JAR and Cassan, A and Cole, A and Corrales, R and Coutures, C and Dieters, S and Prester, DD and Donatowicz, J and Greenhill, J and Kubas, D and Marquette, JB and Martin, R and Menzies, J and Sahu, KC and Waldman, I and Williams, A and Zub, M and Bourhrous, H and Matsuoka, Y and Nagayama, T and Oi, N and Randriamanakoto, Z and Bozza, V and Burgdorf, MJ and Novati, SC and Dreizler, S and Finet, F and Glitrup, M and Harpsoe, K and Hinse, TC and Hundertmark, M and Liebig, C and Maier, G and Mancini, L and Mathiasen, M and Rahvar, S and Ricci, D and Scarpetta, G and Skottfelt, J and Surdej, J and Southworth, J and Wambsganss, J and Zimmer, F and Udalski, A and Poleski, R and Wyrzykowski, L and Ulaczyk, K and Szymanski, MK and Kubiak, M and Pietrzynski, G and Soszynski, I, Discovery and mass measurements of a cold, 10 earth mass planet and its host star, The Astrophysical Journal: An International Review of Astronomy and Astronomical Physics, 741, (1) Article 22. ISSN 0004-637X (2011) [Refereed Article]

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Copyright 2011 The American Astronomical Society.

DOI: doi:10.1088/0004-637X/741/1/22


We present the discovery and mass measurement of the cold, low-mass planet MOA-2009-BLG-266Lb, performed with the gravitational microlensing method. This planet has a mass of mp = 10.4 ± 1.7 M⊕ and orbits a star of mass M sstarf = 0.56 ± 0.09 Msun at a semimajor axis of $a = 3.2{+1.9\atop -0.5}$ AU and an orbital period of $P = 7.6{+7.7\atop -1.5}$ yrs. The planet and host star mass measurements are enabled by the measurement of the microlensing parallax effect, which is seen primarily in the light curve distortion due to the orbital motion of the Earth. But the analysis also demonstrates the capability to measure the microlensing parallax with the Deep Impact (or EPOXI) spacecraft in a heliocentric orbit. The planet mass and orbital distance are similar to predictions for the critical core mass needed to accrete a substantial gaseous envelope, and thus may indicate that this planet is a "failed" gas giant. This and future microlensing detections will test planet formation theory predictions regarding the prevalence and masses of such planets.

Item Details

Item Type:Refereed Article
Keywords:gravitational lensing: micro; planetary systems
Research Division:Physical Sciences
Research Group:Astronomical sciences
Research Field:Stellar astronomy and planetary systems
Objective Division:Expanding Knowledge
Objective Group:Expanding knowledge
Objective Field:Expanding knowledge in the physical sciences
UTAS Author:Cole, A (Professor Andrew Cole)
UTAS Author:Dieters, S (Dr Stefan Dieters)
UTAS Author:Greenhill, J (Dr John Greenhill)
ID Code:74360
Year Published:2011
Web of Science® Times Cited:83
Deposited By:Mathematics and Physics
Deposited On:2011-11-24
Last Modified:2017-11-06

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