|
|
| Discovery of a Low-mass Planet Orbiting a Low-mass Star in Microlensing Event MOA-2007-BLG-192 |
| Category:
03. Extrasolar Planets, Substellar Companions |
David P. Bennett1, I. A. Bond2, A. Udalski3, T. Sumi4, F. Abe4, A. Fukui4, K. Furusawa4, J. B. Hearnshaw5, S. Holderness6, Y. Itow4, K. Kamiya4, A. V. Korpela7, P. M. Kilmartin8, W. Lin2, C. H. Ling2, K. Masuda4, Y. Matsubura4, N. Miyake4, Y. Muraki9, M. Nagaya4, T. Okumura4, K. Ohnishi10, Y. C. Perrott6, N. J. Rattenbury11, T. Sako4, T. Saito12, S. Sato4, L. Skuljan2, D. J. Sullivan7, W. L. Sweatman2, P. J. Tristram8, P. C. M. Yock6, M. Kubiak3, M. K. Szymanski3, G. Pietrzynski13, I. Soszynski3, O. Szewczyk13, L. Wyrzykowski14, K. Ulaczyk3, V. Batista15, J. Beaulieu15, S. Brillant16, A. Cassan17, P. Fouque18, P. Kervella19, D. Kubas16, J. B. Marquette15
1University of Notre Dame, 2Massey University, New Zealand, 3Warsaw University Observatory, Poland, 4Nagoya University, Japan, 5Univ. of Canterbury, New Zealand, 6University of Auckland, New Zealand, 7Victoria University, New Zealand, 8Mt. John Observatory, New Zealand, 9Konan University, Japan, 10Nagano National College of Technology, Japan, 11Jodrell Bank Observatroy, United Kingdom, 12Tokyo Metropolitan College of Aeronautics, Japan, 13Universidad de Concepcion, Chile, 14University of Cambridge, United Kingdom, 15Institut d'Astrophysique de Paris, France, 16European Southern Observatory, Chile, 17Heidelberg University, Germany, 18Observatoire Midi-Pyrenees, France, 19Observatoire de Paris, France. |
| Presentation Number: 10.12 |
We present the analysis of microlensing event MOA-2007-BLG-192, which is the first microlensing planet discovery without the benefit of follow-up observations. The light curve reveals both the microlensing parallax effect and finite source effects, which imply that both the planet and its host must have low masses. However, the light curve coverage is somewhat sparse, so these mass estimates are not yet precise. High resolution adaptive optics images with the VLT/NACO instrument confirm the conclusion from the light curve that the host star must be very faint, and future observations with HST should determine the properties of the planet and its host star more precisely.
This work was funded in part by NASA and the NSF. |
| |
|
|
|
|
|
|
The Online Abstract Submission and Invitation System
© 1996 - 2010 Coe-Truman Technologies, Inc. All rights reserved.
|
|
|
|
|
|
