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dc.contributor.authorBoss, APen_US
dc.contributor.authorWeinberger, AJen_US
dc.contributor.authorAnglada-Escudé, Gen_US
dc.contributor.authorThompson, IBen_US
dc.contributor.authorBrahm, Ren_US
dc.date.accessioned2015-06-04T11:45:12Z
dc.date.issued2012-01-01en_US
dc.identifier.isbn9781107033825en_US
dc.identifier.issn1743-9213en_US
dc.identifier.urihttp://qmro.qmul.ac.uk/xmlui/handle/123456789/7598
dc.description.abstractM dwarf stars are attractive targets in the search for habitable worlds as a result of their relative abundance and proximity, making them likely targets for future direct detection efforts. Hot super-Earths as well as gas giants have already been detected around a number of early M dwarfs, and the former appear to be the high-mass end of the population of rocky, terrestrial exoplanets. The Carnegie Astrometric Planet Search (CAPS) program has been underway since March 2007, searching ~ 100 nearby late M, L, and T dwarfs for gas giant planets on orbits wide enough for habitable worlds to orbit interior to them. The CAPSCam-N camera on the 2.5-m du Pont telescope at the Las Campanas Observatory has demonstrated the ability to detect planets as low in mass as Saturn orbiting at several AU around late M dwarfs within 15 pc. Over the next decade, the CAPS program will provide new constraints on the planetary census around late M dwarf stars, and hence on the suitability of these nearby planetary systems for supporting life. Copyright © International Astronomical Union 2014.en_US
dc.format.extent183 - 188en_US
dc.titleHabitable worlds around M dwarf stars: The CAPSCam astrometric planet searchen_US
dc.typeConference Proceeding
dc.identifier.doi10.1017/S1743921313012799en_US
pubs.issueS293en_US
pubs.notesNot knownen_US
pubs.publication-statusPublisheden_US
pubs.volume8en_US


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