Methane Imaging Search for Planetary Mass Objects in Rho Ophiuchi

Details Methane Imaging Search for Planetary Mass Objects in Rho Ophiuchi Methane Imaging Search for Planetary Mass Objects in Rho Ophiuchi

Oct 2009

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2009aps..4cf.c5004h&link_type=abstract

American Physical Society, Fall 2009 Meeting of the Four Corners Section of the APS, October 23-24, 2009, abstract #C5.004

Astronomy and Astrophysics

Astrophysics

Scientific paper

T dwarfs are the coolest and least massive compact astrophysical objects that we can directly observe outside our Solar System. They share many properties with the expanding population of known exoplanets (almost all of which are inaccessible to direct observation themselves). An understanding of T dwarf atmospheres, therefore, is critical to our developing understanding of exoplanets. Moreover, T dwarf surveys in young star clusters can provide important answers to questions such as ``Is there a minimum mass for star formation?'' and ``How important is dynamical evolution for cluster mass functions?'' In recent years, methane imaging has emerged as a powerful tool for identifying T dwarf candidates in very young clusters, where T dwarfs are at their brightest and have not yet been subject to possible dynamical ejection from their clusters. We have recently conducted a methane imaging survey of the Rho Ophiuchi cluster for T dwarfs using the IRIS2 near-infrared imaging spectrograph on the Anglo-Australian Telescope. The Rho Ophiuchi cluster is the closest (d ˜ 120 parsecs) star-forming region to Earth that has a compact core harboring several hundred young (˜ 1 Myr) stellar objects. In this talk, we present the results of our imaging survey.

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