A Doppler search for habitable satellites of ɛ Indi B

Details A Doppler search for habitable satellites of ɛ Indi B A Doppler search for habitable satellites of ɛ Indi B

Oct 2003

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2003esasp.539..647w&link_type=abstract

In: Proceedings of the Conference on Towards Other Earths: DARWIN/TPF and the Search for Extrasolar Terrestrial Planets, 22-25 A

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Extrasolar Planets, Epsilon Indi

Scientific paper

The recently discovered T2.5 companion to ɛ Ind is 1.7 mag brighter (J=12) than any previously known T dwarf. The Phoenix spectrograph on Gemini-South offers a unique opportunity to detect radial velocity perturbations <100 m/s caused by any satellites >0.1 Jupiter-mass (x 1/sini) orbiting near the habitable zone (P<2 d) of ɛ Ind B within a few nights. Unfortunately, Phoenix has a very limited band-pass (~60 Å). A spectrograph of similar resolution (~50,000) and a band pass of ~1000 Å operating in the 1 to 2 μm region would be capable of detecting terrestrial-mass satellites in the habitable zone. The possibility of Doppler detection of habitable planets around brown dwarfs makes a powerful case for a 'super' Phoenix. In 1999 we observed the T6.5 dwarf Gliese 229 B (J=14) on UKIRT with CGS4 but, proximity of A and for other reasons, radial velocity precision was limited to >1 km/s - insufficient to detect even Jupiter-mass satellites despite the smaller habitable zone.

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