All Sky Doppler Extrasolar Planet Surveys with a Multi-object Dispersed Fixed-delay Interferometer

Details All Sky Doppler Extrasolar Planet Surveys with a Multi-object Dispersed Fixed-delay Interferometer All Sky Doppler Extrasolar Planet Surveys with a Multi-object Dispersed Fixed-delay Interferometer

2002-12-11

arxiv.org/abs/astro-ph/0212250v1

Astronomy and Astrophysics

Astrophysics

8 pages, 4 figures, to be published in the Scientif Frontiers in Research on Extrasolar Planets, ASP Conf. Proceedings, eds. D

Scientific paper

We propose to use a high throughput and high precision multi-object dispersed fixed-delay interferometer for all sky Doppler surveys for extrasolar planets. This instrument, a combination of a fixed-delay interferometer with a moderate resolution spectrometer,is completely different from current echelle spectrometers. Doppler RV is measured through monitoring interference fringe shifts of stellar absorption lines over a broad band. Coupling this multi-object instrument with a wide field telescope (a few degree, such as Sloan and WIYN) and UV, visible and near-IR detectors will allow to simultaneously obtain hundreds of stellar fringing spectra for searching for planets. The RV survey speed can be increased by more than 2 orders of magnitude over that for the echelles. A prototype dispersed fixed-delay interferometer has been observed at the Hobby-Eberly 9m and Palomar 5m telescopes in 2001 and demonstrated photo noise limited Doppler precision with Aldebaran. Our recent observations at the KPNO 2.1m telescope in 2002 demonstrate a short term Doppler precision of ~ 3 m/s with eta Cas (V = 3.5), a RV stable star and also obtained a RV curve for 51 Peg. (V = 5.5), confirming previous planet detection with an independent RV technique. The total measured detection efficiency including the sky, telescope and fiber transmission losses, the instrument and iodine transmission losses and detector quantum efficiency is 3.4% under 1.5 arcsec seeing conditions, which is comparable to all of the echelle spectrometers for planet detection.

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