Surfing the photon noise: New techniques to find low-mass planets around M dwarfs

The current precision radial velocities techniques to detect low mass planets in M dwarf are quickly reviewed. This includes high resolution spectroscopic observations made both in the optical and in the near infrared. We discuss that, given the current instrumental performance, optical RVs are stil...

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Bibliographic Details
Published in:Astronomische Nachrichten 2013-02, Vol.334 (1-2), p.184-187
Main Authors: Anglada-Escudé, G., Butler, R.P., Reiners, A., Jones, H.R.A., Tuomi, M., Jenkins, J.S., Barnes, J.R., Vogt, S.S., Zechmeister, M.
Format: Article
Language:English
Subjects:
Astrophysics
brown dwarfs
Dwarf stars
Infrared
Noise
Photons
Planet detection
planetary systems
Planets
Spectrographs
Stars
stars: low-mass
stars: low‐mass, brown dwarfs
techniques: radial velocities
Wavelengths
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Summary:The current precision radial velocities techniques to detect low mass planets in M dwarf are quickly reviewed. This includes high resolution spectroscopic observations made both in the optical and in the near infrared. We discuss that, given the current instrumental performance, optical RVs are still far ahead over other approaches. However, this situation might change soon with the advent of new spectrographs with red/nIR capabilities. We review a newly developed method to obtain precision RV measurements on stabilized spectrographs and how it is implemented to archival HARPS observations. In addition to get much closer to the photon noise, this approach allows us to identify and filter out wavelength dependent noise sources achieving unprecedented accuracy on G, K and specially M dwarfs. We show how including red/infrared observations is of paramount importance to efficiently and unambiguously detect very low mass planets around cool spectral types. As examples, we show new measurements on Barnard's star indicating that the star is stable down to 0.9 cm s–1over a time‐span of 4 years and how RV signals correlated with activity indices disappear when using the reddest half of the HARPS wavelength range. To conclude, we present new results, detections and describe the implications in terms of planet/multi‐planet abundances around cool stars. (© 2013 WILEY‐VCH Verlag GmbH & Co. KGaA, Weinheim)
ISSN:0004-6337
1521-3994
DOI:10.1002/asna.201211775