English (United Kingdom)

https://curated-unify.zendy.io/wp-json/zendy-region/v1/featured_content/oa?rat=en

https://curated-unify.zendy.io/wp-json/zendy-region/v1/highlighted_journal/

Global: Zendy Plus annual

Presents the access of premium content as premium feature

Premium Content

Presents the keyphrase highlighting as premium feature

Keyphrase Highlighting

Presents the summarisation as premium feature

Summarisation

Insights

Presents the pdf analysis as premium feature

PDF Analysis

Presents the zaia usage as premium feature

ZAIA

Global: Zendy Tools annual

Global: Zendy Free Plan

Global: Zendy Tools monthly

Global: Zendy Plus monthly

Due to its proximity, youth, and solar-like characteristics with a spectraltype of K2V, Eps Eri is one of the most extensively studied systems in anextrasolar planet context. Based on radial velocity, astrometry, and studies ofthe structure of its circumstellar debris disk, at least two planetarycompanion candidates to Eps Eri have been inferred in the literature (Eps Erib, Eps Eri c). Some of these methods also hint at additional companionsresiding in the system. Here we present a new adaptive optics assistedhigh-contrast imaging approach that takes advantage of the favourable planetspectral energy distribution at 4 microns, using narrow-band angulardifferential imaging to provide an improved contrast at small and intermediateseparations from the star. We use this method to search for planets at orbitsintermediate between Eps Eri b (3.4 AU) and Eps Eri c (40 AU). The method isdescribed in detail, and important issues related to the detectability ofplanets such as the age of Eps Eri and constraints from indirect measurementsare discussed. The non-detection of companion candidates provides stringentupper limits for the masses of additional planets. Using a combination of theexisting dynamic and imaging data, we exclude the presence of any planetarycompanion more massive than 3 Mjup anywhere in the Eps Eri system.Specifically, with regards to the possible residual linear radial velocitytrend, we find that it is unlikely to correspond to a real physical companionif the system is as young as 200 Myr, whereas if it is as old as 800 Myr, thereis an allowed semi-major axis range between about 8.5 and 25 AU.

A comprehensive examination of the Eps Eri system -- Verification of a 4 micron narrow-band high-contrast imaging approach for planet searches