2008A&A...488..771J


C.D.S. - SIMBAD4 rel 1.7 - 2019.12.12CET01:45:41

2008A&A...488..771J - Astronomy and Astrophysics, volume 488, 771-780 (2008/9-3)

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

JANSON M., REFFERT S., BRANDNER W., HENNING T., LENZEN R. and HIPPLER S.

Abstract (from CDS):

Due to its proximity, youth, and solar-like characteristics with a spectral type of K2V, ε Eri is one of the most extensively studied systems in an extrasolar planet context. Based on radial velocity, astrometry, and studies of the structure of its circumstellar debris disk, at least two planetary companion candidates to ε Eri have been inferred in the literature (ε Eri b, ε Eri c). Some of these methods also hint at additional companions residing in the system. Here we present a new adaptive optics assisted high-contrast imaging approach that takes advantage of the favourable planet spectral energy distribution at 4 µm, using narrow-band angular differential imaging to provide an improved contrast at small and intermediate separations from the star. We use this method to search for planets at orbits intermediate between ε Eri b (3.4AU) and ε Eri c (40AU). The method is described in detail, and important issues related to the detectability of planets such as the age of ε Eri and constraints from indirect measurements are discussed. The non-detection of companion candidates provides stringent upper limits for the masses of additional planets. Using a combination of the existing dynamic and imaging data, we exclude the presence of any planetary companion more massive than 3Mjup anywhere in the ε Eri system. Specifically, with regards to the possible residual linear radial velocity trend, we find that it is unlikely to correspond to a real physical companion if the system is as young as 200Myr, whereas if it is as old as 800Myr, there is an allowed semi-major axis range between about 8.5 and 25AU.

Abstract Copyright:

Journal keyword(s): instrumentation: adaptive optics - planetary systems - stars: late-type - instrumentation: high angular resolution

Simbad objects: 6

goto Full paper

goto View the reference in ADS

Number of rows : 6

N Identifier Otype ICRS (J2000)
RA
ICRS (J2000)
DEC
Mag U Mag B Mag V Mag R Mag I Sp type #ref
1850 - 2020
#notes
1 * eps Eri c Pl? 03 32 55.84496 -09 27 29.7312           ~ 3 1
2 * eps Eri b Pl 03 32 55.84496 -09 27 29.7312           ~ 102 1
3 * eps Eri BY* 03 32 55.8449634 -09 27 29.731165 5.19 4.61 3.73 3.00 2.54 K2V 1662 1
4 Cl Melotte 22 OpC 03 47 00 +24 07.0           ~ 2916 0
5 Cl Melotte 25 OpC 04 26 54.00 +15 52 00.0           ~ 2588 0
6 NAME Ursa Major Moving Group MGr 12 32 +57.0           ~ 371 2

    Equat.    Gal    SGal    Ecl

To bookmark this query, right click on this link: simbad:objects in 2008A&A...488..771J and select 'bookmark this link' or equivalent in the popup menu


2019.12.12-01:45:41

© Université de Strasbourg/CNRS

    • Contact