SIMBAD references

2016A&A...595A..79M - Astronomy and Astrophysics, volume 595A, 79-79 (2016/11-1)

High-contrast imaging of ε Eridani with ground-based instruments.

MIZUKI T., YAMADA T., CARSON J.C., KUZUHARA M., NAKAGAWA T., NISHIKAWA J., SITKO M.L., KUDO T., KUSAKABE N., HASHIMOTO J., ABE L., BRANDER W., BRANDT T.D., EGNER S., FELDT M., GOTO M., GRADY C.A., GUYON O., HAYANO Y., HAYASHI M., HAYASHI S.S., HENNING T., HODAPP K.W., ISHII M., IYE M., JANSON M., KANDORI R., KNAPP G.R., KWON J., MATSUO T., McELWAIN M.W., MIYAMA S., MORINO J., MORO-MARTIN A., NISHIMURA T., PYO T., SERABYN E., SUENAGA T., SUTO H., SUZUKI R., TAKAHASHI Y.H., TAKAMI M., TAKATO N., TERADA H., THALMANN C., TURNER E.L., WATANABE M., WISNIEWSKI J., TAKAMI H., USUDA T. and TAMURA M.

Abstract (from CDS):

ε Eridani is one of the nearest solar-type stars. Its proximity and relatively young age allow high-contrast imaging observations to achieve sensitivities to planets at narrow separations down to an inner radius of ∼5AU. Previous observational studies of the system report a dust disk with asymmetric morphology as well as a giant planet with large orbital eccentricity, which may require another massive companion to induce the peculiar morphology and to enhance the large orbital eccentricity. In this paper, we report results from deep high-contrastimaging observations to detect the previously reported planet and search for other unseen less massive companions with Subaru/HiCIAO, Gemini-South/NICI, and VLT/NACO. No positive detection was made, but high-contrast measurements with the CH4S narrow-band filter of HiCIAO achieved sensitivities at 14.7mag differential magnitude level, at an angular separation of 1.0''. In terms of planetary mass, as determined by cooling evolutionary models, the highest sensitivities were achieved by the Lp broad-band filter of NACO, resulting in sensitivities corresponding to 1.8, 2.8, and 4.5Mjup at the projected separation of 3AU, if 200, 400, and 800Myr is assumed for the age of the system, respectively. We also discuss origins of the dust disk from the detection sensitivity in the planetary mass and find that a less massive eccentric planet is preferred for disk stirring, which is consistent with the orbital parameters of ε Eri b claimed from the previous long-term radial velocity monitoring.

Abstract Copyright: © ESO 2016

Journal keyword(s): planets and satellites: general - stars: individual: epsilon Eridani - instrumentation: adaptive optics - techniques: image processing

Simbad objects: 3

goto Full paper

goto View the references in ADS

To bookmark this query, right click on this link: simbad:2016A&A...595A..79M and select 'bookmark this link' or equivalent in the popup menu


2021.08.04-01:51:37

© Université de Strasbourg/CNRS

    • Contact