High-resolution imaging of transiting extrasolar planetary systems (HITEP) II. Lucky imaging results from 2015 and 2016

Dynamical evolution and stability - planets and satellites; Formation -Techniques; High angular resolution - binaries; Planets and satellites; Visual; Bins; Extrasolar planets; Orbits; Photometry; Planets; Satellites; Surveys; High angular resolutions; High-resolution imaging; Historical measurements; Relative positions; Southern Hemisphere; Stars

Abstract :

[en] Context. The formation and dynamical history of hot Jupiters is currently debated, with wide stellar binaries having been suggested as a potential formation pathway. Additionally, contaminating light from both binary companions and unassociated stars can significantly bias the results of planet characterisation studies, but can be corrected for if the properties of the contaminating star are known. Aims. We search for binary companions to known transiting exoplanet host stars, in order to determine the multiplicity properties of hot Jupiter host stars. We also search for and characterise unassociated stars along the line of sight, allowing photometric and spectroscopic observations of the planetary system to be corrected for contaminating light. Methods. We analyse lucky imaging observations of 97 Southern hemisphere exoplanet host stars, using the Two Colour Instrument on the Danish 1.54 m telescope. For each detected companion star, we determine flux ratios relative to the planet host star in two passbands, and measure the relative position of the companion. The probability of each companion being physically associated was determined using our two-colour photometry. Results. A catalogue of close companion stars is presented, including flux ratios, position measurements, and estimated companion star temperature. For companions that are potential binary companions, we review archival and catalogue data for further evidence. For WASP-77AB and WASP-85AB, we combine our data with historical measurements to determine the binary orbits, showing them to be moderately eccentric and inclined to the line of sight (and hence planetary orbital axis). Combining our survey with the similar Friends of Hot Jupiters survey, we conclude that known hot Jupiter host stars show a deficit of high mass stellar companions compared to the field star population; however, this may be a result of the biases in detection and target selection by ground-based surveys. ©ESO 2018.

Disciplines :

Space science, astronomy & astrophysics

Author, co-author :

Evans, D. F.; Astrophysics Group, Keele University, Staffordshire, ST5 5BG, United Kingdom

Southworth, J.; Astrophysics Group, Keele University, Staffordshire, ST5 5BG, United Kingdom

Smalley, B.; Astrophysics Group, Keele University, Staffordshire, ST5 5BG, United Kingdom

Jørgensen, U. G.; Centre for Star and Planet Formation, Niels Bohr Institute, University of Copenhagen ØSter Voldgade 5, Copenhagen, 1350, Denmark

Dominik, M.; Centre for Exoplanet Science, SUPA School of Physics and Astronomy, University of St.Andrews, North Haugh, St.Andrews, KY16 9SS, United Kingdom

Andersen, M. I.; Dark Cosmology Centre, Niels Bohr Institute, University of Copenhagen, Juliane Maries Vej 30, Copenhagen, 2100, Denmark

Bozza, V.; Dipartimento di Fisica E.R. Caianiello, Universita di Salerno, via Giovanni Paolo II 132, Fisciano, 84084, Italy, Sezione di Napoli, Istituto Nazionale di Fisica Nucleare, Napoli, 80126, Italy

Bramich, D. M.

Burgdorf, M. J.; Department of Mathematics, Informatics and Natural Sciences, Meteorological Institute, Universität Hamburg, Bundesstraße 55, Hamburg, 20146, Germany

Ciceri, S.; Max Planck Institute for Astronomy, Königstuhl 17, Heidelberg, 69117, Germany

More authors (26 more)

Language :

English

Title :

High-resolution imaging of transiting extrasolar planetary systems (HITEP) II. Lucky imaging results from 2015 and 2016

Publication date :

2018

Journal title :

Astronomy and Astrophysics

ISSN :

0004-6361

eISSN :

1432-0746

Publisher :

EDP Sciences

Volume :

610

Peer reviewed :

Peer Reviewed verified by ORBi

Available on ORBi :

since 17 December 2018

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