A long-period planet orbiting a nearby Sun-like star

Jones, Hugh R. A. and Butler, R. Paul and Tinney, C. G. and O'Toole, Simon and Wittenmyer, Rob and Henry, Gregory W. and Meschiari, Stefano and Vogt, Steve and Rivera, Eugenio and Laughlin, Greg and Carter, Brad D. and Bailey, Jeremy and Jenkins, James S. (2010) A long-period planet orbiting a nearby Sun-like star. Monthly Notices of the Royal Astronomical Society, 403 (4). pp. 1703-1713. ISSN 0035-8711

[img]
Preview
Text (Submitted Version)
Jones_Butler_Tinney_etal_2009_AV.pdf
Available under License Creative Commons Attribution.

Download (2674Kb)
[img]
Preview
Text (Published Version)
Jones_Butler_Tinney_O'Toole_Wittenmyer_Henry_Vogt_Rivera_Laughlin_Carter_Bailey_Jenkins_MNRAS_v403n4_PV.pdf
Available under License Creative Commons Attribution.

Download (1001Kb)

Abstract

The Doppler wobble induced by the extra-solar planet HD 134987b was first detected by data from the Keck Telescope nearly a decade ago, and was subsequently confirmed by data from the Anglo-Australian Telescope. However, as more data have been acquired for this star over the years since, the quality of a single Keplerian fit to that data has been getting steadily worse. The best fit single Keplerian to the 138 Keck and AAT observations now in hand has an root-mean-square (RMS) scatter of 6.6 m/s. This is significantly in excess of both the instrumental precision achieved by both the Keck and Anglo-Australian Planet Searches for stars of this magnitude, and of the jitter expected for a star with the properties of HD134987. However, a double Keplerian (i.e. dual planet) fit delivers a significantly reduced RMS of 3.3 m/s. The best-fit double planet solution has minimum planet masses of 1.59 and 0.82Mjup, orbital periods of 258 and 5000d, and eccentricities of 0.23 and 0.12 respectively. We find evidence that activity-induced jitter is a significant factor in our fits and do not find evidence for asteroseismological p-modes. We also present seven years of photometry at a typical precision of 0.003mag with the T8 0.8m automatic photometric telescope at Fairborn observatory. These observations do not detect photometric variability and support the inference that the detected radial-velocity periods are due to planetary mass companions rather than due to photospheric spots and plages.


Statistics for USQ ePrint 6556
Statistics for this ePrint Item
Item Type: Article (Commonwealth Reporting Category C)
Refereed: Yes
Item Status: Live Archive
Additional Information: Submitted version deposited in accordance with the copyright policy of the publisher.
Depositing User: Dr Brad Carter
Faculty / Department / School: Historic - Faculty of Sciences - Department of Biological and Physical Sciences
Date Deposited: 28 Jan 2010 10:40
Last Modified: 07 Nov 2013 02:01
Uncontrolled Keywords: solar and stellar astrophysics; earth and planetary astrophysics
Fields of Research (FOR2008): 02 Physical Sciences > 0201 Astronomical and Space Sciences > 020110 Stellar Astronomy and Planetary Systems
02 Physical Sciences > 0201 Astronomical and Space Sciences > 020108 Planetary Science (excl. Extraterrestrial Geology)
01 Mathematical Sciences > 0103 Numerical and Computational Mathematics > 010301 Numerical Analysis
Socio-Economic Objective (SEO2008): E Expanding Knowledge > 97 Expanding Knowledge > 970102 Expanding Knowledge in the Physical Sciences
Identification Number or DOI: doi: 10.1111/j.1365-2966.2009.16232.x
URI: http://eprints.usq.edu.au/id/eprint/6556

Actions (login required)

View Item Archive Repository Staff Only