The Anglo-Australian Planet Search. Xxiii. Two New Jupiter Analogs

Wittenmyer, Robert A.; Horner, Jonathan; Tinney, C. G.; Butler, R. Paul; Jones, H. R. A.; Tuomi, Mikko; Salter, G.; Carter, B. D.; Koch, Florian; O'Toole, S. J.; Bailey, Jeremy; Wright, D. E.

doi:10.1088/0004-637x/783/2/103

Cited by 70 publications

(51 citation statements)

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“…Our results are consistent with the literature, i.e.,that Jupiter-like planets in Jupiter-like orbits are relatively uncommon, occurring around less than 10% of stars. For giant planets beyond 3 au, frequencies of f~3% are reported by several teams (Cumming et al 2008;Wittenmyer et al 2014a;Rowan et al 2016), with uncertainties of 1%-3%. The recent work of Rowan et al (2016;R16), whose techniques most closely mirror our own, resulted in an estimate of f 1% 4% -(90% confidence interval).…”

Section: Discussionmentioning

confidence: 99%

“…This sets an inner limit of ∼3 au, which has been used by previous studies of Jupiter analogs (Wittenmyer et al 2014a;Rowan et al 2016). Giant planets that stay beyond this point should not prevent the accretion of telluric worlds.…”

Section: Introductionmentioning

confidence: 88%

“…If the goal is a detection limit equal to the rms scatter of the velocity data, then approximately N=190 observations would be required. As legacy radial-velocity searches such as the AAPS, Texas, and California Planet Survey (Fischer et al 2014;Wittenmyer et al 2014a;Endl et al 2016) extend their time baselines toward Saturn-like orbits (P Saturn = 29 years), then a long-term precision of 3 m s −1 or better is required to detect or exclude a Saturn analog (K 3 Saturn = m s −1 ).…”

Section: Detection Limitsmentioning

confidence: 99%

“…The occurrence rate of Jupiter analogs has been estimated from radial-velocity surveys (e.g., Cumming et al 2008;Wittenmyer et al 2014a;Rowan et al 2016) and from microlensing (Gould et al 2010). The former studies have generally arrived at a Jupiter-analog frequency of ∼3%-4% (agreeing with each other within uncertainties) while the latter arrived at a solar system analog frequency of ∼17% based on one detection of a Jupiter/Saturn analog pair.…”

Section: Introductionmentioning

confidence: 99%

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The Anglo-Australian Planet Search Xxiv: The Frequency of Jupiter Analogs

Wittenmyer

Butler

Tinney

et al. 2016

ApJ

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133

109

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We present updated simulations of the detectability of Jupiter analogs by the 17-year Anglo-Australian Planet Search. The occurrence rate of Jupiter-like planets that have remained near their formation locations beyond the ice line is a critical datum necessary to constrain the details of planet formation. It is also vital in our quest to fully understand how common (or rare) planetary systems like our own are in the Galaxy. From a sample of 202 solartype stars, and correcting for imperfect detectability on a star-by-star basis, we derive a frequency of 6.2 1.6 2.8 -+ % for giant planets in orbits from 3 to 7 au. When a consistent definition of "Jupiter analog" is used, our results are in agreement with those from other legacy radial-velocity surveys.

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Section: Discussionmentioning

confidence: 99%

Section: Introductionmentioning

confidence: 88%

Section: Detection Limitsmentioning

confidence: 99%

Section: Introductionmentioning

confidence: 99%

See 2 more Smart Citations

The Anglo-Australian Planet Search Xxiv: The Frequency of Jupiter Analogs

Wittenmyer

Butler

Tinney

et al. 2016

ApJ

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133

109

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“…In spite of these challenges, a number of Jupiter analog candidates have been discovered from long-duration planet surveys (see, e.g., Vogt et al 2000;Naef et al 2003;Wright et al 2007Wright et al , 2008Howard et al 2010;Boisse et al 2012;Marmier et al 2013;Wittenmyer et al 2014;Feng et al 2015). These surveys also demonstrate the prevalence of solar-like magnetic activity cycles, which can manifest in the stellar RVs Zechmeister et al 2013).…”

Section: Introductionmentioning

confidence: 99%

The Solar Twin Planet Search

Bedell

Meléndez

Bean

et al. 2015

A&A

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Context. With high-precision radial velocity surveys reaching a sufficiently long time baseline, the domain of long-period planet detections has recently opened up. The search for Jupiter-like planets is especially important if we wish to investigate the prevalence of solar system analogs, but their detection is complicated by the existence of stellar activity cycles on similar timescales. Radial velocity data with sufficiently long-term instrumental precision and robust methods of diagnosing activity are crucial to the detection of extrasolar Jupiters. Aims. Through our HARPS survey for planets around solar twin stars, we have identified a promising Jupiter twin candidate around the star HIP11915. We characterize this Keplerian signal and investigate its potential origins in stellar activity. Methods. We carry out a Markov chain Monte Carlo (MCMC) analysis of the radial velocity data. To examine the signal's origin, we employ a variety of statistical tests using activity diagnostics such as the Ca II H and K lines and line asymmetry tracers. Results. Our analysis indicates that HIP11915 hosts a Jupiter-mass planet with a 3800-day orbital period and low eccentricity. Although we cannot definitively rule out an activity cycle interpretation, we find that a planet interpretation is more likely based on a joint analysis of radial velocity and activity index data. Conclusions. The challenges of long-period radial velocity signals addressed in this paper are critical for the ongoing discovery of Jupiter-like exoplanets. If planetary in nature, the signal investigated here represents a very close analog to the solar system in terms of both Sun-like host star and Jupiter-like planet.

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The Dynamical Structure of HR 8799’s Inner Debris Disk

Contro

Wittenmyer

Horner

et al. 2015

Orig Life Evol Biosph

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The HR 8799 system, with its four giant planets and two debris belts, has an architecture closely mirroring that of our Solar system where the inner, warm asteroid belt and outer, cool Edgeworth-Kuiper belt bracket the giant planets. As such, it is a valuable laboratory for examining exoplanetary dynamics and debris disk-exoplanet interactions. Whilst the outer debris belt of HR 8799 has been well resolved by previous observations, the spatial extent of the inner disk remains unknown. This leaves a significant question mark over both the location of the planetesimals responsible for producing the belt's visible dust and the physical properties of those grains. We have performed the most extensive simulations to date of the inner, unresolved debris belt around HR 8799, using UNSW Australia's Katana supercomputing facility to follow the dynamical evolution of a model inner disk comprising 300,298 particles for a period of 60 million years. These simulations have enabled the characterisation of the extent and structure of the inner disk in detail, and will in future allow us to provide a first estimate of the small-body impact rate and water delivery prospects for possible (as-yet undetected) terrestrial planet(s) in the inner system.

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The Anglo-Australian Planet Search. Xxiii. Two New Jupiter Analogs

Cited by 70 publications

References 70 publications

The Anglo-Australian Planet Search Xxiv: The Frequency of Jupiter Analogs

The Anglo-Australian Planet Search Xxiv: The Frequency of Jupiter Analogs

The Solar Twin Planet Search

The Dynamical Structure of HR 8799’s Inner Debris Disk

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