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

Robert A. Wittenmyer; R. Paul Butler; C. G. Tinney; Jonathan Horner; B. D.  Carter; D. J.  Wright; Hugh Jones; J.  Bailey; Simon J. O'Toole

doi:10.3847/0004-637X/819/1/28

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

Robert A. Wittenmyer, R. Paul Butler, C. G. Tinney, Jonathan Horner, B. D. Carter, D. J. Wright, Hugh Jones, J. Bailey, Simon J. O'Toole

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Abstract

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 solar-type 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.

Original language	English
Pages (from-to)	28
Number of pages	11
Journal	The Astrophysical Journal
Volume	819
Issue number	1
Early online date	24 Feb 2016
DOIs	https://doi.org/10.3847/0004-637X/819/1/28
Publication status	Published - 1 Mar 2016

Keywords

planetary systems
radial velocities

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http://arxiv.org/abs/1601.05465Licence: CC BY

Cite this

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title = "The Anglo-Australian Planet Search XXIV: The Frequency of Jupiter Analogs",

abstract = "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 solar-type 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.",

keywords = "planetary systems, radial velocities",

author = "Wittenmyer, {Robert A.} and Butler, {R. Paul} and Tinney, {C. G.} and Jonathan Horner and Carter, {B. D.} and Wright, {D. J.} and Hugh Jones and J. Bailey and O'Toole, {Simon J.}",

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AU - Wright, D. J.

AU - Jones, Hugh

AU - Bailey, J.

AU - O'Toole, Simon J.

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N2 - 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 solar-type 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.

AB - 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 solar-type 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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The Anglo-Australian Planet Search XXIV: The Frequency of Jupiter Analogs

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