A Search for Jupiter-Mass Companions to Nearby Stars

Walker, G. A. H.; Walker, A. R.; Irwin, Alan; Larson, Ana M.; Yang, S.; Richardson, D. C.

doi:10.1006/icar.1995.1130

Cited by 164 publications

(145 citation statements)

References 20 publications

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“…Companion limits for different planet search samples were presented by Murdoch et al (1993), Walker et al (1995) and Cumming et al (1999) for the Mount John Observatory, CFHT and Lick Observatory surveys, respectively. Nelson & Angel (1998) derived an analytical expression for detection limits and re-examined the CFHT data set.…”

Section: The Methodsmentioning

confidence: 99%

“…Although listed as a target, τ Cet was mainly included as a reference object since it is a known long-term RV-constant star (Campbell et al 1988;Walker et al 1995) and two other stars with known extrasolar planets, 51 Peg (Mayor & Queloz 1995) and 70 Vir , were also observed after 1995 to serve as RV precision check stars.…”

Section: The Target Samplementioning

confidence: 99%

“…The pioneering study by Walker et al (1995) first presented longterm (12 years) RV results for a sample of 21 stars and discussed the implications of their non-detections on the occurrence of Jovian-type planets around solar-type stars. In an even earlier work, Murdoch et al (1993) presented an analysis of their RV measurements for 29 stars over 2.5 years, finding no brown dwarf companions within 10 AU in their sample.…”

Section: Introductionmentioning

confidence: 99%

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The planet search program at the ESO Coudé Echelle spectrometer

Endl

Kürster

Els

et al. 2002

A&A

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Abstract. We present the complete results of the planet search program carried out at the ESO Coudé Echelle Spectrometer (CES) on La Silla, using the Long Camera from Nov. 1992 to April 1998. The CES survey has monitored 37 late-type (F8V -M5V) stars in the southern hemisphere for variations in their differential radial velocities (RV) in order to detect Doppler reflex motions caused by planetary companions. This led to the discovery of the first extrasolar planet in an Earth-like orbit around the young (ZAMS) and active G0V star ι Horologii . Here we present the RV results for all survey stars and perform a statistical examination of the whole data-set. Each star is tested for RV variability, RV trends (linear and non-linear) and significant periodic signals. β Hyi and Ind are identified as long-term, low-amplitude RV variables. Furthermore, for 30 CES survey stars we determine quantitative upper mass-limits for giant planets based on our long-term RV results. We find that the CES Long Camera survey would have detected short-period ("51 Peg-type") planets around all 30 stars but no planets with m sin i < 1 M Jup at orbital separations larger than 2 AU. Finally, we demonstrate that the CES planet search can be continued without applying velocity corrections to the RV results coming from the currently installed Very Long Camera at the CES.

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Section: The Methodsmentioning

confidence: 99%

Section: The Target Samplementioning

confidence: 99%

Section: Introductionmentioning

confidence: 99%

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The planet search program at the ESO Coudé Echelle spectrometer

Endl

Kürster

Els

et al. 2002

A&A

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“…These imply that for every observed star, the existence of planets below a certain minimum mass, depending on the semimajor axis a of the system and the stellar mass, cannot be excluded. Addressing and quantifying these limits is time consuming and the only results published up to now are from Walker et al (1995), Cumming, Marcy, & Butler (1999), and Endl et al (2002), based on CFHT, Lick, and ESO planet searches, respectively.…”

Section: Sample Selectionmentioning

confidence: 99%

Abundance Analysis of Planetary Host Stars. I. Differential Iron Abundances

Heiter¹,

Luck²

2003

102

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We present atmospheric parameters and iron abundances derived from high-resolution spectra for three samples of dwarf stars: stars that are known to host close-in giant planets (CGP), stars for which radial velocity data exclude the presence of a close-in giant planetary companion (no-CGP), as well as a random sample of dwarfs with a spectral type and magnitude distribution similar to that of the planetary host stars (control). All stars have been observed with the same instrument and have been analyzed using the same model atmospheres, atomic data, and equivalent width modeling program. Abundances have been derived differentially to the Sun, using a solar spectrum obtained with Callisto as the reflector with the same instrumentation. We find that the iron abundances of CGP dwarfs are on average 0.22 dex greater than that of no-CGP dwarfs. The iron abundance distributions of both the CGP and no-CGP dwarfs are different than that of the control dwarfs, while the combined iron abundances have a distribution that is very similar to that of the control dwarfs. All four samples (CGP, no-CGP, combined, and control) have different effective temperature distributions. We show that metal enrichment occurs only for CGP dwarfs with temperatures just below solar and %300 K higher than solar, whereas the abundance difference is insignificant at T eff around 6000 K.

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“…At first, only Jupiter-mass gas-giant planets were detectable (e.g. Murdoch et al 1993, Walker et al 1995, but now, with radial-velocity precision approaching 1 m/s, "super-Earths" are being discovered with masses below 10 Earth-masses (Vogt et al 2010, Mayor et al 2009). Models of planet formation predict a vast number of terrestrial-mass planets (e.g.…”

Section: Introductionmentioning

confidence: 99%

A Campaign for the Detection of Earth-Mass Planets in the Habitable Zone of Alpha Centauri

Wittenmyer

Endl²,

Bergmann

et al. 2012

Proc. IAU

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Abstract.We review the possible formation and orbital stability of Earth-mass or super Earthmass planets around either of the stars Alpha Centauri A or B and describe a program at Mt John University Observatory using the Doppler method that aims to detect such planets. From New Zealand, we are able to observe the Alpha Centauri system year-round. This is critical in order to acquire data of sufficient quantity and phase coverage to detect the orbit of a terrestrial-mass planet in the habitable zone. Our observations are being made at high resolution (R = 70, 000) and high signal-to-noise with the Hercules vacuum echelle spectrograph attached to the 1-m McLellan telescope by a 25-m long optical fibre and using an iodine cell. We discuss the velocity precision and instrumental stability required for success and outline the progress of the observations so far. At present we are collecting about 10,000 observations of each star, A and B, per year with a typical precision of 2.5 m/s per observation.

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A Search for Jupiter-Mass Companions to Nearby Stars

Cited by 164 publications

References 20 publications

The planet search program at the ESO Coudé Echelle spectrometer

The planet search program at the ESO Coudé Echelle spectrometer

Abundance Analysis of Planetary Host Stars. I. Differential Iron Abundances

A Campaign for the Detection of Earth-Mass Planets in the Habitable Zone of Alpha Centauri

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