University of Hertfordshire

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From the same journal

By the same authors

Benchmark cool companions: Ages and abundances for the PZ Tel system

Research output: Contribution to journalArticle

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  • 904651

    Accepted author manuscript, 3.22 MB, PDF document

  • J. S. Jenkins
  • Yakiv pavlenko
  • Oleksiy Ivanyuk
  • Jose Gallardo
  • Matias jones
  • Avril day-jones
  • H.R.A. Jones
  • Maria-Teresa Ruiz
  • D.J. Pinfield
  • Larissa Yakovina
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Original languageEnglish
Pages (from-to)3587–3598
JournalMonthly Notices of the Royal Astronomical Society
Volume420
Issue4
DOIs
Publication statusPublished - Mar 2012

Abstract

We present new ages and abundance measurements for the pre-main sequence star PZ Tel. PZ Tel was recently found to host a young and low-mass companion. Using FEROS spectra we have measured atomic abundances (e.g. Fe and Li) and chromospheric activity for PZ Tel and used these to obtain metallicity and age estimates for the companion. We find PZ Tel to be a rapidly rotating (vsini=73\pm5km/s), ~solar metallicity star (logN(Fe)=-4.37 dex or [Fe/H]=0.05 dex) with a measured mean logR'HK of -4.12. We measure a NLTE lithium abundance of logN(Li)=3.1\pm0.1dex, which from depletion models gives rise to an age of 7+4-2 Myrs for the system. The measured chromospheric activity returns an age of 26\pm2Myrs, as does fitting pre-main sequence evolutionary tracks (Tau_evol=22\pm3Myrs), both of which are in disagreement with the lithium age. We speculate on reasons for this difference and introduce new models for lithium depletion that incorporates both rotation and magnetic field affects. We also synthesize solar, metal-poor and metal-rich substellar evolutionary models to better determine the bulk properties of PZ Tel B, showing that PZ Tel B is probably more massive than previous estimates, meaning the companion is not a giant exoplanet. We show how PZ Tel B compares to other currently known age and metallicity benchmark systems and try to empirically test the effects of dust opacity as a function of metallicity on the near infrared colours of brown dwarfs. Current models suggest that in the near infrared observations are more sensitive to low-mass companions orbiting more metal-rich stars. We also look for trends between infrared photometry and metallicity amongst a growing population of substellar benchmark objects, and identify the need for more data in mass-age-metallicity parameter space. [Abridged]

Notes

16 pages, 10 figures and 3 tables. Accepted for publication in MNRAS

ID: 697589