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Frank Grundahl

Determining the Age of the Kepler Open Cluster NGC 6819 With a New Triple System and Other Eclipsing Binary Stars

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DOI

  • Lauren N. Brewer, San Diego State University, Department of Astronomy, San Diego, CA 92182, USA ezereve@gmail.com
  • ,
  • Eric L. Sandquist, San Diego State University, Department of Astronomy, San Diego, CA 92182, USA esandquist@mail.sdsu.edu
  • ,
  • Robert D. Mathieu, jorosz@mail.sdsu.edu
  • ,
  • Katelyn Milliman, mjeffries11@gmail.com
  • ,
  • Aaron M. Geller, Department of Astronomy, San Diego State University, San Diego, CA 92182, USA mathieu@astro.wisc.edu
  • ,
  • Mark W., Jr. Jeffries, Department of Astronomy, San Diego State University, San Diego, CA 92182, USA milliman@astro.wisc.edu
  • ,
  • Jerome A. Orosz, San Diego State University, Department of Astronomy, San Diego, CA 92182, USA a-geller@northwestern.edu
  • ,
  • Karsten Brogaard
  • Imants Platais, Department of Physics and Astronomy, The Johns Hopkins University, Baltimore, MD 21218, USA bruntt@gmail.com
  • ,
  • Hans Bruntt
  • ,
  • Frank Grundahl
  • Dennis Stello, Sydney Institute for Astronomy (SIfA), School of Physics, University of Sydney, Sydney, NSW 2006, Australia imants@pha.jhu.edu
  • ,
  • Søren Frandsen
As part of our study of the old (˜2.5 Gyr) open cluster NGC 6819 in the Kepler field, we present photometric (Kepler and ground-based BVRCIC) and spectroscopic observations of the detached eclipsing binary WOCS 24009 (Auner 665; KIC 5023948) with a short orbital period of 3.6 days. WOCS 24009 is a triple-lined system, and we verify that the brightest star is physically orbiting the eclipsing binary using radial velocities and eclipse timing variations. The eclipsing binary components have masses MB = 1.090 ± 0.010 M⊙ and MC = 1.075 ± 0.013 M⊙, and radii RB = 1.099 ± 0.006 ± 0.005 R⊙ and RC = 1.069 ± 0.006 ± 0.013 R⊙. The bright non-eclipsing star resides at the cluster turnoff, and ultimately its mass will directly constrain the turnoff mass: our preliminary determination is MA = 1.251 ± 0.057 M⊙. A careful examination of the light curves indicates that the fainter star in the eclipsing binary undergoes a very brief period of total eclipse, which enables us to precisely decompose the light of the three stars and place them in the color-magnitude diagram (CMD). We also present improved analysis of two previously discussed detached eclipsing stars in NGC 6819 (WOCS 40007 and WOCS 23009) en route to a combined determination of the cluster’s distance modulus (m - M)V = 12.38 ± 0.04. Because this paper significantly increases the number of measured stars in the cluster, we can better constrain the age of the CMD to be 2.21 ± 0.10 ± 0.20 Gyr. Additionally, using all measured eclipsing binary star masses and radii, we constrain the age to 2.38 ± 0.05 ± 0.22 Gyr. The quoted uncertainties are estimates of measurement and systematic uncertainties (due to model physics differences and metal content), respectively. This is paper 57 of the WIYN Open Cluster Study (WOCS).
Original languageEnglish
JournalThe Astronomical Journal
Volume151
Issue3
Pages (from-to)66
ISSN0004-6256
DOIs
Publication statusPublished - 1 Mar 2016

    Research areas

  • binaries: eclipsing, binaries: spectroscopic, open clusters and associations: individual: NGC 6819, stars: evolution, techniques: photometric, techniques: spectroscopic

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ID: 99418218