Precise Age for the Binary Star System 12 Com in the Coma Berenices Cluster
We present measurements of the interferometrically resolved binary star system 12 Com and the single giant star 31 Com in the cluster Coma Berenices. 12 Com is a double-lined spectroscopic binary system consisting of a G7 giant and an A3 dwarf at the cluster turnoff. Using an extensive radial veloci...
| Main Authors: | , , , , , , , , , , , , , |
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| Format: | Article |
| Language: | English |
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IOP Publishing
2023-01-01
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| Series: | The Astronomical Journal |
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| Online Access: | https://doi.org/10.3847/1538-3881/accddb |
| _version_ | 1797698501723815936 |
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| author | Rex Lam Eric L. Sandquist Gail H. Schaefer Christopher D. Farrington John D. Monnier Narsireddy Anugu Cyprien Lanthermann Robert Klement Jacob Ennis Benjamin R. Setterholm Tyler Gardner Stefan Kraus Claire L. Davies Jerome A. Orosz |
| author_facet | Rex Lam Eric L. Sandquist Gail H. Schaefer Christopher D. Farrington John D. Monnier Narsireddy Anugu Cyprien Lanthermann Robert Klement Jacob Ennis Benjamin R. Setterholm Tyler Gardner Stefan Kraus Claire L. Davies Jerome A. Orosz |
| author_sort | Rex Lam |
| collection | DOAJ |
| description | We present measurements of the interferometrically resolved binary star system 12 Com and the single giant star 31 Com in the cluster Coma Berenices. 12 Com is a double-lined spectroscopic binary system consisting of a G7 giant and an A3 dwarf at the cluster turnoff. Using an extensive radial velocity data set and interferometric measurements from the Palomar Testbed Interferometer and the Center for High Angular Resolution Astronomy array, we measured masses M _1 = 2.64 ± 0.07 M _⊙ and M _2 = 2.10 ± 0.03 M _⊙ . Interferometry also allows us to resolve the giant and measure its size as R _1 = 9.12 ± 0.12 ± 0.01 R _⊙ . With the measured masses and radii, we find an age of 533 ± 41 ± 42 Myr. For comparison, we measure the radius of 31 Com to be 8.36 ± 0.15 R _⊙ . Based on the photometry and radius measurements, 12 Com A is likely the most evolved bright star in the cluster, large enough to be in the red giant phase, but too small to have core helium burning. Simultaneous knowledge of 12 Com A’s mass and photometry puts strong constraints on convective core overshooting during the main-sequence phase, which in turn reduces systematic uncertainties in the age. Increased precision in measuring this system also improves our knowledge of the progenitor of the cluster white dwarf WD1216+260. |
| first_indexed | 2024-03-12T03:55:02Z |
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| id | doaj.art-ba7343c603ab47fca87b391537e1afbb |
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| issn | 1538-3881 |
| language | English |
| last_indexed | 2024-03-12T03:55:02Z |
| publishDate | 2023-01-01 |
| publisher | IOP Publishing |
| record_format | Article |
| series | The Astronomical Journal |
| spelling | doaj.art-ba7343c603ab47fca87b391537e1afbb2023-09-03T11:59:32ZengIOP PublishingThe Astronomical Journal1538-38812023-01-0116612910.3847/1538-3881/accddbPrecise Age for the Binary Star System 12 Com in the Coma Berenices ClusterRex Lam0Eric L. Sandquist1https://orcid.org/0000-0003-4070-4881Gail H. Schaefer2https://orcid.org/0000-0001-5415-9189Christopher D. Farrington3https://orcid.org/0000-0001-9939-2830John D. Monnier4https://orcid.org/0000-0002-3380-3307Narsireddy Anugu5https://orcid.org/0000-0002-2208-6541Cyprien Lanthermann6https://orcid.org/0000-0001-9745-5834Robert Klement7https://orcid.org/0000-0002-4313-0169Jacob Ennis8https://orcid.org/0000-0002-1575-4310Benjamin R. Setterholm9https://orcid.org/0000-0001-5980-0246Tyler Gardner10https://orcid.org/0000-0002-3003-3183Stefan Kraus11https://orcid.org/0000-0001-6017-8773Claire L. Davies12https://orcid.org/0000-0001-9764-2357Jerome A. Orosz13https://orcid.org/0000-0001-9647-2886San Diego State University , Department of Astronomy, San Diego, CA 92182 USASan Diego State University , Department of Astronomy, San Diego, CA 92182 USAThe CHARA Array of Georgia State University , Mount Wilson Observatory, Mount Wilson, CA 13 91023, USAThe CHARA Array of Georgia State University , Mount Wilson Observatory, Mount Wilson, CA 13 91023, USAThe CHARA Array of Georgia State University , Mount Wilson Observatory, Mount Wilson, CA 13 91023, USAThe CHARA Array of Georgia State University , Mount Wilson Observatory, Mount Wilson, CA 13 91023, USAThe CHARA Array of Georgia State University , Mount Wilson Observatory, Mount Wilson, CA 13 91023, USAThe CHARA Array of Georgia State University , Mount Wilson Observatory, Mount Wilson, CA 13 91023, USAUniversity of Michigan , Deparment of Astronomy, Ann Arbor, MI 48109, USAAstronomy Department, University of Michigan , Ann Arbor, MI 48109, USAUniversity of Michigan , Deparment of Astronomy, Ann Arbor, MI 48109, USA; Astronomy Department, University of Michigan , Ann Arbor, MI 48109, USAAstrophysics Group, Department of Physics & Astronomy, University of Exeter , Stocker Road, Exeter, EX4 4QL, UKAstrophysics Group, Department of Physics & Astronomy, University of Exeter , Stocker Road, Exeter, EX4 4QL, UKSan Diego State University , Department of Astronomy, San Diego, CA 92182 USAWe present measurements of the interferometrically resolved binary star system 12 Com and the single giant star 31 Com in the cluster Coma Berenices. 12 Com is a double-lined spectroscopic binary system consisting of a G7 giant and an A3 dwarf at the cluster turnoff. Using an extensive radial velocity data set and interferometric measurements from the Palomar Testbed Interferometer and the Center for High Angular Resolution Astronomy array, we measured masses M _1 = 2.64 ± 0.07 M _⊙ and M _2 = 2.10 ± 0.03 M _⊙ . Interferometry also allows us to resolve the giant and measure its size as R _1 = 9.12 ± 0.12 ± 0.01 R _⊙ . With the measured masses and radii, we find an age of 533 ± 41 ± 42 Myr. For comparison, we measure the radius of 31 Com to be 8.36 ± 0.15 R _⊙ . Based on the photometry and radius measurements, 12 Com A is likely the most evolved bright star in the cluster, large enough to be in the red giant phase, but too small to have core helium burning. Simultaneous knowledge of 12 Com A’s mass and photometry puts strong constraints on convective core overshooting during the main-sequence phase, which in turn reduces systematic uncertainties in the age. Increased precision in measuring this system also improves our knowledge of the progenitor of the cluster white dwarf WD1216+260.https://doi.org/10.3847/1538-3881/accddbStellar agesInterferometric binary starsWhite dwarf starsStellar evolutionOpen star clustersSpectroscopic binary stars |
| spellingShingle | Rex Lam Eric L. Sandquist Gail H. Schaefer Christopher D. Farrington John D. Monnier Narsireddy Anugu Cyprien Lanthermann Robert Klement Jacob Ennis Benjamin R. Setterholm Tyler Gardner Stefan Kraus Claire L. Davies Jerome A. Orosz Precise Age for the Binary Star System 12 Com in the Coma Berenices Cluster The Astronomical Journal Stellar ages Interferometric binary stars White dwarf stars Stellar evolution Open star clusters Spectroscopic binary stars |
| title | Precise Age for the Binary Star System 12 Com in the Coma Berenices Cluster |
| title_full | Precise Age for the Binary Star System 12 Com in the Coma Berenices Cluster |
| title_fullStr | Precise Age for the Binary Star System 12 Com in the Coma Berenices Cluster |
| title_full_unstemmed | Precise Age for the Binary Star System 12 Com in the Coma Berenices Cluster |
| title_short | Precise Age for the Binary Star System 12 Com in the Coma Berenices Cluster |
| title_sort | precise age for the binary star system 12 com in the coma berenices cluster |
| topic | Stellar ages Interferometric binary stars White dwarf stars Stellar evolution Open star clusters Spectroscopic binary stars |
| url | https://doi.org/10.3847/1538-3881/accddb |
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