Three-dimensional Orbit and Dynamical Masses of GJ 105 AC
The precision of stellar models is higher than the precision at which we are able to measure the masses of most stars, with the notable exception of binaries where we can determine dynamical masses of the component stars. In addition to well-measured stellar properties, the ideal benchmark star is f...
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| Format: | Article |
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IOP Publishing
2025-01-01
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| Series: | The Astrophysical Journal |
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| Online Access: | https://doi.org/10.3847/1538-4357/adc564 |
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| author | Cayla M. Dedrick Jason T. Wright Jason D. Eastman Cullen H. Blake Samson A. Johnson Peter Plavchan John Asher Johnson David H. Sliski Maurice L. Wilson Robert A. Wittenmyer Thomas Barclay Jonathan Horner Stephen R. Kane Sharon X. Wang |
| author_facet | Cayla M. Dedrick Jason T. Wright Jason D. Eastman Cullen H. Blake Samson A. Johnson Peter Plavchan John Asher Johnson David H. Sliski Maurice L. Wilson Robert A. Wittenmyer Thomas Barclay Jonathan Horner Stephen R. Kane Sharon X. Wang |
| author_sort | Cayla M. Dedrick |
| collection | DOAJ |
| description | The precision of stellar models is higher than the precision at which we are able to measure the masses of most stars, with the notable exception of binaries where we can determine dynamical masses of the component stars. In addition to well-measured stellar properties, the ideal benchmark star is far enough from its companion that its properties are indistinguishable from an otherwise identical single star. Currently, there are a handful of stars with precise (±3%), model-independent mass measurements that are “effectively single” and for which we can obtain clean spectra (i.e., spectra that are not blended with a close companion). In this paper, we introduce GJ 105 AC as the newest members of this exclusive population. We present an updated orbital analysis for the long-period K3+M7 binary GJ 105 AC. We jointly analyze radial velocity (RV) and relative astrometry data, including new RVs from the Miniature Exoplanet Radial Velocity Array that capture the full periapsis passage and the RV minimum of the 76.0 ± 1.3 yr orbit for the first time. We derive precise dynamical masses of M _1 = 0.78 ± 0.02 M _⊙ and M _2 = 0.098 ± 0.002 M _⊙ . We find that of all stars with similarly precise masses (∼2%), GJ 105 AC stands out as having the widest on-sky separation after α Centauri AB, making it one of the most easily accessible to spectroscopy, as well as the the second-widest true separation, ensuring that its members are truly “effectively single” in terms of their evolution. |
| format | Article |
| id | doaj-art-b078f8bce57543bba08b5ef5bc018a06 |
| institution | DOAJ |
| issn | 1538-4357 |
| language | English |
| publishDate | 2025-01-01 |
| publisher | IOP Publishing |
| record_format | Article |
| series | The Astrophysical Journal |
| spelling | doaj-art-b078f8bce57543bba08b5ef5bc018a062025-08-20T03:12:43ZengIOP PublishingThe Astrophysical Journal1538-43572025-01-01985225510.3847/1538-4357/adc564Three-dimensional Orbit and Dynamical Masses of GJ 105 ACCayla M. Dedrick0https://orcid.org/0000-0001-9408-8848Jason T. Wright1https://orcid.org/0000-0001-6160-5888Jason D. Eastman2https://orcid.org/0000-0003-3773-5142Cullen H. Blake3https://orcid.org/0000-0002-6096-1749Samson A. Johnson4https://orcid.org/0000-0001-9397-4768Peter Plavchan5https://orcid.org/0000-0002-8864-1667John Asher Johnson6https://orcid.org/0000-0002-1159-1083David H. Sliski7https://orcid.org/0000-0002-6228-8244Maurice L. Wilson8https://orcid.org/0000-0003-1928-0578Robert A. Wittenmyer9https://orcid.org/0000-0001-9957-9304Thomas Barclay10https://orcid.org/0000-0001-7139-2724Jonathan Horner11https://orcid.org/0000-0002-1160-7970Stephen R. Kane12https://orcid.org/0000-0002-7084-0529Sharon X. Wang13https://orcid.org/0000-0002-6937-9034Department of Astronomy and Astrophysics, The Pennsylvania State University , 525 Davey Laboratory, 251 Pollock Road, University Park, PA 16802, USA ; ckd5370@psu.edu; Center for Exoplanets and Habitable Worlds, The Pennsylvania State University , University Park, PA 16802, USADepartment of Astronomy and Astrophysics, The Pennsylvania State University , 525 Davey Laboratory, 251 Pollock Road, University Park, PA 16802, USA ; ckd5370@psu.edu; Center for Exoplanets and Habitable Worlds, The Pennsylvania State University , University Park, PA 16802, USA; Penn State Extraterrestrial Intelligence Center, The Pennsylvania State University , University Park, PA 16802, USACenter for Astrophysics ∣ Harvard & Smithsonian , 60 Garden St., Cambridge, MA 02138, USADepartment of Physics and Astronomy, University of Pennsylvania , 209 South 33rd Street, Philadelphia, PA 19104, USANASA JPL , 4800 Oak Grove Drive, Pasadena, CA 91109, USAGeorge Mason University , 4400 University Drive, Fairfax, VA 22030, USACenter for Astrophysics ∣ Harvard & Smithsonian , 60 Garden St., Cambridge, MA 02138, USADavid R. Mittelman Observatory , Mayhill, NM 88339, USAHigh Altitude Observatory, National Center for Atmospheric Research , 3080 Center Green Dr., Boulder, CO 80301, USACentre for Astrophysics, University of Southern Queensland , UniSQ Toowoomba, QLD 4350, AustraliaNASA Goddard Space Flight Center , 8800 Greenbelt Road, Greenbelt, MD 20771, USACentre for Astrophysics, University of Southern Queensland , UniSQ Toowoomba, QLD 4350, AustraliaDepartment of Earth and Planetary Sciences, University of California , Riverside, CA 92521, USADepartment of Astronomy, Tsinghua University , Beijing 100084, People’s Republic of ChinaThe precision of stellar models is higher than the precision at which we are able to measure the masses of most stars, with the notable exception of binaries where we can determine dynamical masses of the component stars. In addition to well-measured stellar properties, the ideal benchmark star is far enough from its companion that its properties are indistinguishable from an otherwise identical single star. Currently, there are a handful of stars with precise (±3%), model-independent mass measurements that are “effectively single” and for which we can obtain clean spectra (i.e., spectra that are not blended with a close companion). In this paper, we introduce GJ 105 AC as the newest members of this exclusive population. We present an updated orbital analysis for the long-period K3+M7 binary GJ 105 AC. We jointly analyze radial velocity (RV) and relative astrometry data, including new RVs from the Miniature Exoplanet Radial Velocity Array that capture the full periapsis passage and the RV minimum of the 76.0 ± 1.3 yr orbit for the first time. We derive precise dynamical masses of M _1 = 0.78 ± 0.02 M _⊙ and M _2 = 0.098 ± 0.002 M _⊙ . We find that of all stars with similarly precise masses (∼2%), GJ 105 AC stands out as having the widest on-sky separation after α Centauri AB, making it one of the most easily accessible to spectroscopy, as well as the the second-widest true separation, ensuring that its members are truly “effectively single” in terms of their evolution.https://doi.org/10.3847/1538-4357/adc564Astrometric binary starsSpectroscopic binary starsCompanion starsRadial velocityAstrometryStellar evolution |
| spellingShingle | Cayla M. Dedrick Jason T. Wright Jason D. Eastman Cullen H. Blake Samson A. Johnson Peter Plavchan John Asher Johnson David H. Sliski Maurice L. Wilson Robert A. Wittenmyer Thomas Barclay Jonathan Horner Stephen R. Kane Sharon X. Wang Three-dimensional Orbit and Dynamical Masses of GJ 105 AC The Astrophysical Journal Astrometric binary stars Spectroscopic binary stars Companion stars Radial velocity Astrometry Stellar evolution |
| title | Three-dimensional Orbit and Dynamical Masses of GJ 105 AC |
| title_full | Three-dimensional Orbit and Dynamical Masses of GJ 105 AC |
| title_fullStr | Three-dimensional Orbit and Dynamical Masses of GJ 105 AC |
| title_full_unstemmed | Three-dimensional Orbit and Dynamical Masses of GJ 105 AC |
| title_short | Three-dimensional Orbit and Dynamical Masses of GJ 105 AC |
| title_sort | three dimensional orbit and dynamical masses of gj 105 ac |
| topic | Astrometric binary stars Spectroscopic binary stars Companion stars Radial velocity Astrometry Stellar evolution |
| url | https://doi.org/10.3847/1538-4357/adc564 |
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