| dc.contributor.author | Stassun, Keivan G. | |
| dc.date.accessioned | 2023-02-16T17:58:03Z | |
| dc.date.available | 2023-02-16T17:58:03Z | |
| dc.date.issued | 2023-02-01 | |
| dc.identifier.citation | Victoria DiTomasso et al 2023 AJ 165 38 | en_US |
| dc.identifier.issn | 0004-6256 | |
| dc.identifier.other | eISSN 1538-3881 | |
| dc.identifier.uri | http://hdl.handle.net/1803/18001 | |
| dc.description | Only Vanderbilt University affiliated authors are listed on VUIR. For a full list of authors, access the version of record at https://iopscience.iop.org/article/10.3847/1538-3881/ac9ccd | en_US |
| dc.description.abstract | We present high-precision radial velocities (RVs) from the HARPS-N spectrograph for HD79210 and HD79211, two M0V members of a gravitationally-bound binary system. We detect a planet candidate with a period of 24.421(-0.017)(+0.016) days around HD79211 in these HARPS-N RVs, validating the planet candidate originally identified in CARMENES RV data alone. Using HARPS-N, CARMENES and HIRES RVs spanning a total of 25 years, we further refine the planet candidate parameters to P = 24.422 +/- 0.014 days, K = 3.19 +/- 0.27 m s(-1), M sin i = 10.6 +/- 1.2M(circle plus), and a = 0.142 +/- 0.005 au. We do not find any additional planet candidate signals in the data of HD79211 nor do we find any planet candidate signals in HD79210. This system adds to the number of exoplanets detected in binaries with M dwarf members, and serves as a case study for planet formation in stellar binaries. | en_US |
| dc.description.sponsorship | This material is based upon work supported by the National Science Foundation Graduate Research Fellowship under grant No. DGE1745303. The HARPS-N project was funded by the Prodex Program of the Swiss Space Office (SSO), the HarvardUniversity Origin of Life Initiative (HUOLI), the Scottish Universities Physics Alliance (SUPA), the University of Geneva, the Smithsonian Astrophysical Observatory (SAO), the Italian National Astrophysical Institute (INAF), University of St. Andrews, Queen's University Belfast, and University of Edinburgh. Parts of this work have been supported by the National Aeronautics and Space Administration under grant No. NNX17AB59G, issued through the Exoplanets Research Program. Parts of this work have been supported by the Brinson Foundation. R.D.H. is funded by the UK Science and Technology Facilities Council (STFC)'s Ernest Rutherford Fellowship (grant No. ST/V004735/1). T.G.W and A.C.C acknowledge support from STFC consolidated grant Nos. ST/ R000824/1 and ST/V000861/1, and UKSA grant ST/ R003203/1. This work has made use of data from the European Space Agency (ESA) mission Gaia (https://www. cosmos.esa.int/gaia), processed by the Gaia Data Processing and Analysis Consortium (DPAC, https://www.cosmos.esa. int/web/gaia/dpac/consortium). Funding for the DPAC has been provided by national institutions, in particular the institutions participating in the Gaia Multilateral Agreement. | en_US |
| dc.language.iso | en_US | en_US |
| dc.publisher | Astronomical Journal | en_US |
| dc.rights | Original content from this work may be used under the terms of the Creative Commons Attribution 4.0 licence. Any further distribution of this work must maintain attribution to the author(s) and the title of the work, journal citation and DOI. | |
| dc.source.uri | https://iopscience.iop.org/article/10.3847/1538-3881/ac9ccd | |
| dc.title | Independent Validation of the Temperate Super-Earth HD 79211 b using HARPS-N | en_US |
| dc.type | Article | en_US |
| dc.identifier.doi | 10.3847/1538-3881/ac9ccd | |
