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An Updated 2017 Astrometric Solution for Betelgeuse

Authors :
Alexander Brown
E. O'Gorman
Pierre Kervella
Leen Decin
Graham M. Harper
A. M. S. Richards
Edward F. Guinan
Institut für Astrophysik [Göttingen]
Georg-August-University = Georg-August-Universität Göttingen
Laboratoire d'études spatiales et d'instrumentation en astrophysique (LESIA)
Université Pierre et Marie Curie - Paris 6 (UPMC)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de Paris
Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS)
Instituut voor Sterrenkunde [Leuven]
Catholic University of Leuven - Katholieke Universiteit Leuven (KU Leuven)
Georg-August-University [Göttingen]
Source :
The Astronomical Journal, The Astronomical Journal, 2017, 154 (1), pp.11. ⟨10.3847/1538-3881/aa6ff9⟩, Harper, G M, Brown, A, Guinan, E F, O'Gorman, E, Richards, A M S, Kervella, P & Decin, L 2017, ' An Updated 2017 Astrometric Solution for Betelgeuse ', The Astronomical Journal . https://doi.org/10.3847/1538-3881/aa6ff9, The Astronomical Journal, American Astronomical Society, 2017, 154 (1), pp.11. ⟨10.3847/1538-3881/aa6ff9⟩
Publication Year :
2017
Publisher :
HAL CCSD, 2017.

Abstract

We provide an update for the astrometric solution for the Type II supernova progenitor Betelgeuse using the revised Hipparcos Intermediate Astrometric Data (HIAD) of van Leeuwen, combined with existing VLA and new e-MERLIN and ALMA positions. The 2007 Hipparcos refined abscissa measurements required the addition of so-called Cosmic Noise of 2.4 mas to find an acceptable 5-parameter stochastic solution. We find that a measure of radio Cosmic Noise should also be included for the radio positions because surface inhomogeneities exist at a level significant enough to introduce additional intensity centroid uncertainty. Combining the 2007 HIAD with the proper motions based solely on the radio positions leads to a parallax of π =5.27+/- 0.78 mas ({190}-25+33 pc), smaller than the Hipparcos 2007 value of 6.56 ± 0.83 mas ({152}-17+22 pc). Furthermore, combining the VLA and new e-MERLIN and ALMA radio positions with the 2007 HIAD, and including radio Cosmic Noise of 2.4 mas, leads to a nominal parallax solution of 4.51 ± 0.80 mas ({222}-34+48 pc), which, while only 0.7σ different from the 2008 solution of Harper et al., is 2.6σ different from the solution of van Leeuwen. An accurate and precise parallax for Betelgeuse is always going to be difficult to obtain because it is small compared to the stellar angular diameter (θ =44 mas). We outline an observing strategy utilizing future mm and sub-mm high-spatial resolution interferometry that must be used if substantial improvements in the precision and accuracy of the parallax and distance are to be achieved. ispartof: Astrophysical Journal vol:154 issue:1 pages:6- status: published

Details

Language :
English
ISSN :
00046256, 15383881, 0004637X, and 00046361
Database :
OpenAIRE
Journal :
The Astronomical Journal, The Astronomical Journal, 2017, 154 (1), pp.11. ⟨10.3847/1538-3881/aa6ff9⟩, Harper, G M, Brown, A, Guinan, E F, O'Gorman, E, Richards, A M S, Kervella, P & Decin, L 2017, ' An Updated 2017 Astrometric Solution for Betelgeuse ', The Astronomical Journal . https://doi.org/10.3847/1538-3881/aa6ff9, The Astronomical Journal, American Astronomical Society, 2017, 154 (1), pp.11. ⟨10.3847/1538-3881/aa6ff9⟩
Accession number :
edsair.doi.dedup.....6ac53df97d78bb05f7fa3ac96bab126c
Full Text :
https://doi.org/10.3847/1538-3881/aa6ff9⟩