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Improving distance estimates to nearby bright stars: Combining astrometric data from Hipparcos, Nano-JASMINE and Gaia

Published online by Cambridge University Press:  26 February 2013

Daniel Michalik ,
Lennart Lindegren ,
David Hobbs ,
Uwe Lammers  and
Yoshiyuki Yamada
Daniel Michalik
Affiliation:
Lund Observatory, Lund University, Box 43, SE-22100 Lund, Sweden e-mail: daniel.michalik@astro.lu.se, lennart@astro.lu.se, david@astro.lu.se
Lennart Lindegren
Affiliation:
Lund Observatory, Lund University, Box 43, SE-22100 Lund, Sweden e-mail: daniel.michalik@astro.lu.se, lennart@astro.lu.se, david@astro.lu.se
David Hobbs
Affiliation:
Lund Observatory, Lund University, Box 43, SE-22100 Lund, Sweden e-mail: daniel.michalik@astro.lu.se, lennart@astro.lu.se, david@astro.lu.se
Uwe Lammers
Affiliation:
European Space Agency (ESA/ESAC), P. O. Box 78, ES-28691 Villanueva de la Cañada, Madrid, Spain e-mail: uwe.lammers@sciops.esa.int
Yoshiyuki Yamada
Affiliation:
Department of Physics, Kyoto University, Oiwake-cho Kita-Shirakaw Sakyo-ku, Kyoto, 606-8502Japan e-mail: yamada@amesh.org
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Abstract

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Starting in 2013, Gaia will deliver highly accurate astrometric data, which eventually will supersede most other stellar catalogues in accuracy and completeness. It is, however, limited to observations from magnitude 6 to 20 and will therefore not include the brightest stars. Nano-JASMINE, an ultrasmall Japanese astrometry satellite, will observe these bright stars, but with much lower accuracy. Hence, the Hipparcos catalogue from 1997 will likely remain the main source of accurate distances to bright nearby stars. We are investigating how this might be improved by optimally combining data from all three missions through a joint astrometric solution. This would take advantage of the unique features of each mission: the historic bright-star measurements of Hipparcos, the updated bright-star observations of Nano-JASMINE, and the very accurate reference frame of Gaia. The long temporal baseline between the missions provides additional benefits for the determination of proper motions and binary detection, which indirectly improve the parallax determination further. We present a quantitative analysis of the expected gains based on simulated data for all three missions.

Keywords

astrometrycatalogsmethods: data analysismethods: statisticalreference systems
Type
Contributed Papers
Information
Proceedings of the International Astronomical Union , Volume 8 , Symposium S289: Advancing the Physics of Cosmic Distances , August 2012 , pp. 414 - 417
Copyright
Copyright © International Astronomical Union 2013

References

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Holl, B., Lindegren, L., & Hobbs, D. 2012, A&A, 543, A15Google Scholar
Lindegren, L., Lammers, U., Hobbs, D., O'Mullane, W., Bastian, U., & Hernández, J. 2012, A&A, 538, A78Google Scholar
Michalik, D., Lindegren, L., Hobbs, D., Lammers, U., & Yamada, Y. 2012, Astron. Soc. Pac. Conf. Ser., 461, 549Google Scholar