Hostname: page-component-cd9895bd7-dk4vv Total loading time: 0 Render date: 2024-12-24T19:43:37.215Z Has data issue: false hasContentIssue false
  • English
  • Français

The Differential Astrometric Reference Frame on short timescales in the Gaia Era

Published online by Cambridge University Press:  07 March 2018

Ummi Abbas ,
Beatrice Bucciarelli ,
Mario G. Lattanzi ,
Mariateresa Crosta ,
Mario Gai ,
Richard Smart ,
Alessandro Sozzetti  and
Alberto Vecchiato
Ummi Abbas
Affiliation:
INAF - Osservatorio Astrofisico di Torino, Via Osservatorio 20, Pino Torinese I-10025, Italy email: [email protected]
Beatrice Bucciarelli
Affiliation:
INAF - Osservatorio Astrofisico di Torino, Via Osservatorio 20, Pino Torinese I-10025, Italy email: [email protected]
Mario G. Lattanzi
Affiliation:
INAF - Osservatorio Astrofisico di Torino, Via Osservatorio 20, Pino Torinese I-10025, Italy email: [email protected]
Mariateresa Crosta
Affiliation:
INAF - Osservatorio Astrofisico di Torino, Via Osservatorio 20, Pino Torinese I-10025, Italy email: [email protected]
Mario Gai
Affiliation:
INAF - Osservatorio Astrofisico di Torino, Via Osservatorio 20, Pino Torinese I-10025, Italy email: [email protected]
Richard Smart
Affiliation:
INAF - Osservatorio Astrofisico di Torino, Via Osservatorio 20, Pino Torinese I-10025, Italy email: [email protected]
Alessandro Sozzetti
Affiliation:
INAF - Osservatorio Astrofisico di Torino, Via Osservatorio 20, Pino Torinese I-10025, Italy email: [email protected]
Alberto Vecchiato
Affiliation:
INAF - Osservatorio Astrofisico di Torino, Via Osservatorio 20, Pino Torinese I-10025, Italy email: [email protected]
Rights & Permissions [Opens in a new window]

Abstract

Core share and HTML view are not available for this content. However, as you have access to this content, a full PDF is available via the ‘Save PDF’ action button.

We use methods of differential astrometry to construct a small field inertial reference frame stable at the micro-arcsecond level. Using Gaia measurements of field angles we look at the influence of the number of reference stars and the stars magnitude as well as astrometric systematics on the total error budget with the help of Gaia-like simulations around the Ecliptic Pole in a differential astrometric scenario. We find that the systematic errors are modeled and reliably estimated to the μas level even in fields with a modest number of 37 stars with G <13 mag over a 0.24 sq. degrees field of view for short timescales of the order of a day for a perfect instrument and with high-cadence observations. Accounting for large-scale calibrations by including the geometric instrument model over such short timescales requires fainter stars down to G=14 mag without diminishing the accuracy of the reference frame.

Keywords

astrometryreference systemsmethods: statistical
Type
Contributed Papers
Information
Proceedings of the International Astronomical Union , Volume 12 , Symposium S330: Astrometry and Astrophysics in the Gaia sky , April 2017 , pp. 79 - 80
Copyright
Copyright © International Astronomical Union 2018 

References

Abbas, U., et al., 2017, PASP, 129, 4503 CrossRefGoogle Scholar
Crosta, M. & Mignard, , 2006, Classical and Quantum Gravity, 23, 4853 Google Scholar
Holl, B., et al., 2012, A&A, 543, A15 Google Scholar
Jefferys, W. H., Fitzpatrick, M. J., & McArthur, B. E., 1988, Celestial Mechanics, 41, 39 Google Scholar
Klioner, S. A., 2003, AJ, 125, 1580 CrossRefGoogle Scholar
Lindegren, L., Lammers, U., Hobbs, D., et al., 2012, A&A, 538, A78 Google Scholar
Smart, R. L. & Nicastro, L., 2014, A&A, 570, A87 Google Scholar
Sozzetti, A., 2005, PASP, 117, 1021 Google Scholar