Published 2018-01-01
Abstract
In this paper we attempt to study an ongoing astrometry mission of the European Space Agency (ESA), named Gaia, whose aim is to make the largest and most precise three-dimensional map of our Galaxy. We present the scientific goals of Gaia and give a brief description of the spacecraft. We also present a preliminary analysis of comparing distance estimates of Be stars from the first Gaia data release, Gaia DR1, and Hipparcos mission. From our analysis, we confirm that Gaia stands out as a promising mission in terms of the distance measurements when compared to Hipparcos, particularly for distances greater than 1 kpc.
References
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[26] www.sci.esa.int, “Payload module.” [Online]. Available: http://sci.esa.int/gaia/40129-payload-module/
[2] L. Bass, P. Clements, and R. Kazman, Software Architecture in Practice, 2nd ed. Reading, MA: Addison Wesley, 2003. [E-book] Available: Safari e-book.
[3] K. A. Nelson, R. J. Davis, D. R. Lutz, and W. Smith, “Optical generation of tunable ultrasonic waves,” Journal of Applied Physics, vol. 53, no. 2, Feb., pp. 1144-1149, 2002.
[4] Gaia Collaboration ,Brown, A. G. A. , Vallenari etc. Gaia Data Release 1. Summary of the astrometric, photometric, and survey properties. Astronomy & Astrophysics, 2016.
[5] Lindegren, L. , Lammers, U. , Bastian, U. , Hern´andez, J. etc . Gaia Data Release 1. Astrometry: one billion positions, two million proper motions and parallaxes. Astronomy & Astrophysics, 2016, Gaia DR1.
[6] ESA VizieR Online Data Catalog: The Hipparcos and Tycho Catalogues (ESA 1997). VizieR Online Data Catalog, 1997.
[7] L. Eyer, L. Rimoldini, B. Holl, , P. North, The Gaia Mission, Binary Stars and Exoplanets. Astronomical Society of the Pacific Conference Series, vol. 496, Jul. 2015, p. 121.
[8] Jaschek, M. and Egret, D. A Catalogue of Be-Stars. in Be Stars, ser. IAU Symposium, M. Jaschek and H.-G. Groth, Eds., vol. 98, Apr. 1982, p. 261.
[9] Høg, E, C. Fabricius, V. V. Makarov, S. Urban, et al. The Tycho-2 catalogue of the 2.5 million brightest stars Astronomy & Astrophysics, vol. 355, pp. L27–L30, Mar. 2000.
[10] Mathew, B. , Subramaniam, A. and Bhatt, B. C. Be phenomenon in open clusters: results from a survey of emission-line stars in young open clusters. Monthly Notices of the Royal Astronomical Society, vol. 388, pp. 1879–1888, Aug. 2008.
[11] Martayan, C. Hubert, A.-M. , Floquet, M. , Neiner, C. and Fr´emat, Y. and Zorec, J. Effects of Metallicity, Star Formation Conditions and Evolution of B & Be stars. Astronomical Society of the Pacific Conference Series, vol. 361, Mar. 2007, p. 356.
[12] M. V. McSwain and D. R. Gies, “The Evolutionary Status of Be Stars,” Astronomical Society of the Pacific Conference Series, vol. 361, p. 349, Mar. 2007
[13] Mouret, S. , Tests of fundamental physics with the Gaia mission through the dynamics ofminor planets Physical Review D, vol. 84, no. 12, p. 122001, Dec. 2011.
[14] Okazaki, A. T. Current Status of Our Understanding of Be Disk Physics Invited Review. Astronomical Society of the Pacific Conference Series, vol. 506, Nov. 2016, p. 3.
[15] Perryman, M. and Hartman, J. and Bakos, G. ´A. and Lindegren, L. Astrometric Exoplanet Detection with Gaia. The Astrophysical Journal, 2014.
[16] Perryman, M. A. C. , de Boer, K. S. , Gilmore, G. etc. GAIA: Composition, formation and evolution of the Galaxy. Astronomy & Astrophysics, vol. 369, pp. 339–363, Apr. 2001.
[17] Perryman, M. A. C. , Lindegren, L. and Turon, C. The Scientific Goals of the GAIA Mission. ESA Special Publication, vol. 402, Aug. 1997, pp. 743–748.
[18] Pancino, E. Gaia: unravelling the chemical and dynamical history of our Galaxy. Memorie della Societa Astronomica Italiana Supplementi, vol. 19, p. 354, 2012.
[19] Paul, K. T., A. Subramaniam, B. Mathew, R. E. Mennickent, and B. Sabogal, Study of candidate Be stars in the Magellanic Clouds using near-infrared photometry and optical spectroscopy Monthly Notices of the Royal Astronomical Society, vol. 421, pp. 3622–3640, Apr.2012.
[20] Porter, J. M. and Rivinius, T. Classical Be Stars. Publications of the Astronomical Society of the Pacific, vol. 115, pp. 1153–1170, Oct. 2003.
[21] Rivinius, T. , Carciofi, A. C. and Martayan, C. Classical Be stars. Rapidly rotating B stars with viscous Keplerian decretion disks. Astronomy & Astrophysics Reviews, vol. 21, p. 69, Oct. 2013.
[22] Slettebak, A. and Snow, T. P. Physics of Be stars; Proceedings of the Ninety-second IAU Colloquium, University of Colorado, Boulder, Aug. 18-22, 1986. IAU Colloq. 92: Physics of Be Stars, 1987.
[23] Tanga, P. and Mignard, F. The Solar System as seen by Gaia: The asteroids and their accuracy budget. Planetary and Space Science, vol. 73, pp. 5–9, Dec. 2012.
[24] F. van Leeuwen, “Validation of the new Hipparcos reduction,” Astronomy & Astrophysics, vol. 474, p.653, Nov. 2007.
[25] Wisniewski, J. P., Bjorkman, K. S. A. M. Magalh˜aes, et al. The Role of Evolutionary Age and Metallicity in the Formation of Classical Be Circumstellar Disks. II. Assessing the Evolutionary Nature of Candidate Disk Systems Astrophysical Journal, vol. 671, pp. 2040–2058, Dec. 2007.
[26] www.sci.esa.int, “Payload module.” [Online]. Available: http://sci.esa.int/gaia/40129-payload-module/