Hostname: page-component-cd9895bd7-fscjk Total loading time: 0 Render date: 2024-12-28T02:56:40.246Z Has data issue: false hasContentIssue false
  • English
  • Français

On the characterization of the Galactic warp in the Gaia era

Published online by Cambridge University Press:  17 July 2015

H. Abedi ,
F. Figueras ,
L. Aguilar ,
C. Mateu ,
M. Romero-Gomez ,
M. Lopez-Corredoira  and
F. Garzon Lopez
H. Abedi
Affiliation:
Dept. d'Astronomia i Meteorologia, Institut de Ciències del Cosmos, Universitat de Barcelona, IEEC, Martí i Franquès 1, 08028 Barcelona, Spain
F. Figueras
Affiliation:
Dept. d'Astronomia i Meteorologia, Institut de Ciències del Cosmos, Universitat de Barcelona, IEEC, Martí i Franquès 1, 08028 Barcelona, Spain
L. Aguilar
Affiliation:
Instituto de Astronomia, UNAM, Apartado Postal 877, 22860 Ensenada, B.C., Mexico
C. Mateu
Affiliation:
Dept. d'Astronomia i Meteorologia, Institut de Ciències del Cosmos, Universitat de Barcelona, IEEC, Martí i Franquès 1, 08028 Barcelona, Spain
M. Romero-Gomez
Affiliation:
Dept. d'Astronomia i Meteorologia, Institut de Ciències del Cosmos, Universitat de Barcelona, IEEC, Martí i Franquès 1, 08028 Barcelona, Spain
M. Lopez-Corredoira
Affiliation:
Instituto de Astrofśica de Canarias, 38205 La Laguna, Tenerife, Spain
F. Garzon Lopez
Affiliation:
Dept. d'Astronomia i Meteorologia, Institut de Ciències del Cosmos, Universitat de Barcelona, IEEC, Martí i Franquès 1, 08028 Barcelona, Spain
Get access

Abstract

We explore the possibility of detecting and characterising the warp of the stellar disc of our Galaxy using the synthetic Gaia data and the UCAC4 proper motion catalogue. We develop a new kinematic model for the galactic warp. We generate random realisations of test particles which evolve in a realistic Galactic potential warped adiabatically to various final configurations. The Gaia selection function, its errors model and a realistic 3D extinction map are applied to mimic three tracer populations: OB, A and Red Clump stars. A family of Great Circle Cell Counts (GC3) methods is used. They are ideally suited to find the tilt and twist of a collection of rings, which allow us to detect and measure the warp parameters. Moreover, We look for the kinematic signature of the warp in the μb proper motions of stars as a function of galactic longitude. Using the UCAC4 proper motions, we do not obtain a similar trend as the one we expect from our warp model. We explore a possible source of this discrepancy in terms of systematics caused by a residual spin of the Hipparcos celestial reference frame (HCRF) with respect to the extra-galactic inertial one.

Type
Research Article
Information
European Astronomical Society Publications Series , Volume 68: The Milky Way Unravelled by Gaia: GREAT Science from the Gaia Data Releases , 2014 , pp. 237 - 240
Copyright
© EAS, EDP Sciences, 2015

Access options

Get access to the full version of this content by using one of the access options below. (Log in options will check for institutional or personal access. Content may require purchase if you do not have access.)

References

Bobylev, V.V., 2010, Astron. Lett., 36, 634CrossRef
Burke, B.F., 1957, AJ, 62, 90CrossRef
Drimmel, R., Cabrera-Lavers, A., & Lopez-Corredoira, M., 2003, A&A, 409, 205
Drimmel, R., Smart, R.L., & Lattanzi, M.G., 2000, A&A, 354, 67
Drimmel, R., & Spergel, D.N., 2001 ApJ, 556181
Fedorov, P.N., Myznikov, A.A., & Akhmetov, V.S., 2009, MNRAS, 393, 133CrossRef
Freudenreich, H., et al., 1994, AJ, 429, L69CrossRef
Mateu, C., Bruzual, G., Aguilar, L., Brown, A.G.A., et al., 2011, MNRAS, 415, 214CrossRef
Miyamoto, M., & Zhu, Z., 1998, AJ, 115, 1483CrossRef
Oort, J.H., Kerr, F.J., & Westerhout, G., 1958, MNRAS, 118, 379
Reyle, C., Marshall, D.J., Robin, A.C., & Schultheis, M., 2009, A&A, 495, 819
Zacharias, N., Finch, C.T., Girard, T.M., et al., 2013, AJ, 145, 44CrossRef