Hostname: page-component-848d4c4894-tn8tq Total loading time: 0 Render date: 2024-07-07T14:04:01.066Z Has data issue: false hasContentIssue false

Is the Vorticity Vector of the Galaxy Perpendicular to the Galactic Plane?

Precessional Correction and Equinoctial Motion Correction to the FK5 System and Kinematics of the Galactic Warp

Published online by Cambridge University Press:  07 August 2017

Masanori Miyamoto*
Affiliation:
National Astronomical Observatory, Mitaka, Tokyo 181, Japan

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.

The modern astrometric catalogue ACRS invites attempts to re-examine the systematic stellar motions, together with the luni-solar precessional correction and the fictitious equinoctial motion correction to the FK5 system, and gives encouraging results.

On the basis of the three-dimensional Ogorodnikov-Milne model for the overall pattern analysis of the proper motions, the systematic stellar velocity field of about 30000 K-M giants chosen from the ACRS is first examined in the heliocentric distance interval 0.5 to 1.0 kpc. We have found in an iterative fashion a solution for the K-M giants that yields neither deformation-nor vorticity-field other than the classical ones (the Oort constants A and B). The important point to note here is that the generally accepted idea such that the K-M giants are a steady-state constituent of the galaxy is compatible with the luni-solar precessional correction proposed by the VLBI and LLR observations. The K-M giants give the rational set of corrections to the FK5 system: the luni-solar precessional correction Δp = −0″.27 ± 0″.03 / cent and the equinoctial motion correction including the planetary precessional correction Δe + Δλ = −0″.12 ± 0″.03 / cent. Thus, the precessional correction previously proposed with the modern techniques has been confirmed by the pattern analysis of the proper motions.

Next, applying the corrections obtained above, we have performed the overall pattern analysis of the proper motions of about 3000 O-B5 stars, supergiants, and bright giants, which are chosen again from the ACRS, and considered as an entity of the galactic warp. It is found that the kinematics of these stars is quite different from that of K-M giants. These stars show additional shears and rotations around two mutually orthogonal axes lying in the galactic plane, besides the classical ones. The present finding implies that the young stars are streaming around the galactic center in a tilted sheet (the warp) with the velocity of 225 km/s, and the sheet itself is simultaneously rotating around the nodal line of the warp (galactic center — sun — anticenter line) with the angular velocity of 4 km/s/kpc in increasing sense of the present inclination of the warp.

Type
Impact on Astrophysics
Copyright
Copyright © Kluwer 

References

Bastian, U., & Röser, S. (1990) PPM-South Preliminary, Astron. Rechen-Inst. Heidelberg.Google Scholar
Burton, W.B., & Deul, E.R. (1987) in Gilmore, G. and Carswell, B. (eds.), The Galaxy, (NATO ASI Series), p. 141.Google Scholar
Corbin, T.E., & Urban, S.E. (1991) Astrographic Catalogue Reference Stars (ACRS), U. S. Naval Observatory.Google Scholar
Fricke, W. (1967a) AJ, 72, 642.CrossRefGoogle Scholar
Fricke, W. (1967b) AJ, 72, 1368.CrossRefGoogle Scholar
Fricke, W. (1977a) Veröff. Astron. Rechen-Institut Heidelberg, No. 28, Verlag G. Braun, Karlsruhe.Google Scholar
Fricke, W. (1977b) A&A, 54, 363.Google Scholar
Fricke, W., Schwan, H., & Lederle, T. (1988) Veröff. Astron. Rechen-Institut Heidelberg, No. 32, Verlag G. Braun, Karlsruhe.Google Scholar
Mermilliod, J.-C. (1987) A&A Suppl., 71, 413.Google Scholar
Miyamoto, M., & Sôma, M. (1993 Feb.) to be published in AJ (Paper I).Google Scholar
Miyamoto, M., Sôma, M., & Yoshizawa, M. (1993) to be submitted to AJ (Paper II).Google Scholar
McCarthy, D.D., & Luzum, B.J. (1991) AJ, 102, 1889.CrossRefGoogle Scholar
Milne, E.A. (1935) MNRAS, 95, 560.CrossRefGoogle Scholar
Morrison, L.V. (1982) MNRAS, 198, 1119.CrossRefGoogle Scholar
Ogorodnikov, K.F. (1932) Z. Astrophys., 4, 190.Google Scholar
Röser, S., & Bastian, U. (1989) PPM-North, Astron. Rechen-Inst. Heidelberg.Google Scholar
Schwan, H. (1988) A&A, 198, 116.Google Scholar
Warren, W.H. Jr., & Kang, Young Woon (1987) SKYMAP Catalog of 248516 Stars, Version 3.3, NSSDC/WDC-A-R&S 87-15.Google Scholar
Williams, J.G., Newhall, XX, & Dickey, J.O. (1991) A&A, 241, L9.Google Scholar