The Origin of the Bifurcation in the Sagittarius Stream | Zendy

M. Fellhauer | Zendy; Vasily Belokurov | Zendy; N. W. Evans | Zendy; M. I. Wilkinson | Zendy; D. B. Zucker | Zendy; G. Gilmore | Zendy; M. J. Irwin | Zendy; D. M. Bramich | Zendy; S. Vidrih | Zendy; Rosemary F. Ġ. Wyse | Zendy; Timothy C. Beers | Zendy; J. Brinkmann | Zendy

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The Origin of the Bifurcation in the Sagittarius Stream

Author(s) -

M. Fellhauer,

Vasily Belokurov,

N. W. Evans,

M. I. Wilkinson,

D. B. Zucker,

G. Gilmore,

M. J. Irwin,

D. M. Bramich,

S. Vidrih,

Rosemary F. Ġ. Wyse,

Timothy C. Beers,

J. Brinkmann

Publication year - 2006

Publication title -

the astrophysical journal

Language(s) - English

Resource type - Journals

SCImago Journal Rank - 2.376

H-Index - 489

eISSN - 1538-4357

pISSN - 0004-637X

DOI - 10.1086/507128

Subject(s) - sagittarius , physics , halo , astrophysics , sky , precession , bifurcation , declination , stars , astronomy , milky way , galaxy , nonlinear system , quantum mechanics

The latest Sloan Digital Sky Survey data reveal a prominent bifurcation inthe distribution of debris of the Sagittarius dwarf spheroidal (Sgr) beginningat a right ascension of roughly 190 degrees. Two branches of the stream (A andB) persist at roughly the same heliocentric distance over at least 50 degreesof arc. There is also evidence for a more distant structure (C) well behind theA branch. This paper provides the first explanation for the bifurcation. It iscaused by the projection of the young leading (A) and old trailing (B) tidalarms of the Sgr, whilst the old leading arm (C) lies well behind A. Thisexplanation is only possible if the halo is close to spherical, as the angulardifference between the branches is a measure of the precession of the orbitalplane.Comment: ApJ, in pres

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