The origin of the bifurcation in the Sagittarius stream

M. Fellhauer, V. Belokurov, N. W. Evans, M. I. Wilkinson, D. B. Zucker, G. Gilmore, M. J. Irwin, D. M. Bramich, S. Vidrih, R. F G Wyse, T. C. Beers, J. Brinkmann

Research output: Contribution to journalArticle

178 Citations (Scopus)

Abstract

The latest Sloan Digital Sky Survey data reveal a prominent bifurcation in the distribution of debris of the Sagittarius dwarf spheroidal (Sgr) beginning at a right ascension of α ≈ 190°. Two branches of the stream (A and B) persist at roughly the same heliocentric distance over at least 50° of arc. There is also evidence for a more distant structure (C) well behind the A branch. This paper provides the first explanation for the bifurcation. It is caused by the projection of the young leading (A) and old trailing (B) tidal arms of the Sgr, while the old leading arm (C) lies well behind A. This explanation is only possible if the halo is close to spherical, as the angular difference between the branches is a measure of the precession of the orbital plane.

Original languageEnglish
Pages (from-to)167-173
Number of pages7
JournalAstrophysical Journal
Volume651
Issue number1 I
DOIs
Publication statusPublished - 1 Nov 2006
Externally publishedYes

Fingerprint

bifurcation
precession
debris
halos
arcs
projection
orbitals
distribution
young

Keywords

  • Galaxies: dwarf
  • Galaxies: individual (Sgr dSph)
  • Galaxy: halo
  • Galaxy: structure

ASJC Scopus subject areas

  • Space and Planetary Science

Cite this

Fellhauer, M., Belokurov, V., Evans, N. W., Wilkinson, M. I., Zucker, D. B., Gilmore, G., ... Brinkmann, J. (2006). The origin of the bifurcation in the Sagittarius stream. Astrophysical Journal, 651(1 I), 167-173. https://doi.org/10.1086/507128

The origin of the bifurcation in the Sagittarius stream. / Fellhauer, M.; Belokurov, V.; Evans, N. W.; Wilkinson, M. I.; Zucker, D. B.; Gilmore, G.; Irwin, M. J.; Bramich, D. M.; Vidrih, S.; Wyse, R. F G; Beers, T. C.; Brinkmann, J.

In: Astrophysical Journal, Vol. 651, No. 1 I, 01.11.2006, p. 167-173.

Research output: Contribution to journalArticle

Fellhauer, M, Belokurov, V, Evans, NW, Wilkinson, MI, Zucker, DB, Gilmore, G, Irwin, MJ, Bramich, DM, Vidrih, S, Wyse, RFG, Beers, TC & Brinkmann, J 2006, 'The origin of the bifurcation in the Sagittarius stream', Astrophysical Journal, vol. 651, no. 1 I, pp. 167-173. https://doi.org/10.1086/507128
Fellhauer M, Belokurov V, Evans NW, Wilkinson MI, Zucker DB, Gilmore G et al. The origin of the bifurcation in the Sagittarius stream. Astrophysical Journal. 2006 Nov 1;651(1 I):167-173. https://doi.org/10.1086/507128
Fellhauer, M. ; Belokurov, V. ; Evans, N. W. ; Wilkinson, M. I. ; Zucker, D. B. ; Gilmore, G. ; Irwin, M. J. ; Bramich, D. M. ; Vidrih, S. ; Wyse, R. F G ; Beers, T. C. ; Brinkmann, J. / The origin of the bifurcation in the Sagittarius stream. In: Astrophysical Journal. 2006 ; Vol. 651, No. 1 I. pp. 167-173.
@article{5ebb4fca113d4c699bc5bd69ec9d4f27,
title = "The origin of the bifurcation in the Sagittarius stream",
abstract = "The latest Sloan Digital Sky Survey data reveal a prominent bifurcation in the distribution of debris of the Sagittarius dwarf spheroidal (Sgr) beginning at a right ascension of α ≈ 190°. Two branches of the stream (A and B) persist at roughly the same heliocentric distance over at least 50° of arc. There is also evidence for a more distant structure (C) well behind the A branch. This paper provides the first explanation for the bifurcation. It is caused by the projection of the young leading (A) and old trailing (B) tidal arms of the Sgr, while the old leading arm (C) lies well behind A. This explanation is only possible if the halo is close to spherical, as the angular difference between the branches is a measure of the precession of the orbital plane.",
keywords = "Galaxies: dwarf, Galaxies: individual (Sgr dSph), Galaxy: halo, Galaxy: structure",
author = "M. Fellhauer and V. Belokurov and Evans, {N. W.} and Wilkinson, {M. I.} and Zucker, {D. B.} and G. Gilmore and Irwin, {M. J.} and Bramich, {D. M.} and S. Vidrih and Wyse, {R. F G} and Beers, {T. C.} and J. Brinkmann",
year = "2006",
month = "11",
day = "1",
doi = "10.1086/507128",
language = "English",
volume = "651",
pages = "167--173",
journal = "Astrophysical Journal",
issn = "0004-637X",
publisher = "IOP Publishing Ltd.",
number = "1 I",

}

TY - JOUR

T1 - The origin of the bifurcation in the Sagittarius stream

AU - Fellhauer, M.

AU - Belokurov, V.

AU - Evans, N. W.

AU - Wilkinson, M. I.

AU - Zucker, D. B.

AU - Gilmore, G.

AU - Irwin, M. J.

AU - Bramich, D. M.

AU - Vidrih, S.

AU - Wyse, R. F G

AU - Beers, T. C.

AU - Brinkmann, J.

PY - 2006/11/1

Y1 - 2006/11/1

N2 - The latest Sloan Digital Sky Survey data reveal a prominent bifurcation in the distribution of debris of the Sagittarius dwarf spheroidal (Sgr) beginning at a right ascension of α ≈ 190°. Two branches of the stream (A and B) persist at roughly the same heliocentric distance over at least 50° of arc. There is also evidence for a more distant structure (C) well behind the A branch. This paper provides the first explanation for the bifurcation. It is caused by the projection of the young leading (A) and old trailing (B) tidal arms of the Sgr, while the old leading arm (C) lies well behind A. This explanation is only possible if the halo is close to spherical, as the angular difference between the branches is a measure of the precession of the orbital plane.

AB - The latest Sloan Digital Sky Survey data reveal a prominent bifurcation in the distribution of debris of the Sagittarius dwarf spheroidal (Sgr) beginning at a right ascension of α ≈ 190°. Two branches of the stream (A and B) persist at roughly the same heliocentric distance over at least 50° of arc. There is also evidence for a more distant structure (C) well behind the A branch. This paper provides the first explanation for the bifurcation. It is caused by the projection of the young leading (A) and old trailing (B) tidal arms of the Sgr, while the old leading arm (C) lies well behind A. This explanation is only possible if the halo is close to spherical, as the angular difference between the branches is a measure of the precession of the orbital plane.

KW - Galaxies: dwarf

KW - Galaxies: individual (Sgr dSph)

KW - Galaxy: halo

KW - Galaxy: structure

UR - http://www.scopus.com/inward/record.url?scp=33845700763&partnerID=8YFLogxK

UR - http://www.scopus.com/inward/citedby.url?scp=33845700763&partnerID=8YFLogxK

U2 - 10.1086/507128

DO - 10.1086/507128

M3 - Article

VL - 651

SP - 167

EP - 173

JO - Astrophysical Journal

JF - Astrophysical Journal

SN - 0004-637X

IS - 1 I

ER -