有哪些信誉好的足球投注网站The Virgo stellar over-density Mapping the infall of the Sagittarius tidal stream onto the.pdf
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The Virgo stellar over-density Mapping the infall of the Sagittarius tidal stream onto the
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Draft version February 5, 2008
Preprint typeset using LATEX style emulateapj v. 10/09/06
THE VIRGO STELLAR OVER-DENSITY: MAPPING THE INFALL OF THE SAGITTARIUS TIDAL STREAM
ONTO THE MILKY WAY DISK
David Mart??nez-Delgado1,2, Jorge Pen?arrubia3,4, Mario Juric?5,6, Emilio J. Alfaro2, Zeljko Ivezic?5
Draft version February 5, 2008
ABSTRACT
The recently discovered Virgo stellar over-density, which expands over ～1000deg2 perpendicularly
to the Galactic disk plane (7 Z 15 kpc, R～ 7 kpc), is the largest clump of tidal debris ever
detected in the outer halo and is likely related with the accretion of a nearby dwarf galaxy by the
Milky Way. We carry out N-body simulations of the Sagittarius stream to show that this giant stellar
over-density is a confirmation of theoretical model predictions for the leading tail of the Sagittarius
stream to cross the Milky Way plane in the Solar neighborhood. Radial velocity measurements are
needed to confirm this association and to further constrain the shape of the Milky Way dark matter
halo through a new generation of theoretical models. If the identification of Virgo over-density and
the Sagittarius leading arm is correct, we predict highly negative radial velocities for the stars of Virgo
over-density. The detection of this new portion of the Sagittarius tidal stream would represent an
excellent target for the on-going and future kinematic surveys and for dark matter direct detection
experiments in the proximity of the Sun.
Subject headings: galaxies: individual (Sagittarius) — galaxies:interactions—Galaxy: structure —
Galaxy: halo
1. INTRODUCTION
In the last decade, various large scale CCD surveys
(Sloan Digital Sky Survey, 2MASS7, QUEST) have for
the first time found strong evidence for the presence of
a significant amount of substructure in the halo of the
Milky Way in form of long tidal streams or stellar clumps
(Newberg et al. 2002; Majewski et al. 2003). These
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