On kinematic substructure in the Sextans dwarf spheroidal galaxy

Matthew G. Walker; Mario Mateo; Edward W. Olszewski; Jayanta Kumar Pal; Bodhisattva Sen; Michael Woodroofe

doi:10.1086/504522

On kinematic substructure in the Sextans dwarf spheroidal galaxy

Matthew G. Walker, Mario Mateo, Edward W. Olszewski, Jayanta Kumar Pal, Bodhisattva Sen, Michael Woodroofe

Astronomy

Research output: Contribution to journal › Article › peer-review

64 Scopus citations

Abstract

We present multifiber echelle radial velocity results for 551 stars in the Sextans dwarf spheroidal galaxy and identify 294 stars as probable Sextans members. The projected velocity dispersion profile of the binned data remains flat to a maximum angular radius of 30′. We introduce a nonparametric technique for estimating the projected velocity dispersion surface and use this to search for kinematic substructure. Our data do not confirm previous reports of a kinematically distinct stellar population at the Sextans center. Instead we detect a region near the Sextans core radius that is kinematically colder than the overall Sextans sample with 95% confidence.

Original language	English (US)
Pages (from-to)	L41-L44
Journal	Astrophysical Journal
Volume	642
Issue number	1 II
DOIs	https://doi.org/10.1086/504522
State	Published - May 1 2006

Keywords

Galaxies: dwarf
Galaxies: individual (Sextans)
Galaxies: kinematics and dynamics
Local Group

ASJC Scopus subject areas

Astronomy and Astrophysics
Space and Planetary Science

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10.1086/504522

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title = "On kinematic substructure in the Sextans dwarf spheroidal galaxy",

abstract = "We present multifiber echelle radial velocity results for 551 stars in the Sextans dwarf spheroidal galaxy and identify 294 stars as probable Sextans members. The projected velocity dispersion profile of the binned data remains flat to a maximum angular radius of 30′. We introduce a nonparametric technique for estimating the projected velocity dispersion surface and use this to search for kinematic substructure. Our data do not confirm previous reports of a kinematically distinct stellar population at the Sextans center. Instead we detect a region near the Sextans core radius that is kinematically colder than the overall Sextans sample with 95% confidence.",

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T1 - On kinematic substructure in the Sextans dwarf spheroidal galaxy

AU - Walker, Matthew G.

AU - Mateo, Mario

AU - Olszewski, Edward W.

AU - Pal, Jayanta Kumar

AU - Sen, Bodhisattva

AU - Woodroofe, Michael

PY - 2006/5/1

Y1 - 2006/5/1

N2 - We present multifiber echelle radial velocity results for 551 stars in the Sextans dwarf spheroidal galaxy and identify 294 stars as probable Sextans members. The projected velocity dispersion profile of the binned data remains flat to a maximum angular radius of 30′. We introduce a nonparametric technique for estimating the projected velocity dispersion surface and use this to search for kinematic substructure. Our data do not confirm previous reports of a kinematically distinct stellar population at the Sextans center. Instead we detect a region near the Sextans core radius that is kinematically colder than the overall Sextans sample with 95% confidence.

AB - We present multifiber echelle radial velocity results for 551 stars in the Sextans dwarf spheroidal galaxy and identify 294 stars as probable Sextans members. The projected velocity dispersion profile of the binned data remains flat to a maximum angular radius of 30′. We introduce a nonparametric technique for estimating the projected velocity dispersion surface and use this to search for kinematic substructure. Our data do not confirm previous reports of a kinematically distinct stellar population at the Sextans center. Instead we detect a region near the Sextans core radius that is kinematically colder than the overall Sextans sample with 95% confidence.

KW - Galaxies: dwarf

KW - Galaxies: individual (Sextans)

KW - Galaxies: kinematics and dynamics

KW - Local Group

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On kinematic substructure in the Sextans dwarf spheroidal galaxy

Abstract

Keywords

ASJC Scopus subject areas

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