AustralieFrV1, Main, Exploration, bibRecord, 00A873

Taking measure of the Andromeda halo: a kinematic analysis of the giant stream surrounding M31

Identifieur interne : 00A873 ( Main/Exploration ); précédent : 00A872; suivant : 00A874

Taking measure of the Andromeda halo: a kinematic analysis of the giant stream surrounding M31

Auteurs : R. Ibata [France] ; S. Chapman [États-Unis] ; A. M. N. Ferguson [Allemagne] ; M. Irwin ; G. Lewis [Australie] ; A. Mcconnachie

Source :

Monthly Notices of the Royal Astronomical Society [ 0035-8711 ] ; 2004-06.

RBID : ISTEX:95A23ED686C71EBA4A97D412C1D07B5F7A4C33AE

Descripteurs français

Pascal (Inist)
- Cinématique, Dispersion vitesse, Distribution masse, Dynamique, Galaxies spirales, Gradient radial, Matière sombre, Modèle, Nébuleuse planétaire, Orbite, Spectrométrie, Vitesse radiale.
Wicri :
- topic : Spectrométrie.

English descriptors

Abstract

We present a spectroscopic survey of the giant stellar stream found in the halo of the Andromeda galaxy. Taken with the DEIMOS multi‐object spectrograph on the Keck2 telescope, these data display a narrow velocity dispersion of 11 ± 3 km s−1, with a steady radial velocity gradient of 245 km s−1 over the 125‐kpc radial extent of the stream studied so far. This implies that the Andromeda galaxy possesses a substantial dark matter halo. We fit the orbit of the stream in different galaxy potential models. In a simple model with a composite bulge, disc and halo, where the halo follows a universal profile that is compressed by the formation of the baryonic components, we find that the kinematics of the stream require a total mass inside 125 kpc of M125= 7.5+2.5−1.3× 1011 M⊙, or M125 > 5.4 × 1011 M⊙ at the 99 per cent confidence level. This is the first galaxy in which it has been possible to measure the halo mass distribution by such direct dynamical means over such a large distance range. The resulting orbit shows that if M32 or NGC 205 is connected with the stream, they must either trail or lag the densest region of the stream by more than 100 kpc. Furthermore, according to the best‐fitting orbit, the stream passes very close to M31, causing its demise as a coherent structure and producing a fan of stars that will pollute the inner halo, thereby confusing efforts to measure the properties of genuine halo populations. Our data show that several recently identified planetary nebulae, which have been proposed as evidence for the existence of a new companion of M31, are likely members of the Andromeda stream.

Url:

https://api.istex.fr/document/95A23ED686C71EBA4A97D412C1D07B5F7A4C33AE/fulltext/pdf

DOI: 10.1111/j.1365-2966.2004.07759.x

Affiliations:

Le document en format XML

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<term>Andromeda satellites</term>
<term>Andromeda stream</term>
<term>Approximate limit</term>
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<term>Declination direction</term>
<term>Deimos spectrograph</term>
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<term>Distance data</term>
<term>Distance information</term>
<term>Distance uncertainties</term>
<term>Dwarf galaxies</term>
<term>Dwarf galaxy</term>
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<term>Eld</term>
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<term>Gaussian distribution</term>
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<term>Halo</term>
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<term>Klypin</term>
<term>Large distances</term>
<term>Likely model</term>
<term>Likely orbit</term>
<term>Mass distribution</term>
<term>Mass estimate</term>
<term>Mass model</term>
<term>Mcconnachie</term>
<term>Milky</term>
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<term>Orbit</term>
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<term>Planetary nebulae</term>
<term>Positive velocities</term>
<term>Present analysis</term>
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<term>Projection angle</term>
<term>Radial</term>
<term>Radial gradient</term>
<term>Radial velocities</term>
<term>Radial velocity</term>
<term>Realistic galaxy</term>
<term>Rotation curve</term>
<term>Sagittarius</term>
<term>Sagittarius stream</term>
<term>Simple model</term>
<term>Spectroscopic survey</term>
<term>Spectroscopy</term>
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<term>Tangential velocity</term>
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<term>Total mass</term>
<term>Transverse motion</term>
<term>Velocity dispersion</term>
<term>Velocity distribution</term>
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<term>Distribution masse</term>
<term>Dynamique</term>
<term>Galaxies spirales</term>
<term>Gradient radial</term>
<term>Matière sombre</term>
<term>Modèle</term>
<term>Nébuleuse planétaire</term>
<term>Orbite</term>
<term>Spectrométrie</term>
<term>Vitesse radiale</term>
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<term>Andromeda galaxy</term>
<term>Andromeda satellites</term>
<term>Andromeda stream</term>
<term>Approximate limit</term>
<term>Cent level</term>
<term>Centre</term>
<term>Circular velocity</term>
<term>Circular velocity curve</term>
<term>Coherent structure</term>
<term>Current orbit</term>
<term>Dark halo</term>
<term>Declination direction</term>
<term>Deimos spectrograph</term>
<term>Disc</term>
<term>Dispersion</term>
<term>Distance data</term>
<term>Distance information</term>
<term>Distance uncertainties</term>
<term>Dwarf galaxies</term>
<term>Dwarf galaxy</term>
<term>Eld</term>
<term>Full line</term>
<term>Future studies</term>
<term>Galaxy</term>
<term>Galaxy model</term>
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<term>Halo mass</term>
<term>Ibata</term>
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<term>Likely model</term>
<term>Likely orbit</term>
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<term>Mass model</term>
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<term>Milky</term>
<term>Minor axis</term>
<term>Mnras</term>
<term>Narrow velocity dispersion</term>
<term>Nebula</term>
<term>Orbit</term>
<term>Planetary nebulae</term>
<term>Positive velocities</term>
<term>Present analysis</term>
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<term>Radial velocities</term>
<term>Radial velocity</term>
<term>Realistic galaxy</term>
<term>Rotation curve</term>
<term>Sagittarius</term>
<term>Sagittarius stream</term>
<term>Simple model</term>
<term>Spectroscopic survey</term>
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<term>Stream stars</term>
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<front><div type="abstract" xml:lang="en">We present a spectroscopic survey of the giant stellar stream found in the halo of the Andromeda galaxy. Taken with the DEIMOS multi‐object spectrograph on the Keck2 telescope, these data display a narrow velocity dispersion of 11 ± 3 km s−1, with a steady radial velocity gradient of 245 km s−1 over the 125‐kpc radial extent of the stream studied so far. This implies that the Andromeda galaxy possesses a substantial dark matter halo. We fit the orbit of the stream in different galaxy potential models. In a simple model with a composite bulge, disc and halo, where the halo follows a universal profile that is compressed by the formation of the baryonic components, we find that the kinematics of the stream require a total mass inside 125 kpc of M125= 7.5+2.5−1.3× 1011 M⊙, or M125 > 5.4 × 1011 M⊙ at the 99 per cent confidence level. This is the first galaxy in which it has been possible to measure the halo mass distribution by such direct dynamical means over such a large distance range. The resulting orbit shows that if M32 or NGC 205 is connected with the stream, they must either trail or lag the densest region of the stream by more than 100 kpc. Furthermore, according to the best‐fitting orbit, the stream passes very close to M31, causing its demise as a coherent structure and producing a fan of stars that will pollute the inner halo, thereby confusing efforts to measure the properties of genuine halo populations. Our data show that several recently identified planetary nebulae, which have been proposed as evidence for the existence of a new companion of M31, are likely members of the Andromeda stream.</div>
</front>
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Serveur d'exploration sur les relations entre la France et l'Australie

Taking measure of the Andromeda halo: a kinematic analysis of the giant stream surrounding M31

Taking measure of the Andromeda halo: a kinematic analysis of the giant stream surrounding M31

Source :

Descripteurs français

English descriptors

Abstract

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