AustralieFrV1, PascalFrancis, Corpus, bibRecord, 004D79

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

Identifieur interne : 004D79 ( PascalFrancis/Corpus ); précédent : 004D78; suivant : 004D80

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

Auteurs : R. Ibata ; S. Chapman ; A. M. N. Ferguson ; M. Irwin ; G. Lewis ; A. Mcconnachie

Source :

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

RBID : Pascal:04-0411439

Descripteurs français

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

English descriptors

KwdEn :
- Dark matter, Dynamics, Kinematics, Mass distribution, Models, Orbits, Planetary nebulae, Radial gradient, Radial velocity, Spectroscopy, Spiral galaxies, Velocity dispersion.

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^+2.51.3x 10¹¹M_◦., or M₁₂₅ > 5.4 x 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.

Notice en format standard (ISO 2709)

Pour connaître la documentation sur le format Inist Standard.

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A08	`01`	`1`	`ENG`	`@1 Taking measure of the Andromeda halo: a kinematic analysis of the giant stream surrounding M31`
A11	`01`	`1`		`@1 IBATA (R.)`
A11	`02`	`1`		`@1 CHAPMAN (S.)`
A11	`03`	`1`		`@1 FERGUSON (A. M. N.)`
A11	`04`	`1`		`@1 IRWIN (M.)`
A11	`05`	`1`		`@1 LEWIS (G.)`
A11	`06`	`1`		`@1 MCCONNACHIE (A.)`
A14	`01`			`@1 Observatoire de Strasbourg, 11, rue de l'Université @2 Strasbourg 67000 @3 FRA @Z 1 aut.`
A14	`02`			`@1 California Institute of Technology @2 Pasadena, CA 91125 @3 USA @Z 2 aut.`
A14	`03`			`@1 Max-Plank-Institut für Astrophysik, Karl-Schwarzschild-Str. 1, Postfach 1317 @2 Garching 85741 @3 DEU @Z 3 aut.`
A14	`04`			`@1 Institute of Astronomy, Madingley Road @2 Cambridge CB3 0HA @3 GBR @Z 4 aut. @Z 6 aut.`
A14	`05`			`@1 Institute of Astronomy, School of Physics, A29, University of Sydney @2 NSW 2006 @3 AUS @Z 5 aut.`
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A23	`01`			`@0 ENG`
A43	`01`			`@1 INIST @2 2067 @5 354000110328450160`
A44				`@0 0000 @1 © 2004 INIST-CNRS. All rights reserved.`
A45				`@0 34 ref.`
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A61				`@0 A`
A64	`01`	`1`		`@0 Monthly Notices of the Royal Astronomical Society`
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C01	`01`		`ENG`	@0 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^+2.51.3x 10¹¹M_◦., or M₁₂₅ > 5.4 x 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.
C02	`01`	`3`		`@0 001E03D56N`
C03	`01`	`3`	`FRE`	`@0 Cinématique @5 26`
C03	`01`	`3`	`ENG`	`@0 Kinematics @5 26`
C03	`02`	`X`	`FRE`	`@0 Dispersion vitesse @5 28`
C03	`02`	`X`	`ENG`	`@0 Velocity dispersion @5 28`
C03	`02`	`X`	`SPA`	`@0 Dispersión velocidad @5 28`
C03	`03`	`3`	`FRE`	`@0 Vitesse radiale @5 29`
C03	`03`	`3`	`ENG`	`@0 Radial velocity @5 29`
C03	`04`	`X`	`FRE`	`@0 Gradient radial @5 30`
C03	`04`	`X`	`ENG`	`@0 Radial gradient @5 30`
C03	`04`	`X`	`SPA`	`@0 Gradiente radial @5 30`
C03	`05`	`3`	`FRE`	`@0 Matière sombre @5 31`
C03	`05`	`3`	`ENG`	`@0 Dark matter @5 31`
C03	`06`	`3`	`FRE`	`@0 Orbite @5 32`
C03	`06`	`3`	`ENG`	`@0 Orbits @5 32`
C03	`07`	`X`	`FRE`	`@0 Modèle @5 33`
C03	`07`	`X`	`ENG`	`@0 Models @5 33`
C03	`07`	`X`	`SPA`	`@0 Modelo @5 33`
C03	`08`	`3`	`FRE`	`@0 Distribution masse @5 34`
C03	`08`	`3`	`ENG`	`@0 Mass distribution @5 34`
C03	`09`	`3`	`FRE`	`@0 Nébuleuse planétaire @5 35`
C03	`09`	`3`	`ENG`	`@0 Planetary nebulae @5 35`
C03	`10`	`3`	`FRE`	`@0 Dynamique @5 36`
C03	`10`	`3`	`ENG`	`@0 Dynamics @5 36`
C03	`11`	`3`	`FRE`	`@0 Spectrométrie @5 38`
C03	`11`	`3`	`ENG`	`@0 Spectroscopy @5 38`
C03	`12`	`3`	`FRE`	`@0 Galaxies spirales @5 81`
C03	`12`	`3`	`ENG`	`@0 Spiral galaxies @5 81`
N21				`@1 236`
N44	`01`			`@1 PSI`
N82				`@1 PSI`

Format Inist (serveur)

NO :	PASCAL 04-0411439 INIST
ET :	Taking measure of the Andromeda halo: a kinematic analysis of the giant stream surrounding M31
AU :	IBATA (R.); CHAPMAN (S.); FERGUSON (A. M. N.); IRWIN (M.); LEWIS (G.); MCCONNACHIE (A.)
AF :	Observatoire de Strasbourg, 11, rue de l'Université/Strasbourg 67000/France (1 aut.); California Institute of Technology/Pasadena, CA 91125/Etats-Unis (2 aut.); Max-Plank-Institut für Astrophysik, Karl-Schwarzschild-Str. 1, Postfach 1317/Garching 85741/Allemagne (3 aut.); Institute of Astronomy, Madingley Road/Cambridge CB3 0HA/Royaume-Uni (4 aut., 6 aut.); Institute of Astronomy, School of Physics, A29, University of Sydney/NSW 2006/Australie (5 aut.)
DT :	Publication en série; Niveau analytique
SO :	Monthly Notices of the Royal Astronomical Society; ISSN 0035-8711; Coden MNRAA4; Royaume-Uni; Da. 2004; Vol. 351; No. 1; Pp. 117-124; Bibl. 34 ref.
LA :	Anglais
EA :	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^+2.51.3x 10¹¹M_◦., or M₁₂₅ > 5.4 x 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.
CC :	001E03D56N
FD :	Cinématique; Dispersion vitesse; Vitesse radiale; Gradient radial; Matière sombre; Orbite; Modèle; Distribution masse; Nébuleuse planétaire; Dynamique; Spectrométrie; Galaxies spirales
ED :	Kinematics; Velocity dispersion; Radial velocity; Radial gradient; Dark matter; Orbits; Models; Mass distribution; Planetary nebulae; Dynamics; Spectroscopy; Spiral galaxies
SD :	Dispersión velocidad; Gradiente radial; Modelo
LO :	INIST-2067.354000110328450160
ID :	04-0411439

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Le document en format XML

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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<sup>-1</sup>
, with a steady radial velocity gradient of 245 km s<sup>-1</sup>
 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 M<sub>125</sub>
 = 7.5<sup>+2.5</sup>
1.3x 10<sup>11</sup>
M<sub>◦.</sub>
, or M<sub>125</sub>
 > 5.4 x 10<sup>11</sup>
 M<sub>◦.</sub>
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>
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<fC01 i1="01" l="ENG"><s0>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<sup>-1</sup>
, with a steady radial velocity gradient of 245 km s<sup>-1</sup>
 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 M<sub>125</sub>
 = 7.5<sup>+2.5</sup>
1.3x 10<sup>11</sup>
M<sub>◦.</sub>
, or M<sub>125</sub>
 > 5.4 x 10<sup>11</sup>
 M<sub>◦.</sub>
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.</s0>
</fC01>
<fC02 i1="01" i2="3"><s0>001E03D56N</s0>
</fC02>
<fC03 i1="01" i2="3" l="FRE"><s0>Cinématique</s0>
<s5>26</s5>
</fC03>
<fC03 i1="01" i2="3" l="ENG"><s0>Kinematics</s0>
<s5>26</s5>
</fC03>
<fC03 i1="02" i2="X" l="FRE"><s0>Dispersion vitesse</s0>
<s5>28</s5>
</fC03>
<fC03 i1="02" i2="X" l="ENG"><s0>Velocity dispersion</s0>
<s5>28</s5>
</fC03>
<fC03 i1="02" i2="X" l="SPA"><s0>Dispersión velocidad</s0>
<s5>28</s5>
</fC03>
<fC03 i1="03" i2="3" l="FRE"><s0>Vitesse radiale</s0>
<s5>29</s5>
</fC03>
<fC03 i1="03" i2="3" l="ENG"><s0>Radial velocity</s0>
<s5>29</s5>
</fC03>
<fC03 i1="04" i2="X" l="FRE"><s0>Gradient radial</s0>
<s5>30</s5>
</fC03>
<fC03 i1="04" i2="X" l="ENG"><s0>Radial gradient</s0>
<s5>30</s5>
</fC03>
<fC03 i1="04" i2="X" l="SPA"><s0>Gradiente radial</s0>
<s5>30</s5>
</fC03>
<fC03 i1="05" i2="3" l="FRE"><s0>Matière sombre</s0>
<s5>31</s5>
</fC03>
<fC03 i1="05" i2="3" l="ENG"><s0>Dark matter</s0>
<s5>31</s5>
</fC03>
<fC03 i1="06" i2="3" l="FRE"><s0>Orbite</s0>
<s5>32</s5>
</fC03>
<fC03 i1="06" i2="3" l="ENG"><s0>Orbits</s0>
<s5>32</s5>
</fC03>
<fC03 i1="07" i2="X" l="FRE"><s0>Modèle</s0>
<s5>33</s5>
</fC03>
<fC03 i1="07" i2="X" l="ENG"><s0>Models</s0>
<s5>33</s5>
</fC03>
<fC03 i1="07" i2="X" l="SPA"><s0>Modelo</s0>
<s5>33</s5>
</fC03>
<fC03 i1="08" i2="3" l="FRE"><s0>Distribution masse</s0>
<s5>34</s5>
</fC03>
<fC03 i1="08" i2="3" l="ENG"><s0>Mass distribution</s0>
<s5>34</s5>
</fC03>
<fC03 i1="09" i2="3" l="FRE"><s0>Nébuleuse planétaire</s0>
<s5>35</s5>
</fC03>
<fC03 i1="09" i2="3" l="ENG"><s0>Planetary nebulae</s0>
<s5>35</s5>
</fC03>
<fC03 i1="10" i2="3" l="FRE"><s0>Dynamique</s0>
<s5>36</s5>
</fC03>
<fC03 i1="10" i2="3" l="ENG"><s0>Dynamics</s0>
<s5>36</s5>
</fC03>
<fC03 i1="11" i2="3" l="FRE"><s0>Spectrométrie</s0>
<s5>38</s5>
</fC03>
<fC03 i1="11" i2="3" l="ENG"><s0>Spectroscopy</s0>
<s5>38</s5>
</fC03>
<fC03 i1="12" i2="3" l="FRE"><s0>Galaxies spirales</s0>
<s5>81</s5>
</fC03>
<fC03 i1="12" i2="3" l="ENG"><s0>Spiral galaxies</s0>
<s5>81</s5>
</fC03>
<fN21><s1>236</s1>
</fN21>
<fN44 i1="01"><s1>PSI</s1>
</fN44>
<fN82><s1>PSI</s1>
</fN82>
</pA>
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<server><NO>PASCAL 04-0411439 INIST</NO>
<ET>Taking measure of the Andromeda halo: a kinematic analysis of the giant stream surrounding M31</ET>
<AU>IBATA (R.); CHAPMAN (S.); FERGUSON (A. M. N.); IRWIN (M.); LEWIS (G.); MCCONNACHIE (A.)</AU>
<AF>Observatoire de Strasbourg, 11, rue de l'Université/Strasbourg 67000/France (1 aut.); California Institute of Technology/Pasadena, CA 91125/Etats-Unis (2 aut.); Max-Plank-Institut für Astrophysik, Karl-Schwarzschild-Str. 1, Postfach 1317/Garching 85741/Allemagne (3 aut.); Institute of Astronomy, Madingley Road/Cambridge CB3 0HA/Royaume-Uni (4 aut., 6 aut.); Institute of Astronomy, School of Physics, A29, University of Sydney/NSW 2006/Australie (5 aut.)</AF>
<DT>Publication en série; Niveau analytique</DT>
<SO>Monthly Notices of the Royal Astronomical Society; ISSN 0035-8711; Coden MNRAA4; Royaume-Uni; Da. 2004; Vol. 351; No. 1; Pp. 117-124; Bibl. 34 ref.</SO>
<LA>Anglais</LA>
<EA>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<sup>-1</sup>
, with a steady radial velocity gradient of 245 km s<sup>-1</sup>
 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 M<sub>125</sub>
 = 7.5<sup>+2.5</sup>
1.3x 10<sup>11</sup>
M<sub>◦.</sub>
, or M<sub>125</sub>
 > 5.4 x 10<sup>11</sup>
 M<sub>◦.</sub>
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.</EA>
<CC>001E03D56N</CC>
<FD>Cinématique; Dispersion vitesse; Vitesse radiale; Gradient radial; Matière sombre; Orbite; Modèle; Distribution masse; Nébuleuse planétaire; Dynamique; Spectrométrie; Galaxies spirales</FD>
<ED>Kinematics; Velocity dispersion; Radial velocity; Radial gradient; Dark matter; Orbits; Models; Mass distribution; Planetary nebulae; Dynamics; Spectroscopy; Spiral galaxies</ED>
<SD>Dispersión velocidad; Gradiente radial; Modelo</SD>
<LO>INIST-2067.354000110328450160</LO>
<ID>04-0411439</ID>
</server>
</inist>
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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

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