AustralieFrV1, PascalFrancis, Curation, bibRecord, 004170

DENSITY VARIATIONS IN THE NW STAR STREAM OF M31

Identifieur interne : 004170 ( PascalFrancis/Curation ); précédent : 004169; suivant : 004171

DENSITY VARIATIONS IN THE NW STAR STREAM OF M31

Auteurs : R. G. Carlberg [Canada] ; Harvey B. Richer [Canada] ; Alan W. Mcconnachie [Canada] ; Mike Irwin [Royaume-Uni] ; Rodrigo A. Ibata [France] ; Aaron L. Dotter [Canada] ; Scott Chapman [Royaume-Uni] ; Mark Fardal [États-Unis] ; A. M. N. Ferguson [Royaume-Uni] ; G. F. Lewis [Australie] ; Julio F. Navarro [Canada] ; Thomas H. Puzia [Chili] ; David Valls-Gabaud [France]

Source :

The Astrophysical journal [ 0004-637X ] ; 2011.

RBID : Pascal:11-0230649

Descripteurs français

Pascal (Inist)
- Pan, Matière sombre, Probabilité, Fluctuation, Métallicité, Bruit grenaille, Etoile faible masse, Perturbation, Galaxies compagnons, Fonction masse, Sous structure, Galaxies naines, Groupe local, Satellite Saturne.

English descriptors

KwdEn :
- Dark matter, Disturbances, Dwarf galaxies, Fluctuations, Local group, Low-mass stars, Mass function, Metallicity, Pan, Probability, Satellite galaxies, Saturn satellite, Shot noise, Substructure.

Abstract

The Pan Andromeda Archeological Survey (PAndAS) CFHT Megaprime survey of the M31-M33 system has found a star stream which extends about 120 kpc NW from the center of M31. The great length of the stream, and the likelihood that it does not significantly intersect the disk of M31, means that it is unusually well suited for a measurement of stream gaps and clumps along its length as a test for the predicted thousands of dark matter sub-halos. The main result of this paper is that the density of the stream varies between zero and about three times the mean along its length on scales of 2-20 kpc. The probability that the variations are random fluctuations in the star density is less than 10^-5. As a control sample, we search for density variations at precisely the same location in stars with metallicity higher than the stream [Fe/H] = [0, -0.5] and find no variations above the expected shot noise. The lumpiness of the stream is not compatible with a low mass star stream in a smooth galactic potential, nor is it readily compatible with the disturbance caused by the visible M31 satellite galaxies. The stream's density variations appear to be consistent with the effects of a large population of steep mass function dark matter sub-halos, such as found in LCDM simulations, acting on an approximately 10 Gyr old star stream. The effects of a single set of halo substructure realizations are shown for illustration, reserving a statistical comparison for another study.

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A03		`1`		`@0 Astrophys. j.`
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A08	`01`	`1`	`ENG`	`@1 DENSITY VARIATIONS IN THE NW STAR STREAM OF M31`
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A11	`02`	`1`		`@1 RICHER (Harvey B.)`
A11	`03`	`1`		`@1 MCCONNACHIE (Alan W.)`
A11	`04`	`1`		`@1 IRWIN (Mike)`
A11	`05`	`1`		`@1 IBATA (Rodrigo A.)`
A11	`06`	`1`		`@1 DOTTER (Aaron L.)`
A11	`07`	`1`		`@1 CHAPMAN (Scott)`
A11	`08`	`1`		`@1 FARDAL (Mark)`
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A11	`13`	`1`		`@1 VALLS-GABAUD (David)`
A14	`01`			`@1 Department of Astronomy and Astrophysics, University of Toronto @2 Toronto, ON M5S 3H4 @3 CAN @Z 1 aut.`
A14	`02`			`@1 Department of Physics and Astronomy, University of British Columbia @2 Vancouver, BC V6T 1Z1 @3 CAN @Z 2 aut.`
A14	`03`			`@1 NRC Herzberg Institute for Astrophysics, 5071 West Saanich Road @2 Victoria, BC V9E 2E7 @3 CAN @Z 3 aut.`
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A14	`09`			`@1 Sydney Institute for Astronomy. University of Sydney @2 NSW 2006 @3 AUS @Z 10 aut.`
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C01	`01`		`ENG`	@0 The Pan Andromeda Archeological Survey (PAndAS) CFHT Megaprime survey of the M31-M33 system has found a star stream which extends about 120 kpc NW from the center of M31. The great length of the stream, and the likelihood that it does not significantly intersect the disk of M31, means that it is unusually well suited for a measurement of stream gaps and clumps along its length as a test for the predicted thousands of dark matter sub-halos. The main result of this paper is that the density of the stream varies between zero and about three times the mean along its length on scales of 2-20 kpc. The probability that the variations are random fluctuations in the star density is less than 10^-5. As a control sample, we search for density variations at precisely the same location in stars with metallicity higher than the stream [Fe/H] = [0, -0.5] and find no variations above the expected shot noise. The lumpiness of the stream is not compatible with a low mass star stream in a smooth galactic potential, nor is it readily compatible with the disturbance caused by the visible M31 satellite galaxies. The stream's density variations appear to be consistent with the effects of a large population of steep mass function dark matter sub-halos, such as found in LCDM simulations, acting on an approximately 10 Gyr old star stream. The effects of a single set of halo substructure realizations are shown for illustration, reserving a statistical comparison for another study.
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C03	`03`	`3`	`FRE`	`@0 Probabilité @5 28`
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C03	`10`	`X`	`FRE`	`@0 Fonction masse @5 35`
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C03	`11`	`X`	`FRE`	`@0 Sous structure @5 36`
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C03	`11`	`X`	`SPA`	`@0 Subestructura @5 36`
C03	`12`	`3`	`FRE`	`@0 Galaxies naines @5 37`
C03	`12`	`3`	`ENG`	`@0 Dwarf galaxies @5 37`
C03	`13`	`3`	`FRE`	`@0 Groupe local @5 38`
C03	`13`	`3`	`ENG`	`@0 Local group @5 38`
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C03	`14`	`X`	`ENG`	`@0 Saturn satellite @5 39`
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Le document en format XML

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<author><name sortKey="Valls Gabaud, David" sort="Valls Gabaud, David" uniqKey="Valls Gabaud D" first="David" last="Valls-Gabaud">David Valls-Gabaud</name>
<affiliation wicri:level="1"><inist:fA14 i1="12"><s1>GEPI, CNRS UMR 8111, Observatoire de Paris, 5 Place Jules Janssen</s1>
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<seriesStmt><title level="j" type="main">The Astrophysical journal</title>
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<idno type="ISSN">0004-637X</idno>
</seriesStmt>
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<profileDesc><textClass><keywords scheme="KwdEn" xml:lang="en"><term>Dark matter</term>
<term>Disturbances</term>
<term>Dwarf galaxies</term>
<term>Fluctuations</term>
<term>Local group</term>
<term>Low-mass stars</term>
<term>Mass function</term>
<term>Metallicity</term>
<term>Pan</term>
<term>Probability</term>
<term>Satellite galaxies</term>
<term>Saturn satellite</term>
<term>Shot noise</term>
<term>Substructure</term>
</keywords>
<keywords scheme="Pascal" xml:lang="fr"><term>Pan</term>
<term>Matière sombre</term>
<term>Probabilité</term>
<term>Fluctuation</term>
<term>Métallicité</term>
<term>Bruit grenaille</term>
<term>Etoile faible masse</term>
<term>Perturbation</term>
<term>Galaxies compagnons</term>
<term>Fonction masse</term>
<term>Sous structure</term>
<term>Galaxies naines</term>
<term>Groupe local</term>
<term>Satellite Saturne</term>
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<front><div type="abstract" xml:lang="en">The Pan Andromeda Archeological Survey (PAndAS) CFHT Megaprime survey of the M31-M33 system has found a star stream which extends about 120 kpc NW from the center of M31. The great length of the stream, and the likelihood that it does not significantly intersect the disk of M31, means that it is unusually well suited for a measurement of stream gaps and clumps along its length as a test for the predicted thousands of dark matter sub-halos. The main result of this paper is that the density of the stream varies between zero and about three times the mean along its length on scales of 2-20 kpc. The probability that the variations are random fluctuations in the star density is less than 10<sup>-5</sup>
. As a control sample, we search for density variations at precisely the same location in stars with metallicity higher than the stream [Fe/H] = [0, -0.5] and find no variations above the expected shot noise. The lumpiness of the stream is not compatible with a low mass star stream in a smooth galactic potential, nor is it readily compatible with the disturbance caused by the visible M31 satellite galaxies. The stream's density variations appear to be consistent with the effects of a large population of steep mass function dark matter sub-halos, such as found in LCDM simulations, acting on an approximately 10 Gyr old star stream. The effects of a single set of halo substructure realizations are shown for illustration, reserving a statistical comparison for another study.</div>
</front>
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<fA03 i2="1"><s0>Astrophys. j.</s0>
</fA03>
<fA05><s2>731</s2>
</fA05>
<fA06><s2>2</s2>
<s3>p. 1</s3>
</fA06>
<fA08 i1="01" i2="1" l="ENG"><s1>DENSITY VARIATIONS IN THE NW STAR STREAM OF M31</s1>
</fA08>
<fA11 i1="01" i2="1"><s1>CARLBERG (R. G.)</s1>
</fA11>
<fA11 i1="02" i2="1"><s1>RICHER (Harvey B.)</s1>
</fA11>
<fA11 i1="03" i2="1"><s1>MCCONNACHIE (Alan W.)</s1>
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<fA11 i1="04" i2="1"><s1>IRWIN (Mike)</s1>
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<fA11 i1="05" i2="1"><s1>IBATA (Rodrigo A.)</s1>
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<fA11 i1="06" i2="1"><s1>DOTTER (Aaron L.)</s1>
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<fA11 i1="07" i2="1"><s1>CHAPMAN (Scott)</s1>
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<fA11 i1="08" i2="1"><s1>FARDAL (Mark)</s1>
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<fA11 i1="09" i2="1"><s1>FERGUSON (A. M. N.)</s1>
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<fA11 i1="10" i2="1"><s1>LEWIS (G. F.)</s1>
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<fA11 i1="11" i2="1"><s1>NAVARRO (Julio F.)</s1>
</fA11>
<fA11 i1="12" i2="1"><s1>PUZIA (Thomas H.)</s1>
</fA11>
<fA11 i1="13" i2="1"><s1>VALLS-GABAUD (David)</s1>
</fA11>
<fA14 i1="01"><s1>Department of Astronomy and Astrophysics, University of Toronto</s1>
<s2>Toronto, ON M5S 3H4</s2>
<s3>CAN</s3>
<sZ>1 aut.</sZ>
</fA14>
<fA14 i1="02"><s1>Department of Physics and Astronomy, University of British Columbia</s1>
<s2>Vancouver, BC V6T 1Z1</s2>
<s3>CAN</s3>
<sZ>2 aut.</sZ>
</fA14>
<fA14 i1="03"><s1>NRC Herzberg Institute for Astrophysics, 5071 West Saanich Road</s1>
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<s3>CAN</s3>
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<fA14 i1="04"><s1>Institute of Astronomy, Madingley Road</s1>
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<s3>GBR</s3>
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<sZ>7 aut.</sZ>
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<fA14 i1="05"><s1>Observatoire de Strasbourg, 11, rue de l,Université</s1>
<s2>67000, Strasbourg</s2>
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<fA14 i1="06"><s1>Department of Physics and Astronomy, University of Victoria</s1>
<s2>Victoria, BC, V8P 1A1</s2>
<s3>CAN</s3>
<sZ>6 aut.</sZ>
</fA14>
<fA14 i1="07"><s1>Department of Astronomy, University of Massachusetts</s1>
<s2>Amherst, MA 01003-9305</s2>
<s3>USA</s3>
<sZ>8 aut.</sZ>
</fA14>
<fA14 i1="08"><s1>Institute for Astronomy, University of Edinburgh, Blackford Hill</s1>
<s2>Edinburgh, EH9 3HJ</s2>
<s3>GBR</s3>
<sZ>9 aut.</sZ>
</fA14>
<fA14 i1="09"><s1>Sydney Institute for Astronomy. University of Sydney</s1>
<s2>NSW 2006</s2>
<s3>AUS</s3>
<sZ>10 aut.</sZ>
</fA14>
<fA14 i1="10"><s1>Department of Physics and Astronomy, University of Victoria</s1>
<s2>Victoria, BC V8P 5C2</s2>
<s3>CAN</s3>
<sZ>11 aut.</sZ>
</fA14>
<fA14 i1="11"><s1>Department of Astronomy and Astrophysics, Pontificia Universidad Catlica de Chile</s1>
<s2>Santiago</s2>
<s3>CHL</s3>
<sZ>12 aut.</sZ>
</fA14>
<fA14 i1="12"><s1>GEPI, CNRS UMR 8111, Observatoire de Paris, 5 Place Jules Janssen</s1>
<s2>92195 Meudon</s2>
<s3>FRA</s3>
<sZ>13 aut.</sZ>
</fA14>
<fA20><s2>731.1-10</s2>
</fA20>
<fA21><s1>2011</s1>
</fA21>
<fA23 i1="01"><s0>ENG</s0>
</fA23>
<fA43 i1="01"><s1>INIST</s1>
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<s5>354000189762340470</s5>
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<fA44><s0>0000</s0>
<s1>© 2011 INIST-CNRS. All rights reserved.</s1>
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<fA45><s0>1/2 p.</s0>
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<fA47 i1="01" i2="1"><s0>11-0230649</s0>
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<fA60><s1>P</s1>
</fA60>
<fA61><s0>A</s0>
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<fA64 i1="01" i2="1"><s0>The Astrophysical journal</s0>
</fA64>
<fA66 i1="01"><s0>GBR</s0>
</fA66>
<fC01 i1="01" l="ENG"><s0>The Pan Andromeda Archeological Survey (PAndAS) CFHT Megaprime survey of the M31-M33 system has found a star stream which extends about 120 kpc NW from the center of M31. The great length of the stream, and the likelihood that it does not significantly intersect the disk of M31, means that it is unusually well suited for a measurement of stream gaps and clumps along its length as a test for the predicted thousands of dark matter sub-halos. The main result of this paper is that the density of the stream varies between zero and about three times the mean along its length on scales of 2-20 kpc. The probability that the variations are random fluctuations in the star density is less than 10<sup>-5</sup>
. As a control sample, we search for density variations at precisely the same location in stars with metallicity higher than the stream [Fe/H] = [0, -0.5] and find no variations above the expected shot noise. The lumpiness of the stream is not compatible with a low mass star stream in a smooth galactic potential, nor is it readily compatible with the disturbance caused by the visible M31 satellite galaxies. The stream's density variations appear to be consistent with the effects of a large population of steep mass function dark matter sub-halos, such as found in LCDM simulations, acting on an approximately 10 Gyr old star stream. The effects of a single set of halo substructure realizations are shown for illustration, reserving a statistical comparison for another study.</s0>
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<fC02 i1="01" i2="3"><s0>001E03</s0>
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<fC03 i1="01" i2="X" l="FRE"><s0>Pan</s0>
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<s5>26</s5>
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<fC03 i1="01" i2="X" l="ENG"><s0>Pan</s0>
<s2>NO</s2>
<s5>26</s5>
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<fC03 i1="01" i2="X" l="SPA"><s0>Pan</s0>
<s2>NO</s2>
<s5>26</s5>
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<fC03 i1="02" i2="3" l="FRE"><s0>Matière sombre</s0>
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<fC03 i1="03" i2="3" l="FRE"><s0>Probabilité</s0>
<s5>28</s5>
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<fC03 i1="04" i2="3" l="FRE"><s0>Fluctuation</s0>
<s5>29</s5>
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<fC03 i1="04" i2="3" l="ENG"><s0>Fluctuations</s0>
<s5>29</s5>
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<fC03 i1="05" i2="X" l="FRE"><s0>Métallicité</s0>
<s5>30</s5>
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<fC03 i1="05" i2="X" l="ENG"><s0>Metallicity</s0>
<s5>30</s5>
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<fC03 i1="05" i2="X" l="SPA"><s0>Metalicidad</s0>
<s5>30</s5>
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<fC03 i1="06" i2="3" l="FRE"><s0>Bruit grenaille</s0>
<s5>31</s5>
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<fC03 i1="06" i2="3" l="ENG"><s0>Shot noise</s0>
<s5>31</s5>
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<fC03 i1="07" i2="3" l="FRE"><s0>Etoile faible masse</s0>
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<fC03 i1="07" i2="3" l="ENG"><s0>Low-mass stars</s0>
<s5>32</s5>
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<fC03 i1="08" i2="3" l="FRE"><s0>Perturbation</s0>
<s5>33</s5>
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<s5>33</s5>
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<fC03 i1="09" i2="X" l="FRE"><s0>Galaxies compagnons</s0>
<s5>34</s5>
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<fC03 i1="09" i2="X" l="ENG"><s0>Satellite galaxies</s0>
<s5>34</s5>
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<fC03 i1="09" i2="X" l="SPA"><s0>Galaxias satélite</s0>
<s5>34</s5>
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<s5>35</s5>
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<fC03 i1="10" i2="X" l="SPA"><s0>Función masa</s0>
<s5>35</s5>
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<fC03 i1="11" i2="X" l="FRE"><s0>Sous structure</s0>
<s5>36</s5>
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<fC03 i1="11" i2="X" l="ENG"><s0>Substructure</s0>
<s5>36</s5>
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<fC03 i1="11" i2="X" l="SPA"><s0>Subestructura</s0>
<s5>36</s5>
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<fC03 i1="12" i2="3" l="FRE"><s0>Galaxies naines</s0>
<s5>37</s5>
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<fC03 i1="12" i2="3" l="ENG"><s0>Dwarf galaxies</s0>
<s5>37</s5>
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<fC03 i1="13" i2="3" l="FRE"><s0>Groupe local</s0>
<s5>38</s5>
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<fC03 i1="13" i2="3" l="ENG"><s0>Local group</s0>
<s5>38</s5>
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<fC03 i1="14" i2="X" l="FRE"><s0>Satellite Saturne</s0>
<s5>39</s5>
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<fC03 i1="14" i2="X" l="ENG"><s0>Saturn satellite</s0>
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<fC03 i1="14" i2="X" l="SPA"><s0>Satélite Saturno</s0>
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<fN21><s1>150</s1>
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DENSITY VARIATIONS IN THE NW STAR STREAM OF M31

DENSITY VARIATIONS IN THE NW STAR STREAM OF M31

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