The AAT/WFI survey of the Monoceros Ring and Canis Major dwarf galaxy -I. From l = (193-276)°
Identifieur interne : 003D04 ( PascalFrancis/Corpus ); précédent : 003D03; suivant : 003D05The AAT/WFI survey of the Monoceros Ring and Canis Major dwarf galaxy -I. From l = (193-276)°
Auteurs : Blair C. Conn ; Richard R. Lane ; Geraint F. Lewis ; Rodrigo Gil-Merino ; Mike J. Irwin ; Rodrigo A. Ibata ; Nicolas F. Martin ; Michele Bellazzini ; Robert Sharp ; Artem V. Tuntsov ; Annette M. N. FergusonSource :
- Monthly Notices of the Royal Astronomical Society [ 0035-8711 ] ; 2007.
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- Pascal (Inist)
English descriptors
- KwdEn :
Abstract
We present the results of an Anglo-Australian Telescope (AAT) wide field camera survey of the stars in the Monoceros Ring (MRi) and purported Canis Major (CMa) overdensity in the Galactic longitudes of l = (193-276)°. Current numerical simulations suggest that both of these structures are the result of a single on-going accretion event, although an alternative solution is that the warped and flared disc of the Galaxy can explain the origin of both of these structures. Our results show that, with regards the MRi, the warped and flared disc is unable to reproduce the locations and strengths of the detections observed around the Galaxy. This supports a non-Galactic origin for this structure. We report eight new detections and two tentative detections of the MRi in this survey. The exact nature of the CMa overdensity is still unresolved, although this survey provides evidence that invoking the Galactic warp is not a sufficient solution when compared with observation. Several fields in this survey are highly inconsistent with the current Galactic disc models that include a warp and flare, to such an extent that explaining their origins with these structures is problematic. We also report that the blue plume stars previously invoked to support the dwarf galaxy hypothesis are unfounded, and associating them with an outer spiral arm is equally problematic. Standard Galactic models are unable to accommodate all the observations of these new structures, leading away from a warped/flared disc explanation for their origins and more toward a non-Galactic source. Additionally, evidence is presented in favour of a detection of the CMa dwarf stream away from the CMa region. As the outer reaches of the Galactic disc continue to be probed, the fascinating structures that are the MRi and CMa overdensity will no doubt continue to inform us of the unique structure and formation of the Milky Way.
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| NO : | PASCAL 07-0188894 INIST |
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| ET : | The AAT/WFI survey of the Monoceros Ring and Canis Major dwarf galaxy -I. From l = (193-276)° |
| AU : | CONN (Blair C.); LANE (Richard R.); LEWIS (Geraint F.); GIL-MERINO (Rodrigo); IRWIN (Mike J.); IBATA (Rodrigo A.); MARTIN (Nicolas F.); BELLAZZINI (Michele); SHARP (Robert); TUNTSOV (Artem V.); FERGUSON (Annette M. N.) |
| AF : | Institute of Astronomy, School of Physics, A29 University of Sydney/NSW 2006/Australie (1 aut., 2 aut., 3 aut., 4 aut., 10 aut.); European Southern Observatory, Alonso de Cordova 3107, Vitacura/Santiago/Chili (1 aut.); Institute of Astronomy, Madingley Road/Cambridge CB3 0HA/Royaume-Uni (5 aut.); Observatoire de Strasbourg, 11 rue de l'Université/67000 Strasbourg/France (6 aut., 7 aut.); INAF -Osservatorio Astronomico di Bologna, Via Ranzani 1/40127 Bologna/Italie (8 aut.); Anglo-Australian Observatory/Epping, NSW 1710/Australie (9 aut.); Institute for Astronomy, University of Edinburgh, Royal Observatory, Blackford Hill/Edinburgh EH9 3HJ/Royaume-Uni (11 aut.) |
| DT : | Publication en série; Niveau analytique |
| SO : | Monthly Notices of the Royal Astronomical Society; ISSN 0035-8711; Coden MNRAA4; Royaume-Uni; Da. 2007; Vol. 376; No. 3; Pp. 939-959; Bibl. 1/2 p. |
| LA : | Anglais |
| EA : | We present the results of an Anglo-Australian Telescope (AAT) wide field camera survey of the stars in the Monoceros Ring (MRi) and purported Canis Major (CMa) overdensity in the Galactic longitudes of l = (193-276)°. Current numerical simulations suggest that both of these structures are the result of a single on-going accretion event, although an alternative solution is that the warped and flared disc of the Galaxy can explain the origin of both of these structures. Our results show that, with regards the MRi, the warped and flared disc is unable to reproduce the locations and strengths of the detections observed around the Galaxy. This supports a non-Galactic origin for this structure. We report eight new detections and two tentative detections of the MRi in this survey. The exact nature of the CMa overdensity is still unresolved, although this survey provides evidence that invoking the Galactic warp is not a sufficient solution when compared with observation. Several fields in this survey are highly inconsistent with the current Galactic disc models that include a warp and flare, to such an extent that explaining their origins with these structures is problematic. We also report that the blue plume stars previously invoked to support the dwarf galaxy hypothesis are unfounded, and associating them with an outer spiral arm is equally problematic. Standard Galactic models are unable to accommodate all the observations of these new structures, leading away from a warped/flared disc explanation for their origins and more toward a non-Galactic source. Additionally, evidence is presented in favour of a detection of the CMa dwarf stream away from the CMa region. As the outer reaches of the Galactic disc continue to be probed, the fascinating structures that are the MRi and CMa overdensity will no doubt continue to inform us of the unique structure and formation of the Milky Way. |
| CC : | 001E03 |
| FD : | Galaxies naines; Simulation numérique; Accrétion; Galaxies disques; Disque galactique; Modèle standard; Bras spiral; Voie lactée; Formation galaxies; Structure galaxies |
| ED : | Dwarf galaxies; Digital simulation; Accretion; Disk galaxies; Galactic disks; Standard model; Spiral arm; Milky Way; Galaxy formation; Galaxy structure |
| SD : | Brazo espiral; Estructura galaxias |
| LO : | INIST-2067.354000147122370020 |
| ID : | 07-0188894 |
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Conn</name><affiliation><inist:fA14 i1="01"><s1>Institute of Astronomy, School of Physics, A29 University of Sydney</s1><s2>NSW 2006</s2><s3>AUS</s3><sZ>1 aut.</sZ><sZ>2 aut.</sZ><sZ>3 aut.</sZ><sZ>4 aut.</sZ><sZ>10 aut.</sZ></inist:fA14></affiliation><affiliation><inist:fA14 i1="02"><s1>European Southern Observatory, Alonso de Cordova 3107, Vitacura</s1><s2>Santiago</s2><s3>CHL</s3><sZ>1 aut.</sZ></inist:fA14></affiliation></author><author><name sortKey="Lane, Richard R" sort="Lane, Richard R" uniqKey="Lane R" first="Richard R." last="Lane">Richard R. Lane</name><affiliation><inist:fA14 i1="01"><s1>Institute of Astronomy, School of Physics, A29 University of Sydney</s1><s2>NSW 2006</s2><s3>AUS</s3><sZ>1 aut.</sZ><sZ>2 aut.</sZ><sZ>3 aut.</sZ><sZ>4 aut.</sZ><sZ>10 aut.</sZ></inist:fA14></affiliation></author><author><name sortKey="Lewis, Geraint F" sort="Lewis, Geraint F" uniqKey="Lewis G" first="Geraint F." last="Lewis">Geraint F. Lewis</name><affiliation><inist:fA14 i1="01"><s1>Institute of Astronomy, School of Physics, A29 University of Sydney</s1><s2>NSW 2006</s2><s3>AUS</s3><sZ>1 aut.</sZ><sZ>2 aut.</sZ><sZ>3 aut.</sZ><sZ>4 aut.</sZ><sZ>10 aut.</sZ></inist:fA14></affiliation></author><author><name sortKey="Gil Merino, Rodrigo" sort="Gil Merino, Rodrigo" uniqKey="Gil Merino R" first="Rodrigo" last="Gil-Merino">Rodrigo Gil-Merino</name><affiliation><inist:fA14 i1="01"><s1>Institute of Astronomy, School of Physics, A29 University of Sydney</s1><s2>NSW 2006</s2><s3>AUS</s3><sZ>1 aut.</sZ><sZ>2 aut.</sZ><sZ>3 aut.</sZ><sZ>4 aut.</sZ><sZ>10 aut.</sZ></inist:fA14></affiliation></author><author><name sortKey="Irwin, Mike J" sort="Irwin, Mike J" uniqKey="Irwin M" first="Mike J." last="Irwin">Mike J. Irwin</name><affiliation><inist:fA14 i1="03"><s1>Institute of Astronomy, Madingley Road</s1><s2>Cambridge CB3 0HA</s2><s3>GBR</s3><sZ>5 aut.</sZ></inist:fA14></affiliation></author><author><name sortKey="Ibata, Rodrigo A" sort="Ibata, Rodrigo A" uniqKey="Ibata R" first="Rodrigo A." last="Ibata">Rodrigo A. Ibata</name><affiliation><inist:fA14 i1="04"><s1>Observatoire de Strasbourg, 11 rue de l'Université</s1><s2>67000 Strasbourg</s2><s3>FRA</s3><sZ>6 aut.</sZ><sZ>7 aut.</sZ></inist:fA14></affiliation></author><author><name sortKey="Martin, Nicolas F" sort="Martin, Nicolas F" uniqKey="Martin N" first="Nicolas F." last="Martin">Nicolas F. Martin</name><affiliation><inist:fA14 i1="04"><s1>Observatoire de Strasbourg, 11 rue de l'Université</s1><s2>67000 Strasbourg</s2><s3>FRA</s3><sZ>6 aut.</sZ><sZ>7 aut.</sZ></inist:fA14></affiliation></author><author><name sortKey="Bellazzini, Michele" sort="Bellazzini, Michele" uniqKey="Bellazzini M" first="Michele" last="Bellazzini">Michele Bellazzini</name><affiliation><inist:fA14 i1="05"><s1>INAF -Osservatorio Astronomico di Bologna, Via Ranzani 1</s1><s2>40127 Bologna</s2><s3>ITA</s3><sZ>8 aut.</sZ></inist:fA14></affiliation></author><author><name sortKey="Sharp, Robert" sort="Sharp, Robert" uniqKey="Sharp R" first="Robert" last="Sharp">Robert Sharp</name><affiliation><inist:fA14 i1="06"><s1>Anglo-Australian Observatory</s1><s2>Epping, NSW 1710</s2><s3>AUS</s3><sZ>9 aut.</sZ></inist:fA14></affiliation></author><author><name sortKey="Tuntsov, Artem V" sort="Tuntsov, Artem V" uniqKey="Tuntsov A" first="Artem V." last="Tuntsov">Artem V. Tuntsov</name><affiliation><inist:fA14 i1="01"><s1>Institute of Astronomy, School of Physics, A29 University of Sydney</s1><s2>NSW 2006</s2><s3>AUS</s3><sZ>1 aut.</sZ><sZ>2 aut.</sZ><sZ>3 aut.</sZ><sZ>4 aut.</sZ><sZ>10 aut.</sZ></inist:fA14></affiliation></author><author><name sortKey="Ferguson, Annette M N" sort="Ferguson, Annette M N" uniqKey="Ferguson A" first="Annette M. N." last="Ferguson">Annette M. N. Ferguson</name><affiliation><inist:fA14 i1="07"><s1>Institute for Astronomy, University of Edinburgh, Royal Observatory, Blackford Hill</s1><s2>Edinburgh EH9 3HJ</s2><s3>GBR</s3><sZ>11 aut.</sZ></inist:fA14></affiliation></author></analytic><series><title level="j" type="main">Monthly Notices of the Royal Astronomical Society</title><title level="j" type="abbreviated">Mon. Not. R. Astron. Soc.</title><idno type="ISSN">0035-8711</idno><imprint><date when="2007">2007</date></imprint></series></biblStruct></sourceDesc><seriesStmt><title level="j" type="main">Monthly Notices of the Royal Astronomical Society</title><title level="j" type="abbreviated">Mon. Not. R. Astron. Soc.</title><idno type="ISSN">0035-8711</idno></seriesStmt></fileDesc><profileDesc><textClass><keywords scheme="KwdEn" xml:lang="en"><term>Accretion</term><term>Digital simulation</term><term>Disk galaxies</term><term>Dwarf galaxies</term><term>Galactic disks</term><term>Galaxy formation</term><term>Galaxy structure</term><term>Milky Way</term><term>Spiral arm</term><term>Standard model</term></keywords><keywords scheme="Pascal" xml:lang="fr"><term>Galaxies naines</term><term>Simulation numérique</term><term>Accrétion</term><term>Galaxies disques</term><term>Disque galactique</term><term>Modèle standard</term><term>Bras spiral</term><term>Voie lactée</term><term>Formation galaxies</term><term>Structure galaxies</term></keywords></textClass></profileDesc></teiHeader><front><div type="abstract" xml:lang="en">We present the results of an Anglo-Australian Telescope (AAT) wide field camera survey of the stars in the Monoceros Ring (MRi) and purported Canis Major (CMa) overdensity in the Galactic longitudes of l = (193-276)°. Current numerical simulations suggest that both of these structures are the result of a single on-going accretion event, although an alternative solution is that the warped and flared disc of the Galaxy can explain the origin of both of these structures. Our results show that, with regards the MRi, the warped and flared disc is unable to reproduce the locations and strengths of the detections observed around the Galaxy. This supports a non-Galactic origin for this structure. We report eight new detections and two tentative detections of the MRi in this survey. The exact nature of the CMa overdensity is still unresolved, although this survey provides evidence that invoking the Galactic warp is not a sufficient solution when compared with observation. Several fields in this survey are highly inconsistent with the current Galactic disc models that include a warp and flare, to such an extent that explaining their origins with these structures is problematic. We also report that the blue plume stars previously invoked to support the dwarf galaxy hypothesis are unfounded, and associating them with an outer spiral arm is equally problematic. Standard Galactic models are unable to accommodate all the observations of these new structures, leading away from a warped/flared disc explanation for their origins and more toward a non-Galactic source. Additionally, evidence is presented in favour of a detection of the CMa dwarf stream away from the CMa region. As the outer reaches of the Galactic disc continue to be probed, the fascinating structures that are the MRi and CMa overdensity will no doubt continue to inform us of the unique structure and formation of the Milky Way.</div></front></TEI><inist><standard h6="B"><pA><fA01 i1="01" i2="1"><s0>0035-8711</s0></fA01><fA02 i1="01"><s0>MNRAA4</s0></fA02><fA03 i2="1"><s0>Mon. Not. R. Astron. Soc.</s0></fA03><fA05><s2>376</s2></fA05><fA06><s2>3</s2></fA06><fA08 i1="01" i2="1" l="ENG"><s1>The AAT/WFI survey of the Monoceros Ring and Canis Major dwarf galaxy -I. From l = (193-276)°</s1></fA08><fA11 i1="01" i2="1"><s1>CONN (Blair C.)</s1></fA11><fA11 i1="02" i2="1"><s1>LANE (Richard R.)</s1></fA11><fA11 i1="03" i2="1"><s1>LEWIS (Geraint F.)</s1></fA11><fA11 i1="04" i2="1"><s1>GIL-MERINO (Rodrigo)</s1></fA11><fA11 i1="05" i2="1"><s1>IRWIN (Mike J.)</s1></fA11><fA11 i1="06" i2="1"><s1>IBATA (Rodrigo A.)</s1></fA11><fA11 i1="07" i2="1"><s1>MARTIN (Nicolas F.)</s1></fA11><fA11 i1="08" i2="1"><s1>BELLAZZINI (Michele)</s1></fA11><fA11 i1="09" i2="1"><s1>SHARP (Robert)</s1></fA11><fA11 i1="10" i2="1"><s1>TUNTSOV (Artem V.)</s1></fA11><fA11 i1="11" i2="1"><s1>FERGUSON (Annette M. N.)</s1></fA11><fA14 i1="01"><s1>Institute of Astronomy, School of Physics, A29 University of Sydney</s1><s2>NSW 2006</s2><s3>AUS</s3><sZ>1 aut.</sZ><sZ>2 aut.</sZ><sZ>3 aut.</sZ><sZ>4 aut.</sZ><sZ>10 aut.</sZ></fA14><fA14 i1="02"><s1>European Southern Observatory, Alonso de Cordova 3107, Vitacura</s1><s2>Santiago</s2><s3>CHL</s3><sZ>1 aut.</sZ></fA14><fA14 i1="03"><s1>Institute of Astronomy, Madingley Road</s1><s2>Cambridge CB3 0HA</s2><s3>GBR</s3><sZ>5 aut.</sZ></fA14><fA14 i1="04"><s1>Observatoire de Strasbourg, 11 rue de l'Université</s1><s2>67000 Strasbourg</s2><s3>FRA</s3><sZ>6 aut.</sZ><sZ>7 aut.</sZ></fA14><fA14 i1="05"><s1>INAF -Osservatorio Astronomico di Bologna, Via Ranzani 1</s1><s2>40127 Bologna</s2><s3>ITA</s3><sZ>8 aut.</sZ></fA14><fA14 i1="06"><s1>Anglo-Australian Observatory</s1><s2>Epping, NSW 1710</s2><s3>AUS</s3><sZ>9 aut.</sZ></fA14><fA14 i1="07"><s1>Institute for Astronomy, University of Edinburgh, Royal Observatory, Blackford Hill</s1><s2>Edinburgh EH9 3HJ</s2><s3>GBR</s3><sZ>11 aut.</sZ></fA14><fA20><s1>939-959</s1></fA20><fA21><s1>2007</s1></fA21><fA23 i1="01"><s0>ENG</s0></fA23><fA43 i1="01"><s1>INIST</s1><s2>2067</s2><s5>354000147122370020</s5></fA43><fA44><s0>0000</s0><s1>© 2007 INIST-CNRS. All rights reserved.</s1></fA44><fA45><s0>1/2 p.</s0></fA45><fA47 i1="01" i2="1"><s0>07-0188894</s0></fA47><fA60><s1>P</s1></fA60><fA61><s0>A</s0></fA61><fA64 i1="01" i2="1"><s0>Monthly Notices of the Royal Astronomical Society</s0></fA64><fA66 i1="01"><s0>GBR</s0></fA66><fC01 i1="01" l="ENG"><s0>We present the results of an Anglo-Australian Telescope (AAT) wide field camera survey of the stars in the Monoceros Ring (MRi) and purported Canis Major (CMa) overdensity in the Galactic longitudes of l = (193-276)°. Current numerical simulations suggest that both of these structures are the result of a single on-going accretion event, although an alternative solution is that the warped and flared disc of the Galaxy can explain the origin of both of these structures. Our results show that, with regards the MRi, the warped and flared disc is unable to reproduce the locations and strengths of the detections observed around the Galaxy. This supports a non-Galactic origin for this structure. We report eight new detections and two tentative detections of the MRi in this survey. The exact nature of the CMa overdensity is still unresolved, although this survey provides evidence that invoking the Galactic warp is not a sufficient solution when compared with observation. Several fields in this survey are highly inconsistent with the current Galactic disc models that include a warp and flare, to such an extent that explaining their origins with these structures is problematic. We also report that the blue plume stars previously invoked to support the dwarf galaxy hypothesis are unfounded, and associating them with an outer spiral arm is equally problematic. Standard Galactic models are unable to accommodate all the observations of these new structures, leading away from a warped/flared disc explanation for their origins and more toward a non-Galactic source. Additionally, evidence is presented in favour of a detection of the CMa dwarf stream away from the CMa region. As the outer reaches of the Galactic disc continue to be probed, the fascinating structures that are the MRi and CMa overdensity will no doubt continue to inform us of the unique structure and formation of the Milky Way.</s0></fC01><fC02 i1="01" i2="3"><s0>001E03</s0></fC02><fC03 i1="01" i2="3" l="FRE"><s0>Galaxies naines</s0><s5>26</s5></fC03><fC03 i1="01" i2="3" l="ENG"><s0>Dwarf galaxies</s0><s5>26</s5></fC03><fC03 i1="02" i2="3" l="FRE"><s0>Simulation numérique</s0><s5>27</s5></fC03><fC03 i1="02" i2="3" l="ENG"><s0>Digital simulation</s0><s5>27</s5></fC03><fC03 i1="03" i2="3" l="FRE"><s0>Accrétion</s0><s5>28</s5></fC03><fC03 i1="03" i2="3" l="ENG"><s0>Accretion</s0><s5>28</s5></fC03><fC03 i1="04" i2="3" l="FRE"><s0>Galaxies disques</s0><s5>29</s5></fC03><fC03 i1="04" i2="3" l="ENG"><s0>Disk galaxies</s0><s5>29</s5></fC03><fC03 i1="05" i2="3" l="FRE"><s0>Disque galactique</s0><s5>30</s5></fC03><fC03 i1="05" i2="3" l="ENG"><s0>Galactic disks</s0><s5>30</s5></fC03><fC03 i1="06" i2="3" l="FRE"><s0>Modèle standard</s0><s5>31</s5></fC03><fC03 i1="06" i2="3" l="ENG"><s0>Standard model</s0><s5>31</s5></fC03><fC03 i1="07" i2="X" l="FRE"><s0>Bras spiral</s0><s5>32</s5></fC03><fC03 i1="07" i2="X" l="ENG"><s0>Spiral arm</s0><s5>32</s5></fC03><fC03 i1="07" i2="X" l="SPA"><s0>Brazo espiral</s0><s5>32</s5></fC03><fC03 i1="08" i2="3" l="FRE"><s0>Voie lactée</s0><s5>33</s5></fC03><fC03 i1="08" i2="3" l="ENG"><s0>Milky Way</s0><s5>33</s5></fC03><fC03 i1="09" i2="3" l="FRE"><s0>Formation galaxies</s0><s5>34</s5></fC03><fC03 i1="09" i2="3" l="ENG"><s0>Galaxy formation</s0><s5>34</s5></fC03><fC03 i1="10" i2="3" l="FRE"><s0>Structure galaxies</s0><s4>CD</s4><s5>96</s5></fC03><fC03 i1="10" i2="3" l="ENG"><s0>Galaxy structure</s0><s4>CD</s4><s5>96</s5></fC03><fC03 i1="10" i2="3" l="SPA"><s0>Estructura galaxias</s0><s4>CD</s4><s5>96</s5></fC03><fN21><s1>128</s1></fN21><fN44 i1="01"><s1>OTO</s1></fN44><fN82><s1>OTO</s1></fN82></pA></standard><server><NO>PASCAL 07-0188894 INIST</NO><ET>The AAT/WFI survey of the Monoceros Ring and Canis Major dwarf galaxy -I. From l = (193-276)°</ET><AU>CONN (Blair C.); LANE (Richard R.); LEWIS (Geraint F.); GIL-MERINO (Rodrigo); IRWIN (Mike J.); IBATA (Rodrigo A.); MARTIN (Nicolas F.); BELLAZZINI (Michele); SHARP (Robert); TUNTSOV (Artem V.); FERGUSON (Annette M. N.)</AU><AF>Institute of Astronomy, School of Physics, A29 University of Sydney/NSW 2006/Australie (1 aut., 2 aut., 3 aut., 4 aut., 10 aut.); European Southern Observatory, Alonso de Cordova 3107, Vitacura/Santiago/Chili (1 aut.); Institute of Astronomy, Madingley Road/Cambridge CB3 0HA/Royaume-Uni (5 aut.); Observatoire de Strasbourg, 11 rue de l'Université/67000 Strasbourg/France (6 aut., 7 aut.); INAF -Osservatorio Astronomico di Bologna, Via Ranzani 1/40127 Bologna/Italie (8 aut.); Anglo-Australian Observatory/Epping, NSW 1710/Australie (9 aut.); Institute for Astronomy, University of Edinburgh, Royal Observatory, Blackford Hill/Edinburgh EH9 3HJ/Royaume-Uni (11 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. 2007; Vol. 376; No. 3; Pp. 939-959; Bibl. 1/2 p.</SO><LA>Anglais</LA><EA>We present the results of an Anglo-Australian Telescope (AAT) wide field camera survey of the stars in the Monoceros Ring (MRi) and purported Canis Major (CMa) overdensity in the Galactic longitudes of l = (193-276)°. Current numerical simulations suggest that both of these structures are the result of a single on-going accretion event, although an alternative solution is that the warped and flared disc of the Galaxy can explain the origin of both of these structures. Our results show that, with regards the MRi, the warped and flared disc is unable to reproduce the locations and strengths of the detections observed around the Galaxy. This supports a non-Galactic origin for this structure. We report eight new detections and two tentative detections of the MRi in this survey. The exact nature of the CMa overdensity is still unresolved, although this survey provides evidence that invoking the Galactic warp is not a sufficient solution when compared with observation. Several fields in this survey are highly inconsistent with the current Galactic disc models that include a warp and flare, to such an extent that explaining their origins with these structures is problematic. We also report that the blue plume stars previously invoked to support the dwarf galaxy hypothesis are unfounded, and associating them with an outer spiral arm is equally problematic. Standard Galactic models are unable to accommodate all the observations of these new structures, leading away from a warped/flared disc explanation for their origins and more toward a non-Galactic source. Additionally, evidence is presented in favour of a detection of the CMa dwarf stream away from the CMa region. As the outer reaches of the Galactic disc continue to be probed, the fascinating structures that are the MRi and CMa overdensity will no doubt continue to inform us of the unique structure and formation of the Milky Way.</EA><CC>001E03</CC><FD>Galaxies naines; Simulation numérique; Accrétion; Galaxies disques; Disque galactique; Modèle standard; Bras spiral; Voie lactée; Formation galaxies; Structure galaxies</FD><ED>Dwarf galaxies; Digital simulation; Accretion; Disk galaxies; Galactic disks; Standard model; Spiral arm; Milky Way; Galaxy formation; Galaxy structure</ED><SD>Brazo espiral; Estructura galaxias</SD><LO>INIST-2067.354000147122370020</LO><ID>07-0188894</ID></server></inist></record>Pour manipuler ce document sous Unix (Dilib)
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