The AAT/WFI survey of the Monoceros Ring and Canis Major dwarf galaxy – I. From l= (193–276)°
Identifieur interne : 001073 ( Istex/Corpus ); précédent : 001072; suivant : 001074The 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 ] ; 2007-04-11.
English descriptors
- KwdEn :
- 2mass, 2mass catalogue, Ared disc, Bellazzini, Besan, Carraro, Cent completeness, Cent completeness level, Centre, Clump stars, Cmds, Colour, Completeness, Completeness estimate, Conn, Corresponding besan, Data quality, Detection, Disc, Distance estimate, Distance estimates, Distant spiral, Dominant sequence, Ducial, Ducial sequence, Ducial sequences, Ducials, Dust extinction, Dwarf, Dwarf galaxies, Dwarf galaxy, Eld, Empty symbols, Fainter, Fainter magnitudes, Fainter sequence, February, Galactic, Galactic centre, Galactic components, Galactic disc, Galactic longitude, Galactic plane, Galactic warp, Galaxy, Grillmair, Gure, Halo, Heliocentric, Heliocentric distance, Hess, Hess plot, Hess plots, Ibata, Irwin, January, Journal compilation, Lled symbols, Longitude, Lower panel, Main sequence, Main sequences, Mnras, Momany, Monoceros ring, More stars, Newberg, Number density, Outer disc, Outer spiral, Overdensity, Pointings, Present paper, Present survey, Ratio estimate, Robin, Scenario, Sdss, Spiral arms, Square root, Star, Star symbols, Stellar, Stellar densities, Stellar density, Stellar populations, Strong sequence, Synthetic galaxy model, Tanvir, Thick disc, Thin disc, Tidal, Tted, Vega system, Vertical lines, Warp, Yusifov.
- Teeft :
- 2mass, 2mass catalogue, Ared disc, Bellazzini, Besan, Carraro, Cent completeness, Cent completeness level, Centre, Clump stars, Cmds, Colour, Completeness, Completeness estimate, Conn, Corresponding besan, Data quality, Detection, Disc, Distance estimate, Distance estimates, Distant spiral, Dominant sequence, Ducial, Ducial sequence, Ducial sequences, Ducials, Dust extinction, Dwarf, Dwarf galaxies, Dwarf galaxy, Eld, Empty symbols, Fainter, Fainter magnitudes, Fainter sequence, February, Galactic, Galactic centre, Galactic components, Galactic disc, Galactic longitude, Galactic plane, Galactic warp, Galaxy, Grillmair, Gure, Halo, Heliocentric, Heliocentric distance, Hess, Hess plot, Hess plots, Ibata, Irwin, January, Journal compilation, Lled symbols, Longitude, Lower panel, Main sequence, Main sequences, Mnras, Momany, Monoceros ring, More stars, Newberg, Number density, Outer disc, Outer spiral, Overdensity, Pointings, Present paper, Present survey, Ratio estimate, Robin, Scenario, Sdss, Spiral arms, Square root, Star, Star symbols, Stellar, Stellar densities, Stellar density, Stellar populations, Strong sequence, Synthetic galaxy model, Tanvir, Thick disc, Thin disc, Tidal, Tted, Vega system, Vertical lines, Warp, Yusifov.
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.
Url:
DOI: 10.1111/j.1365-2966.2007.11503.x
Links to Exploration step
ISTEX:588B3A4D79438292A0795B27F32EF0CC09B2B3EDLe document en format XML
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From <hi rend="italic">l</hi>= (193–276)°</title><author><name sortKey="Conn, Blair C" sort="Conn, Blair C" uniqKey="Conn B" first="Blair C." last="Conn">Blair C. Conn</name><affiliation><mods:affiliation>Institute of Astronomy, School of Physics, A29 University of Sydney, NSW 2006, Australia</mods:affiliation></affiliation><affiliation><mods:affiliation>European Southern Observatory, Alonso de Cordova 3107, Vitacura, Santiago, Chile</mods:affiliation></affiliation><affiliation><mods:affiliation>E-mail: bconn@physics.usyd.edu.au</mods:affiliation></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><mods:affiliation>Institute of Astronomy, School of Physics, A29 University of Sydney, NSW 2006, Australia</mods:affiliation></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><mods:affiliation>Institute of Astronomy, School of Physics, A29 University of Sydney, NSW 2006, Australia</mods:affiliation></affiliation></author><author><name sortKey="Gil Erino, Rodrigo" sort="Gil Erino, Rodrigo" uniqKey="Gil Erino R" first="Rodrigo" last="Gil-Merino">Rodrigo Gil-Merino</name><affiliation><mods:affiliation>Institute of Astronomy, School of Physics, A29 University of Sydney, NSW 2006, Australia</mods:affiliation></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><mods:affiliation>Institute of Astronomy, Madingley Road, Cambridge CB3 0HA</mods:affiliation></affiliation></author><author><name sortKey="Ibata, Rodrigo A" sort="Ibata, Rodrigo A" uniqKey="Ibata R" first="Rodrigo A." last="Ibata">Rodrigo A. 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Tuntsov</name><affiliation><mods:affiliation>Institute of Astronomy, School of Physics, A29 University of Sydney, NSW 2006, Australia</mods:affiliation></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. 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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><istex><corpusName>wiley</corpusName><keywords><teeft><json:string>eld</json:string><json:string>overdensity</json:string><json:string>ducial</json:string><json:string>besan</json:string><json:string>cmds</json:string><json:string>mnras</json:string><json:string>dwarf galaxy</json:string><json:string>newberg</json:string><json:string>galactic</json:string><json:string>strong sequence</json:string><json:string>journal compilation</json:string><json:string>fainter</json:string><json:string>ibata</json:string><json:string>sdss</json:string><json:string>galaxy</json:string><json:string>ducial sequence</json:string><json:string>january</json:string><json:string>gure</json:string><json:string>grillmair</json:string><json:string>colour</json:string><json:string>synthetic galaxy model</json:string><json:string>galactic plane</json:string><json:string>stellar</json:string><json:string>distance estimates</json:string><json:string>corresponding besan</json:string><json:string>stellar density</json:string><json:string>yusifov</json:string><json:string>momany</json:string><json:string>spiral arms</json:string><json:string>present survey</json:string><json:string>tted</json:string><json:string>hess plot</json:string><json:string>thick disc</json:string><json:string>bellazzini</json:string><json:string>heliocentric distance</json:string><json:string>pointings</json:string><json:string>irwin</json:string><json:string>cent completeness</json:string><json:string>main sequence</json:string><json:string>distance estimate</json:string><json:string>galactic disc</json:string><json:string>hess</json:string><json:string>dwarf</json:string><json:string>heliocentric</json:string><json:string>thin disc</json:string><json:string>completeness estimate</json:string><json:string>carraro</json:string><json:string>2mass</json:string><json:string>longitude</json:string><json:string>ducials</json:string><json:string>hess plots</json:string><json:string>star symbols</json:string><json:string>tanvir</json:string><json:string>february</json:string><json:string>dominant sequence</json:string><json:string>galactic warp</json:string><json:string>disc</json:string><json:string>tidal</json:string><json:string>warp</json:string><json:string>cent completeness level</json:string><json:string>dwarf galaxies</json:string><json:string>square root</json:string><json:string>monoceros ring</json:string><json:string>ared disc</json:string><json:string>main sequences</json:string><json:string>empty symbols</json:string><json:string>stellar populations</json:string><json:string>lower panel</json:string><json:string>fainter sequence</json:string><json:string>dust extinction</json:string><json:string>galactic longitude</json:string><json:string>distant spiral</json:string><json:string>conn</json:string><json:string>completeness</json:string><json:string>scenario</json:string><json:string>halo</json:string><json:string>detection</json:string><json:string>more stars</json:string><json:string>outer spiral</json:string><json:string>2mass catalogue</json:string><json:string>vega system</json:string><json:string>ducial sequences</json:string><json:string>present paper</json:string><json:string>fainter magnitudes</json:string><json:string>ratio estimate</json:string><json:string>lled symbols</json:string><json:string>outer disc</json:string><json:string>galactic centre</json:string><json:string>number density</json:string><json:string>vertical lines</json:string><json:string>stellar densities</json:string><json:string>data quality</json:string><json:string>clump stars</json:string><json:string>galactic components</json:string><json:string>centre</json:string><json:string>robin</json:string><json:string>star</json:string></teeft></keywords><author><json:item><name>Blair C. Conn</name><affiliations><json:string>Institute of Astronomy, School of Physics, A29 University of Sydney, NSW 2006, Australia</json:string><json:string>European Southern Observatory, Alonso de Cordova 3107, Vitacura, Santiago, Chile</json:string><json:string>E-mail: bconn@physics.usyd.edu.au</json:string></affiliations></json:item><json:item><name>Richard R. Lane</name><affiliations><json:string>Institute of Astronomy, School of Physics, A29 University of Sydney, NSW 2006, Australia</json:string></affiliations></json:item><json:item><name>Geraint F. Lewis</name><affiliations><json:string>Institute of Astronomy, School of Physics, A29 University of Sydney, NSW 2006, Australia</json:string></affiliations></json:item><json:item><name>Rodrigo Gil‐Merino</name><affiliations><json:string>Institute of Astronomy, School of Physics, A29 University of Sydney, NSW 2006, Australia</json:string></affiliations></json:item><json:item><name>Mike J. Irwin</name><affiliations><json:string>Institute of Astronomy, Madingley Road, Cambridge CB3 0HA</json:string></affiliations></json:item><json:item><name>Rodrigo A. Ibata</name><affiliations><json:string>Observatoire de Strasbourg, 11 rue de l'Université, F‐67000 Strasbourg, France</json:string></affiliations></json:item><json:item><name>Nicolas F. Martin</name><affiliations><json:string>Observatoire de Strasbourg, 11 rue de l'Université, F‐67000 Strasbourg, France</json:string></affiliations></json:item><json:item><name>Michele Bellazzini</name><affiliations><json:string>INAF – Osservatorio Astronomico di Bologna, Via Ranzani 1, 40127 Bologna, Italy</json:string></affiliations></json:item><json:item><name>Robert Sharp</name><affiliations><json:string>Anglo‐Australian Observatory, Epping, NSW 1710, Australia</json:string></affiliations></json:item><json:item><name>Artem V. Tuntsov</name><affiliations><json:string>Institute of Astronomy, School of Physics, A29 University of Sydney, NSW 2006, Australia</json:string></affiliations></json:item><json:item><name>Annette M. N. Ferguson</name><affiliations><json:string>Institute for Astronomy, University of Edinburgh, Royal Observatory, Blackford Hill, Edinburgh EH9 3HJ</json:string></affiliations></json:item></author><subject><json:item><lang><json:string>eng</json:string></lang><value>Galaxy: formation</value></json:item><json:item><lang><json:string>eng</json:string></lang><value>Galaxy: structure</value></json:item><json:item><lang><json:string>eng</json:string></lang><value>galaxies: interactions</value></json:item></subject><articleId><json:string>MNR11503</json:string></articleId><arkIstex>ark:/67375/WNG-4LZ1GMN2-R</arkIstex><language><json:string>eng</json:string></language><originalGenre><json:string>article</json:string></originalGenre><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.</abstract><qualityIndicators><score>10</score><pdfWordCount>16442</pdfWordCount><pdfCharCount>84392</pdfCharCount><pdfVersion>1.3</pdfVersion><pdfPageCount>21</pdfPageCount><pdfPageSize>612 x 792 pts (letter)</pdfPageSize><refBibsNative>true</refBibsNative><abstractWordCount>305</abstractWordCount><abstractCharCount>1906</abstractCharCount><keywordCount>3</keywordCount></qualityIndicators><title>The AAT/WFI survey of the Monoceros Ring and Canis Major dwarf galaxy – I. 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(2003)</json:string><json:string>Irwin & Lewis 2001</json:string><json:string>Momany et al. 2006</json:string><json:string>Corredoira et al. 2002</json:string><json:string>Martin et al. 2004a</json:string><json:string>Momany et al. (2006)</json:string><json:string>Lewis et al. 2004</json:string><json:string>Ibata et al. 2001</json:string><json:string>Zucker et al. (2006)</json:string><json:string>Skrutskie et al. 2006</json:string><json:string>Martin et al. (2004b)</json:string><json:string>Moitinho et al. (2006)</json:string><json:string>Gunn (1994)</json:string><json:string>Martin et al. 2006</json:string><json:string>Corredoira et al. (2002)</json:string><json:string>Newberg et al. (2002)</json:string><json:string>Ibata, Gilmore & Irwin 1994</json:string><json:string>B. C. Conn et al.</json:string><json:string>Conn et al. (2005a)</json:string><json:string>Zucker et al. 2004</json:string><json:string>Adelman-McCarthy et al. 2006</json:string><json:string>Carraro et al. 2005</json:string><json:string>Yanny et al. (2003)</json:string><json:string>Martin et al. (2005)</json:string><json:string>Belokurov et al. (2006a)</json:string><json:string>Abadi et al. 2003a,b</json:string><json:string>Robin et al. (1996, 2000)</json:string><json:string>Conn et al. (2005b)</json:string><json:string>Moitinho et al. 2006</json:string><json:string>Momany et al. (2004)</json:string><json:string>Rocha-Pinto et al. 2004</json:string><json:string>Robin et al. 2003</json:string><json:string>Huxor et al. 2005</json:string><json:string>Ferguson et al. (2002)</json:string><json:string>Martin et al. (2006)</json:string><json:string>Bellazzini et al. (2007)</json:string><json:string>Newberg et al. 2002</json:string><json:string>Bellazzini et al. 2006</json:string><json:string>Ibata et al. 2003</json:string><json:string>Carraro et al. (2005)</json:string><json:string>Grillmair (2006b)</json:string><json:string>Schlegel et al. 1998</json:string><json:string>Conn et al. 2005a</json:string></ref_bibl><bibl></bibl></unitex></namedEntities><ark><json:string>ark:/67375/WNG-4LZ1GMN2-R</json:string></ark><categories><wos><json:string>1 - science</json:string><json:string>2 - astronomy & astrophysics</json:string></wos><scienceMetrix><json:string>1 - natural sciences</json:string><json:string>2 - physics & astronomy</json:string><json:string>3 - astronomy & astrophysics</json:string></scienceMetrix><scopus><json:string>1 - Physical Sciences</json:string><json:string>2 - Earth and Planetary Sciences</json:string><json:string>3 - Space and Planetary Science</json:string><json:string>1 - Physical Sciences</json:string><json:string>2 - Physics and Astronomy</json:string><json:string>3 - Astronomy and Astrophysics</json:string></scopus><inist><json:string>1 - sciences appliquees, technologies et medecines</json:string><json:string>2 - sciences exactes et technologie</json:string><json:string>3 - terre, ocean, espace</json:string><json:string>4 - astronomie</json:string></inist></categories><publicationDate>2007</publicationDate><copyrightDate>2007</copyrightDate><doi><json:string>10.1111/j.1365-2966.2007.11503.x</json:string></doi><id>588B3A4D79438292A0795B27F32EF0CC09B2B3ED</id><score>1</score><fulltext><json:item><extension>pdf</extension><original>true</original><mimetype>application/pdf</mimetype><uri>https://api.istex.fr/document/588B3A4D79438292A0795B27F32EF0CC09B2B3ED/fulltext/pdf</uri></json:item><json:item><extension>zip</extension><original>false</original><mimetype>application/zip</mimetype><uri>https://api.istex.fr/document/588B3A4D79438292A0795B27F32EF0CC09B2B3ED/fulltext/zip</uri></json:item><istex:fulltextTEI uri="https://api.istex.fr/document/588B3A4D79438292A0795B27F32EF0CC09B2B3ED/fulltext/tei"><teiHeader><fileDesc><titleStmt><title level="a" type="main">The AAT/WFI survey of the Monoceros Ring and Canis Major dwarf galaxy – I. 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From l= (193–276)°</title><author xml:id="author-0000" role="corresp"><persName><forename type="first">Blair C.</forename><surname>Conn</surname></persName><affiliation>Institute of Astronomy, School of Physics, A29 University of Sydney, NSW 2006, Australia<address><country key="AU"></country></address></affiliation><affiliation>European Southern Observatory, Alonso de Cordova 3107, Vitacura, Santiago, Chile<address><country key="CL"></country></address></affiliation><affiliation>E‐mail: bconn@physics.usyd.edu.au</affiliation></author><author xml:id="author-0001"><persName><forename type="first">Richard R.</forename><surname>Lane</surname></persName><affiliation>Institute of Astronomy, School of Physics, A29 University of Sydney, NSW 2006, Australia<address><country key="AU"></country></address></affiliation></author><author xml:id="author-0002"><persName><forename type="first">Geraint F.</forename><surname>Lewis</surname></persName><affiliation>Institute of Astronomy, School of Physics, A29 University of Sydney, NSW 2006, Australia<address><country key="AU"></country></address></affiliation></author><author xml:id="author-0003"><persName><forename type="first">Rodrigo</forename><surname>Gil‐Merino</surname></persName><affiliation>Institute of Astronomy, School of Physics, A29 University of Sydney, NSW 2006, Australia<address><country key="AU"></country></address></affiliation></author><author xml:id="author-0004"><persName><forename type="first">Mike J.</forename><surname>Irwin</surname></persName><affiliation>Institute of Astronomy, Madingley Road, Cambridge CB3 0HA</affiliation></author><author xml:id="author-0005"><persName><forename type="first">Rodrigo A.</forename><surname>Ibata</surname></persName><affiliation>Observatoire de Strasbourg, 11 rue de l'Université, F‐67000 Strasbourg, France<address><country key="FR"></country></address></affiliation></author><author xml:id="author-0006"><persName><forename type="first">Nicolas F.</forename><surname>Martin</surname></persName><affiliation>Observatoire de Strasbourg, 11 rue de l'Université, F‐67000 Strasbourg, France<address><country key="FR"></country></address></affiliation></author><author xml:id="author-0007"><persName><forename type="first">Michele</forename><surname>Bellazzini</surname></persName><affiliation>INAF – Osservatorio Astronomico di Bologna, Via Ranzani 1, 40127 Bologna, Italy<address><country key="IT"></country></address></affiliation></author><author xml:id="author-0008"><persName><forename type="first">Robert</forename><surname>Sharp</surname></persName><affiliation>Anglo‐Australian Observatory, Epping, NSW 1710, Australia<address><country key="AU"></country></address></affiliation></author><author xml:id="author-0009"><persName><forename type="first">Artem V.</forename><surname>Tuntsov</surname></persName><affiliation>Institute of Astronomy, School of Physics, A29 University of Sydney, NSW 2006, Australia<address><country key="AU"></country></address></affiliation></author><author xml:id="author-0010"><persName><forename type="first">Annette M. 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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.</p></abstract><textClass><keywords xml:lang="en"><term xml:id="k1">Galaxy: formation</term><term xml:id="k2">Galaxy: structure</term><term xml:id="k3">galaxies: interactions</term></keywords><keywords rend="tocHeading1"><term>Papers</term></keywords></textClass><langUsage><language ident="en"></language></langUsage></profileDesc></teiHeader></istex:fulltextTEI><json:item><extension>txt</extension><original>false</original><mimetype>text/plain</mimetype><uri>https://api.istex.fr/document/588B3A4D79438292A0795B27F32EF0CC09B2B3ED/fulltext/txt</uri></json:item></fulltext><metadata><istex:metadataXml wicri:clean="Wiley, elements deleted: body"><istex:xmlDeclaration>version="1.0" encoding="UTF-8" standalone="yes"</istex:xmlDeclaration><istex:document><component version="2.0" type="serialArticle" xml:lang="en"><header><publicationMeta level="product"><publisherInfo><publisherName>Blackwell Publishing Ltd</publisherName><publisherLoc>Oxford, UK</publisherLoc></publisherInfo><doi origin="wiley" registered="yes">10.1111/(ISSN)1365-2966</doi><issn type="print">0035-8711</issn><issn type="electronic">1365-2966</issn><idGroup><id type="product" value="MNR"></id><id type="publisherDivision" value="ST"></id></idGroup><titleGroup><title type="main" sort="MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY">Monthly Notices of the Royal Astronomical Society</title></titleGroup></publicationMeta><publicationMeta level="part" position="04003"><doi origin="wiley">10.1111/mnr.2007.376.issue-3</doi><numberingGroup><numbering type="journalVolume" number="376">376</numbering><numbering type="journalIssue" number="3">3</numbering></numberingGroup><coverDate startDate="2007-04-11">April 2007</coverDate></publicationMeta><publicationMeta level="unit" type="article" position="2" status="forIssue"><doi origin="wiley">10.1111/j.1365-2966.2007.11503.x</doi><idGroup><id type="unit" value="MNR11503"></id></idGroup><countGroup><count type="pageTotal" number="21"></count></countGroup><titleGroup><title type="tocHeading1">Papers</title></titleGroup><eventGroup><event type="firstOnline" date="2007-03-06"></event><event type="publishedOnlineFinalForm" date="2007-03-16"></event><event type="xmlConverted" agent="Converter:BPG_TO_WML3G version:2.3.10 mode:FullText source:FullText result:FullText" date="2010-07-01"></event><event type="xmlConverted" agent="Converter:WILEY_ML3G_TO_WILEY_ML3GV2 version:3.8.8" date="2014-02-02"></event><event type="xmlConverted" agent="Converter:WML3G_To_WML3G version:4.1.7 mode:FullText,remove_FC" date="2014-10-31"></event></eventGroup><numberingGroup><numbering type="pageFirst" number="939">939</numbering><numbering type="pageLast" number="959">959</numbering></numberingGroup><correspondenceTo>
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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.</p></abstract></abstractGroup></contentMeta></header></component></istex:document></istex:metadataXml><mods version="3.6"><titleInfo lang="en"><title>The AAT/WFI survey of the Monoceros Ring and Canis Major dwarf galaxy – I. From l= (193–276)°</title></titleInfo><titleInfo type="abbreviated" lang="en"><title>The AAT/WFI survey – I. From l= (193–276)°</title></titleInfo><titleInfo type="alternative" contentType="CDATA" lang="en"><title>The AAT/WFI survey of the Monoceros Ring and Canis Major dwarf galaxy – I. From l= (193–276)°</title></titleInfo><name type="personal"><namePart type="given">Blair C.</namePart><namePart type="family">Conn</namePart><affiliation>Institute of Astronomy, School of Physics, A29 University of Sydney, NSW 2006, Australia</affiliation><affiliation>European Southern Observatory, Alonso de Cordova 3107, Vitacura, Santiago, Chile</affiliation><affiliation>E-mail: bconn@physics.usyd.edu.au</affiliation><role><roleTerm type="text">author</roleTerm></role></name><name type="personal"><namePart type="given">Richard R.</namePart><namePart type="family">Lane</namePart><affiliation>Institute of Astronomy, School of Physics, A29 University of Sydney, NSW 2006, Australia</affiliation><role><roleTerm type="text">author</roleTerm></role></name><name type="personal"><namePart type="given">Geraint F.</namePart><namePart type="family">Lewis</namePart><affiliation>Institute of Astronomy, School of Physics, A29 University of Sydney, NSW 2006, Australia</affiliation><role><roleTerm type="text">author</roleTerm></role></name><name type="personal"><namePart type="given">Rodrigo</namePart><namePart type="family">Gil‐Merino</namePart><affiliation>Institute of Astronomy, School of Physics, A29 University of Sydney, NSW 2006, Australia</affiliation><role><roleTerm type="text">author</roleTerm></role></name><name type="personal"><namePart type="given">Mike J.</namePart><namePart type="family">Irwin</namePart><affiliation>Institute of Astronomy, Madingley Road, Cambridge CB3 0HA</affiliation><role><roleTerm type="text">author</roleTerm></role></name><name type="personal"><namePart type="given">Rodrigo A.</namePart><namePart type="family">Ibata</namePart><affiliation>Observatoire de Strasbourg, 11 rue de l'Université, F‐67000 Strasbourg, France</affiliation><role><roleTerm type="text">author</roleTerm></role></name><name type="personal"><namePart type="given">Nicolas F.</namePart><namePart type="family">Martin</namePart><affiliation>Observatoire de Strasbourg, 11 rue de l'Université, F‐67000 Strasbourg, France</affiliation><role><roleTerm type="text">author</roleTerm></role></name><name type="personal"><namePart type="given">Michele</namePart><namePart type="family">Bellazzini</namePart><affiliation>INAF – Osservatorio Astronomico di Bologna, Via Ranzani 1, 40127 Bologna, Italy</affiliation><role><roleTerm type="text">author</roleTerm></role></name><name type="personal"><namePart type="given">Robert</namePart><namePart type="family">Sharp</namePart><affiliation>Anglo‐Australian Observatory, Epping, NSW 1710, Australia</affiliation><role><roleTerm type="text">author</roleTerm></role></name><name type="personal"><namePart type="given">Artem V.</namePart><namePart type="family">Tuntsov</namePart><affiliation>Institute of Astronomy, School of Physics, A29 University of Sydney, NSW 2006, Australia</affiliation><role><roleTerm type="text">author</roleTerm></role></name><name type="personal"><namePart type="given">Annette M. N.</namePart><namePart type="family">Ferguson</namePart><affiliation>Institute for Astronomy, University of Edinburgh, Royal Observatory, Blackford Hill, Edinburgh EH9 3HJ</affiliation><role><roleTerm type="text">author</roleTerm></role></name><typeOfResource>text</typeOfResource><genre type="article" displayLabel="article" authority="ISTEX" authorityURI="https://content-type.data.istex.fr" valueURI="https://content-type.data.istex.fr/ark:/67375/XTP-6N5SZHKN-D">article</genre><originInfo><publisher>Blackwell Publishing Ltd</publisher><place><placeTerm type="text">Oxford, UK</placeTerm></place><dateIssued encoding="w3cdtf">2007-04-11</dateIssued><edition>Accepted 2007 January 15. Received 2007 January 12; in original form 2006 October 13</edition><copyrightDate encoding="w3cdtf">2007</copyrightDate></originInfo><language><languageTerm type="code" authority="rfc3066">en</languageTerm><languageTerm type="code" authority="iso639-2b">eng</languageTerm></language><physicalDescription><extent unit="figures">33</extent><extent unit="tables">3</extent><extent unit="formulas">187</extent><extent unit="references">58</extent><extent unit="linksCrossRef">280</extent></physicalDescription><abstract 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.</abstract><subject lang="en"><genre>keywords</genre><topic>Galaxy: formation</topic><topic>Galaxy: structure</topic><topic>galaxies: interactions</topic></subject><relatedItem type="host"><titleInfo><title>Monthly Notices of the Royal Astronomical Society</title></titleInfo><genre type="journal" authority="ISTEX" authorityURI="https://publication-type.data.istex.fr" valueURI="https://publication-type.data.istex.fr/ark:/67375/JMC-0GLKJH51-B">journal</genre><identifier type="ISSN">0035-8711</identifier><identifier type="eISSN">1365-2966</identifier><identifier type="DOI">10.1111/(ISSN)1365-2966</identifier><identifier type="PublisherID">MNR</identifier><part><date>2007</date><detail type="volume"><caption>vol.</caption><number>376</number></detail><detail type="issue"><caption>no.</caption><number>3</number></detail><extent unit="pages"><start>939</start><end>959</end><total>21</total></extent></part></relatedItem><identifier type="istex">588B3A4D79438292A0795B27F32EF0CC09B2B3ED</identifier><identifier type="ark">ark:/67375/WNG-4LZ1GMN2-R</identifier><identifier type="DOI">10.1111/j.1365-2966.2007.11503.x</identifier><identifier type="ArticleID">MNR11503</identifier><recordInfo><recordContentSource authority="ISTEX" authorityURI="https://loaded-corpus.data.istex.fr" valueURI="https://loaded-corpus.data.istex.fr/ark:/67375/XBH-L0C46X92-X">wiley</recordContentSource><recordOrigin>Blackwell Publishing Ltd</recordOrigin></recordInfo></mods><json:item><extension>json</extension><original>false</original><mimetype>application/json</mimetype><uri>https://api.istex.fr/document/588B3A4D79438292A0795B27F32EF0CC09B2B3ED/metadata/json</uri></json:item></metadata><serie></serie></istex></record>Pour manipuler ce document sous Unix (Dilib)
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