The Isaac Newton Telescope Wide Field Camera survey of the Monoceros Ring: accretion origin or Galactic anomaly?
Identifieur interne : 000F73 ( Istex/Corpus ); précédent : 000F72; suivant : 000F74The Isaac Newton Telescope Wide Field Camera survey of the Monoceros Ring: accretion origin or Galactic anomaly?
Auteurs : Blair C. Conn ; Geraint F. Lewis ; Mike J. Irwin ; Rodrigo A. Ibata ; Annette M. N. Ferguson ; Nial Tanvir ; Jonathan M. IrwinSource :
- Monthly Notices of the Royal Astronomical Society [ 0035-8711 ] ; 2005-09.
English descriptors
- KwdEn :
- Accreting dwarf galaxy, Accretion, Accretion event, Arrubia, Base position, Bulk halo, Camera survey, Canary islands, Canis, Cent completeness, Cmds, Completeness curve, Corresponding model plot, Dark matter, Detection, Disc, Distance estimates, Dwarf, Dwarf galaxy, Eld, Field camera, Field camera survey, Galactic, Galactic anticentre, Galactic centre, Galactic component, Galactic components, Galactic disc, Galactic equator, Galactic features, Galactic halo, Galactic longitude, Galactic plane, Galactic population, Galactic view, Galactic warp, Galactocentric, Galactocentric distance, Galactocentric distance estimates, Galactocentric distances, Galaxy, Globular clusters, Gures, Halo, Halo component, Heliocentric, Heliocentric distance, Heliocentric distances, Hess, Hess plot, Hess plots, Ibata, Inner ring, Irwin, Irwin lewis, Isaac newton telescope, Kinematic survey, Local density, Longitude, Lower panels, Lower plot, Lower side, Magnitude completeness, Magnitude range, Main sequence, Main sequences, Majewski, Milky, Mnras, Model cmds, Monoceros, Monoceros ring, Newberg, Numerical simulations, Obvious feature, Open clusters, Opposite side, Outer ring, Overdensity, Overlap regions, Overlay, Panels show, Potential detections, Prograde, Prograde orbit, Real data, Redward, Redward trend, Robin, Robin creze, Sagittarius dwarf galaxy, Same manner, Sdss, Solar circle, Stellar, Stellar population, Style overlay, Symmetric pairs, Synthetic cmds, Synthetic galaxy model, Synthetic model, Systematic errors, Tentative detection, Tentative detections, Thick disc, Thin disc, Tidal, Tidal arms, Tidal debris, Tidal stream, Tidal streams, Total area, Triand, Triand structure, Various components, Velocity dispersion, Warp, Yanny.
- Teeft :
- Accreting dwarf galaxy, Accretion, Accretion event, Arrubia, Base position, Bulk halo, Camera survey, Canary islands, Canis, Cent completeness, Cmds, Completeness curve, Corresponding model plot, Dark matter, Detection, Disc, Distance estimates, Dwarf, Dwarf galaxy, Eld, Field camera, Field camera survey, Galactic, Galactic anticentre, Galactic centre, Galactic component, Galactic components, Galactic disc, Galactic equator, Galactic features, Galactic halo, Galactic longitude, Galactic plane, Galactic population, Galactic view, Galactic warp, Galactocentric, Galactocentric distance, Galactocentric distance estimates, Galactocentric distances, Galaxy, Globular clusters, Gures, Halo, Halo component, Heliocentric, Heliocentric distance, Heliocentric distances, Hess, Hess plot, Hess plots, Ibata, Inner ring, Irwin, Irwin lewis, Isaac newton telescope, Kinematic survey, Local density, Longitude, Lower panels, Lower plot, Lower side, Magnitude completeness, Magnitude range, Main sequence, Main sequences, Majewski, Milky, Mnras, Model cmds, Monoceros, Monoceros ring, Newberg, Numerical simulations, Obvious feature, Open clusters, Opposite side, Outer ring, Overdensity, Overlap regions, Overlay, Panels show, Potential detections, Prograde, Prograde orbit, Real data, Redward, Redward trend, Robin, Robin creze, Sagittarius dwarf galaxy, Same manner, Sdss, Solar circle, Stellar, Stellar population, Style overlay, Symmetric pairs, Synthetic cmds, Synthetic galaxy model, Synthetic model, Systematic errors, Tentative detection, Tentative detections, Thick disc, Thin disc, Tidal, Tidal arms, Tidal debris, Tidal stream, Tidal streams, Total area, Triand, Triand structure, Various components, Velocity dispersion, Warp, Yanny.
Abstract
We present the results of a wide‐field camera survey of the stars in the Monoceros Ring, thought to be an additional structure in the Milky Way of unknown origin. Lying roughly in the plane of the Milky Way, this may represent a unique equatorial accretion event which is contributing to the thick disc of the Galaxy. Alternatively, the Monoceros Ring may be a natural part of the disc formation process. With 10 pointings in symmetric pairs above and below the plane of the Galaxy, this survey spans 90° about the equator of the Milky Way. Signatures of the stream of stars were detected in three fields, (l, b) = (118°, +16°) and (150°, +15°) plus a more tentative detection at (150°, −15°). Galactocentric distance estimates to these structures gave ∼17, ∼17, and ∼13 kpc, respectively. The Monoceros Ring seems to be present on both sides of the Galactic plane, in a form different from that of the Galactic warp, suggestive of a tidal origin with streams multiply wrapping the Galaxy. A new model of the stream has shown a strong coincidence with our results and has also provided the opportunity to make several more detections in fields in which the stream is less significant. The confirmed detection at (l, b) = (123°, −19°) at ∼14, kpc from the Galactic Centre allows a re‐examination revealing a tentative new detection with a Galactocentric distance of ∼21 kpc. These detections also lie very close to the newly discovered structure in Triangulum–Andromedae hinting at a link between the two. The remaining six fields are apparently non‐detections although in light of these new models, closer inspection reveals tentative structure. With the overdensity of M giant stars in Canis Major being claimed both as a progenitor to the Monoceros Ring and alternatively a manifestation of the Milky Way warp, much is still unknown concerning this structure and its connection to the Monoceros Ring. Further constraints are needed for the numerical simulations to adequately resolve the increasingly complex view of this structure.
Url:
DOI: 10.1111/j.1365-2966.2005.09311.x
Links to Exploration step
ISTEX:536CB4E7BD4119712CEEEE2235992BB2CBB25374Le document en format XML
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Conn</name><affiliation><mods:affiliation>Institute of Astronomy, School of Physics, A29, University of Sydney, NSW 2006, Australia</mods:affiliation></affiliation><affiliation><mods:affiliation>E-mail: bconn@physics.usyd.edu.au</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><affiliation><mods:affiliation>E-mail: bconn@physics.usyd.edu.au</mods:affiliation></affiliation></author><author><name sortKey="Irwin, Mike J" sort="Irwin, Mike J" uniqKey="Irwin M" first="Mike J." last="Irwin">Mike J. 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Telephone (0131) 226 7232 Fax (0131) 226 3803 </pubPlace><date type="published" when="2005-09">2005-09</date></imprint><idno type="ISSN">0035-8711</idno></series></biblStruct></sourceDesc><seriesStmt><idno type="ISSN">0035-8711</idno></seriesStmt></fileDesc><profileDesc><textClass><keywords scheme="KwdEn" xml:lang="en"><term>Accreting dwarf galaxy</term><term>Accretion</term><term>Accretion event</term><term>Arrubia</term><term>Base position</term><term>Bulk halo</term><term>Camera survey</term><term>Canary islands</term><term>Canis</term><term>Cent completeness</term><term>Cmds</term><term>Completeness curve</term><term>Corresponding model plot</term><term>Dark matter</term><term>Detection</term><term>Disc</term><term>Distance estimates</term><term>Dwarf</term><term>Dwarf galaxy</term><term>Eld</term><term>Field camera</term><term>Field camera survey</term><term>Galactic</term><term>Galactic anticentre</term><term>Galactic centre</term><term>Galactic component</term><term>Galactic components</term><term>Galactic disc</term><term>Galactic equator</term><term>Galactic features</term><term>Galactic halo</term><term>Galactic longitude</term><term>Galactic plane</term><term>Galactic population</term><term>Galactic view</term><term>Galactic warp</term><term>Galactocentric</term><term>Galactocentric distance</term><term>Galactocentric distance estimates</term><term>Galactocentric distances</term><term>Galaxy</term><term>Globular clusters</term><term>Gures</term><term>Halo</term><term>Halo component</term><term>Heliocentric</term><term>Heliocentric distance</term><term>Heliocentric distances</term><term>Hess</term><term>Hess plot</term><term>Hess plots</term><term>Ibata</term><term>Inner ring</term><term>Irwin</term><term>Irwin lewis</term><term>Isaac newton telescope</term><term>Kinematic survey</term><term>Local density</term><term>Longitude</term><term>Lower panels</term><term>Lower plot</term><term>Lower side</term><term>Magnitude completeness</term><term>Magnitude range</term><term>Main sequence</term><term>Main sequences</term><term>Majewski</term><term>Milky</term><term>Mnras</term><term>Model cmds</term><term>Monoceros</term><term>Monoceros ring</term><term>Newberg</term><term>Numerical simulations</term><term>Obvious feature</term><term>Open clusters</term><term>Opposite side</term><term>Outer ring</term><term>Overdensity</term><term>Overlap regions</term><term>Overlay</term><term>Panels show</term><term>Potential detections</term><term>Prograde</term><term>Prograde orbit</term><term>Real data</term><term>Redward</term><term>Redward trend</term><term>Robin</term><term>Robin creze</term><term>Sagittarius dwarf galaxy</term><term>Same manner</term><term>Sdss</term><term>Solar circle</term><term>Stellar</term><term>Stellar population</term><term>Style overlay</term><term>Symmetric pairs</term><term>Synthetic cmds</term><term>Synthetic galaxy model</term><term>Synthetic model</term><term>Systematic errors</term><term>Tentative detection</term><term>Tentative detections</term><term>Thick disc</term><term>Thin disc</term><term>Tidal</term><term>Tidal arms</term><term>Tidal debris</term><term>Tidal stream</term><term>Tidal streams</term><term>Total area</term><term>Triand</term><term>Triand structure</term><term>Various components</term><term>Velocity dispersion</term><term>Warp</term><term>Yanny</term></keywords><keywords scheme="Teeft" xml:lang="en"><term>Accreting dwarf galaxy</term><term>Accretion</term><term>Accretion event</term><term>Arrubia</term><term>Base position</term><term>Bulk halo</term><term>Camera survey</term><term>Canary islands</term><term>Canis</term><term>Cent completeness</term><term>Cmds</term><term>Completeness curve</term><term>Corresponding model plot</term><term>Dark matter</term><term>Detection</term><term>Disc</term><term>Distance estimates</term><term>Dwarf</term><term>Dwarf galaxy</term><term>Eld</term><term>Field camera</term><term>Field camera survey</term><term>Galactic</term><term>Galactic anticentre</term><term>Galactic centre</term><term>Galactic component</term><term>Galactic components</term><term>Galactic disc</term><term>Galactic equator</term><term>Galactic features</term><term>Galactic halo</term><term>Galactic longitude</term><term>Galactic plane</term><term>Galactic population</term><term>Galactic view</term><term>Galactic warp</term><term>Galactocentric</term><term>Galactocentric distance</term><term>Galactocentric distance estimates</term><term>Galactocentric distances</term><term>Galaxy</term><term>Globular clusters</term><term>Gures</term><term>Halo</term><term>Halo component</term><term>Heliocentric</term><term>Heliocentric distance</term><term>Heliocentric distances</term><term>Hess</term><term>Hess plot</term><term>Hess plots</term><term>Ibata</term><term>Inner ring</term><term>Irwin</term><term>Irwin lewis</term><term>Isaac newton telescope</term><term>Kinematic survey</term><term>Local density</term><term>Longitude</term><term>Lower panels</term><term>Lower plot</term><term>Lower side</term><term>Magnitude completeness</term><term>Magnitude range</term><term>Main sequence</term><term>Main sequences</term><term>Majewski</term><term>Milky</term><term>Mnras</term><term>Model cmds</term><term>Monoceros</term><term>Monoceros ring</term><term>Newberg</term><term>Numerical simulations</term><term>Obvious feature</term><term>Open clusters</term><term>Opposite side</term><term>Outer ring</term><term>Overdensity</term><term>Overlap regions</term><term>Overlay</term><term>Panels show</term><term>Potential detections</term><term>Prograde</term><term>Prograde orbit</term><term>Real data</term><term>Redward</term><term>Redward trend</term><term>Robin</term><term>Robin creze</term><term>Sagittarius dwarf galaxy</term><term>Same manner</term><term>Sdss</term><term>Solar circle</term><term>Stellar</term><term>Stellar population</term><term>Style overlay</term><term>Symmetric pairs</term><term>Synthetic cmds</term><term>Synthetic galaxy model</term><term>Synthetic model</term><term>Systematic errors</term><term>Tentative detection</term><term>Tentative detections</term><term>Thick disc</term><term>Thin disc</term><term>Tidal</term><term>Tidal arms</term><term>Tidal debris</term><term>Tidal stream</term><term>Tidal streams</term><term>Total area</term><term>Triand</term><term>Triand structure</term><term>Various components</term><term>Velocity dispersion</term><term>Warp</term><term>Yanny</term></keywords></textClass></profileDesc></teiHeader><front><div type="abstract" xml:lang="en">We present the results of a wide‐field camera survey of the stars in the Monoceros Ring, thought to be an additional structure in the Milky Way of unknown origin. Lying roughly in the plane of the Milky Way, this may represent a unique equatorial accretion event which is contributing to the thick disc of the Galaxy. Alternatively, the Monoceros Ring may be a natural part of the disc formation process. With 10 pointings in symmetric pairs above and below the plane of the Galaxy, this survey spans 90° about the equator of the Milky Way. Signatures of the stream of stars were detected in three fields, (l, b) = (118°, +16°) and (150°, +15°) plus a more tentative detection at (150°, −15°). Galactocentric distance estimates to these structures gave ∼17, ∼17, and ∼13 kpc, respectively. The Monoceros Ring seems to be present on both sides of the Galactic plane, in a form different from that of the Galactic warp, suggestive of a tidal origin with streams multiply wrapping the Galaxy. A new model of the stream has shown a strong coincidence with our results and has also provided the opportunity to make several more detections in fields in which the stream is less significant. The confirmed detection at (l, b) = (123°, −19°) at ∼14, kpc from the Galactic Centre allows a re‐examination revealing a tentative new detection with a Galactocentric distance of ∼21 kpc. These detections also lie very close to the newly discovered structure in Triangulum–Andromedae hinting at a link between the two. The remaining six fields are apparently non‐detections although in light of these new models, closer inspection reveals tentative structure. With the overdensity of M giant stars in Canis Major being claimed both as a progenitor to the Monoceros Ring and alternatively a manifestation of the Milky Way warp, much is still unknown concerning this structure and its connection to the Monoceros Ring. Further constraints are needed for the numerical simulations to adequately resolve the increasingly complex view of this structure.</div></front></TEI><istex><corpusName>wiley</corpusName><keywords><teeft><json:string>eld</json:string><json:string>ibata</json:string><json:string>galactic</json:string><json:string>cmds</json:string><json:string>arrubia</json:string><json:string>mnras</json:string><json:string>galactocentric</json:string><json:string>monoceros</json:string><json:string>redward</json:string><json:string>main sequence</json:string><json:string>monoceros ring</json:string><json:string>canis</json:string><json:string>thick disc</json:string><json:string>hess plots</json:string><json:string>majewski</json:string><json:string>triand</json:string><json:string>sdss</json:string><json:string>galactocentric distance</json:string><json:string>tidal</json:string><json:string>galaxy</json:string><json:string>irwin</json:string><json:string>overdensity</json:string><json:string>dwarf galaxy</json:string><json:string>heliocentric distance</json:string><json:string>gures</json:string><json:string>heliocentric</json:string><json:string>halo</json:string><json:string>milky</json:string><json:string>newberg</json:string><json:string>halo component</json:string><json:string>prograde</json:string><json:string>yanny</json:string><json:string>hess</json:string><json:string>galactic longitude</json:string><json:string>synthetic cmds</json:string><json:string>galactic centre</json:string><json:string>galactic warp</json:string><json:string>tidal stream</json:string><json:string>galactic plane</json:string><json:string>lower panels</json:string><json:string>isaac newton telescope</json:string><json:string>redward trend</json:string><json:string>panels show</json:string><json:string>accretion event</json:string><json:string>model cmds</json:string><json:string>galactic equator</json:string><json:string>distance estimates</json:string><json:string>local density</json:string><json:string>robin</json:string><json:string>stellar</json:string><json:string>longitude</json:string><json:string>velocity dispersion</json:string><json:string>tidal debris</json:string><json:string>galactic components</json:string><json:string>heliocentric distances</json:string><json:string>stellar population</json:string><json:string>real data</json:string><json:string>tentative detections</json:string><json:string>synthetic galaxy model</json:string><json:string>overlay</json:string><json:string>dwarf</json:string><json:string>warp</json:string><json:string>numerical simulations</json:string><json:string>triand structure</json:string><json:string>accreting dwarf galaxy</json:string><json:string>galactic disc</json:string><json:string>galactic halo</json:string><json:string>irwin lewis</json:string><json:string>same manner</json:string><json:string>cent completeness</json:string><json:string>tidal streams</json:string><json:string>field camera</json:string><json:string>galactocentric distances</json:string><json:string>sagittarius dwarf galaxy</json:string><json:string>galactic features</json:string><json:string>main sequences</json:string><json:string>tentative detection</json:string><json:string>outer ring</json:string><json:string>detection</json:string><json:string>disc</json:string><json:string>accretion</json:string><json:string>kinematic survey</json:string><json:string>symmetric pairs</json:string><json:string>galactic component</json:string><json:string>thin disc</json:string><json:string>lower side</json:string><json:string>total area</json:string><json:string>hess plot</json:string><json:string>prograde orbit</json:string><json:string>field camera survey</json:string><json:string>completeness curve</json:string><json:string>obvious feature</json:string><json:string>magnitude completeness</json:string><json:string>overlap regions</json:string><json:string>globular clusters</json:string><json:string>galactic anticentre</json:string><json:string>open clusters</json:string><json:string>base position</json:string><json:string>style overlay</json:string><json:string>systematic errors</json:string><json:string>various components</json:string><json:string>camera survey</json:string><json:string>dark matter</json:string><json:string>potential detections</json:string><json:string>bulk halo</json:string><json:string>lower plot</json:string><json:string>opposite side</json:string><json:string>robin creze</json:string><json:string>tidal arms</json:string><json:string>canary islands</json:string><json:string>magnitude range</json:string><json:string>galactic population</json:string><json:string>galactic view</json:string><json:string>solar circle</json:string><json:string>inner ring</json:string><json:string>galactocentric distance estimates</json:string><json:string>corresponding model plot</json:string><json:string>synthetic model</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>E-mail: bconn@physics.usyd.edu.au</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><json:string>E-mail: bconn@physics.usyd.edu.au</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><json:string>E-mail: bconn@physics.usyd.edu.au</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><json:string>E-mail: bconn@physics.usyd.edu.au</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><json:string>E-mail: bconn@physics.usyd.edu.au</json:string></affiliations></json:item><json:item><name>Nial Tanvir</name><affiliations><json:string>Centre for Astrophysics Research, University of Hertfordshire, College Lane, Hatfield AL10 9AB</json:string><json:string>E-mail: bconn@physics.usyd.edu.au</json:string></affiliations></json:item><json:item><name>Jonathan M. Irwin</name><affiliations><json:string>Institute of Astronomy, Madingley Road, Cambridge CB3 0HA</json:string><json:string>E-mail: bconn@physics.usyd.edu.au</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>MNR9311</json:string></articleId><arkIstex>ark:/67375/WNG-XZ6R60DB-X</arkIstex><language><json:string>eng</json:string></language><originalGenre><json:string>article</json:string></originalGenre><abstract>We present the results of a wide‐field camera survey of the stars in the Monoceros Ring, thought to be an additional structure in the Milky Way of unknown origin. Lying roughly in the plane of the Milky Way, this may represent a unique equatorial accretion event which is contributing to the thick disc of the Galaxy. Alternatively, the Monoceros Ring may be a natural part of the disc formation process. With 10 pointings in symmetric pairs above and below the plane of the Galaxy, this survey spans 90° about the equator of the Milky Way. Signatures of the stream of stars were detected in three fields, (l, b) = (118°, +16°) and (150°, +15°) plus a more tentative detection at (150°, −15°). Galactocentric distance estimates to these structures gave ∼17, ∼17, and ∼13 kpc, respectively. The Monoceros Ring seems to be present on both sides of the Galactic plane, in a form different from that of the Galactic warp, suggestive of a tidal origin with streams multiply wrapping the Galaxy. A new model of the stream has shown a strong coincidence with our results and has also provided the opportunity to make several more detections in fields in which the stream is less significant. The confirmed detection at (l, b) = (123°, −19°) at ∼14, kpc from the Galactic Centre allows a re‐examination revealing a tentative new detection with a Galactocentric distance of ∼21 kpc. These detections also lie very close to the newly discovered structure in Triangulum–Andromedae hinting at a link between the two. The remaining six fields are apparently non‐detections although in light of these new models, closer inspection reveals tentative structure. With the overdensity of M giant stars in Canis Major being claimed both as a progenitor to the Monoceros Ring and alternatively a manifestation of the Milky Way warp, much is still unknown concerning this structure and its connection to the Monoceros Ring. Further constraints are needed for the numerical simulations to adequately resolve the increasingly complex view of this structure.</abstract><qualityIndicators><score>10</score><pdfWordCount>10997</pdfWordCount><pdfCharCount>56121</pdfCharCount><pdfVersion>1.3</pdfVersion><pdfPageCount>14</pdfPageCount><pdfPageSize>612 x 792 pts (letter)</pdfPageSize><refBibsNative>true</refBibsNative><abstractWordCount>335</abstractWordCount><abstractCharCount>2034</abstractCharCount><keywordCount>3</keywordCount></qualityIndicators><title>The Isaac Newton Telescope Wide Field Camera survey of the Monoceros Ring: accretion origin or Galactic anomaly?</title><genre><json:string>article</json:string></genre><host><title>Monthly Notices of the Royal Astronomical Society</title><language><json:string>unknown</json:string></language><doi><json:string>10.1111/(ISSN)1365-2966</json:string></doi><issn><json:string>0035-8711</json:string></issn><eissn><json:string>1365-2966</json:string></eissn><publisherId><json:string>MNR</json:string></publisherId><volume>362</volume><issue>2</issue><pages><first>475</first><last>488</last></pages><genre><json:string>journal</json:string></genre></host><namedEntities><unitex><date><json:string>2005</json:string><json:string>05/09/03</json:string><json:string>31/08/03</json:string><json:string>02/09/03</json:string></date><geogName><json:string>Canis Major region</json:string><json:string>region of Galactic</json:string></geogName><orgName><json:string>Institute for Astronomy, University of Edinburgh, Royal Observatory, Blackford Hill, Edinburgh EH</json:string><json:string>University of Sydney</json:string><json:string>Australia of Astronomy, Madingley Road, Cambridge CB</json:string><json:string>Cambridge University</json:string><json:string>Institute Accepted</json:string><json:string>Astrophysics Research, University of Hertfordshire, College Lane, Hat</json:string></orgName><orgName_funder></orgName_funder><orgName_provider></orgName_provider><persName><json:string>Sky Survey</json:string><json:string>Mike Irwin</json:string><json:string>Rodrigo A. Ibata</json:string><json:string>Unit</json:string><json:string>Blair C. Conn</json:string><json:string>Dwarf</json:string><json:string>F. Lewis</json:string><json:string>TriAnd</json:string><json:string>Tidal</json:string><json:string>Jorge Pe</json:string><json:string>M. N. Ferguson</json:string><json:string>Mike J. Irwin</json:string><json:string>Jonathan M. Irwin</json:string></persName><placeName><json:string>La Palma</json:string><json:string>Model</json:string><json:string>Metallicity</json:string><json:string>Strasbourg</json:string><json:string>France</json:string><json:string>Cambridge</json:string><json:string>Los Muchachos</json:string></placeName><ref_url><json:string>http://www.obs-besancon.fr/www/modele</json:string><json:string>http://www.astro.princeton.edu/</json:string><json:string>http://www.ast.cam.ac.uk/</json:string></ref_url><ref_bibl><json:string>Majewski et al. 2003</json:string><json:string>Windhorst et al. (1991)</json:string><json:string>Helmi et al. 2003</json:string><json:string>Robin et al. (2000)</json:string><json:string>Ibata et al. 2001a</json:string><json:string>Martin et al. (2004a)</json:string><json:string>Yanny et al. 2003</json:string><json:string>Ibata et al. (2003)</json:string><json:string>Irwin & Lewis 2001</json:string><json:string>Bellazzini et al. (2004)</json:string><json:string>Johnston et al. 1999</json:string><json:string>Morrison et al. 2000</json:string><json:string>Martin et al. (2004b)</json:string><json:string>Klypin et al. 1999</json:string><json:string>Helmi et al. 1999</json:string><json:string>Ferguson et al. 2002</json:string><json:string>Rocha-Pinto et al. (2003)</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>Ibata & Lewis 1998</json:string><json:string>Martin et al. 2005</json:string><json:string>Yanny et al. (2003)</json:string><json:string>Rocha-Pinto et al. (2004)</json:string><json:string>Martin et al. (2005)</json:string><json:string>Abadi et al. 2003a,b</json:string><json:string>Crane et al. (2003)</json:string><json:string>Ibata et al. 2001c</json:string><json:string>Robin et al. (2003)</json:string><json:string>Momany et al. (2004)</json:string><json:string>Rocha-Pinto et al. 2004</json:string><json:string>Majewski et al. 2004</json:string><json:string>Newberg et al. 2002</json:string><json:string>Frinchaboy et al. (2004)</json:string><json:string>Penarrubia et al. (2005)</json:string><json:string>Ibata et al. 2001b</json:string><json:string>Helmi et al. (2003)</json:string><json:string>Ibata et al. 2003</json:string><json:string>Stoughton et al. 2002</json:string><json:string>Schlegel et al. 1998</json:string><json:string>Yanny et al. 2004</json:string><json:string>McMahon et al. 2001</json:string><json:string>Robin et al. (1996)</json:string><json:string>Ibata et al.</json:string><json:string>Delgado et al.</json:string><json:string>Rocha-Pinto et al. 2003</json:string></ref_bibl><bibl></bibl></unitex></namedEntities><ark><json:string>ark:/67375/WNG-XZ6R60DB-X</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>2005</publicationDate><copyrightDate>2005</copyrightDate><doi><json:string>10.1111/j.1365-2966.2005.09311.x</json:string></doi><id>536CB4E7BD4119712CEEEE2235992BB2CBB25374</id><score>1</score><fulltext><json:item><extension>pdf</extension><original>true</original><mimetype>application/pdf</mimetype><uri>https://api.istex.fr/document/536CB4E7BD4119712CEEEE2235992BB2CBB25374/fulltext/pdf</uri></json:item><json:item><extension>zip</extension><original>false</original><mimetype>application/zip</mimetype><uri>https://api.istex.fr/document/536CB4E7BD4119712CEEEE2235992BB2CBB25374/fulltext/zip</uri></json:item><istex:fulltextTEI uri="https://api.istex.fr/document/536CB4E7BD4119712CEEEE2235992BB2CBB25374/fulltext/tei"><teiHeader><fileDesc><titleStmt><title level="a" type="main">The Isaac Newton Telescope Wide Field Camera survey of the Monoceros Ring: accretion origin or Galactic anomaly?</title></titleStmt><publicationStmt><authority>ISTEX</authority><publisher>Blackwell Science Ltd</publisher><pubPlace> 23 Ainslie Place , Edinburgh EH3 6AJ , UK . Telephone (0131) 226 7232 Fax (0131) 226 3803 </pubPlace><date type="published" when="2005-09"></date></publicationStmt><notesStmt><note type="content-type" subtype="article" source="article" scheme="https://content-type.data.istex.fr/ark:/67375/XTP-6N5SZHKN-D">article</note><note type="publication-type" subtype="journal" scheme="https://publication-type.data.istex.fr/ark:/67375/JMC-0GLKJH51-B">journal</note></notesStmt><sourceDesc><biblStruct type="article"><analytic><title level="a" type="main">The Isaac Newton Telescope Wide Field Camera survey of the Monoceros Ring: accretion origin or Galactic anomaly?</title><title level="a" type="short">The INT/WFC survey of the MRi</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>★ E‐mail: bconn@physics.usyd.edu.au (BCC); gfl@physics.usyd.edu.au (GFL); mike@ast.cam.ac.uk (MJI); ibata@astro.u‐strasbg.fr (RAB); ferguson@roe.ac.uk (AMNF); nrt@star.herts.ac.uk (NT); jmi@ast.cam.ac.uk (JMI)</affiliation></author><author xml:id="author-0001" role="corresp"><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><affiliation>★ E‐mail: bconn@physics.usyd.edu.au (BCC); gfl@physics.usyd.edu.au (GFL); mike@ast.cam.ac.uk (MJI); ibata@astro.u‐strasbg.fr (RAB); ferguson@roe.ac.uk (AMNF); nrt@star.herts.ac.uk (NT); jmi@ast.cam.ac.uk (JMI)</affiliation></author><author xml:id="author-0002" role="corresp"><persName><forename type="first">Mike J.</forename><surname>Irwin</surname></persName><affiliation>Institute of Astronomy, Madingley Road, Cambridge CB3 0HA</affiliation><affiliation>★ E‐mail: bconn@physics.usyd.edu.au (BCC); gfl@physics.usyd.edu.au (GFL); mike@ast.cam.ac.uk (MJI); ibata@astro.u‐strasbg.fr (RAB); ferguson@roe.ac.uk (AMNF); nrt@star.herts.ac.uk (NT); jmi@ast.cam.ac.uk (JMI)</affiliation></author><author xml:id="author-0003" role="corresp"><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><affiliation>★ E‐mail: bconn@physics.usyd.edu.au (BCC); gfl@physics.usyd.edu.au (GFL); mike@ast.cam.ac.uk (MJI); ibata@astro.u‐strasbg.fr (RAB); ferguson@roe.ac.uk (AMNF); nrt@star.herts.ac.uk (NT); jmi@ast.cam.ac.uk (JMI)</affiliation></author><author xml:id="author-0004" role="corresp"><persName><forename type="first">Annette M. N.</forename><surname>Ferguson</surname></persName><affiliation>Institute for Astronomy, University of Edinburgh, Royal Observatory, Blackford Hill, Edinburgh EH9 3HJ</affiliation><affiliation>★ E‐mail: bconn@physics.usyd.edu.au (BCC); gfl@physics.usyd.edu.au (GFL); mike@ast.cam.ac.uk (MJI); ibata@astro.u‐strasbg.fr (RAB); ferguson@roe.ac.uk (AMNF); nrt@star.herts.ac.uk (NT); jmi@ast.cam.ac.uk (JMI)</affiliation></author><author xml:id="author-0005" role="corresp"><persName><forename type="first">Nial</forename><surname>Tanvir</surname></persName><affiliation>Centre for Astrophysics Research, University of Hertfordshire, College Lane, Hatfield AL10 9AB</affiliation><affiliation>★ E‐mail: bconn@physics.usyd.edu.au (BCC); gfl@physics.usyd.edu.au (GFL); mike@ast.cam.ac.uk (MJI); ibata@astro.u‐strasbg.fr (RAB); ferguson@roe.ac.uk (AMNF); nrt@star.herts.ac.uk (NT); jmi@ast.cam.ac.uk (JMI)</affiliation></author><author xml:id="author-0006" role="corresp"><persName><forename type="first">Jonathan M.</forename><surname>Irwin</surname></persName><affiliation>Institute of Astronomy, Madingley Road, Cambridge CB3 0HA</affiliation><affiliation>★ E‐mail: bconn@physics.usyd.edu.au (BCC); gfl@physics.usyd.edu.au (GFL); mike@ast.cam.ac.uk (MJI); ibata@astro.u‐strasbg.fr (RAB); ferguson@roe.ac.uk (AMNF); nrt@star.herts.ac.uk (NT); jmi@ast.cam.ac.uk (JMI)</affiliation></author><idno type="istex">536CB4E7BD4119712CEEEE2235992BB2CBB25374</idno><idno type="ark">ark:/67375/WNG-XZ6R60DB-X</idno><idno type="DOI">10.1111/j.1365-2966.2005.09311.x</idno><idno type="unit">MNR9311</idno><idno type="supplier">mnr9311</idno><idno type="toTypesetVersion">file:MNR.MNR9311.pdf</idno></analytic><monogr><title level="j" type="main">Monthly Notices of the Royal Astronomical Society</title><title level="j" type="alt">MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY</title><idno type="pISSN">0035-8711</idno><idno type="eISSN">1365-2966</idno><idno type="book-DOI">10.1111/(ISSN)1365-2966</idno><idno type="book-part-DOI">10.1111/mnr.2005.362.issue-2</idno><idno type="product">MNR</idno><idno type="publisherDivision">ST</idno><imprint><biblScope unit="vol">362</biblScope><biblScope unit="issue">2</biblScope><biblScope unit="page" from="475">475</biblScope><biblScope unit="page" to="488">488</biblScope><publisher>Blackwell Science Ltd</publisher><pubPlace> 23 Ainslie Place , Edinburgh EH3 6AJ , UK . Telephone (0131) 226 7232 Fax (0131) 226 3803 </pubPlace><date type="published" when="2005-09"></date></imprint></monogr></biblStruct></sourceDesc></fileDesc><profileDesc><abstract xml:lang="en" style="main"><head>ABSTRACT</head><p>We present the results of a wide‐field camera survey of the stars in the Monoceros Ring, thought to be an additional structure in the Milky Way of unknown origin. Lying roughly in the plane of the Milky Way, this may represent a unique equatorial accretion event which is contributing to the thick disc of the Galaxy. Alternatively, the Monoceros Ring may be a natural part of the disc formation process. With 10 pointings in symmetric pairs above and below the plane of the Galaxy, this survey spans 90° about the equator of the Milky Way. Signatures of the stream of stars were detected in three fields, <emph><span>(<hi rend="italic">l</hi>, <hi rend="italic">b</hi>) = (118°, +16°)</span></emph> and (150°, +15°) plus a more tentative detection at (150°, −15°). Galactocentric distance estimates to these structures gave ∼17, ∼17, and ∼13 kpc, respectively. The Monoceros Ring seems to be present on both sides of the Galactic plane, in a form different from that of the Galactic warp, suggestive of a tidal origin with streams multiply wrapping the Galaxy. A new model of the stream has shown a strong coincidence with our results and has also provided the opportunity to make several more detections in fields in which the stream is less significant. The confirmed detection at <emph><span>(<hi rend="italic">l</hi>, <hi rend="italic">b</hi>) = (123°, −19°)</span></emph> at ∼14, kpc from the Galactic Centre allows a re‐examination revealing a tentative new detection with a Galactocentric distance of ∼21 kpc. These detections also lie very close to the newly discovered structure in Triangulum–Andromedae hinting at a link between the two. The remaining six fields are apparently non‐detections although in light of these new models, closer inspection reveals tentative structure. With the overdensity of M giant stars in Canis Major being claimed both as a progenitor to the Monoceros Ring and alternatively a manifestation of the Milky Way warp, much is still unknown concerning this structure and its connection to the Monoceros Ring. Further constraints are needed for the numerical simulations to adequately resolve the increasingly complex view of this structure.</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/536CB4E7BD4119712CEEEE2235992BB2CBB25374/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 Science Ltd</publisherName><publisherLoc> 23 Ainslie Place , Edinburgh EH3 6AJ , UK . Telephone (0131) 226 7232 Fax (0131) 226 3803 </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="09002"><doi origin="wiley">10.1111/mnr.2005.362.issue-2</doi><numberingGroup><numbering type="journalVolume" number="362">362</numbering><numbering type="journalIssue" number="2">2</numbering></numberingGroup><coverDate startDate="2005-09">September 2005</coverDate></publicationMeta><publicationMeta level="unit" type="article" position="9" status="forIssue"><doi origin="wiley">10.1111/j.1365-2966.2005.09311.x</doi><idGroup><id type="unit" value="MNR9311"></id><id type="supplier" value="mnr9311"></id></idGroup><titleGroup><title type="tocHeading1">Papers</title></titleGroup><eventGroup><event type="firstOnline" date="2005-07-28"></event><event type="publishedOnlineFinalForm" date="2005-07-28"></event><event type="xmlConverted" agent="Converter:BPG_TO_WML3G version:2.3.5 mode:FullText source:FullText result:FullText" date="2010-04-06"></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="475">475</numbering><numbering type="pageLast" number="488">488</numbering></numberingGroup><correspondenceTo><sup>★</sup>
E‐mail: <email>bconn@physics.usyd.edu.au</email> (BCC); <email>gfl@physics.usyd.edu.au</email> (GFL); <email>mike@ast.cam.ac.uk</email> (MJI); <email normalForm="ibata@astro.u-strasbg.fr">ibata@astro.u‐strasbg.fr</email> (RAB); <email>ferguson@roe.ac.uk</email> (AMNF); <email>nrt@star.herts.ac.uk</email> (NT); <email>jmi@ast.cam.ac.uk</email> (JMI)</correspondenceTo><linkGroup><link type="toTypesetVersion" href="file:MNR.MNR9311.pdf"></link></linkGroup></publicationMeta><contentMeta><unparsedEditorialHistory>Accepted 2005 June 16. Received 2005 May 30; in original form 2005 January 18</unparsedEditorialHistory><countGroup><count type="figureTotal" number="14"></count><count type="tableTotal" number="3"></count><count type="formulaTotal" number="118"></count><count type="referenceTotal" number="49"></count><count type="linksCrossRef" number="204"></count></countGroup><titleGroup><title type="main">The Isaac Newton Telescope Wide Field Camera survey of the Monoceros Ring: accretion origin or Galactic anomaly?</title><title type="shortAuthors"><i>B. C. Conn et al.</i></title><title type="short"><i>The INT/WFC survey of the MRi</i></title></titleGroup><creators><creator creatorRole="author" xml:id="cr1" affiliationRef="#a1" corresponding="yes"><personName><givenNames>Blair C.</givenNames><familyName>Conn</familyName></personName></creator><creator creatorRole="author" xml:id="cr2" affiliationRef="#a1" corresponding="yes"><personName><givenNames>Geraint F.</givenNames><familyName>Lewis</familyName></personName></creator><creator creatorRole="author" xml:id="cr3" affiliationRef="#a2" corresponding="yes"><personName><givenNames>Mike J.</givenNames><familyName>Irwin</familyName></personName></creator><creator creatorRole="author" xml:id="cr4" affiliationRef="#a3" corresponding="yes"><personName><givenNames>Rodrigo A.</givenNames><familyName>Ibata</familyName></personName></creator><creator creatorRole="author" xml:id="cr5" affiliationRef="#a4" corresponding="yes"><personName><givenNames>Annette M. N.</givenNames><familyName>Ferguson</familyName></personName></creator><creator creatorRole="author" xml:id="cr6" affiliationRef="#a5" corresponding="yes"><personName><givenNames>Nial</givenNames><familyName>Tanvir</familyName></personName></creator><creator creatorRole="author" xml:id="cr7" affiliationRef="#a2" corresponding="yes"><personName><givenNames>Jonathan M.</givenNames><familyName>Irwin</familyName></personName></creator></creators><affiliationGroup><affiliation xml:id="a1" countryCode="AU"><unparsedAffiliation>Institute of Astronomy, School of Physics, A29, University of Sydney, NSW 2006, Australia</unparsedAffiliation></affiliation><affiliation xml:id="a2"><unparsedAffiliation>Institute of Astronomy, Madingley Road, Cambridge CB3 0HA</unparsedAffiliation></affiliation><affiliation xml:id="a3" countryCode="FR"><unparsedAffiliation>Observatoire de Strasbourg, 11, rue de l'Université, F‐67000, Strasbourg, France</unparsedAffiliation></affiliation><affiliation xml:id="a4"><unparsedAffiliation>Institute for Astronomy, University of Edinburgh, Royal Observatory, Blackford Hill, Edinburgh EH9 3HJ</unparsedAffiliation></affiliation><affiliation xml:id="a5"><unparsedAffiliation>Centre for Astrophysics Research, University of Hertfordshire, College Lane, Hatfield AL10 9AB</unparsedAffiliation></affiliation></affiliationGroup><keywordGroup xml:lang="en"><keyword xml:id="k1">Galaxy: formation</keyword><keyword xml:id="k2">Galaxy: structure</keyword><keyword xml:id="k3">galaxies: interactions</keyword></keywordGroup><abstractGroup><abstract type="main" xml:lang="en"><title type="main">ABSTRACT</title><p>We present the results of a wide‐field camera survey of the stars in the Monoceros Ring, thought to be an additional structure in the Milky Way of unknown origin. Lying roughly in the plane of the Milky Way, this may represent a unique equatorial accretion event which is contributing to the thick disc of the Galaxy. Alternatively, the Monoceros Ring may be a natural part of the disc formation process. With 10 pointings in symmetric pairs above and below the plane of the Galaxy, this survey spans 90° about the equator of the Milky Way. Signatures of the stream of stars were detected in three fields, <span type="mathematics">(<i>l</i>, <i>b</i>) = (118°, +16°)</span> and (150°, +15°) plus a more tentative detection at (150°, −15°). Galactocentric distance estimates to these structures gave ∼17, ∼17, and ∼13 kpc, respectively. The Monoceros Ring seems to be present on both sides of the Galactic plane, in a form different from that of the Galactic warp, suggestive of a tidal origin with streams multiply wrapping the Galaxy. A new model of the stream has shown a strong coincidence with our results and has also provided the opportunity to make several more detections in fields in which the stream is less significant. The confirmed detection at <span type="mathematics">(<i>l</i>, <i>b</i>) = (123°, −19°)</span> at ∼14, kpc from the Galactic Centre allows a re‐examination revealing a tentative new detection with a Galactocentric distance of ∼21 kpc. These detections also lie very close to the newly discovered structure in Triangulum–Andromedae hinting at a link between the two. The remaining six fields are apparently non‐detections although in light of these new models, closer inspection reveals tentative structure. With the overdensity of M giant stars in Canis Major being claimed both as a progenitor to the Monoceros Ring and alternatively a manifestation of the Milky Way warp, much is still unknown concerning this structure and its connection to the Monoceros Ring. Further constraints are needed for the numerical simulations to adequately resolve the increasingly complex view of this structure.</p></abstract></abstractGroup></contentMeta></header></component></istex:document></istex:metadataXml><mods version="3.6"><titleInfo lang="en"><title>The Isaac Newton Telescope Wide Field Camera survey of the Monoceros Ring: accretion origin or Galactic anomaly?</title></titleInfo><titleInfo type="abbreviated" lang="en"><title>The INT/WFC survey of the MRi</title></titleInfo><titleInfo type="alternative" contentType="CDATA" lang="en"><title>The Isaac Newton Telescope Wide Field Camera survey of the Monoceros Ring: accretion origin or Galactic anomaly?</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>E-mail: bconn@physics.usyd.edu.au</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><affiliation>E-mail: bconn@physics.usyd.edu.au</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><affiliation>E-mail: bconn@physics.usyd.edu.au</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><affiliation>E-mail: bconn@physics.usyd.edu.au</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><affiliation>E-mail: bconn@physics.usyd.edu.au</affiliation><role><roleTerm type="text">author</roleTerm></role></name><name type="personal"><namePart type="given">Nial</namePart><namePart type="family">Tanvir</namePart><affiliation>Centre for Astrophysics Research, University of Hertfordshire, College Lane, Hatfield AL10 9AB</affiliation><affiliation>E-mail: bconn@physics.usyd.edu.au</affiliation><role><roleTerm type="text">author</roleTerm></role></name><name type="personal"><namePart type="given">Jonathan M.</namePart><namePart type="family">Irwin</namePart><affiliation>Institute of Astronomy, Madingley Road, Cambridge CB3 0HA</affiliation><affiliation>E-mail: bconn@physics.usyd.edu.au</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 Science Ltd</publisher><place><placeTerm type="text">23 Ainslie Place , Edinburgh EH3 6AJ , UK . Telephone (0131) 226 7232 Fax (0131) 226 3803</placeTerm></place><dateIssued encoding="w3cdtf">2005-09</dateIssued><edition>Accepted 2005 June 16. Received 2005 May 30; in original form 2005 January 18</edition><copyrightDate encoding="w3cdtf">2005</copyrightDate></originInfo><language><languageTerm type="code" authority="rfc3066">en</languageTerm><languageTerm type="code" authority="iso639-2b">eng</languageTerm></language><physicalDescription><extent unit="figures">14</extent><extent unit="tables">3</extent><extent unit="formulas">118</extent><extent unit="references">49</extent><extent unit="linksCrossRef">204</extent></physicalDescription><abstract lang="en">We present the results of a wide‐field camera survey of the stars in the Monoceros Ring, thought to be an additional structure in the Milky Way of unknown origin. Lying roughly in the plane of the Milky Way, this may represent a unique equatorial accretion event which is contributing to the thick disc of the Galaxy. Alternatively, the Monoceros Ring may be a natural part of the disc formation process. With 10 pointings in symmetric pairs above and below the plane of the Galaxy, this survey spans 90° about the equator of the Milky Way. Signatures of the stream of stars were detected in three fields, (l, b) = (118°, +16°) and (150°, +15°) plus a more tentative detection at (150°, −15°). Galactocentric distance estimates to these structures gave ∼17, ∼17, and ∼13 kpc, respectively. The Monoceros Ring seems to be present on both sides of the Galactic plane, in a form different from that of the Galactic warp, suggestive of a tidal origin with streams multiply wrapping the Galaxy. A new model of the stream has shown a strong coincidence with our results and has also provided the opportunity to make several more detections in fields in which the stream is less significant. The confirmed detection at (l, b) = (123°, −19°) at ∼14, kpc from the Galactic Centre allows a re‐examination revealing a tentative new detection with a Galactocentric distance of ∼21 kpc. These detections also lie very close to the newly discovered structure in Triangulum–Andromedae hinting at a link between the two. The remaining six fields are apparently non‐detections although in light of these new models, closer inspection reveals tentative structure. With the overdensity of M giant stars in Canis Major being claimed both as a progenitor to the Monoceros Ring and alternatively a manifestation of the Milky Way warp, much is still unknown concerning this structure and its connection to the Monoceros Ring. Further constraints are needed for the numerical simulations to adequately resolve the increasingly complex view of this structure.</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>2005</date><detail type="volume"><caption>vol.</caption><number>362</number></detail><detail type="issue"><caption>no.</caption><number>2</number></detail><extent unit="pages"><start>475</start><end>488</end></extent></part></relatedItem><identifier type="istex">536CB4E7BD4119712CEEEE2235992BB2CBB25374</identifier><identifier type="ark">ark:/67375/WNG-XZ6R60DB-X</identifier><identifier type="DOI">10.1111/j.1365-2966.2005.09311.x</identifier><identifier type="ArticleID">MNR9311</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 Science Ltd</recordOrigin></recordInfo></mods><json:item><extension>json</extension><original>false</original><mimetype>application/json</mimetype><uri>https://api.istex.fr/document/536CB4E7BD4119712CEEEE2235992BB2CBB25374/metadata/json</uri></json:item></metadata><serie></serie></istex></record>Pour manipuler ce document sous Unix (Dilib)
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