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The Isaac Newton Telescope Wide Field Camera survey of the Monoceros Ring: accretion origin or Galactic anomaly?

Identifieur interne : 000F73 ( Istex/Curation ); précédent : 000F72; suivant : 000F74

The Isaac Newton Telescope Wide Field Camera survey of the Monoceros Ring: accretion origin or Galactic anomaly?

Auteurs : Blair C. Conn [Australie] ; Geraint F. Lewis [Australie] ; Mike J. Irwin [Australie] ; Rodrigo A. Ibata [France, Australie] ; Annette M. N. Ferguson [Royaume-Uni, Australie] ; Nial Tanvir [Australie] ; Jonathan M. Irwin [Australie]

Source :

Monthly Notices of the Royal Astronomical Society [ 0035-8711 ] ; 2005-09.

RBID : ISTEX:536CB4E7BD4119712CEEEE2235992BB2CBB25374

English descriptors

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:

https://api.istex.fr/document/536CB4E7BD4119712CEEEE2235992BB2CBB25374/fulltext/pdf

DOI: 10.1111/j.1365-2966.2005.09311.x

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<profileDesc><textClass><keywords scheme="KwdEn" xml:lang="en"><term>Accreting dwarf galaxy</term>
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<term>Cent completeness</term>
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<term>Detection</term>
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<term>Distance estimates</term>
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<term>Galactic features</term>
<term>Galactic halo</term>
<term>Galactic longitude</term>
<term>Galactic plane</term>
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<term>Galactic view</term>
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<term>Galactocentric distance</term>
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<term>Heliocentric distances</term>
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<term>Lower panels</term>
<term>Lower plot</term>
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<term>Magnitude completeness</term>
<term>Magnitude range</term>
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<term>Main sequences</term>
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<term>Redward trend</term>
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<term>Sagittarius dwarf galaxy</term>
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<term>Systematic errors</term>
<term>Tentative detection</term>
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<term>Tidal debris</term>
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<term>Triand structure</term>
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<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>
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<term>Mnras</term>
<term>Model cmds</term>
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<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>
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<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>
</record>

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The Isaac Newton Telescope Wide Field Camera survey of the Monoceros Ring: accretion origin or Galactic anomaly?

The Isaac Newton Telescope Wide Field Camera survey of the Monoceros Ring: accretion origin or Galactic anomaly?

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