AustralieFrV1, Main, Exploration, bibRecord, 00A310

Distances and metallicities for 17 Local Group galaxies

Identifieur interne : 00A310 ( Main/Exploration ); précédent : 00A309; suivant : 00A311

Distances and metallicities for 17 Local Group galaxies

Auteurs : A. W. Mcconnachie [Royaume-Uni] ; M. J. Irwin ; A. M. N. Ferguson [Allemagne] ; R. A. Ibata [France] ; G. F. Lewis [Australie] ; N. Tanvir

Source :

Monthly Notices of the Royal Astronomical Society [ 0035-8711 ] ; 2005-01.

RBID : ISTEX:72AA634C0514A6DE50BDF8B40D403202489B61DC

Descripteurs français

Pascal (Inist)
- Contenu stellaire, Etude comparative, Galaxies géantes, Galaxies naines, Galaxies spirales, Groupe galaxies, Groupe local, Géante rouge, Incertitude, Magnitude absolue, Métallicité, Photométrie, Population stellaire, Sous groupe.

English descriptors

Abstract

We have obtained Johnson V and Gunn i photometry for a large number of Local Group galaxies using the Isaac Newton Telescope Wide Field Camera (INT WFC). The majority of these galaxies are members of the M31 subgroup and the observations are deep enough to study the top few magnitudes of the red giant branch in each system. We previously measured the location of the tip of the red giant branch (TRGB) for Andromeda I, Andromeda II and M33 to within systematic uncertainties of typically <0.05 mag. As the TRGB acts as a standard candle in old, metal‐poor stellar populations, we were able to derive distances to each of these galaxies. Here we derive TRGB distances to the giant spiral galaxy M31 and 13 additional dwarf galaxies – NGC 205, 185, 147, Pegasus, WLM, LGS3, Cetus, Aquarius, And III, V, VI, VII and the newly discovered dwarf spheroidal And IX. The observations for each of the dwarf galaxies were intentionally taken in photometric conditions. In addition to the distances, we also self‐consistently derive the median metallicity of each system from the colour of their red giant branches. This allows us to take into account the small metallicity variation of the absolute I magnitude of the TRGB. The homogeneous nature of our data and the identical analysis applied to each of the 17 Local Group galaxies ensures that these estimates form a reliable set of distance and metallicity determinations that are ideal for comparative studies of Local Group galaxy properties.

Url:

DOI: 10.1111/j.1365-2966.2004.08514.x

Affiliations:

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<term>Algorithm</term>
<term>Andromeda</term>
<term>Aparicio</term>
<term>Aquarius</term>
<term>Armandroff</term>
<term>Astron</term>
<term>Bellazzini</term>
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<term>Centre</term>
<term>Cetus</term>
<term>Colour</term>
<term>Comparative study</term>
<term>Costa</term>
<term>Distance determinations</term>
<term>Distance estimates</term>
<term>Distance modulus</term>
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<term>Dwarf galaxies</term>
<term>Elliptical annulus</term>
<term>Error budget</term>
<term>Evolutionary track</term>
<term>Fainter</term>
<term>Foreground</term>
<term>Foreground contamination</term>
<term>Foreground stars</term>
<term>Freedman</term>
<term>Freedman madore</term>
<term>Galaxy</term>
<term>Galaxy groups</term>
<term>Gallagher</term>
<term>Giant branch</term>
<term>Giant galaxies</term>
<term>Globular clusters</term>
<term>Good agreement</term>
<term>Grebel guhathakurta</term>
<term>Guhathakurta</term>
<term>Heuristic</term>
<term>Heuristic signal</term>
<term>Hoessel</term>
<term>Irwin</term>
<term>Isaac newton telescope</term>
<term>Itrgb</term>
<term>Itrgb algorithm</term>
<term>Lgs3</term>
<term>Local foreground correction</term>
<term>Local group</term>
<term>Local group galaxies</term>
<term>Locus</term>
<term>Lower right panel</term>
<term>Luminosity</term>
<term>Luminosity function</term>
<term>Luminosity functions</term>
<term>Madore</term>
<term>Mcconnachie</term>
<term>Median</term>
<term>Median metallicity</term>
<term>Metallicities</term>
<term>Metallicity</term>
<term>Minniti zijlstra</term>
<term>Mnras</term>
<term>Modulus</term>
<term>Pegasus</term>
<term>Photometric</term>
<term>Photometric conditions</term>
<term>Photometry</term>
<term>Previous estimates</term>
<term>Red giant stars</term>
<term>Reddening</term>
<term>Representative metallicity</term>
<term>Sarajedini</term>
<term>Semimajor axis</term>
<term>Spheroidal</term>
<term>Spiral galaxies</term>
<term>Stellar</term>
<term>Stellar content</term>
<term>Stellar locus</term>
<term>Stellar objects</term>
<term>Stellar population</term>
<term>Stellar populations</term>
<term>Subgroup</term>
<term>Systematic uncertainties</term>
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<term>Trgb algorithm</term>
<term>Trgb location</term>
<term>Uncertainty</term>
<term>Upper right panel</term>
<term>Zucker</term>
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<term>Etude comparative</term>
<term>Galaxies géantes</term>
<term>Galaxies naines</term>
<term>Galaxies spirales</term>
<term>Groupe galaxies</term>
<term>Groupe local</term>
<term>Géante rouge</term>
<term>Incertitude</term>
<term>Magnitude absolue</term>
<term>Métallicité</term>
<term>Photométrie</term>
<term>Population stellaire</term>
<term>Sous groupe</term>
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<term>Andromeda</term>
<term>Aparicio</term>
<term>Aquarius</term>
<term>Armandroff</term>
<term>Astron</term>
<term>Bellazzini</term>
<term>Bergh</term>
<term>Centre</term>
<term>Cetus</term>
<term>Colour</term>
<term>Costa</term>
<term>Distance determinations</term>
<term>Distance estimates</term>
<term>Distance modulus</term>
<term>Dwarf</term>
<term>Dwarf galaxies</term>
<term>Elliptical annulus</term>
<term>Error budget</term>
<term>Evolutionary track</term>
<term>Fainter</term>
<term>Foreground</term>
<term>Foreground contamination</term>
<term>Foreground stars</term>
<term>Freedman</term>
<term>Freedman madore</term>
<term>Galaxy</term>
<term>Gallagher</term>
<term>Giant branch</term>
<term>Globular clusters</term>
<term>Good agreement</term>
<term>Grebel guhathakurta</term>
<term>Guhathakurta</term>
<term>Heuristic</term>
<term>Heuristic signal</term>
<term>Hoessel</term>
<term>Irwin</term>
<term>Isaac newton telescope</term>
<term>Itrgb</term>
<term>Itrgb algorithm</term>
<term>Lgs3</term>
<term>Local foreground correction</term>
<term>Local group</term>
<term>Local group galaxies</term>
<term>Locus</term>
<term>Lower right panel</term>
<term>Luminosity</term>
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<term>Luminosity functions</term>
<term>Madore</term>
<term>Mcconnachie</term>
<term>Median</term>
<term>Median metallicity</term>
<term>Metallicities</term>
<term>Metallicity</term>
<term>Minniti zijlstra</term>
<term>Mnras</term>
<term>Modulus</term>
<term>Pegasus</term>
<term>Photometric</term>
<term>Photometric conditions</term>
<term>Photometry</term>
<term>Previous estimates</term>
<term>Reddening</term>
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<term>Sarajedini</term>
<term>Semimajor axis</term>
<term>Spheroidal</term>
<term>Stellar</term>
<term>Stellar content</term>
<term>Stellar locus</term>
<term>Stellar objects</term>
<term>Stellar populations</term>
<term>Systematic uncertainties</term>
<term>Trgb</term>
<term>Trgb algorithm</term>
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<front><div type="abstract" xml:lang="en">We have obtained Johnson V and Gunn i photometry for a large number of Local Group galaxies using the Isaac Newton Telescope Wide Field Camera (INT WFC). The majority of these galaxies are members of the M31 subgroup and the observations are deep enough to study the top few magnitudes of the red giant branch in each system. We previously measured the location of the tip of the red giant branch (TRGB) for Andromeda I, Andromeda II and M33 to within systematic uncertainties of typically <0.05 mag. As the TRGB acts as a standard candle in old, metal‐poor stellar populations, we were able to derive distances to each of these galaxies. Here we derive TRGB distances to the giant spiral galaxy M31 and 13 additional dwarf galaxies – NGC 205, 185, 147, Pegasus, WLM, LGS3, Cetus, Aquarius, And III, V, VI, VII and the newly discovered dwarf spheroidal And IX. The observations for each of the dwarf galaxies were intentionally taken in photometric conditions. In addition to the distances, we also self‐consistently derive the median metallicity of each system from the colour of their red giant branches. This allows us to take into account the small metallicity variation of the absolute I magnitude of the TRGB. The homogeneous nature of our data and the identical analysis applied to each of the 17 Local Group galaxies ensures that these estimates form a reliable set of distance and metallicity determinations that are ideal for comparative studies of Local Group galaxy properties.</div>
</front>
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Serveur d'exploration sur les relations entre la France et l'Australie

Distances and metallicities for 17 Local Group galaxies

Distances and metallicities for 17 Local Group galaxies

Source :

Descripteurs français

English descriptors

Abstract

Links toward previous steps (curation, corpus...)

Le document en format XML

Pour manipuler ce document sous Unix (Dilib)

Pour mettre un lien sur cette page dans le réseau Wicri

	Serveur d'exploration sur les relations entre la France et l'Australie
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