AustralieFrV1, Main, Exploration, bibRecord, 005867

THE RESOLVED STRUCTURE AND DYNAMICS OF AN ISOLATED DWARF GALAXY: A VLT AND KECK SPECTROSCOPIC SURVEY OF WLM

Identifieur interne : 005867 ( Main/Exploration ); précédent : 005866; suivant : 005868

THE RESOLVED STRUCTURE AND DYNAMICS OF AN ISOLATED DWARF GALAXY: A VLT AND KECK SPECTROSCOPIC SURVEY OF WLM

Auteurs : Ryan Leaman [Canada] ; Kim A. Venn [Canada] ; Alyson M. Brooks [États-Unis] ; Giuseppina Battaglia [Allemagne] ; Andrew A. Cole [Australie] ; Rodrigo A. Ibata [France] ; Mike J. Irwin [Royaume-Uni] ; Alan W. Mcconnachie [Canada] ; J. Trevor Mendel [Canada] ; Eline Tolstoy [Pays-Bas]

Source :

The Astrophysical journal [ 0004-637X ] ; 2012.

RBID : Pascal:12-0195455

Descripteurs français

Pascal (Inist)
- Dynamique, Galaxies naines, Géante rouge, Etoile géante, Galaxies irrégulières, Triplet, Deimos, Métallicité, Age, Population stellaire, Rotation stellaire, Alignement, Cinématique, Courbe rotation, Dispersion vitesse, Nuage moléculaire géant, Sous structure, Boucle réaction, Groupe local, Groupe galaxies, Formation stellaire, Evolution dynamique, Abondance, Evolution galaxies, Satellite Mars.

English descriptors

KwdEn :
- Abundance, Age, Alignment, Deimos, Dwarf galaxies, Dynamical evolution, Dynamics, Feedback, Galaxy evolution, Galaxy groups, Giant molecular cloud, Giant stars, Irregular galaxies, Kinematics, Local group, Mars satellite, Metallicity, Red giant stars, Rotation curve, Star formation, Stellar population, Stellar rotation, Substructure, Triplets, Velocity dispersion.

Abstract

We present spectroscopic data for 180 red giant branch (RGB) stars in the isolated dwarf irregular galaxy Wolf-Lundmark-Mellote (WLM). Observations of the calcium II triplet lines in spectra of RGB stars covering the entire galaxy were obtained with FORS2 at the Very Large Telescope and DEIMOS on Keck II, allowing us to derive velocities, metallicities, and ages for the stars. With accompanying photometric and radio data we have measured the structural parameters of the stellar and gaseous populations over the full galaxy. The stellar populations show an intrinsically thick configuration with 0.39 ≤ _q0 ≤ 0.57. The stellar rotation in WLM is measured to be 17±1 km s^-1; however, the ratio of rotation to pressure support for the stars is V/σ ∼ 1, in contrast to the gas, whose ratio is seven times larger. This, along with the structural data and alignment of the kinematic and photometric axes, suggests we are viewing WLM as a highly inclined oblate spheroid. Stellar rotation curves, corrected for asymmetric drift, are used to compute a dynamical mass of (4.3 ± 0.3) x 10⁸ M_◦. at the half-light radius (r_h = 1656 ± 49 pc). The stellar velocity dispersion increases with stellar age in a manner consistent with giant molecular cloud and substructure interactions producing the heating in WLM. Coupled with WLM's isolation, this suggests that the extended vertical structure of its stellar and gaseous components and increase in stellar velocity dispersion with age are due to internal feedback, rather than tidally driven evolution. These represent some of the first observational results from an isolated Local Group dwarf galaxy that can offer important constraints on how strongly internal feedback and secular processes modulate star formation and dynamical evolution in low-mass isolated objects.

Affiliations:

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<series><title level="j" type="main">The Astrophysical journal</title>
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<profileDesc><textClass><keywords scheme="KwdEn" xml:lang="en"><term>Abundance</term>
<term>Age</term>
<term>Alignment</term>
<term>Deimos</term>
<term>Dwarf galaxies</term>
<term>Dynamical evolution</term>
<term>Dynamics</term>
<term>Feedback</term>
<term>Galaxy evolution</term>
<term>Galaxy groups</term>
<term>Giant molecular cloud</term>
<term>Giant stars</term>
<term>Irregular galaxies</term>
<term>Kinematics</term>
<term>Local group</term>
<term>Mars satellite</term>
<term>Metallicity</term>
<term>Red giant stars</term>
<term>Rotation curve</term>
<term>Star formation</term>
<term>Stellar population</term>
<term>Stellar rotation</term>
<term>Substructure</term>
<term>Triplets</term>
<term>Velocity dispersion</term>
</keywords>
<keywords scheme="Pascal" xml:lang="fr"><term>Dynamique</term>
<term>Galaxies naines</term>
<term>Géante rouge</term>
<term>Etoile géante</term>
<term>Galaxies irrégulières</term>
<term>Triplet</term>
<term>Deimos</term>
<term>Métallicité</term>
<term>Age</term>
<term>Population stellaire</term>
<term>Rotation stellaire</term>
<term>Alignement</term>
<term>Cinématique</term>
<term>Courbe rotation</term>
<term>Dispersion vitesse</term>
<term>Nuage moléculaire géant</term>
<term>Sous structure</term>
<term>Boucle réaction</term>
<term>Groupe local</term>
<term>Groupe galaxies</term>
<term>Formation stellaire</term>
<term>Evolution dynamique</term>
<term>Abondance</term>
<term>Evolution galaxies</term>
<term>Satellite Mars</term>
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<front><div type="abstract" xml:lang="en">We present spectroscopic data for 180 red giant branch (RGB) stars in the isolated dwarf irregular galaxy Wolf-Lundmark-Mellote (WLM). Observations of the calcium II triplet lines in spectra of RGB stars covering the entire galaxy were obtained with FORS2 at the Very Large Telescope and DEIMOS on Keck II, allowing us to derive velocities, metallicities, and ages for the stars. With accompanying photometric and radio data we have measured the structural parameters of the stellar and gaseous populations over the full galaxy. The stellar populations show an intrinsically thick configuration with 0.39 ≤ <sub>q0</sub>
 ≤ 0.57. The stellar rotation in WLM is measured to be 17±1 km s<sup>-1</sup>
; however, the ratio of rotation to pressure support for the stars is V/σ ∼ 1, in contrast to the gas, whose ratio is seven times larger. This, along with the structural data and alignment of the kinematic and photometric axes, suggests we are viewing WLM as a highly inclined oblate spheroid. Stellar rotation curves, corrected for asymmetric drift, are used to compute a dynamical mass of (4.3 ± 0.3) x 10<sup>8</sup>
 M<sub>◦.</sub>
 at the half-light radius (r<sub>h</sub>
 = 1656 ± 49 pc). The stellar velocity dispersion increases with stellar age in a manner consistent with giant molecular cloud and substructure interactions producing the heating in WLM. Coupled with WLM's isolation, this suggests that the extended vertical structure of its stellar and gaseous components and increase in stellar velocity dispersion with age are due to internal feedback, rather than tidally driven evolution. These represent some of the first observational results from an isolated Local Group dwarf galaxy that can offer important constraints on how strongly internal feedback and secular processes modulate star formation and dynamical evolution in low-mass isolated objects.</div>
</front>
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<country name="Royaume-Uni"><region name="Angleterre"><name sortKey="Irwin, Mike J" sort="Irwin, Mike J" uniqKey="Irwin M" first="Mike J." last="Irwin">Mike J. Irwin</name>
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   |texte=   THE RESOLVED STRUCTURE AND DYNAMICS OF AN ISOLATED DWARF GALAXY: A VLT AND KECK SPECTROSCOPIC SURVEY OF WLM
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	Serveur d'exploration sur les relations entre la France et l'Australie
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Serveur d'exploration sur les relations entre la France et l'Australie

THE RESOLVED STRUCTURE AND DYNAMICS OF AN ISOLATED DWARF GALAXY: A VLT AND KECK SPECTROSCOPIC SURVEY OF WLM

THE RESOLVED STRUCTURE AND DYNAMICS OF AN ISOLATED DWARF GALAXY: A VLT AND KECK SPECTROSCOPIC SURVEY OF WLM

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