AustralieFrV1, Main, Exploration, bibRecord, 007369

A Keck/DEIMOS spectroscopic survey of the faint M31 satellites And IX, And XI, And XII and And XIII

Identifieur interne : 007369 ( Main/Exploration ); précédent : 007368; suivant : 007370

A Keck/DEIMOS spectroscopic survey of the faint M31 satellites And IX, And XI, And XII and And XIII

Auteurs : M. L. M. Collins [Royaume-Uni] ; S. C. Chapman ; M. J. Irwin ; N. F. Martin [Allemagne] ; R. A. Ibata [France] ; D. B. Zucker [Australie] ; A. Blain [États-Unis] ; A. M. N. Ferguson [Royaume-Uni] ; G. F. Lewis [Australie] ; A. W. Mcconnachie [Canada] ; J. Pe Arrubia

Source :

Monthly Notices of the Royal Astronomical Society [ 0035-8711 ] ; 2010-10-01.

RBID : ISTEX:F5BA0CE9CBE76E0E53AA2F6B479C12162E00C587

Descripteurs français

Pascal (Inist)
- Abondance, Borne supérieure, Cinématique, Deimos, Dispersion vitesse, Dynamique, Etoile membre, Galaxies compagnons, Galaxies faibles, Galaxies naines, Galaxies sphéroïdales naines, Groupe local, Luminosité, Matière sombre, Métallicité, Photométrie, Rapport signal bruit, Satellite Mars, Vitesse radiale, Voie lactée.
Wicri :
- topic : Satellite.

English descriptors

Abstract

We present the first spectroscopic analysis of the faint M31 satellite galaxies, And XI and And XIII, as well as a re‐analysis of existing spectroscopic data for two further faint companions, And IX (correcting for an error in earlier geometric modelling that caused a misclassification of member stars in previous work) and And XII. By combining data obtained using the Deep Imaging Multi‐Object Spectrograph (DEIMOS) mounted on the Keck II telescope with deep photometry from the Suprime‐Cam instrument on Subaru, we have identified the most probable members for each of the satellites based on their radial velocities (precise to several down to i∼ 22), distance from the centre of the dwarf spheroidal galaxies (dSphs) and their photometric [Fe/H]. Using both the photometric and spectroscopic data, we have also calculated global properties for the dwarfs, such as systemic velocities, metallicities and half‐light radii. We find each dwarf to be very metal poor ([Fe/H]∼−2 both photometrically and spectroscopically, from their stacked spectrum), and as such, they continue to follow the luminosity–metallicity relationship established with brighter dwarfs. We are unable to resolve dispersion for And XI due to small sample size and low signal‐to‐noise ratio, but we set a 1σ upper limit of σv < 4.5 km s−1. For And IX, And XII and And XIII we resolve velocity dispersions of σv= 4.5+3.6−3.4, 2.6+5.1−2.6 and 9.7+8.9−4.5 km s−1, though we note that the dispersion for And XIII is based on just three stars. We derive masses within the half‐light radii for these galaxies of 6.2+5.3−5.1× 106, 2.4+6.5−2.4× 106 and 1.1+1.4−0.7× 107 M⊙, respectively. We discuss each satellite in the context of the Mateo relations for dSphs, and in reference to the universal halo profiles established for Milky Way dwarfs. Both And IX and And XII fall below the universal halo profiles of Walker et al., indicating that they are less massive than would be expected for objects of their half‐light radius. When combined with the findings of McConnachie & Irwin, which reveal that the M31 satellites are twice as extended (in terms of both half‐light and tidal radii) as their Milky Way counterparts, these results suggest that the satellite population of the Andromeda system could inhabit haloes that with regard to their central densities are significantly different from those of the Milky Way.

Url:

DOI: 10.1111/j.1365-2966.2010.17069.x

Affiliations:

Le document en format XML

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<profileDesc><textClass><keywords scheme="KwdEn" xml:lang="en"><term>Absolute magnitude</term>
<term>Abundance</term>
<term>Arcmin</term>
<term>Arrubia</term>
<term>Average value</term>
<term>Background level</term>
<term>Bottom panel</term>
<term>Candidate member stars</term>
<term>Candidate members</term>
<term>Centre</term>
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<term>Common mass scale</term>
<term>Composite spectra</term>
<term>Composite spectrum</term>
<term>Contaminant</term>
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<term>Dark matter halo</term>
<term>Dark matter haloes</term>
<term>Dartmouth isochrones</term>
<term>Deimos</term>
<term>Deimos candidate members</term>
<term>Dispersion</term>
<term>Distance modulus</term>
<term>Dotter</term>
<term>Dsph</term>
<term>Dsph population</term>
<term>Dsphs</term>
<term>Dsphs population</term>
<term>Dwarf</term>
<term>Dwarf centre</term>
<term>Dwarf galaxies</term>
<term>Dwarf spheroidal galaxies</term>
<term>Dynamics</term>
<term>Error bars</term>
<term>Exponential</term>
<term>Exponential models</term>
<term>Faint dsphs</term>
<term>Faint galaxies</term>
<term>Faint satellites</term>
<term>Fainter</term>
<term>Galaxy</term>
<term>Geha</term>
<term>Good agreement</term>
<term>Grating</term>
<term>Grebel</term>
<term>Halo</term>
<term>Halo stars</term>
<term>Harbeck</term>
<term>Ibata</term>
<term>Illingworth</term>
<term>Irwin</term>
<term>Isochrone</term>
<term>Journal compilation</term>
<term>Kalirai</term>
<term>Keck</term>
<term>Kinematic</term>
<term>Kinematic data</term>
<term>Kinematic grouping</term>
<term>Kinematic properties</term>
<term>Kinematic results</term>
<term>Kinematics</term>
<term>Koch</term>
<term>Likelihood distributions</term>
<term>Line grating</term>
<term>Local group</term>
<term>Local group dsphs</term>
<term>Lower panel</term>
<term>Luminosity</term>
<term>Luminosity function</term>
<term>Mars satellite</term>
<term>Mass estimators</term>
<term>Mass limit</term>
<term>Mateo</term>
<term>Matter haloes</term>
<term>Maximum likelihood analysis</term>
<term>Mcconnachie</term>
<term>Mcconnachie irwin</term>
<term>Median</term>
<term>Member star</term>
<term>Member stars</term>
<term>Metallicities</term>
<term>Metallicity</term>
<term>Metallicity range</term>
<term>Milky Way</term>
<term>Mnras</term>
<term>Modulus</term>
<term>More metal</term>
<term>Ndings</term>
<term>Outlier</term>
<term>Overplotted</term>
<term>Photometric</term>
<term>Photometric conditions</term>
<term>Photometric metallicities</term>
<term>Photometric metallicity</term>
<term>Photometric properties</term>
<term>Photometrically</term>
<term>Photometry</term>
<term>Pink squares</term>
<term>Plausible members</term>
<term>Plummer</term>
<term>Private communication</term>
<term>Probable members</term>
<term>Radial velocity</term>
<term>Radius</term>
<term>Respective radii</term>
<term>Richstone</term>
<term>Richstone tremaine</term>
<term>Same format</term>
<term>Same trgb monte carlo procedure</term>
<term>Satellite</term>
<term>Satellite galaxies</term>
<term>Signal-to-noise ratio</term>
<term>Similar luminosity</term>
<term>Simon geha</term>
<term>Small sample size</term>
<term>Spectroscopic</term>
<term>Spectroscopic data</term>
<term>Spectroscopic properties</term>
<term>Spectroscopic results</term>
<term>Spectroscopically</term>
<term>Spectroscopically panel</term>
<term>Star</term>
<term>Star star</term>
<term>Stellar</term>
<term>Structural parameters</term>
<term>Structural properties</term>
<term>Subaru</term>
<term>Subaru data</term>
<term>Subaru photometry</term>
<term>Subaru telescope</term>
<term>Systematic error</term>
<term>Systemic velocities</term>
<term>Systemic velocity</term>
<term>Tanvir</term>
<term>Telluric</term>
<term>Third line</term>
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<term>Tidal radii</term>
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<term>Tremaine</term>
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<term>Borne supérieure</term>
<term>Cinématique</term>
<term>Deimos</term>
<term>Dispersion vitesse</term>
<term>Dynamique</term>
<term>Etoile membre</term>
<term>Galaxies compagnons</term>
<term>Galaxies faibles</term>
<term>Galaxies naines</term>
<term>Galaxies sphéroïdales naines</term>
<term>Groupe local</term>
<term>Luminosité</term>
<term>Matière sombre</term>
<term>Métallicité</term>
<term>Photométrie</term>
<term>Rapport signal bruit</term>
<term>Satellite Mars</term>
<term>Vitesse radiale</term>
<term>Voie lactée</term>
</keywords>
<keywords scheme="Teeft" xml:lang="en"><term>Absolute magnitude</term>
<term>Arcmin</term>
<term>Arrubia</term>
<term>Average value</term>
<term>Background level</term>
<term>Bottom panel</term>
<term>Candidate member stars</term>
<term>Candidate members</term>
<term>Centre</term>
<term>Chapman</term>
<term>Clear peak</term>
<term>Common mass scale</term>
<term>Composite spectra</term>
<term>Composite spectrum</term>
<term>Contaminant</term>
<term>Dark matter content</term>
<term>Dark matter halo</term>
<term>Dark matter haloes</term>
<term>Dartmouth isochrones</term>
<term>Deimos</term>
<term>Deimos candidate members</term>
<term>Dispersion</term>
<term>Distance modulus</term>
<term>Dotter</term>
<term>Dsph</term>
<term>Dsph population</term>
<term>Dsphs</term>
<term>Dsphs population</term>
<term>Dwarf</term>
<term>Dwarf centre</term>
<term>Dwarf galaxies</term>
<term>Error bars</term>
<term>Exponential</term>
<term>Exponential models</term>
<term>Faint dsphs</term>
<term>Faint satellites</term>
<term>Fainter</term>
<term>Galaxy</term>
<term>Geha</term>
<term>Good agreement</term>
<term>Grating</term>
<term>Grebel</term>
<term>Halo</term>
<term>Halo stars</term>
<term>Harbeck</term>
<term>Ibata</term>
<term>Illingworth</term>
<term>Irwin</term>
<term>Isochrone</term>
<term>Journal compilation</term>
<term>Kalirai</term>
<term>Keck</term>
<term>Kinematic</term>
<term>Kinematic data</term>
<term>Kinematic grouping</term>
<term>Kinematic properties</term>
<term>Kinematic results</term>
<term>Koch</term>
<term>Likelihood distributions</term>
<term>Line grating</term>
<term>Local group</term>
<term>Local group dsphs</term>
<term>Lower panel</term>
<term>Luminosity</term>
<term>Luminosity function</term>
<term>Mass estimators</term>
<term>Mass limit</term>
<term>Mateo</term>
<term>Matter haloes</term>
<term>Maximum likelihood analysis</term>
<term>Mcconnachie</term>
<term>Mcconnachie irwin</term>
<term>Median</term>
<term>Member stars</term>
<term>Metallicities</term>
<term>Metallicity</term>
<term>Metallicity range</term>
<term>Mnras</term>
<term>Modulus</term>
<term>More metal</term>
<term>Ndings</term>
<term>Outlier</term>
<term>Overplotted</term>
<term>Photometric</term>
<term>Photometric conditions</term>
<term>Photometric metallicities</term>
<term>Photometric metallicity</term>
<term>Photometric properties</term>
<term>Photometrically</term>
<term>Photometry</term>
<term>Pink squares</term>
<term>Plausible members</term>
<term>Plummer</term>
<term>Private communication</term>
<term>Probable members</term>
<term>Radial velocity</term>
<term>Radius</term>
<term>Respective radii</term>
<term>Richstone</term>
<term>Richstone tremaine</term>
<term>Same format</term>
<term>Same trgb monte carlo procedure</term>
<term>Satellite</term>
<term>Similar luminosity</term>
<term>Simon geha</term>
<term>Small sample size</term>
<term>Spectroscopic</term>
<term>Spectroscopic data</term>
<term>Spectroscopic properties</term>
<term>Spectroscopic results</term>
<term>Spectroscopically</term>
<term>Spectroscopically panel</term>
<term>Star</term>
<term>Star star</term>
<term>Stellar</term>
<term>Structural parameters</term>
<term>Structural properties</term>
<term>Subaru</term>
<term>Subaru data</term>
<term>Subaru photometry</term>
<term>Subaru telescope</term>
<term>Systematic error</term>
<term>Systemic velocities</term>
<term>Systemic velocity</term>
<term>Tanvir</term>
<term>Telluric</term>
<term>Third line</term>
<term>Tidal</term>
<term>Tidal radii</term>
<term>Tidal radius</term>
<term>Total luminosity</term>
<term>Tremaine</term>
<term>Trgb</term>
<term>Triplet</term>
<term>Triplet lines</term>
<term>True trgb</term>
<term>Upper limit</term>
<term>Velocity dispersion</term>
<term>Velocity dispersions</term>
<term>Virial equilibrium</term>
<term>Wavelength range</term>
<term>Willman</term>
<term>Xiii</term>
<term>Zucker</term>
</keywords>
<keywords scheme="Wicri" type="topic" xml:lang="fr"><term>Satellite</term>
</keywords>
</textClass>
</profileDesc>
</teiHeader>
<front><div type="abstract" xml:lang="en">We present the first spectroscopic analysis of the faint M31 satellite galaxies, And XI and And XIII, as well as a re‐analysis of existing spectroscopic data for two further faint companions, And IX (correcting for an error in earlier geometric modelling that caused a misclassification of member stars in previous work) and And XII. By combining data obtained using the Deep Imaging Multi‐Object Spectrograph (DEIMOS) mounted on the Keck II telescope with deep photometry from the Suprime‐Cam instrument on Subaru, we have identified the most probable members for each of the satellites based on their radial velocities (precise to several down to i∼ 22), distance from the centre of the dwarf spheroidal galaxies (dSphs) and their photometric [Fe/H]. Using both the photometric and spectroscopic data, we have also calculated global properties for the dwarfs, such as systemic velocities, metallicities and half‐light radii. We find each dwarf to be very metal poor ([Fe/H]∼−2 both photometrically and spectroscopically, from their stacked spectrum), and as such, they continue to follow the luminosity–metallicity relationship established with brighter dwarfs. We are unable to resolve dispersion for And XI due to small sample size and low signal‐to‐noise ratio, but we set a 1σ upper limit of σv < 4.5 km s−1. For And IX, And XII and And XIII we resolve velocity dispersions of σv= 4.5+3.6−3.4, 2.6+5.1−2.6 and 9.7+8.9−4.5 km s−1, though we note that the dispersion for And XIII is based on just three stars. We derive masses within the half‐light radii for these galaxies of 6.2+5.3−5.1× 106, 2.4+6.5−2.4× 106 and 1.1+1.4−0.7× 107 M⊙, respectively. We discuss each satellite in the context of the Mateo relations for dSphs, and in reference to the universal halo profiles established for Milky Way dwarfs. Both And IX and And XII fall below the universal halo profiles of Walker et al., indicating that they are less massive than would be expected for objects of their half‐light radius. When combined with the findings of McConnachie & Irwin, which reveal that the M31 satellites are twice as extended (in terms of both half‐light and tidal radii) as their Milky Way counterparts, these results suggest that the satellite population of the Andromeda system could inhabit haloes that with regard to their central densities are significantly different from those of the Milky Way.</div>
</front>
</TEI>
<affiliations><list><country><li>Allemagne</li>
<li>Australie</li>
<li>Canada</li>
<li>France</li>
<li>Royaume-Uni</li>
<li>États-Unis</li>
</country>
<region><li>Bade-Wurtemberg</li>
<li>Californie</li>
<li>District de Karlsruhe</li>
<li>Nouvelle-Galles du Sud</li>
<li>Écosse</li>
</region>
<settlement><li>Heidelberg</li>
<li>Sydney</li>
<li>Édimbourg</li>
</settlement>
<orgName><li>Université d'Édimbourg</li>
<li>Université de Sydney</li>
</orgName>
</list>
<tree><noCountry><name sortKey="Chapman, S C" sort="Chapman, S C" uniqKey="Chapman S" first="S. C." last="Chapman">S. C. Chapman</name>
<name sortKey="Irwin, M J" sort="Irwin, M J" uniqKey="Irwin M" first="M. J." last="Irwin">M. J. Irwin</name>
<name sortKey="Pe Arrubia, J" sort="Pe Arrubia, J" uniqKey="Pe Arrubia J" first="J." last="Pe Arrubia">J. Pe Arrubia</name>
</noCountry>
<country name="Royaume-Uni"><noRegion><name sortKey="Collins, M L M" sort="Collins, M L M" uniqKey="Collins M" first="M. L. M." last="Collins">M. L. M. Collins</name>
</noRegion>
<name sortKey="Ferguson, A M N" sort="Ferguson, A M N" uniqKey="Ferguson A" first="A. M. N." last="Ferguson">A. M. N. Ferguson</name>
</country>
<country name="Allemagne"><region name="Bade-Wurtemberg"><name sortKey="Martin, N F" sort="Martin, N F" uniqKey="Martin N" first="N. F." last="Martin">N. F. Martin</name>
</region>
</country>
<country name="France"><noRegion><name sortKey="Ibata, R A" sort="Ibata, R A" uniqKey="Ibata R" first="R. A." last="Ibata">R. A. Ibata</name>
</noRegion>
</country>
<country name="Australie"><noRegion><name sortKey="Zucker, D B" sort="Zucker, D B" uniqKey="Zucker D" first="D. B." last="Zucker">D. B. Zucker</name>
</noRegion>
<name sortKey="Lewis, G F" sort="Lewis, G F" uniqKey="Lewis G" first="G. F." last="Lewis">G. F. Lewis</name>
<name sortKey="Zucker, D B" sort="Zucker, D B" uniqKey="Zucker D" first="D. B." last="Zucker">D. B. Zucker</name>
</country>
<country name="États-Unis"><region name="Californie"><name sortKey="Blain, A" sort="Blain, A" uniqKey="Blain A" first="A." last="Blain">A. Blain</name>
</region>
</country>
<country name="Canada"><noRegion><name sortKey="Mcconnachie, A W" sort="Mcconnachie, A W" uniqKey="Mcconnachie A" first="A. W." last="Mcconnachie">A. W. Mcconnachie</name>
</noRegion>
</country>
</tree>
</affiliations>
</record>

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A Keck/DEIMOS spectroscopic survey of the faint M31 satellites And IX, And XI, And XII and And XIII

A Keck/DEIMOS spectroscopic survey of the faint M31 satellites And IX, And XI, And XII and And XIII

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