AustralieFrV1, PascalFrancis, Corpus, bibRecord, 004A88

Distances and metallicities for 17 Local Group galaxies

Identifieur interne : 004A88 ( PascalFrancis/Corpus ); précédent : 004A87; suivant : 004A89

Distances and metallicities for 17 Local Group galaxies

Auteurs : A. W. Mcconnachie ; M. J. Irwin ; A. M. N. Ferguson ; R. A. Ibata ; G. F. Lewis ; N. Tanvir

Source :

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

RBID : Pascal:05-0109855

Descripteurs français

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

English descriptors

KwdEn :
- Absolute magnitude, Comparative study, Dwarf galaxies, Galaxy groups, Giant galaxies, Local group, Metallicity, Photometry, Red giant stars, Spiral galaxies, Stellar content, Stellar population, Subgroup, Uncertainty.

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.

Notice en format standard (ISO 2709)

Pour connaître la documentation sur le format Inist Standard.

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A05				`@2 356`
A06				`@2 3`
A08	`01`	`1`	`ENG`	`@1 Distances and metallicities for 17 Local Group galaxies`
A11	`01`	`1`		`@1 MCCONNACHIE (A. W.)`
A11	`02`	`1`		`@1 IRWIN (M. J.)`
A11	`03`	`1`		`@1 FERGUSON (A. M. N.)`
A11	`04`	`1`		`@1 IBATA (R. A.)`
A11	`05`	`1`		`@1 LEWIS (G. F.)`
A11	`06`	`1`		`@1 TANVIR (N.)`
A14	`01`			`@1 Institute of Astronomy, Madingley Road @2 Cambridge CB3 0HA @3 USA @Z 1 aut. @Z 2 aut.`
A14	`02`			`@1 Max-Planck-Institut für Astrophysik, Karl-Schwarzschild-Str 1, Postfach 1317 @2 85741 Garching @3 DEU @Z 3 aut.`
A14	`03`			`@1 Observatoire de Strasbourg, 11, rue de l'Universite @2 67000, Strasbourg @3 FRA @Z 4 aut.`
A14	`04`			`@1 Institute of Astronomy, School of Physics, A29, University of Sydney @2 NSW 2006 @3 AUS @Z 5 aut.`
A14	`05`			`@1 Physical Sciences, University of Hertfordshire @2 Hatfield AL10 9AB @3 GBR @Z 6 aut.`
A20				`@1 979-997`
A21				`@1 2005`
A23	`01`			`@0 ENG`
A43	`01`			`@1 INIST @2 2067 @5 354000126732660190`
A44				`@0 0000 @1 © 2005 INIST-CNRS. All rights reserved.`
A45				`@0 98 ref.`
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C01	`01`		`ENG`	@0 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.
C02	`01`	`3`		`@0 001E03`
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C03	`01`	`X`	`ENG`	`@0 Metallicity @5 26`
C03	`01`	`X`	`SPA`	`@0 Metalicidad @5 26`
C03	`02`	`3`	`FRE`	`@0 Groupe local @5 27`
C03	`02`	`3`	`ENG`	`@0 Local group @5 27`
C03	`03`	`3`	`FRE`	`@0 Groupe galaxies @5 28`
C03	`03`	`3`	`ENG`	`@0 Galaxy groups @5 28`
C03	`04`	`3`	`FRE`	`@0 Photométrie @5 29`
C03	`04`	`3`	`ENG`	`@0 Photometry @5 29`
C03	`05`	`X`	`FRE`	`@0 Galaxies géantes @5 30`
C03	`05`	`X`	`ENG`	`@0 Giant galaxies @5 30`
C03	`05`	`X`	`SPA`	`@0 Galaxias gigantes @5 30`
C03	`06`	`X`	`FRE`	`@0 Sous groupe @5 31`
C03	`06`	`X`	`ENG`	`@0 Subgroup @5 31`
C03	`06`	`X`	`SPA`	`@0 Subgrupo @5 31`
C03	`07`	`3`	`FRE`	`@0 Géante rouge @5 32`
C03	`07`	`3`	`ENG`	`@0 Red giant stars @5 32`
C03	`08`	`X`	`FRE`	`@0 Incertitude @5 33`
C03	`08`	`X`	`ENG`	`@0 Uncertainty @5 33`
C03	`08`	`X`	`SPA`	`@0 Incertidumbre @5 33`
C03	`09`	`X`	`FRE`	`@0 Population stellaire @5 34`
C03	`09`	`X`	`ENG`	`@0 Stellar population @5 34`
C03	`09`	`X`	`SPA`	`@0 Población estelar @5 34`
C03	`10`	`3`	`FRE`	`@0 Galaxies spirales @5 35`
C03	`10`	`3`	`ENG`	`@0 Spiral galaxies @5 35`
C03	`11`	`3`	`FRE`	`@0 Galaxies naines @5 36`
C03	`11`	`3`	`ENG`	`@0 Dwarf galaxies @5 36`
C03	`12`	`X`	`FRE`	`@0 Magnitude absolue @5 37`
C03	`12`	`X`	`ENG`	`@0 Absolute magnitude @5 37`
C03	`12`	`X`	`SPA`	`@0 Magnitud absoluta @5 37`
C03	`13`	`X`	`FRE`	`@0 Etude comparative @5 38`
C03	`13`	`X`	`ENG`	`@0 Comparative study @5 38`
C03	`13`	`X`	`SPA`	`@0 Estudio comparativo @5 38`
C03	`14`	`X`	`FRE`	`@0 Contenu stellaire @5 39`
C03	`14`	`X`	`ENG`	`@0 Stellar content @5 39`
C03	`14`	`X`	`SPA`	`@0 Contenido estelar @5 39`
N21				`@1 073`
N44	`01`			`@1 OTO`
N82				`@1 OTO`

Format Inist (serveur)

NO :	PASCAL 05-0109855 INIST
ET :	Distances and metallicities for 17 Local Group galaxies
AU :	MCCONNACHIE (A. W.); IRWIN (M. J.); FERGUSON (A. M. N.); IBATA (R. A.); LEWIS (G. F.); TANVIR (N.)
AF :	Institute of Astronomy, Madingley Road/Cambridge CB3 0HA/Etats-Unis (1 aut., 2 aut.); Max-Planck-Institut für Astrophysik, Karl-Schwarzschild-Str 1, Postfach 1317/85741 Garching/Allemagne (3 aut.); Observatoire de Strasbourg, 11, rue de l'Universite/67000, Strasbourg/France (4 aut.); Institute of Astronomy, School of Physics, A29, University of Sydney/NSW 2006/Australie (5 aut.); Physical Sciences, University of Hertfordshire/Hatfield AL10 9AB/Royaume-Uni (6 aut.)
DT :	Publication en série; Niveau analytique
SO :	Monthly Notices of the Royal Astronomical Society; ISSN 0035-8711; Coden MNRAA4; Royaume-Uni; Da. 2005; Vol. 356; No. 3; Pp. 979-997; Bibl. 98 ref.
LA :	Anglais
EA :	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.
CC :	001E03
FD :	Métallicité; Groupe local; Groupe galaxies; Photométrie; Galaxies géantes; Sous groupe; Géante rouge; Incertitude; Population stellaire; Galaxies spirales; Galaxies naines; Magnitude absolue; Etude comparative; Contenu stellaire
ED :	Metallicity; Local group; Galaxy groups; Photometry; Giant galaxies; Subgroup; Red giant stars; Uncertainty; Stellar population; Spiral galaxies; Dwarf galaxies; Absolute magnitude; Comparative study; Stellar content
SD :	Metalicidad; Galaxias gigantes; Subgrupo; Incertidumbre; Población estelar; Magnitud absoluta; Estudio comparativo; Contenido estelar
LO :	INIST-2067.354000126732660190
ID :	05-0109855

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Pascal:05-0109855

Le document en format XML

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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>
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<fC01 i1="01" l="ENG"><s0>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.</s0>
</fC01>
<fC02 i1="01" i2="3"><s0>001E03</s0>
</fC02>
<fC03 i1="01" i2="X" l="FRE"><s0>Métallicité</s0>
<s5>26</s5>
</fC03>
<fC03 i1="01" i2="X" l="ENG"><s0>Metallicity</s0>
<s5>26</s5>
</fC03>
<fC03 i1="01" i2="X" l="SPA"><s0>Metalicidad</s0>
<s5>26</s5>
</fC03>
<fC03 i1="02" i2="3" l="FRE"><s0>Groupe local</s0>
<s5>27</s5>
</fC03>
<fC03 i1="02" i2="3" l="ENG"><s0>Local group</s0>
<s5>27</s5>
</fC03>
<fC03 i1="03" i2="3" l="FRE"><s0>Groupe galaxies</s0>
<s5>28</s5>
</fC03>
<fC03 i1="03" i2="3" l="ENG"><s0>Galaxy groups</s0>
<s5>28</s5>
</fC03>
<fC03 i1="04" i2="3" l="FRE"><s0>Photométrie</s0>
<s5>29</s5>
</fC03>
<fC03 i1="04" i2="3" l="ENG"><s0>Photometry</s0>
<s5>29</s5>
</fC03>
<fC03 i1="05" i2="X" l="FRE"><s0>Galaxies géantes</s0>
<s5>30</s5>
</fC03>
<fC03 i1="05" i2="X" l="ENG"><s0>Giant galaxies</s0>
<s5>30</s5>
</fC03>
<fC03 i1="05" i2="X" l="SPA"><s0>Galaxias gigantes</s0>
<s5>30</s5>
</fC03>
<fC03 i1="06" i2="X" l="FRE"><s0>Sous groupe</s0>
<s5>31</s5>
</fC03>
<fC03 i1="06" i2="X" l="ENG"><s0>Subgroup</s0>
<s5>31</s5>
</fC03>
<fC03 i1="06" i2="X" l="SPA"><s0>Subgrupo</s0>
<s5>31</s5>
</fC03>
<fC03 i1="07" i2="3" l="FRE"><s0>Géante rouge</s0>
<s5>32</s5>
</fC03>
<fC03 i1="07" i2="3" l="ENG"><s0>Red giant stars</s0>
<s5>32</s5>
</fC03>
<fC03 i1="08" i2="X" l="FRE"><s0>Incertitude</s0>
<s5>33</s5>
</fC03>
<fC03 i1="08" i2="X" l="ENG"><s0>Uncertainty</s0>
<s5>33</s5>
</fC03>
<fC03 i1="08" i2="X" l="SPA"><s0>Incertidumbre</s0>
<s5>33</s5>
</fC03>
<fC03 i1="09" i2="X" l="FRE"><s0>Population stellaire</s0>
<s5>34</s5>
</fC03>
<fC03 i1="09" i2="X" l="ENG"><s0>Stellar population</s0>
<s5>34</s5>
</fC03>
<fC03 i1="09" i2="X" l="SPA"><s0>Población estelar</s0>
<s5>34</s5>
</fC03>
<fC03 i1="10" i2="3" l="FRE"><s0>Galaxies spirales</s0>
<s5>35</s5>
</fC03>
<fC03 i1="10" i2="3" l="ENG"><s0>Spiral galaxies</s0>
<s5>35</s5>
</fC03>
<fC03 i1="11" i2="3" l="FRE"><s0>Galaxies naines</s0>
<s5>36</s5>
</fC03>
<fC03 i1="11" i2="3" l="ENG"><s0>Dwarf galaxies</s0>
<s5>36</s5>
</fC03>
<fC03 i1="12" i2="X" l="FRE"><s0>Magnitude absolue</s0>
<s5>37</s5>
</fC03>
<fC03 i1="12" i2="X" l="ENG"><s0>Absolute magnitude</s0>
<s5>37</s5>
</fC03>
<fC03 i1="12" i2="X" l="SPA"><s0>Magnitud absoluta</s0>
<s5>37</s5>
</fC03>
<fC03 i1="13" i2="X" l="FRE"><s0>Etude comparative</s0>
<s5>38</s5>
</fC03>
<fC03 i1="13" i2="X" l="ENG"><s0>Comparative study</s0>
<s5>38</s5>
</fC03>
<fC03 i1="13" i2="X" l="SPA"><s0>Estudio comparativo</s0>
<s5>38</s5>
</fC03>
<fC03 i1="14" i2="X" l="FRE"><s0>Contenu stellaire</s0>
<s5>39</s5>
</fC03>
<fC03 i1="14" i2="X" l="ENG"><s0>Stellar content</s0>
<s5>39</s5>
</fC03>
<fC03 i1="14" i2="X" l="SPA"><s0>Contenido estelar</s0>
<s5>39</s5>
</fC03>
<fN21><s1>073</s1>
</fN21>
<fN44 i1="01"><s1>OTO</s1>
</fN44>
<fN82><s1>OTO</s1>
</fN82>
</pA>
</standard>
<server><NO>PASCAL 05-0109855 INIST</NO>
<ET>Distances and metallicities for 17 Local Group galaxies</ET>
<AU>MCCONNACHIE (A. W.); IRWIN (M. J.); FERGUSON (A. M. N.); IBATA (R. A.); LEWIS (G. F.); TANVIR (N.)</AU>
<AF>Institute of Astronomy, Madingley Road/Cambridge CB3 0HA/Etats-Unis (1 aut., 2 aut.); Max-Planck-Institut für Astrophysik, Karl-Schwarzschild-Str 1, Postfach 1317/85741 Garching/Allemagne (3 aut.); Observatoire de Strasbourg, 11, rue de l'Universite/67000, Strasbourg/France (4 aut.); Institute of Astronomy, School of Physics, A29, University of Sydney/NSW 2006/Australie (5 aut.); Physical Sciences, University of Hertfordshire/Hatfield AL10 9AB/Royaume-Uni (6 aut.)</AF>
<DT>Publication en série; Niveau analytique</DT>
<SO>Monthly Notices of the Royal Astronomical Society; ISSN 0035-8711; Coden MNRAA4; Royaume-Uni; Da. 2005; Vol. 356; No. 3; Pp. 979-997; Bibl. 98 ref.</SO>
<LA>Anglais</LA>
<EA>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.</EA>
<CC>001E03</CC>
<FD>Métallicité; Groupe local; Groupe galaxies; Photométrie; Galaxies géantes; Sous groupe; Géante rouge; Incertitude; Population stellaire; Galaxies spirales; Galaxies naines; Magnitude absolue; Etude comparative; Contenu stellaire</FD>
<ED>Metallicity; Local group; Galaxy groups; Photometry; Giant galaxies; Subgroup; Red giant stars; Uncertainty; Stellar population; Spiral galaxies; Dwarf galaxies; Absolute magnitude; Comparative study; Stellar content</ED>
<SD>Metalicidad; Galaxias gigantes; Subgrupo; Incertidumbre; Población estelar; Magnitud absoluta; Estudio comparativo; Contenido estelar</SD>
<LO>INIST-2067.354000126732660190</LO>
<ID>05-0109855</ID>
</server>
</inist>
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Distances and metallicities for 17 Local Group galaxies

Distances and metallicities for 17 Local Group galaxies

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