1 Ocak 2018 Dergi makalesi Açık Erişim

Sen, S.; Peletier, R. F.; Boselli, A.; den Brok, M.; Falcon-Barroso, J.; Hensler, G.; Janz, J.; Laurikainen, E.; Lisker, T.; Mentz, J. J.; Paudel, S.; Salo, H.; Sybilska, A.; Toloba, E.; van de Ven, G.; Vazdekis, A.; Yesilyaprak, C.

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  <identifier identifierType="URL">https://aperta.ulakbim.gov.tr/record/36177</identifier>
  <creators>
    <creator>
      <creatorName>Sen, S.</creatorName>
      <givenName>S.</givenName>
      <familyName>Sen</familyName>
    </creator>
    <creator>
      <creatorName>Peletier, R. F.</creatorName>
      <givenName>R. F.</givenName>
      <familyName>Peletier</familyName>
      <affiliation>Univ Groningen, Kapteyn Astron Inst, POB 800, NL-9700 AV Groningen, Netherlands</affiliation>
    </creator>
    <creator>
      <creatorName>Boselli, A.</creatorName>
      <givenName>A.</givenName>
      <familyName>Boselli</familyName>
      <affiliation>Aix Marseille Univ, CNRS, LAM, UMR 7326, F-13388 Marseille, France</affiliation>
    </creator>
    <creator>
      <creatorName>den Brok, M.</creatorName>
      <givenName>M.</givenName>
      <familyName>den Brok</familyName>
      <affiliation>ETH, Inst Astron, Wolfgang Pauli Str 27, CH-8093 Zurich, Switzerland</affiliation>
    </creator>
    <creator>
      <creatorName>Falcon-Barroso, J.</creatorName>
      <givenName>J.</givenName>
      <familyName>Falcon-Barroso</familyName>
    </creator>
    <creator>
      <creatorName>Hensler, G.</creatorName>
      <givenName>G.</givenName>
      <familyName>Hensler</familyName>
      <affiliation>Univ Vienna, Dept Astrophys, Turkenschanzstr 17, A-1180 Vienna, Austria</affiliation>
    </creator>
    <creator>
      <creatorName>Janz, J.</creatorName>
      <givenName>J.</givenName>
      <familyName>Janz</familyName>
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    <creator>
      <creatorName>Laurikainen, E.</creatorName>
      <givenName>E.</givenName>
      <familyName>Laurikainen</familyName>
      <affiliation>Univ Oulu, Astron Res Unit, FI-90014 Oulu, Finland</affiliation>
    </creator>
    <creator>
      <creatorName>Lisker, T.</creatorName>
      <givenName>T.</givenName>
      <familyName>Lisker</familyName>
      <affiliation>Heidelberg Univ, Zentrum Astron, Astron Rech Inst, Monchhofstr 12-14, D-69120 Heidelberg, Germany</affiliation>
    </creator>
    <creator>
      <creatorName>Mentz, J. J.</creatorName>
      <givenName>J. J.</givenName>
      <familyName>Mentz</familyName>
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    <creator>
      <creatorName>Paudel, S.</creatorName>
      <givenName>S.</givenName>
      <familyName>Paudel</familyName>
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    <creator>
      <creatorName>Salo, H.</creatorName>
      <givenName>H.</givenName>
      <familyName>Salo</familyName>
      <affiliation>Univ Oulu, Astron Res Unit, FI-90014 Oulu, Finland</affiliation>
    </creator>
    <creator>
      <creatorName>Sybilska, A.</creatorName>
      <givenName>A.</givenName>
      <familyName>Sybilska</familyName>
      <affiliation>European Southern Observ, Karl Schwarzschild Str 2, D-85748 Garching, Germany</affiliation>
    </creator>
    <creator>
      <creatorName>Toloba, E.</creatorName>
      <givenName>E.</givenName>
      <familyName>Toloba</familyName>
      <affiliation>Univ Pacific, Dept Phys, 3601 Pacific Ave, Stockton, CA 95211 USA</affiliation>
    </creator>
    <creator>
      <creatorName>van de Ven, G.</creatorName>
      <givenName>G.</givenName>
      <familyName>van de Ven</familyName>
      <affiliation>Max Planck Inst Astron, Konigstuhl 17, D-69117 Heidelberg, Germany</affiliation>
    </creator>
    <creator>
      <creatorName>Vazdekis, A.</creatorName>
      <givenName>A.</givenName>
      <familyName>Vazdekis</familyName>
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    <creator>
      <creatorName>Yesilyaprak, C.</creatorName>
      <givenName>C.</givenName>
      <familyName>Yesilyaprak</familyName>
      <affiliation>Ataturk Univ, Dept Astron &amp; Astrophys, Fac Sci, TR-25030 Erzurum, Turkey</affiliation>
    </creator>
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  <titles>
    <title>Abundance Ratios In Dwarf Elliptical Galaxies</title>
  </titles>
  <publisher>Aperta</publisher>
  <publicationYear>2018</publicationYear>
  <dates>
    <date dateType="Issued">2018-01-01</date>
  </dates>
  <resourceType resourceTypeGeneral="Text">Journal article</resourceType>
  <alternateIdentifiers>
    <alternateIdentifier alternateIdentifierType="url">https://aperta.ulakbim.gov.tr/record/36177</alternateIdentifier>
  </alternateIdentifiers>
  <relatedIdentifiers>
    <relatedIdentifier relatedIdentifierType="DOI" relationType="IsIdenticalTo">10.1093/mnras/stx3254</relatedIdentifier>
  </relatedIdentifiers>
  <rightsList>
    <rights rightsURI="http://www.opendefinition.org/licenses/cc-by">Creative Commons Attribution</rights>
    <rights rightsURI="info:eu-repo/semantics/openAccess">Open Access</rights>
  </rightsList>
  <descriptions>
    <description descriptionType="Abstract">We determine abundance ratios of 37 dwarf ellipticals (dEs) in the nearby Virgo cluster. This sample is representative of the early-type population of galaxies in the absolute magnitude range -19.0 &amp;lt; M-r &amp;lt; -16.0. We analyse their absorption line-strength indices by means of index-index diagrams and scaling relations and use the stellar population models to interpret them. We present ages, metallicities, and abundance ratios obtained from these dEs within an aperture size of R-e/8. We calculate [Na/Fe] from NaD, [Ca/Fe] from Ca4227, and [Mg/Fe] from Mgb. We find that [Na/Fe] is underabundant with respect to solar, whereas [Mg/Fe] is around solar. This is exactly opposite to what is found for giant ellipticals, but follows the trend with metallicity found previously for the Fornax dwarf NGC 1396. We discuss possible formation scenarios that can result in such elemental abundance patterns, and we speculate that dEs have disc-like star formation history (SFH) favouring them to originate from late-type dwarfs or small spirals. Na-yields appear to be very metal-dependent, in agreement with studies of giant ellipticals, probably due to the large dependence on the neutron-excess in stars. We conclude that dEs have undergone a considerable amount of chemical evolution, they are therefore not uniformly old, but have extended SFH, similar to many of the Local Group galaxies.</description>
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