APOGEE Chemical Abundances of the Sagittarius Dwarf Galaxy
- Autores
- Hasselquist, Sten; Shetrone, Matthew; Smith, Verne; Holtzman, Jon; McWilliam, Andrew; Fernández Trincado, J. G.; Beers, Timothy C.; Majewski, Steven R.; Nidever, David L.; Tang, Baitian; Tissera, Patricia Beatriz; Alvar, Emma Fernández; Allende Prieto, Carlos; Almeida, Andres; Anguiano, Borja; Battaglia, Giuseppina; Carigi, Leticia; Delgado Inglada, Gloria; Frinchaboy, Peter; García-Hernández, D. A.; Geisler, Doug; Minniti, Dante; Placco, Vinicius M.; Schultheis, Mathias; Sobeck, Jennifer; Villanova, Sandro
- Año de publicación
- 2017
- Idioma
- inglés
- Tipo de recurso
- artículo
- Estado
- versión publicada
- Descripción
- The Apache Point Observatory Galactic Evolution Experiment provides the opportunity of measuring elemental abundances for C, N, O, Na, Mg, Al, Si, P, K, Ca, V, Cr, Mn, Fe, Co, and Ni in vast numbers of stars. We analyze thechemical-abundance patterns of these elements for 158 red giant stars belonging to the Sagittarius dwarf galaxy (Sgr). This is the largest sample of Sgr stars with detailed chemical abundances, and it is the first time that C, N, P, K, V, Cr, Co, and Ni have been studied at high resolution in this galaxy. We find that the Sgr stars with [Fe/H] ≳ -0.8 are deficient in all elemental abundance ratios (expressed as [X/Fe]) relative to the Milky Way, suggesting that the Sgr stars observed today were formed from gas that was less enriched by Type II SNe than stars formed in the Milky Way. By examining the relative deficiencies of the hydrostatic (O, Na, Mg, and Al) and explosive (Si, P, K, and Mn) elements, our analysis supports the argument that previous generations of Sgr stars were formed with a top-light initial mass function, one lacking the most massive stars that would normally pollute the interstellar medium with the hydrostatic elements. We use a simple chemical-evolution model, flexCE, to further support our claim and conclude that recent stellar generations of Fornax and the Large Magellanic Cloud could also have formed according to a top-light initial mass function.
Fil: Hasselquist, Sten. Universidad Andrés Bello; Chile
Fil: Shetrone, Matthew. Universidad Andrés Bello; Chile
Fil: Smith, Verne. Universidad Andrés Bello; Chile
Fil: Holtzman, Jon. Universidad Andrés Bello; Chile
Fil: McWilliam, Andrew. Universidad Andrés Bello; Chile
Fil: Fernández Trincado, J. G.. Universidad Andrés Bello; Chile
Fil: Beers, Timothy C.. Universidad Andrés Bello; Chile
Fil: Majewski, Steven R.. Universidad Andrés Bello; Chile
Fil: Nidever, David L.. Universidad Andrés Bello; Chile
Fil: Tang, Baitian. Universidad Andrés Bello; Chile
Fil: Tissera, Patricia Beatriz. Universidad Andrés Bello; Chile. Consejo Nacional de Investigaciónes Científicas y Técnicas. Oficina de Coordinación Administrativa Ciudad Universitaria. Instituto de Astronomía y Física del Espacio. - Universidad de Buenos Aires. Facultad de Ciencias Exactas y Naturales. Instituto de Astronomía y Física del Espacio; Argentina
Fil: Alvar, Emma Fernández. Universidad Andrés Bello; Chile
Fil: Allende Prieto, Carlos. Universidad Andrés Bello; Chile
Fil: Almeida, Andres. Universidad Andrés Bello; Chile
Fil: Anguiano, Borja. Universidad Andrés Bello; Chile
Fil: Battaglia, Giuseppina. Universidad Andrés Bello; Chile
Fil: Carigi, Leticia. Universidad Andrés Bello; Chile
Fil: Delgado Inglada, Gloria. Universidad Andrés Bello; Chile
Fil: Frinchaboy, Peter. Universidad Andrés Bello; Chile
Fil: García-Hernández, D. A.. Universidad Andrés Bello; Chile
Fil: Geisler, Doug. Universidad Andrés Bello; Chile
Fil: Minniti, Dante. Universidad Andrés Bello; Chile
Fil: Placco, Vinicius M.. Universidad Andrés Bello; Chile
Fil: Schultheis, Mathias. Universidad Andrés Bello; Chile
Fil: Sobeck, Jennifer. Universidad Andrés Bello; Chile
Fil: Villanova, Sandro. Universidad Andrés Bello; Chile - Materia
-
galaxies: dwarf
galaxies: individual (Sagittarius dSph)
galaxies: stellar content - Nivel de accesibilidad
- acceso abierto
- Condiciones de uso
- https://creativecommons.org/licenses/by-nc-sa/2.5/ar/
- Repositorio
.jpg)
- Institución
- Consejo Nacional de Investigaciones Científicas y Técnicas
- OAI Identificador
- oai:ri.conicet.gov.ar:11336/292089
Ver los metadatos del registro completo
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APOGEE Chemical Abundances of the Sagittarius Dwarf GalaxyHasselquist, StenShetrone, MatthewSmith, VerneHoltzman, JonMcWilliam, AndrewFernández Trincado, J. G.Beers, Timothy C.Majewski, Steven R.Nidever, David L.Tang, BaitianTissera, Patricia BeatrizAlvar, Emma FernándezAllende Prieto, CarlosAlmeida, AndresAnguiano, BorjaBattaglia, GiuseppinaCarigi, LeticiaDelgado Inglada, GloriaFrinchaboy, PeterGarcía-Hernández, D. A.Geisler, DougMinniti, DantePlacco, Vinicius M.Schultheis, MathiasSobeck, JenniferVillanova, Sandrogalaxies: dwarfgalaxies: individual (Sagittarius dSph)galaxies: stellar contenthttps://purl.org/becyt/ford/1.3https://purl.org/becyt/ford/1The Apache Point Observatory Galactic Evolution Experiment provides the opportunity of measuring elemental abundances for C, N, O, Na, Mg, Al, Si, P, K, Ca, V, Cr, Mn, Fe, Co, and Ni in vast numbers of stars. We analyze thechemical-abundance patterns of these elements for 158 red giant stars belonging to the Sagittarius dwarf galaxy (Sgr). This is the largest sample of Sgr stars with detailed chemical abundances, and it is the first time that C, N, P, K, V, Cr, Co, and Ni have been studied at high resolution in this galaxy. We find that the Sgr stars with [Fe/H] ≳ -0.8 are deficient in all elemental abundance ratios (expressed as [X/Fe]) relative to the Milky Way, suggesting that the Sgr stars observed today were formed from gas that was less enriched by Type II SNe than stars formed in the Milky Way. By examining the relative deficiencies of the hydrostatic (O, Na, Mg, and Al) and explosive (Si, P, K, and Mn) elements, our analysis supports the argument that previous generations of Sgr stars were formed with a top-light initial mass function, one lacking the most massive stars that would normally pollute the interstellar medium with the hydrostatic elements. We use a simple chemical-evolution model, flexCE, to further support our claim and conclude that recent stellar generations of Fornax and the Large Magellanic Cloud could also have formed according to a top-light initial mass function.Fil: Hasselquist, Sten. Universidad Andrés Bello; ChileFil: Shetrone, Matthew. Universidad Andrés Bello; ChileFil: Smith, Verne. Universidad Andrés Bello; ChileFil: Holtzman, Jon. Universidad Andrés Bello; ChileFil: McWilliam, Andrew. Universidad Andrés Bello; ChileFil: Fernández Trincado, J. G.. Universidad Andrés Bello; ChileFil: Beers, Timothy C.. Universidad Andrés Bello; ChileFil: Majewski, Steven R.. Universidad Andrés Bello; ChileFil: Nidever, David L.. Universidad Andrés Bello; ChileFil: Tang, Baitian. Universidad Andrés Bello; ChileFil: Tissera, Patricia Beatriz. Universidad Andrés Bello; Chile. Consejo Nacional de Investigaciónes Científicas y Técnicas. Oficina de Coordinación Administrativa Ciudad Universitaria. Instituto de Astronomía y Física del Espacio. - Universidad de Buenos Aires. Facultad de Ciencias Exactas y Naturales. Instituto de Astronomía y Física del Espacio; ArgentinaFil: Alvar, Emma Fernández. Universidad Andrés Bello; ChileFil: Allende Prieto, Carlos. Universidad Andrés Bello; ChileFil: Almeida, Andres. Universidad Andrés Bello; ChileFil: Anguiano, Borja. Universidad Andrés Bello; ChileFil: Battaglia, Giuseppina. Universidad Andrés Bello; ChileFil: Carigi, Leticia. Universidad Andrés Bello; ChileFil: Delgado Inglada, Gloria. Universidad Andrés Bello; ChileFil: Frinchaboy, Peter. Universidad Andrés Bello; ChileFil: García-Hernández, D. A.. Universidad Andrés Bello; ChileFil: Geisler, Doug. Universidad Andrés Bello; ChileFil: Minniti, Dante. Universidad Andrés Bello; ChileFil: Placco, Vinicius M.. Universidad Andrés Bello; ChileFil: Schultheis, Mathias. Universidad Andrés Bello; ChileFil: Sobeck, Jennifer. Universidad Andrés Bello; ChileFil: Villanova, Sandro. Universidad Andrés Bello; ChileIOP Publishing2017-08info:eu-repo/semantics/articleinfo:eu-repo/semantics/publishedVersionhttp://purl.org/coar/resource_type/c_6501info:ar-repo/semantics/articuloapplication/pdfapplication/pdfapplication/pdfhttp://hdl.handle.net/11336/292089Hasselquist, Sten; Shetrone, Matthew; Smith, Verne; Holtzman, Jon; McWilliam, Andrew; et al.; APOGEE Chemical Abundances of the Sagittarius Dwarf Galaxy; IOP Publishing; Astrophysical Journal; 845; 2; 8-2017; 1-140004-637XCONICET DigitalCONICETenginfo:eu-repo/semantics/altIdentifier/url/https://iopscience.iop.org/article/10.3847/1538-4357/aa7ddcinfo:eu-repo/semantics/altIdentifier/doi/10.3847/1538-4357/aa7ddcinfo:eu-repo/semantics/openAccesshttps://creativecommons.org/licenses/by-nc-sa/2.5/ar/reponame:CONICET Digital (CONICET)instname:Consejo Nacional de Investigaciones Científicas y Técnicas2026-08-25T15:42:28Zoai:ri.conicet.gov.ar:11336/292089instacron:CONICETInstitucionalhttp://ri.conicet.gov.ar/Organismo científico-tecnológicoNo correspondehttp://ri.conicet.gov.ar/oai/requestdasensio@conicet.gov.ar; lcarlino@conicet.gov.arArgentinaNo correspondeNo correspondeNo correspondeopendoar:34982026-08-25 15:42:28.724CONICET Digital (CONICET) - Consejo Nacional de Investigaciones Científicas y Técnicasfalse |
| dc.title.none.fl_str_mv |
APOGEE Chemical Abundances of the Sagittarius Dwarf Galaxy |
| title |
APOGEE Chemical Abundances of the Sagittarius Dwarf Galaxy |
| spellingShingle |
APOGEE Chemical Abundances of the Sagittarius Dwarf Galaxy Hasselquist, Sten galaxies: dwarf galaxies: individual (Sagittarius dSph) galaxies: stellar content |
| title_short |
APOGEE Chemical Abundances of the Sagittarius Dwarf Galaxy |
| title_full |
APOGEE Chemical Abundances of the Sagittarius Dwarf Galaxy |
| title_fullStr |
APOGEE Chemical Abundances of the Sagittarius Dwarf Galaxy |
| title_full_unstemmed |
APOGEE Chemical Abundances of the Sagittarius Dwarf Galaxy |
| title_sort |
APOGEE Chemical Abundances of the Sagittarius Dwarf Galaxy |
| dc.creator.none.fl_str_mv |
Hasselquist, Sten Shetrone, Matthew Smith, Verne Holtzman, Jon McWilliam, Andrew Fernández Trincado, J. G. Beers, Timothy C. Majewski, Steven R. Nidever, David L. Tang, Baitian Tissera, Patricia Beatriz Alvar, Emma Fernández Allende Prieto, Carlos Almeida, Andres Anguiano, Borja Battaglia, Giuseppina Carigi, Leticia Delgado Inglada, Gloria Frinchaboy, Peter García-Hernández, D. A. Geisler, Doug Minniti, Dante Placco, Vinicius M. Schultheis, Mathias Sobeck, Jennifer Villanova, Sandro |
| author |
Hasselquist, Sten |
| author_facet |
Hasselquist, Sten Shetrone, Matthew Smith, Verne Holtzman, Jon McWilliam, Andrew Fernández Trincado, J. G. Beers, Timothy C. Majewski, Steven R. Nidever, David L. Tang, Baitian Tissera, Patricia Beatriz Alvar, Emma Fernández Allende Prieto, Carlos Almeida, Andres Anguiano, Borja Battaglia, Giuseppina Carigi, Leticia Delgado Inglada, Gloria Frinchaboy, Peter García-Hernández, D. A. Geisler, Doug Minniti, Dante Placco, Vinicius M. Schultheis, Mathias Sobeck, Jennifer Villanova, Sandro |
| author_role |
author |
| author2 |
Shetrone, Matthew Smith, Verne Holtzman, Jon McWilliam, Andrew Fernández Trincado, J. G. Beers, Timothy C. Majewski, Steven R. Nidever, David L. Tang, Baitian Tissera, Patricia Beatriz Alvar, Emma Fernández Allende Prieto, Carlos Almeida, Andres Anguiano, Borja Battaglia, Giuseppina Carigi, Leticia Delgado Inglada, Gloria Frinchaboy, Peter García-Hernández, D. A. Geisler, Doug Minniti, Dante Placco, Vinicius M. Schultheis, Mathias Sobeck, Jennifer Villanova, Sandro |
| author2_role |
author author author author author author author author author author author author author author author author author author author author author author author author author |
| dc.subject.none.fl_str_mv |
galaxies: dwarf galaxies: individual (Sagittarius dSph) galaxies: stellar content |
| topic |
galaxies: dwarf galaxies: individual (Sagittarius dSph) galaxies: stellar content |
| purl_subject.fl_str_mv |
https://purl.org/becyt/ford/1.3 https://purl.org/becyt/ford/1 |
| dc.description.none.fl_txt_mv |
The Apache Point Observatory Galactic Evolution Experiment provides the opportunity of measuring elemental abundances for C, N, O, Na, Mg, Al, Si, P, K, Ca, V, Cr, Mn, Fe, Co, and Ni in vast numbers of stars. We analyze thechemical-abundance patterns of these elements for 158 red giant stars belonging to the Sagittarius dwarf galaxy (Sgr). This is the largest sample of Sgr stars with detailed chemical abundances, and it is the first time that C, N, P, K, V, Cr, Co, and Ni have been studied at high resolution in this galaxy. We find that the Sgr stars with [Fe/H] ≳ -0.8 are deficient in all elemental abundance ratios (expressed as [X/Fe]) relative to the Milky Way, suggesting that the Sgr stars observed today were formed from gas that was less enriched by Type II SNe than stars formed in the Milky Way. By examining the relative deficiencies of the hydrostatic (O, Na, Mg, and Al) and explosive (Si, P, K, and Mn) elements, our analysis supports the argument that previous generations of Sgr stars were formed with a top-light initial mass function, one lacking the most massive stars that would normally pollute the interstellar medium with the hydrostatic elements. We use a simple chemical-evolution model, flexCE, to further support our claim and conclude that recent stellar generations of Fornax and the Large Magellanic Cloud could also have formed according to a top-light initial mass function. Fil: Hasselquist, Sten. Universidad Andrés Bello; Chile Fil: Shetrone, Matthew. Universidad Andrés Bello; Chile Fil: Smith, Verne. Universidad Andrés Bello; Chile Fil: Holtzman, Jon. Universidad Andrés Bello; Chile Fil: McWilliam, Andrew. Universidad Andrés Bello; Chile Fil: Fernández Trincado, J. G.. Universidad Andrés Bello; Chile Fil: Beers, Timothy C.. Universidad Andrés Bello; Chile Fil: Majewski, Steven R.. Universidad Andrés Bello; Chile Fil: Nidever, David L.. Universidad Andrés Bello; Chile Fil: Tang, Baitian. Universidad Andrés Bello; Chile Fil: Tissera, Patricia Beatriz. Universidad Andrés Bello; Chile. Consejo Nacional de Investigaciónes Científicas y Técnicas. Oficina de Coordinación Administrativa Ciudad Universitaria. Instituto de Astronomía y Física del Espacio. - Universidad de Buenos Aires. Facultad de Ciencias Exactas y Naturales. Instituto de Astronomía y Física del Espacio; Argentina Fil: Alvar, Emma Fernández. Universidad Andrés Bello; Chile Fil: Allende Prieto, Carlos. Universidad Andrés Bello; Chile Fil: Almeida, Andres. Universidad Andrés Bello; Chile Fil: Anguiano, Borja. Universidad Andrés Bello; Chile Fil: Battaglia, Giuseppina. Universidad Andrés Bello; Chile Fil: Carigi, Leticia. Universidad Andrés Bello; Chile Fil: Delgado Inglada, Gloria. Universidad Andrés Bello; Chile Fil: Frinchaboy, Peter. Universidad Andrés Bello; Chile Fil: García-Hernández, D. A.. Universidad Andrés Bello; Chile Fil: Geisler, Doug. Universidad Andrés Bello; Chile Fil: Minniti, Dante. Universidad Andrés Bello; Chile Fil: Placco, Vinicius M.. Universidad Andrés Bello; Chile Fil: Schultheis, Mathias. Universidad Andrés Bello; Chile Fil: Sobeck, Jennifer. Universidad Andrés Bello; Chile Fil: Villanova, Sandro. Universidad Andrés Bello; Chile |
| description |
The Apache Point Observatory Galactic Evolution Experiment provides the opportunity of measuring elemental abundances for C, N, O, Na, Mg, Al, Si, P, K, Ca, V, Cr, Mn, Fe, Co, and Ni in vast numbers of stars. We analyze thechemical-abundance patterns of these elements for 158 red giant stars belonging to the Sagittarius dwarf galaxy (Sgr). This is the largest sample of Sgr stars with detailed chemical abundances, and it is the first time that C, N, P, K, V, Cr, Co, and Ni have been studied at high resolution in this galaxy. We find that the Sgr stars with [Fe/H] ≳ -0.8 are deficient in all elemental abundance ratios (expressed as [X/Fe]) relative to the Milky Way, suggesting that the Sgr stars observed today were formed from gas that was less enriched by Type II SNe than stars formed in the Milky Way. By examining the relative deficiencies of the hydrostatic (O, Na, Mg, and Al) and explosive (Si, P, K, and Mn) elements, our analysis supports the argument that previous generations of Sgr stars were formed with a top-light initial mass function, one lacking the most massive stars that would normally pollute the interstellar medium with the hydrostatic elements. We use a simple chemical-evolution model, flexCE, to further support our claim and conclude that recent stellar generations of Fornax and the Large Magellanic Cloud could also have formed according to a top-light initial mass function. |
| publishDate |
2017 |
| dc.date.none.fl_str_mv |
2017-08 |
| dc.type.none.fl_str_mv |
info:eu-repo/semantics/article info:eu-repo/semantics/publishedVersion http://purl.org/coar/resource_type/c_6501 info:ar-repo/semantics/articulo |
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article |
| status_str |
publishedVersion |
| dc.identifier.none.fl_str_mv |
http://hdl.handle.net/11336/292089 Hasselquist, Sten; Shetrone, Matthew; Smith, Verne; Holtzman, Jon; McWilliam, Andrew; et al.; APOGEE Chemical Abundances of the Sagittarius Dwarf Galaxy; IOP Publishing; Astrophysical Journal; 845; 2; 8-2017; 1-14 0004-637X CONICET Digital CONICET |
| url |
http://hdl.handle.net/11336/292089 |
| identifier_str_mv |
Hasselquist, Sten; Shetrone, Matthew; Smith, Verne; Holtzman, Jon; McWilliam, Andrew; et al.; APOGEE Chemical Abundances of the Sagittarius Dwarf Galaxy; IOP Publishing; Astrophysical Journal; 845; 2; 8-2017; 1-14 0004-637X CONICET Digital CONICET |
| dc.language.none.fl_str_mv |
eng |
| language |
eng |
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info:eu-repo/semantics/altIdentifier/url/https://iopscience.iop.org/article/10.3847/1538-4357/aa7ddc info:eu-repo/semantics/altIdentifier/doi/10.3847/1538-4357/aa7ddc |
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info:eu-repo/semantics/openAccess https://creativecommons.org/licenses/by-nc-sa/2.5/ar/ |
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openAccess |
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application/pdf application/pdf application/pdf |
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IOP Publishing |
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IOP Publishing |
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