Chemical Analysis of the Brightest Star of the Cetus II Ultrafaint Dwarf Galaxy Candidate
We present a detailed chemical abundance analysis of the brightest star in the ultrafaint dwarf (UFD) galaxy candidate Cetus II from high-resolution Magellan/MIKE spectra. For this star, DES J011740.53-173053, abundances or upper limits of 18 elements from carbon to europium are derived. Its chemica...
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IOP Publishing
2023-01-01
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| Series: | The Astrophysical Journal |
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| Online Access: | https://doi.org/10.3847/1538-4357/ad0385 |
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| author | K. B. Webber T. T. Hansen J. L. Marshall J. D. Simon A. B. Pace B. Mutlu-Pakdil A. Drlica-Wagner C. E. Martínez-Vázquez M. Aguena S. S. Allam O. Alves E. Bertin D. Brooks A. Carnero Rosell J. Carretero L. N. da Costa J. De Vicente P. Doel I. Ferrero D. Friedel J. Frieman J. García-Bellido G. Giannini D. Gruen R. A. Gruendl S. R. Hinton D. L. Hollowood K. Honscheid K. Kuehn J. Mena-Fernández F. Menanteau R. Miquel R. L. C. Ogando M. E. S. Pereira A. Pieres A. A. Plazas Malagón E. Sanchez B. Santiago J. Allyn Smith M. Smith E. Suchyta G. Tarle C. To N. Weaverdyck B. Yanny |
| author_facet | K. B. Webber T. T. Hansen J. L. Marshall J. D. Simon A. B. Pace B. Mutlu-Pakdil A. Drlica-Wagner C. E. Martínez-Vázquez M. Aguena S. S. Allam O. Alves E. Bertin D. Brooks A. Carnero Rosell J. Carretero L. N. da Costa J. De Vicente P. Doel I. Ferrero D. Friedel J. Frieman J. García-Bellido G. Giannini D. Gruen R. A. Gruendl S. R. Hinton D. L. Hollowood K. Honscheid K. Kuehn J. Mena-Fernández F. Menanteau R. Miquel R. L. C. Ogando M. E. S. Pereira A. Pieres A. A. Plazas Malagón E. Sanchez B. Santiago J. Allyn Smith M. Smith E. Suchyta G. Tarle C. To N. Weaverdyck B. Yanny |
| author_sort | K. B. Webber |
| collection | DOAJ |
| description | We present a detailed chemical abundance analysis of the brightest star in the ultrafaint dwarf (UFD) galaxy candidate Cetus II from high-resolution Magellan/MIKE spectra. For this star, DES J011740.53-173053, abundances or upper limits of 18 elements from carbon to europium are derived. Its chemical abundances generally follow those of other UFD galaxy stars, with a slight enhancement of the α -elements (Mg, Si, and Ca) and low neutron-capture element (Sr, Ba, and Eu) abundances supporting the classification of Cetus II as a likely UFD. The star exhibits lower Sc, Ti, and V abundances than Milky Way (MW) halo stars with similar metallicity. This signature is consistent with yields from a supernova originating from a star with a mass of ∼11.2 M _⊙ . In addition, the star has a potassium abundance of [K/Fe] = 0.81, which is somewhat higher than the K abundances of MW halo stars with similar metallicity, a signature that is also present in a number of UFD galaxies. A comparison including globular clusters and stellar stream stars suggests that high K is a specific characteristic of some UFD galaxy stars and can thus be used to help classify objects as UFD galaxies. |
| first_indexed | 2024-03-08T23:06:31Z |
| format | Article |
| id | doaj.art-829cad72c7524cfeaf9acfcf2c5d6dc6 |
| institution | Directory Open Access Journal |
| issn | 1538-4357 |
| language | English |
| last_indexed | 2024-03-08T23:06:31Z |
| publishDate | 2023-01-01 |
| publisher | IOP Publishing |
| record_format | Article |
| series | The Astrophysical Journal |
| spelling | doaj.art-829cad72c7524cfeaf9acfcf2c5d6dc62023-12-15T11:39:23ZengIOP PublishingThe Astrophysical Journal1538-43572023-01-01959214110.3847/1538-4357/ad0385Chemical Analysis of the Brightest Star of the Cetus II Ultrafaint Dwarf Galaxy CandidateK. B. Webber0https://orcid.org/0000-0002-9762-4308T. T. Hansen1https://orcid.org/0000-0001-6154-8983J. L. Marshall2J. D. Simon3https://orcid.org/0000-0002-4733-4994A. B. Pace4https://orcid.org/0000-0002-6021-8760B. Mutlu-Pakdil5https://orcid.org/0000-0001-9649-4815A. Drlica-Wagner6https://orcid.org/0000-0001-8251-933XC. E. Martínez-Vázquez7https://orcid.org/0000-0002-9144-7726M. Aguena8https://orcid.org/0000-0001-5679-6747S. S. Allam9https://orcid.org/0000-0002-7069-7857O. Alves10https://orcid.org/0000-0002-7394-9466E. Bertin11https://orcid.org/0000-0002-3602-3664D. Brooks12https://orcid.org/0000-0002-8458-5047A. Carnero Rosell13https://orcid.org/0000-0003-3044-5150J. Carretero14https://orcid.org/0000-0002-3130-0204L. N. da Costa15https://orcid.org/0000-0002-7731-277XJ. De Vicente16https://orcid.org/0000-0001-8318-6813P. Doel17I. Ferrero18https://orcid.org/0000-0002-1295-1132D. Friedel19https://orcid.org/0000-0002-3632-7668J. Frieman20https://orcid.org/0000-0003-4079-3263J. García-Bellido21https://orcid.org/0000-0002-9370-8360G. Giannini22https://orcid.org/0000-0002-3730-1750D. Gruen23https://orcid.org/0000-0003-3270-7644R. A. Gruendl24https://orcid.org/0000-0002-4588-6517S. R. Hinton25https://orcid.org/0000-0003-2071-9349D. L. Hollowood26https://orcid.org/0000-0002-9369-4157K. Honscheid27https://orcid.org/0000-0002-6550-2023K. Kuehn28https://orcid.org/0000-0003-0120-0808J. Mena-Fernández29https://orcid.org/0000-0001-9497-7266F. Menanteau30https://orcid.org/0000-0002-1372-2534R. Miquel31https://orcid.org/0000-0002-6610-4836R. L. C. Ogando32https://orcid.org/0000-0003-2120-1154M. E. S. Pereira33https://orcid.org/0000-0002-7131-7684A. Pieres34https://orcid.org/0000-0001-9186-6042A. A. Plazas Malagón35https://orcid.org/0000-0002-2598-0514E. Sanchez36https://orcid.org/0000-0002-9646-8198B. Santiago37J. Allyn Smith38https://orcid.org/0000-0002-6261-4601M. Smith39https://orcid.org/0000-0002-3321-1432E. Suchyta40https://orcid.org/0000-0002-7047-9358G. Tarle41https://orcid.org/0000-0003-1704-0781C. To42https://orcid.org/0000-0001-7836-2261N. Weaverdyck43https://orcid.org/0000-0001-9382-5199B. Yanny44https://orcid.org/0000-0002-9541-2678Mitchell Institute for Fundamental Physics and Astronomy and Department of Physics and Astronomy, Texas A&M University , College Station, TX 77843-4242, USA ; kbwebber@tamu.eduDepartment of Astronomy, Stockholm University , AlbaNova University Center, SE-106 91 Stockholm, SwedenMitchell Institute for Fundamental Physics and Astronomy and Department of Physics and Astronomy, Texas A&M University , College Station, TX 77843-4242, USA ; kbwebber@tamu.eduObservatories of the Carnegie Institution for Science , 813 Santa Barbara St., Pasadena, CA 91101, USAMcWilliams Center for Cosmology, Carnegie Mellon University , 5000 Forbes Ave., Pittsburgh, PA 15213, USADepartment of Physics and Astronomy, Dartmouth College , Hanover, NH 03755, USAFermi National Accelerator Laboratory , P.O. Box 500, Batavia, IL 60510, USA; Kavli Institute for Cosmological Physics, University of Chicago , Chicago, IL 60637, USA; Department of Astronomy and Astrophysics, University of Chicago , Chicago, IL 60637, USAGemini Observatory, NSF's NOIRLab , 670 N. A’ohoku Pl., Hilo, HI 96720, USA; Cerro Tololo Inter-American Observatory, NSF's NOIRLab , Casilla 603, La Serena, ChileLaboratório Interinstitucional de e-Astronomia—LIneA , Rua Gal. José Cristino 77, Rio de Janeiro, RJ—20921-400, BrazilFermi National Accelerator Laboratory , P.O. Box 500, Batavia, IL 60510, USADepartment of Physics, University of Michigan , Ann Arbor, MI:48109, USACNRS, UMR 7095, Institut d’Astrophysique de Paris , F-75014, Paris, France; Sorbonne Universités, UPMC Univ Paris 06 , UMR 7095, Institut d’Astrophysique de Paris, F-75014, Paris, FranceDepartment of Physics & Astronomy, University College London , Gower St., London, WC1E 6BT, UKLaboratório Interinstitucional de e-Astronomia—LIneA , Rua Gal. José Cristino 77, Rio de Janeiro, RJ—20921-400, Brazil; Instituto de Astrofisica de Canarias , E-38205 La Laguna, Tenerife, Spain; Universidad de La Laguna , Dpto. Astrofísica, E-38206 La Laguna, Tenerife, SpainInstitut de Física d’Altes Energies (IFAE) , The Barcelona Institute of Science and Technology, Campus UAB, E-08193 Bellaterra Barcelona, SpainLaboratório Interinstitucional de e-Astronomia—LIneA , Rua Gal. José Cristino 77, Rio de Janeiro, RJ—20921-400, BrazilCentro de Investigaciones Energéticas , Medioambientales y Tecnológicas (CIEMAT), Madrid, SpainDepartment of Physics & Astronomy, University College London , Gower St., London, WC1E 6BT, UKInstitute of Theoretical Astrophysics, University of Oslo.P.O. Box 1029 Blindern , NO-0315 Oslo, NorwayCenter for Astrophysical Surveys , National Center for Supercomputing Applications, 1205 West Clark St., Urbana, IL 61801, USAFermi National Accelerator Laboratory , P.O. Box 500, Batavia, IL 60510, USA; Kavli Institute for Cosmological Physics, University of Chicago , Chicago, IL 60637, USAInstituto de Fisica Teorica UAM/CSIC, Universidad Autonoma de Madrid , E-28049 Madrid, SpainInstitut de Física d’Altes Energies (IFAE) , The Barcelona Institute of Science and Technology, Campus UAB, E-08193 Bellaterra Barcelona, SpainUniversity Observatory, Faculty of Physics, Ludwig-Maximilians-Universität , Scheinerstr. 1, D-81679 Munich, GermanyCenter for Astrophysical Surveys , National Center for Supercomputing Applications, 1205 West Clark St., Urbana, IL 61801, USA; Department of Astronomy, University of Illinois at Urbana-Champaign , 1002 W. Green St., Urbana, IL 61801, USASchool of Mathematics and Physics, University of Queensland , Brisbane, QLD 4072, AustraliaSanta Cruz Institute for Particle Physics , Santa Cruz, CA 95064, USACenter for Cosmology and Astro-Particle Physics, The Ohio State University , Columbus, OH 43210, USA; Department of Physics, The Ohio State University , Columbus, OH 43210, USAAustralian Astronomical Optics, Macquarie University , North Ryde, NSW 2113, Australia; Lowell Observatory , 1400 Mars Hill Rd., Flagstaff, AZ 86001, USACentro de Investigaciones Energéticas , Medioambientales y Tecnológicas (CIEMAT), Madrid, SpainCenter for Astrophysical Surveys , National Center for Supercomputing Applications, 1205 West Clark St., Urbana, IL 61801, USA; Department of Astronomy, University of Illinois at Urbana-Champaign , 1002 W. Green St., Urbana, IL 61801, USAInstitut de Física d’Altes Energies (IFAE) , The Barcelona Institute of Science and Technology, Campus UAB, E-08193 Bellaterra Barcelona, Spain; Institució Catalana de Recerca i Estudis Avançats , E-08010 Barcelona, SpainObservatório Nacional , Rua Gal. José Cristino 77, Rio de Janeiro, RJ—20921-400, BrazilHamburger Sternwarte, Universität Hamburg , Gojenbergsweg 112, D-21029 Hamburg, GermanyLaboratório Interinstitucional de e-Astronomia—LIneA , Rua Gal. José Cristino 77, Rio de Janeiro, RJ—20921-400, Brazil; Observatório Nacional , Rua Gal. José Cristino 77, Rio de Janeiro, RJ—20921-400, BrazilKavli Institute for Particle Astrophysics & Cosmology, P.O. Box 2450, Stanford University , Stanford, CA 94305, USA; SLAC National Accelerator Laboratory , Menlo Park, CA 94025, USACentro de Investigaciones Energéticas , Medioambientales y Tecnológicas (CIEMAT), Madrid, SpainLaboratório Interinstitucional de e-Astronomia—LIneA , Rua Gal. José Cristino 77, Rio de Janeiro, RJ—20921-400, Brazil; Instituto de Física , UFRGS, Caixa Postal 15051, Porto Alegre, RS—91501-970, BrazilAustin Peay State University , Dept. Physics, Engineering and Astronomy, P.O. Box 4608 Clarksville, TN 37044, USASchool of Physics and Astronomy, University of Southampton , Southampton, SO17 1BJ, UKComputer Science and Mathematics Division , Oak Ridge National Laboratory, Oak Ridge, TN 37831, USADepartment of Physics, University of Michigan , Ann Arbor, MI:48109, USACenter for Cosmology and Astro-Particle Physics, The Ohio State University , Columbus, OH 43210, USADepartment of Physics, University of Michigan , Ann Arbor, MI:48109, USA; Lawrence Berkeley National Laboratory , 1 Cyclotron Rd., Berkeley, CA 94720, USAFermi National Accelerator Laboratory , P.O. Box 500, Batavia, IL 60510, USAWe present a detailed chemical abundance analysis of the brightest star in the ultrafaint dwarf (UFD) galaxy candidate Cetus II from high-resolution Magellan/MIKE spectra. For this star, DES J011740.53-173053, abundances or upper limits of 18 elements from carbon to europium are derived. Its chemical abundances generally follow those of other UFD galaxy stars, with a slight enhancement of the α -elements (Mg, Si, and Ca) and low neutron-capture element (Sr, Ba, and Eu) abundances supporting the classification of Cetus II as a likely UFD. The star exhibits lower Sc, Ti, and V abundances than Milky Way (MW) halo stars with similar metallicity. This signature is consistent with yields from a supernova originating from a star with a mass of ∼11.2 M _⊙ . In addition, the star has a potassium abundance of [K/Fe] = 0.81, which is somewhat higher than the K abundances of MW halo stars with similar metallicity, a signature that is also present in a number of UFD galaxies. A comparison including globular clusters and stellar stream stars suggests that high K is a specific characteristic of some UFD galaxy stars and can thus be used to help classify objects as UFD galaxies.https://doi.org/10.3847/1538-4357/ad0385Chemical abundancesStellar abundances |
| spellingShingle | K. B. Webber T. T. Hansen J. L. Marshall J. D. Simon A. B. Pace B. Mutlu-Pakdil A. Drlica-Wagner C. E. Martínez-Vázquez M. Aguena S. S. Allam O. Alves E. Bertin D. Brooks A. Carnero Rosell J. Carretero L. N. da Costa J. De Vicente P. Doel I. Ferrero D. Friedel J. Frieman J. García-Bellido G. Giannini D. Gruen R. A. Gruendl S. R. Hinton D. L. Hollowood K. Honscheid K. Kuehn J. Mena-Fernández F. Menanteau R. Miquel R. L. C. Ogando M. E. S. Pereira A. Pieres A. A. Plazas Malagón E. Sanchez B. Santiago J. Allyn Smith M. Smith E. Suchyta G. Tarle C. To N. Weaverdyck B. Yanny Chemical Analysis of the Brightest Star of the Cetus II Ultrafaint Dwarf Galaxy Candidate The Astrophysical Journal Chemical abundances Stellar abundances |
| title | Chemical Analysis of the Brightest Star of the Cetus II Ultrafaint Dwarf Galaxy Candidate |
| title_full | Chemical Analysis of the Brightest Star of the Cetus II Ultrafaint Dwarf Galaxy Candidate |
| title_fullStr | Chemical Analysis of the Brightest Star of the Cetus II Ultrafaint Dwarf Galaxy Candidate |
| title_full_unstemmed | Chemical Analysis of the Brightest Star of the Cetus II Ultrafaint Dwarf Galaxy Candidate |
| title_short | Chemical Analysis of the Brightest Star of the Cetus II Ultrafaint Dwarf Galaxy Candidate |
| title_sort | chemical analysis of the brightest star of the cetus ii ultrafaint dwarf galaxy candidate |
| topic | Chemical abundances Stellar abundances |
| url | https://doi.org/10.3847/1538-4357/ad0385 |
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