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| Verfasst von: | Johnson, Christian I. [VerfasserIn]  |
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| | Rich, R Michael [VerfasserIn] |
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| | Simion, Iulia T [VerfasserIn] |
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| | Young, Michael D [VerfasserIn] |
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| | Clarkson, William I [VerfasserIn] |
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| | Pilachowski, Catherine A [VerfasserIn] |
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| | Michael, Scott [VerfasserIn] |
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| | Marchetti, Tommaso [VerfasserIn] |
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| | Soto, Mario [VerfasserIn] |
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| | Kunder, Andrea [VerfasserIn] |
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| | Koch-Hansen, Andreas [VerfasserIn] |
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| | Katherina Vivas, A [VerfasserIn] |
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| | Joyce, Meridith [VerfasserIn] |
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| | Shen, Juntai [VerfasserIn] |
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| | Osmond, Alexis [VerfasserIn] |
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| Titel: | Blanco DECam Bulge Survey (BDBS), IV. Metallicity distributions and bulge structure from 2.6 million red clump stars |
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| Verf.angabe: | Christian I. Johnson, R. Michael Rich, Iulia T. Simion, Michael D.Young, William I. Clarkson, Catherine A. Pilachowski, Scott Michael, Tommaso Marchetti, Mario Soto, Andrea Kunder, Andreas J. Koch-Hansen, A.Katherina Vivas, Meridith Joyce, Juntai Shen and Alexis Osmond |
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| E-Jahr: | 2022 |
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| Jahr: | 09 July 2022 |
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| Umfang: | 23 S. |
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| Fussnoten: | Gesehen am 14.09.2022 |
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| Titel Quelle: | Enthalten in: Royal Astronomical SocietyMonthly notices of the Royal Astronomical Society |
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| Ort Quelle: | Oxford : Oxford Univ. Press, 1827 |
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| Jahr Quelle: | 2022 |
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| Band/Heft Quelle: | 515(2022), 1, Seite 1469-1491 |
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| ISSN Quelle: | 1365-2966 |
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| Abstract: | We present photometric metallicity measurements for a sample of 2.6 million bulge red clump stars extracted from the Blanco DECam Bulge Survey (BDBS). Similar to previous studies, we find that the bulge exhibits a strong vertical metallicity gradient, and that at least two peaks in the metallicity distribution functions appear at b < −5°. We can discern a metal-poor ([Fe/H] ∼ −0.3) and metal-rich ([Fe/H] ∼ +0.2) abundance distribution that each show clear systematic trends with latitude, and may be best understood by changes in the bulge’s star formation/enrichment processes. Both groups exhibit asymmetric tails, and as a result we argue that the proximity of a star to either peak in [Fe/H] space is not necessarily an affirmation of group membership. The metal-poor peak shifts to lower [Fe/H] values at larger distances from the plane while the metal-rich tail truncates. Close to the plane, the metal-rich tail appears broader along the minor axis than in off-axis fields. We also posit that the bulge has two metal-poor populations - one that belongs to the metal-poor tail of the low latitude and predominantly metal-rich group, and another belonging to the metal-poor group that dominates in the outer bulge. We detect the X-shape structure in fields with |Z| > 0.7 kpc and for stars with [Fe/H] > −0.5. Stars with [Fe/H] < −0.5 may form a spheroidal or ‘thick bar’ distribution while those with [Fe/H] $\gtrsim$ −0.1 are strongly concentrated near the plane. |
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| DOI: | doi:10.1093/mnras/stac1840 |
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| URL: | Bitte beachten Sie: Dies ist ein Bibliographieeintrag. Ein Volltextzugriff für Mitglieder der Universität besteht hier nur, falls für die entsprechende Zeitschrift/den entsprechenden Sammelband ein Abonnement besteht oder es sich um einen OpenAccess-Titel handelt.
Volltext: https://doi.org/10.1093/mnras/stac1840 |
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| | DOI: https://doi.org/10.1093/mnras/stac1840 |
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| Datenträger: | Online-Ressource |
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| Sprache: | eng |
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| K10plus-PPN: | 1816647705 |
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| Verknüpfungen: | → Zeitschrift |
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Blanco DECam Bulge Survey (BDBS), IV. Metallicity distributions and bulge structure from 2.6 million red clump stars / Johnson, Christian I. [VerfasserIn]; 09 July 2022 (Online-Ressource)
