Blanco DECam Bulge Survey (BDBS), IV. Metallicity distributions and bulge structure from 2.6 million red clump stars
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 d...
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| Autori principali: | , , , , , , , , , , , , , , |
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| Natura: | Article (Journal) |
| Lingua: | inglese |
| Pubblicazione: |
09 July 2022
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| In: |
Monthly notices of the Royal Astronomical Society
Year: 2022, Volume: 515, Fascicolo: 1, Pages: 1469-1491 |
| ISSN: | 1365-2966 |
| DOI: | 10.1093/mnras/stac1840 |
| Accesso online: | Verlag, lizenzpflichtig, Volltext: https://doi.org/10.1093/mnras/stac1840
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| Note sull'autore: | 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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| 245 | 1 | 0 | |a Blanco DECam Bulge Survey (BDBS), IV. Metallicity distributions and bulge structure from 2.6 million red clump stars |c 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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| 520 | |a 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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| 700 | 1 | |a Young, Michael D |e VerfasserIn |4 aut | |
| 700 | 1 | |a Clarkson, William I |e VerfasserIn |4 aut | |
| 700 | 1 | |a Pilachowski, Catherine A |e VerfasserIn |4 aut | |
| 700 | 1 | |a Michael, Scott |e VerfasserIn |4 aut | |
| 700 | 1 | |a Marchetti, Tommaso |e VerfasserIn |0 (DE-588)1268133086 |0 (DE-627)1816709840 |4 aut | |
| 700 | 1 | |a Soto, Mario |e VerfasserIn |4 aut | |
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| 700 | 1 | |a Katherina Vivas, A |e VerfasserIn |4 aut | |
| 700 | 1 | |a Joyce, Meridith |e VerfasserIn |4 aut | |
| 700 | 1 | |a Shen, Juntai |e VerfasserIn |4 aut | |
| 700 | 1 | |a Osmond, Alexis |e VerfasserIn |4 aut | |
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