Chemical abundance gradients from open clusters in the Milky Way disk: Results from the APOGEE survey

Cunha, Kátia; Frinchaboy, Peter M.; Souto, Diogo; Thompson, B. J.; Zasowski, Gail; Prieto, C. Allende; Carrera, R.; Chiappini, Cristina; Donor, John; Garcia-Hernandez, Anibal; Pérez, Ana E. García; Hayden, Michael R.; Holtzman, Jon A.; Jackson, Kelly M.; Johnson, Jennifer A.; Majewski, Steven R.; Mészáros, Szabolcs; Meyer, B. S.; Nidever, David L.; O’Connell, Julia; Schiavon, Ricardo P.; Schultheis, M.; Shetrone, Matthew; Simmons, Audrey; Smith, Verne V.; Zamora, Olga

doi:10.1002/asna.201612398

Cited by 45 publications

(41 citation statements)

References 28 publications

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“…Overall, the OC works of Friel et al (2002); Chen et al (2003); Magrini et al (2009), and also the later studies of Frinchaboy et al (2013) and Cunha et al (2016), using APOGEE data, all reach the same conclusions: that the radial metallicity gradient has been steeper in the past. However, this paradigm has been challenged by Salaris et al (2004) who, using the old OC sample of Friel (1995), reach the opposite conclusion, namely that the radial [Fe/H] gradient of the old OC population is shallower than the gradient of the young population.…”

Section: A Comparison With the Literaturesupporting

confidence: 60%

“…To date, the only results that claim to trace the evolution of abundance gradients are based on planetary nebulae (PNe; e.g., Maciel & Chiappini 1994;Maciel & Quireza 1999;Stanghellini et al 2006;Maciel & Costa 2009;Stanghellini & Haywood 2010) and star clusters (e.g., Janes 1979; Twarog et al 1997;Carraro et al 1998;Friel et al 2002;Chen et al 2003;Magrini et al 2009;Yong et al 2012;Frinchaboy et al 2013;Cunha et al 2016), but the former are based on uncertain age and distance estimates and remain inconclusive 1 , while the latter allow essentially only for two wide age bins, and are affected by low-number statistics and non-trivial biases due to the rapid disruption of disc clusters. In addition to the value of the abundance gradient itself, the scatter of the R Gal −[Fe/H] relation can in principle be used to quantify the strength of radial heating and migration over cosmic time.…”

Section: Introductionmentioning

confidence: 99%

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Red giants observed by CoRoT and APOGEE: The evolution of the Milky Way’s radial metallicity gradient

Anders

Chiappini

Minchev

et al. 2017

A&A

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Using combined asteroseismic and spectroscopic observations of 418 red-giant stars close to the Galactic disc plane (6 kpc < R Gal 13 kpc, |Z Gal | < 0.3 kpc), we measure the age dependence of the radial metallicity distribution in the Milky Way's thin disc over cosmic time. The slope of the radial iron gradient of the young red-giant population (−0.058 ± 0.008 [stat.] ±0.003 [syst.] dex/kpc) is consistent with recent Cepheid measurements. For stellar populations with ages of 1 − 4 Gyr the gradient is slightly steeper, at a value of −0.066 ± 0.007 ± 0.002 dex/kpc, and then flattens again to reach a value of ∼ −0.03 dex/kpc for stars with ages between 6 and 10 Gyr. Our results are in good agreement with a state-of-the-art chemo-dynamical Milky-Way model in which the evolution of the abundance gradient and its scatter can be entirely explained by a non-varying negative metallicity gradient in the interstellar medium, together with stellar radial heating and migration. We also offer an explanation for why intermediate-age open clusters in the Solar Neighbourhood can be more metal-rich, and why their radial metallicity gradient seems to be much steeper than that of the youngest clusters. Already within 2 Gyr, radial mixing can bring metal-rich clusters from the innermost regions of the disc to Galactocentric radii of 5 to 8 kpc. We suggest that these outward-migrating clusters may be less prone to tidal disruption and therefore steepen the local intermediate-age cluster metallicity gradient. Our scenario also explains why the strong steepening of the local iron gradient with age is not seen in field stars. In the near future, asteroseismic data from the K2 mission will allow for improved statistics and a better coverage of the inner-disc regions, thereby providing tighter constraints on the evolution of the central parts of the Milky Way.

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Section: A Comparison With the Literaturesupporting

confidence: 60%

Section: Introductionmentioning

confidence: 99%

Red giants observed by CoRoT and APOGEE: The evolution of the Milky Way’s radial metallicity gradient

Anders

Chiappini

Minchev

et al. 2017

A&A

Self Cite

141

142

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“…a 7.0-11.5 in MaNGA-led fields. Cunha et al (2016), and APOGEE-2S is extending this large, homogeneous sample with 100 clusters in the rich star formation regions of the southern Galactic disk.…”

Section: Open and Globular Clustersmentioning

confidence: 70%

Target Selection for the SDSS-IV APOGEE-2 Survey

Zasowski

Cohen

Chojnowski

et al. 2017

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APOGEE-2 is a high-resolution, near-infrared spectroscopic survey observing ∼3×10 5 stars across the entire sky. It is the successor to APOGEE and is part of the Sloan Digital Sky Survey IV (SDSS-IV). APOGEE-2 is expanding on APOGEE's goals of addressing critical questions of stellar astrophysics, stellar populations, and Galactic chemodynamical evolution using (1) an enhanced set of target types and (2) a second spectrograph at Las Campanas Observatory in Chile. APOGEE-2 is targeting red giant branch and red clump stars, RR Lyrae, lowmass dwarf stars, young stellar objects, and numerous other Milky Way and Local Group sources across the entire sky from both hemispheres. In this paper, we describe the APOGEE-2 observational design, target selection catalogs and algorithms, and the targeting-related documentation included in the SDSS data releases.

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“…Since open clusters can range in age from a few Myr to more than 6 Gyr, they also provide a unique opportunity to study the evolution of Galactic abundance gradient s. A number of authors have measured metallicity gradients for open clusters in various age bins (e.g., Carraro * Hubble Fellow Carnegie-Princeton Fellow † NSF Astronomy and Astrophysics Fellow et al 1998;Friel et al 2002;Jacobson et al 2011;Carrera & Pancino 2011;Cunha et al 2016), and while all studies agree that the gradient is shallower for younger clusters, further comparison is difficult due to a somewhat heterogeneous choice of age bins; there does not seem to be a consensus as to the measured gradient for clusters of any given age range.…”

Section: Introductionmentioning

confidence: 99%

The Open Cluster Chemical Abundances and Mapping Survey. IV. Abundances for 128 Open Clusters Using SDSS/APOGEE DR16

et al. 2020

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Chemical abundance gradients from open clusters in the Milky Way disk: Results from the APOGEE survey

Abstract: Metallicity gradients provide strong constraints for understanding the chemical evolution of the Galaxy. We report on radial abundance gradients of

Cited by 45 publications

References 28 publications

Red giants observed by CoRoT and APOGEE: The evolution of the Milky Way’s radial metallicity gradient

Red giants observed by CoRoT and APOGEE: The evolution of the Milky Way’s radial metallicity gradient

Target Selection for the SDSS-IV APOGEE-2 Survey

The Open Cluster Chemical Abundances and Mapping Survey. IV. Abundances for 128 Open Clusters Using SDSS/APOGEE DR16

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