Mapping the Galactic Metallicity Gradient with Open Clusters: The State-of-the-Art and Future Challenges
In this paper, we make use of data collected for open cluster members by high-resolution spectroscopic surveys and programmes (i.e., APOGEE, Gaia-ESO, GALAH, OCCASO, and SPA). These data have been homogenised and then analysed as a whole. The resulting catalogue contains [Fe/H] and orbital parameter...
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| Format: | Article |
| Language: | English |
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MDPI AG
2022-01-01
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| Series: | Universe |
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| Online Access: | https://www.mdpi.com/2218-1997/8/2/87 |
| _version_ | 1797476228878303232 |
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| author | Lorenzo Spina Laura Magrini Katia Cunha |
| author_facet | Lorenzo Spina Laura Magrini Katia Cunha |
| author_sort | Lorenzo Spina |
| collection | DOAJ |
| description | In this paper, we make use of data collected for open cluster members by high-resolution spectroscopic surveys and programmes (i.e., APOGEE, Gaia-ESO, GALAH, OCCASO, and SPA). These data have been homogenised and then analysed as a whole. The resulting catalogue contains [Fe/H] and orbital parameters for 251 Galactic open clusters. The slope of the radial metallicity gradient obtained through 175 open clusters with high-quality metallicity determinations is −0.064 ± 0.007 dex kpc<inline-formula><math xmlns="http://www.w3.org/1998/Math/MathML" display="inline"><semantics><msup><mrow></mrow><mrow><mo>−</mo><mn>1</mn></mrow></msup></semantics></math></inline-formula>. The radial metallicity distribution traced by open clusters flattens beyond R<inline-formula><math xmlns="http://www.w3.org/1998/Math/MathML" display="inline"><semantics><msub><mrow></mrow><mi>Gal</mi></msub></semantics></math></inline-formula> = 12.1 ± 1.1 kpc. The slope traced by open clusters in the [Fe/H]-L<inline-formula><math xmlns="http://www.w3.org/1998/Math/MathML" display="inline"><semantics><msub><mrow></mrow><mi mathvariant="normal">z</mi></msub></semantics></math></inline-formula> diagram is −0.31 ± 0.02 × 10<inline-formula><math xmlns="http://www.w3.org/1998/Math/MathML" display="inline"><semantics><msup><mrow></mrow><mn>3</mn></msup></semantics></math></inline-formula> dex km<inline-formula><math xmlns="http://www.w3.org/1998/Math/MathML" display="inline"><semantics><msup><mrow></mrow><mrow><mo>−</mo><mn>1</mn></mrow></msup></semantics></math></inline-formula> kpc<inline-formula><math xmlns="http://www.w3.org/1998/Math/MathML" display="inline"><semantics><msup><mrow></mrow><mrow><mo>−</mo><mn>1</mn></mrow></msup></semantics></math></inline-formula> s, but it flattens beyond L<inline-formula><math xmlns="http://www.w3.org/1998/Math/MathML" display="inline"><semantics><msub><mrow></mrow><mi mathvariant="normal">z</mi></msub></semantics></math></inline-formula> = 2769 ± 177 km kpc s<inline-formula><math xmlns="http://www.w3.org/1998/Math/MathML" display="inline"><semantics><msup><mrow></mrow><mrow><mo>−</mo><mn>1</mn></mrow></msup></semantics></math></inline-formula>. In this paper, we also review some high-priority practical challenges around the study of open clusters that will significantly push our understanding beyond the state-of-the-art. Finally, we compare the shape of the galactic radial metallicity gradient to those of other spiral galaxies. |
| first_indexed | 2024-03-09T20:55:58Z |
| format | Article |
| id | doaj.art-ecb0d5e5f88e4f9c915ba26156a7e8ca |
| institution | Directory Open Access Journal |
| issn | 2218-1997 |
| language | English |
| last_indexed | 2024-03-09T20:55:58Z |
| publishDate | 2022-01-01 |
| publisher | MDPI AG |
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| series | Universe |
| spelling | doaj.art-ecb0d5e5f88e4f9c915ba26156a7e8ca2023-11-23T22:23:07ZengMDPI AGUniverse2218-19972022-01-01828710.3390/universe8020087Mapping the Galactic Metallicity Gradient with Open Clusters: The State-of-the-Art and Future ChallengesLorenzo Spina0Laura Magrini1Katia Cunha2Instituto Nazionale di Astrofisica—Padova Observatory, Vicolo dell’Osservatorio 5, 35122 Padova, ItalyInstituto Nazionale di Astrofisica—Osservatorio Astrofisico di Arcetri, Largo E. Fermi 5, 50125 Firenze, ItalyObservatório Nacional, Rua General José Cristino, 77, Rio de Janeiro 20921-400, RJ, BrazilIn this paper, we make use of data collected for open cluster members by high-resolution spectroscopic surveys and programmes (i.e., APOGEE, Gaia-ESO, GALAH, OCCASO, and SPA). These data have been homogenised and then analysed as a whole. The resulting catalogue contains [Fe/H] and orbital parameters for 251 Galactic open clusters. The slope of the radial metallicity gradient obtained through 175 open clusters with high-quality metallicity determinations is −0.064 ± 0.007 dex kpc<inline-formula><math xmlns="http://www.w3.org/1998/Math/MathML" display="inline"><semantics><msup><mrow></mrow><mrow><mo>−</mo><mn>1</mn></mrow></msup></semantics></math></inline-formula>. The radial metallicity distribution traced by open clusters flattens beyond R<inline-formula><math xmlns="http://www.w3.org/1998/Math/MathML" display="inline"><semantics><msub><mrow></mrow><mi>Gal</mi></msub></semantics></math></inline-formula> = 12.1 ± 1.1 kpc. The slope traced by open clusters in the [Fe/H]-L<inline-formula><math xmlns="http://www.w3.org/1998/Math/MathML" display="inline"><semantics><msub><mrow></mrow><mi mathvariant="normal">z</mi></msub></semantics></math></inline-formula> diagram is −0.31 ± 0.02 × 10<inline-formula><math xmlns="http://www.w3.org/1998/Math/MathML" display="inline"><semantics><msup><mrow></mrow><mn>3</mn></msup></semantics></math></inline-formula> dex km<inline-formula><math xmlns="http://www.w3.org/1998/Math/MathML" display="inline"><semantics><msup><mrow></mrow><mrow><mo>−</mo><mn>1</mn></mrow></msup></semantics></math></inline-formula> kpc<inline-formula><math xmlns="http://www.w3.org/1998/Math/MathML" display="inline"><semantics><msup><mrow></mrow><mrow><mo>−</mo><mn>1</mn></mrow></msup></semantics></math></inline-formula> s, but it flattens beyond L<inline-formula><math xmlns="http://www.w3.org/1998/Math/MathML" display="inline"><semantics><msub><mrow></mrow><mi mathvariant="normal">z</mi></msub></semantics></math></inline-formula> = 2769 ± 177 km kpc s<inline-formula><math xmlns="http://www.w3.org/1998/Math/MathML" display="inline"><semantics><msup><mrow></mrow><mrow><mo>−</mo><mn>1</mn></mrow></msup></semantics></math></inline-formula>. In this paper, we also review some high-priority practical challenges around the study of open clusters that will significantly push our understanding beyond the state-of-the-art. Finally, we compare the shape of the galactic radial metallicity gradient to those of other spiral galaxies.https://www.mdpi.com/2218-1997/8/2/87open clustersMilky Waymetallicitystarsstellar spectroscopychemical evolution |
| spellingShingle | Lorenzo Spina Laura Magrini Katia Cunha Mapping the Galactic Metallicity Gradient with Open Clusters: The State-of-the-Art and Future Challenges Universe open clusters Milky Way metallicity stars stellar spectroscopy chemical evolution |
| title | Mapping the Galactic Metallicity Gradient with Open Clusters: The State-of-the-Art and Future Challenges |
| title_full | Mapping the Galactic Metallicity Gradient with Open Clusters: The State-of-the-Art and Future Challenges |
| title_fullStr | Mapping the Galactic Metallicity Gradient with Open Clusters: The State-of-the-Art and Future Challenges |
| title_full_unstemmed | Mapping the Galactic Metallicity Gradient with Open Clusters: The State-of-the-Art and Future Challenges |
| title_short | Mapping the Galactic Metallicity Gradient with Open Clusters: The State-of-the-Art and Future Challenges |
| title_sort | mapping the galactic metallicity gradient with open clusters the state of the art and future challenges |
| topic | open clusters Milky Way metallicity stars stellar spectroscopy chemical evolution |
| url | https://www.mdpi.com/2218-1997/8/2/87 |
| work_keys_str_mv | AT lorenzospina mappingthegalacticmetallicitygradientwithopenclustersthestateoftheartandfuturechallenges AT lauramagrini mappingthegalacticmetallicitygradientwithopenclustersthestateoftheartandfuturechallenges AT katiacunha mappingthegalacticmetallicitygradientwithopenclustersthestateoftheartandfuturechallenges |