Gaia Data Release 3: Chemical cartography of the Milky Way

Recio-Blanco, A.; Kordopatis, G.; Laverny, P. de; Palicio, P. A.; Spagna, A.; Spina, L.; Katz, David; Fiorentin, P. Re; Poggio, E.; Mcmillan, P. J.; Vallenari, A.; Lattanzi, M. G.; Seabroke, G. M.; Casamiquela, L.; Bragaglia, A.; Antoja, T.; Bailer‐Jones, C. A. L.; Andrae, R.; Fouesneau, M.; Cropper, M.; Cantat-Gaudin, T.; Heiter, U.; Bijaoui, A.; Brown, Andy; Prusti, T.; Bruijne, J. H. J. de; Arenou, F.; Babusiaux, C.; Biermann, M.; Creevey, O. L.; Ducourant, C.; Evans, D. W.; Eyer, L.; Guerra, R.; Hutton, A.; Jordi, C.; Klioner, S. A.; Lammers, U. L.; Lindegren, L.; Luri, X.; Mignard, F.; Panem, C.; Pourbaix, D.; Randich, S.; Sartoretti, P.; Soubiran, C.; Tanga, P.; Walton, N. A.; Bastian, U.; Drimmel, R.; Jansen, F.; Leeuwen, F. van; Bakker, J.; Cacciari, C.; Castañeda, J.; Angeli, F. de; Fabricius, C.; Frémat, Y.; Galluccio, L.; Guerrier, A.; Masana, E.; Messineo, R.; Mowlavi, N.; Nicolas, C.; Nienartowicz, K.; Pailler, F.; Panuzzo, P.; Riclet, F.; Roux, W.; Thévenin, F.; Gracia-Abril, G.; Portell, J.; Teyssier, D.; Altmann, M.; Audard, M.; Bellas-Velidis, I.; Benson, K.; Berthier, J.; Blomme, R.; Burgess, P. W.; Busonero, D.; Busso, G.; Carry, B.; Cellino, A.; Cheek, N.; Clementini, G.; Damerdji, Y.; Davidson, M.; Teodoro, P. de; Campos, M. Nuñez; Delchambre, L.; Dell'Oro, A.; Esquej, P.; Fernández-Hernández, J.; Fraile, E.; Garabato, D.; García-Lario, P.; Gosset, E.; Haigron, R.; Halbwachs, J. L.; Hambly, N. C.; Harrison, D. L.; Hernández, J.; Hestroffer, D.; Hodgkin, S. T.; Holl, B.; Janßen, K.; Fombelle, G. Jévardat de; Jordan, S.; Krone-Martins, A.; Lanzafame, A. C.; Löffler, W.; Marchal, O.; Marrese, P. M.; Moitinho, A.; Muinonen, K.; Osborne, P.; Pancino, E.; Pauwels, T.; Reylé, C.; Riello, M.; Rimoldini, L.; Roegiers, T.; Rybizki, J.; Sarro, L. M.; Siopis, C.; Smith, M.; Sozzetti, A.; Utrilla, E.; Leeuwen, M. van; Abbas, U.; Ábrahám, P.; Aramburu, A. Abreu; Aerts, C.; Aguado, J. J.; Ajaj, M.; Aldea-Montero, F.; Altavilla, G.; Álvarez, M. A.; Alves, J.; Anders, F.; Anderson, R. I.; Varela, E. Anglada; Baines, D.; Baker, S. G.; Balaguer-Núñez, L.; Balbinot, E.; Balog, Z.; Barache, C.; Barbato, D.; Barros, M.; Barstow, M. A.; Bartolomé, S.; Bassilana, J.-L.; Bauchet, N.; Becciani, U.; Bellazzini, M.; Berihuete, A.; Bernet, M.; Bertone, S.; Bianchi, L.; Binnenfeld, A.; Blanco-Cuaresma, S.; Boch, T.; Bombrun, A.; Bossini, D.; Bouquillon, S.; Bramante, L.; Breedt, E.; Bressan, A.; Brouillet, N.; Brugaletta, E.; Bucciarelli, B.; Burlacu, A.; Butkevich, A. G.; Buzzi, R.; Caffau, E.; Cancelliere, R.; Carballo, R.; Carlucci, T.; Carnerero, M. I.; Carrasco, J. M.; Castellani, M.; Castro-Ginard, A.; Chaoul, L.; Charlot, P.; Chemin, L.; Chiaramida, V.; Chiavassa, A.; Chornay, N.; Comoretto, G.; Contursi, G.; Cooper, W. J.; Cowell, S.; Crifo, F.; Crosta, M.; Crowley, C.; Dafonte, C.; Dapergolas, A.; David, P.; Luise, F. de; March, R. de; Ridder, J. de; Souza, R. de; Torres, A. de; Peloso, E. F. del; Pozo, E. del; Delbo, M.; Delgado, A.; Delisle, J. -B.; Demouchy, C.; Dharmawardena, T. E.; Matteo, P. Di; Diakite, S.; Diener, C.; Distefano, E.; Dolding, C.; Edvardsson, B.; Enke, H.; Fabre, C.; Fabrizio, M.; Faigler, S.; Fedorets, G.; Fernique, P.; Figueras, F.; Fournier, Y.; Fouron, C.; Fragkoudi, F.; Gai, M.; Garcia-Gutierrez, A.; Garcia-Reinaldos, M.; García-Torres, M.; Garofalo, A.; Gavel, A.; Gavras, P.; Gerlach, E.; Geyer, R.; Giacobbe, P.; Gilmore, G.; Girona, S.; Giuffrida, G.; Gomel, R.; González-Núñez, J.; González-Santamaría, I.; González‐Vidal, J. J.; Granvik, M.; Guillout, P.; Guiraud, J.; Gutiérrez-Sánchez, R.; Guy, L. P.; Hatzidimitriou, D.; Hauser, M.; Haywood, M.; Helmer, A.; Helmi, Amina; Sarmiento, M. H.; Hidalgo, S. L.; Hładczuk, N.; Hobbs, D.; Holland, G.; Huckle, H. E.; Jardine, K.; Jasniewicz, G.; Piccolo, A. Jean-Antoine; Jiménez-Arranz, Ó.; Campillo, J. Juaristi; Julbe, F.; Karbevska, L.; Kervella, P.; Khanna, S.; Korn, A. J.; Kóspál, Á; Kostrzewa-Rutkowska, Z.; Kruszyńska, K.; Kun, M.; Laizeau, P.; Lambert, S.; Lanza, A. F.; Lasne, Y.; Campion, J. -F. Le; Lebreton, Y.; Lebzelter, T.; Leccia, S.; Leclerc, N.; Lecoeur-Taibi, I.; Liao, S.; Licata, E. L.; Lindstrøm, H. E. P.; Lister, T. A.; Livanou, E.; Lobel, A.; Lorca, A.; Loup, C.; Pardo, P. Madrero; Romeo, A. Magdaleno; Managau, S.; Mann, R. G.; Manteiga, M.; Marchant, J. M.; Marconi, M.; Marcos, J.; Santos, M. M. S. Marcos; Pina, D. Marín; Marinoni, S.; Marocco, F.; Marshall, D. J.; Polo, L. Martin; Martín-Fleitas, J. M.; Marton, G.; Mary, N.; Masip, A.; Massari, D.; Mastrobuono-Battisti, Alessandra; Mazeh, T.; Messina, S.; Michalik, D.; Millar, N. R.; Mints, A.; Molina, D.; Molinaro, R.; Molnár, L.; Monari, G.; Monguió, M.; Montegriffo, P.; Montero, A.; Mor, R.; Mora, A.; Morbidelli, R.; Morel, T.; Morris, D.; Muraveva, T.; Murphy, C. P.; Musella, I.; Nagy, Z.; Noval, L.; Ocaña, F.; Ogden, A.; Ordenovic, C.; Osinde, J. O.; Pagani, C.; Pagano, I.; Palaversa, L.; Pallas-Quintela, L.; Panahi, A.; Payne-Wardenaar, S.; Esteller, X. Peñalosa; Penttilä, A.; Pichon, B.; Piersimoni, A. M.; Pineau, F. -X.; Plachy, E.; Plum, G.; Prša, A.; Pulone, L.; Racero, E.; Ragaini, S.; Rainer, M.; Raiteri, C. M.; Ramos, P.; Ramos-Lerate, M.; Regibo, S.; Richards, P. J.; Diaz, C. Rios; Ripepi, V.; Riva, A.; Rix, H. -W.; Rixon, G.; Robichon, N.; Robin, A. C.; Robin, C.; Roelens, M.; Rogues, H. R. O.; Rohrbasser, L.; Romero-Gómez, M.; Rowell, N.; Royer, F.; Mieres, D. Ruz; Rybicki, K. A.; Sadowski, G.; Núñez, A. Sáez; Sellés, A. Sagristà; Sahlmann, J.; Salguero, E.; Samaras, N.; Gimenez, V. Sanchez; Sanna, N.; Santoveña, R.; Sarasso, M.; Schultheis, M.; Sciacca, E.; Segol, M.; Segovia, J. C.; Semeux, D.; Shahaf, S.; Siddiqui, H. I.; Siebert, A.; Siltala, L.; Silvelo, A.; Slezak, E.; Slezak, I.; Smart, R. L.; Snaith, O. N.; Solano, E.; Solitro, F.; Souami, D.; Souchay, J.; Spoto, F.; Steele, I. A.; Steidelmüller, H.; Stephenson, C. A.; Süveges, M.; Surdej, J.; Szabados, L.; Szegedi-Elek, E.; Taris, F.; Taylor, M. B.; Teixeira, R.; Tolomei, L.; Tonello, N.; Torra, F.; Torra, J.; Elipe, G. Torralba; Trabucchi, M.; Tsounis, A. T.; Turon, C.; Ulla, A.; Unger, N.; Vaillant, M. V.; Dillen, E. van; Reeven, W. van; Vanel, O.; Vecchiato, A.; Viala, Y.; Vicente, D.; Voutsinas, S.; Weiler, M.; Wevers, T.; Wyrzykowski, Ł.; Yoldas, A.; Yvard, P.; Zhao, H.; Zorec, J.; Zucker, S.; Zwitter, T.

doi:10.48550/arxiv.2206.05534

Cited by 5 publications

(2 citation statements)

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“…However, they did not investigate more details using radial velocity, chemistry, mass, and age populations for the ridge, which are explored in this work. Recio-Blanco et al (2022) have also adopted RGB stars from Gaia DR3 to investigate the distribution of diagonal ridges in chemical space, and found seven diagonal ridges using general sample in the actions space; it seems that four of which are significant in their Figure 31. But the volume of the disk probed here is a bit farther for chemistry compared to the recent DR3 work and we are using the new chemistry information like [α/Fe] and ages in this work, then present the north-south asymmetries analysis for the ridge.…”

Section: More Comparisons and The Bar Contributionmentioning

confidence: 99%

“…They found that stars in angular momentum overdensities can track density ridges over many kpc with the help of high-resolution spiral galaxy simulation as well as Gaia DR2 and EDR3 data. Recio-Blanco et al (2022) have also found that most diagonal ridges are metal-rich using metallicity in Gaia DR3 red-giant branch (RGB) stars without age information. They also identified seven ridge structures in the chemistry.…”

Section: Introductionmentioning

confidence: 99%

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Kinematic-chemical Analysis and Time Tagging for the Diagonal Ridge Structure of the Galactic Outer Disk with LAMOST Red-giant Branch Stars

Yang

Wang

Zhi-Quan

et al. 2023

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We investigate the kinematic-chemical distribution of red-giant branch stars from the LAMOST survey crossed matched with Gaia DR2 proper motions, and present time tagging for the well-known ridge structures (diagonal distributions for V R in the R, V ϕ plane) in the range of Galactocentric distance R = 8 to 15 kpc. We detect six ridge structures, including five ridges apparent in the radial velocity distribution and three ridges apparent in the vertical velocity, the sensitive time of which to the perturbations are from young population (0–3 Gyr) to old population (9–14 Gyr). Based on an analysis of the evolution of angular momentum distribution, we find that four ridges are relatively stationary, while another is evolving with time, which is confirmed by the difference analysis at different populations and supporting that there might be two kinds of dynamical origins. Furthermore, ridge features are also vividly present in the chemical properties ([Fe/H], [α/Fe]). The comparison between the north and south hemispheres of the Galaxy does show some differences and the ridge features are asymmetrical. Moreover, we find that diagonal ridge structures may affect the shape of the rotation curve, which is manifested as fluctuations and undulations on top of a smooth profile. Finally we speculate that the bar dynamics should be not enough to explain all ridge properties including the break feature in the V Z –L Z plane.

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Section: More Comparisons and The Bar Contributionmentioning

confidence: 99%

Section: Introductionmentioning

confidence: 99%

Kinematic-chemical Analysis and Time Tagging for the Diagonal Ridge Structure of the Galactic Outer Disk with LAMOST Red-giant Branch Stars

Yang

Wang

Zhi-Quan

et al. 2023

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On the origin of the Galactic thin and thick discs, their abundance gradients and the diagnostic potential of their abundance ratios

Prantzos

Abia

Chen

et al. 2023

Monthly Notices of the Royal Astronomical Society

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Using a semi-analytical model of the evolution of the Milky Way, we show how secular evolution can create distinct overdensities in the phase space of various properties (e.g. age vs metallicity or abundance ratios vs age) corresponding to the thin and thick discs. In particular, we show how key properties of the Solar vicinity can be obtained by secular evolution, with no need for external or special events, like galaxy mergers or paucity in star formation. This concerns the long established double-branch behaviour of [alpha/Fe] vs metallicity and the recently found non-monotonic evolution of the stellar abundance gradient, evaluated at the birth radii of stars. We extend the discussion to other abundance ratios and we suggest a classification scheme, based on the nature of the corresponding yields (primary vs secondary or odd elements) and on the lifetimes of their sources (short-lived vs long-lived ones). The latter property is critical in determining the single- or double- branch behavior of an elementary abundance ratio in the Solar neighborhood. We underline the high diagnostic potential of this finding, which can help to separate clearly elements with sources evolving on different timescales and help determining the site of e.g. the r-process(es). We define the ‘abundance distance’ between the thin and thick disc sequences as an important element for such a separation. We also show how the inside-out evolution of the Milky Way disc leads rather to a single-branch behavior in other disc regions.

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Unveiling the time evolution of chemical abundances across the Milky Way disc with APOGEE

Ratcliffe

Minchev

Anders

et al. 2023

Monthly Notices of the Royal Astronomical Society

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Chemical abundances are an essential tool in untangling the Milky Way’s enrichment history. However, the evolution of the interstellar medium abundance gradient with cosmic time is lost as a result of radial mixing processes. For the first time, we quantify the evolution of many observational abundances across the Galactic disk as a function of lookback time and birth radius, $\rm \text{R}_\text{birth}$. Using an empirical approach, we derive $\rm \text{R}_\text{birth}$ estimates for 145,447 APOGEE DR17 red giant disk stars, based solely on their ages and $\rm [Fe/H]$. We explore the detailed evolution of 6 abundances (Mg, Ca (α), Mn (iron-peak), Al, C (light), Ce (s-process)) across the Milky Way disk using 87,426 APOGEE DR17 red giant stars. We discover that the interstellar medium had three fluctuations in the metallicity gradient ∼9, ∼6, and ∼4 Gyr ago. The first coincides with the end of high-α sequence formation around the time of the Gaia-Sausage-Enceladus disruption, while the others are likely related to passages of the Sagittarius dwarf galaxy. A clear distinction is found between present-day observed radial gradients with age and the evolution with lookback time for both [X/Fe] and [X/H], resulting from the significant flattening and inversion in old populations due to radial migration. We find the $\rm [Fe/H]$–$\rm [\alpha /Fe]$ bimodality is also seen as a separation in the $\rm \text{R}_\text{birth}$–$\rm [X/Fe]$ plane for the light and α-elements. Our results recover the chemical enrichment of the Galactic disk over the past 12 Gyr, providing tight constraints on Galactic disk chemical evolution models.

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Gaia Data Release 3: Chemical cartography of the Milky Way

Cited by 5 publications

References 0 publications

Kinematic-chemical Analysis and Time Tagging for the Diagonal Ridge Structure of the Galactic Outer Disk with LAMOST Red-giant Branch Stars

Kinematic-chemical Analysis and Time Tagging for the Diagonal Ridge Structure of the Galactic Outer Disk with LAMOST Red-giant Branch Stars

On the origin of the Galactic thin and thick discs, their abundance gradients and the diagnostic potential of their abundance ratios

Unveiling the time evolution of chemical abundances across the Milky Way disc with APOGEE

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