11institutetext:  Université Côte d’Azur, Observatoire de la Côte d’Azur,
CNRS, Laboratoire Lagrange, Bd de l’Observatoire, CS 34229, 06304 Nice Cedex
4, France 22institutetext: INAF - Osservatorio Astrofisico di Torino, via
Osservatorio 20, 10025 Pino Torinese (TO), Italy33institutetext: INAF -
Osservatorio astronomico di Padova, Vicolo Osservatorio 5, 35122 Padova,
Italy44institutetext: GEPI, Observatoire de Paris, Université PSL, CNRS, 5
Place Jules Janssen, 92190 Meudon, France55institutetext: Lund Observatory,
Department of Astronomy and Theoretical Physics, Lund University, Box 43,
22100 Lund, Sweden66institutetext: University of Turin, Department of Physics,
Via Pietro Giuria 1, 10125 Torino, Italy77institutetext: Mullard Space Science
Laboratory, University College London, Holmbury St Mary, Dorking, Surrey RH5
6NT, United Kingdom88institutetext: Laboratoire d’astrophysique de Bordeaux,
Univ. Bordeaux, CNRS, B18N, allée Geoffroy Saint-Hilaire, 33615 Pessac,
France99institutetext: INAF - Osservatorio di Astrofisica e Scienza dello
Spazio di Bologna, via Piero Gobetti 93/3, 40129 Bologna,
Italy1010institutetext: Institut de Ciències del Cosmos (ICCUB), Universitat
de Barcelona (IEEC-UB), Martí i Franquès 1, 08028 Barcelona,
Spain1111institutetext: Max Planck Institute for Astronomy, K ̈onigstuhl 17,
69117 Heidelberg, Germany1212institutetext: Observational Astrophysics,
Division of Astronomy and Space Physics, Department of Physics and Astronomy,
Uppsala University, Box 516, 751 20 Uppsala, Sweden1313institutetext: Leiden
Observatory, Leiden University, Niels Bohrweg 2, 2333 CA Leiden, The
Netherlands1414institutetext: European Space Agency (ESA), European Space
Research and Technology Centre (ESTEC), Keplerlaan 1, 2201AZ, Noordwijk, The
Netherlands1515institutetext: Univ. Grenoble Alpes, CNRS, IPAG, 38000
Grenoble, France1616institutetext: Astronomisches Rechen-Institut, Zentrum f
̈ur Astronomie der Universit ̈at Heidelberg, M ̈onchhofstr. 12-14, 69120
Heidelberg, Germany1717institutetext: Institute of Astronomy, University of
Cambridge, Madingley Road, Cambridge CB3 0HA, United Kingdom1818institutetext:
Department of Astronomy, University of Geneva, Chemin Pegasi 51, 1290 Versoix,
Switzerland1919institutetext: European Space Agency (ESA), European Space
Astronomy Centre (ESAC), Camino bajo del Castillo, s/n, Urbanizacion
Villafranca del Castillo, Villanueva de la Cañada, 28692 Madrid,
Spain2020institutetext: Aurora Technology for European Space Agency (ESA),
Camino bajo del Castillo, s/n, Urbanizacion Villafranca del Castillo,
Villanueva de la Cañada, 28692 Madrid, Spain2121institutetext: Lohrmann
Observatory, Technische Universit ̈at Dresden, Mommsenstraße 13, 01062
Dresden, Germany2222institutetext: CNES Centre Spatial de Toulouse, 18 avenue
Edouard Belin, 31401 Toulouse Cedex 9, France2323institutetext: Institut
d’Astronomie et d’Astrophysique, Université Libre de Bruxelles CP 226,
Boulevard du Triomphe, 1050 Brussels, Belgium2424institutetext: F.R.S.-FNRS,
Rue d’Egmont 5, 1000 Brussels, Belgium2525institutetext: INAF - Osservatorio
Astrofisico di Arcetri, Largo Enrico Fermi 5, 50125 Firenze,
Italy2626institutetext: European Space Agency (ESA, retired)2727institutetext:
DAPCOM for Institut de Ciències del Cosmos (ICCUB), Universitat de Barcelona
(IEEC-UB), Martí i Franquès 1, 08028 Barcelona, Spain2828institutetext: Royal
Observatory of Belgium, Ringlaan 3, 1180 Brussels, Belgium2929institutetext:
ALTEC S.p.a, Corso Marche, 79,10146 Torino, Italy3030institutetext: Sàrl,
Geneva, Switzerland3131institutetext: Department of Astronomy, University of
Geneva, Chemin d’Ecogia 16, 1290 Versoix, Switzerland3232institutetext: Gaia
DPAC Project Office, ESAC, Camino bajo del Castillo, s/n, Urbanizacion
Villafranca del Castillo, Villanueva de la Cañada, 28692 Madrid,
Spain3333institutetext: Telespazio UK S.L. for European Space Agency (ESA),
Camino bajo del Castillo, s/n, Urbanizacion Villafranca del Castillo,
Villanueva de la Cañada, 28692 Madrid, Spain3434institutetext: SYRTE,
Observatoire de Paris, Université PSL, CNRS, Sorbonne Université, LNE, 61
avenue de l’Observatoire 75014 Paris, France3535institutetext: National
Observatory of Athens, I. Metaxa and Vas. Pavlou, Palaia Penteli, 15236
Athens, Greece3636institutetext: IMCCE, Observatoire de Paris, Université PSL,
CNRS, Sorbonne Université, Univ. Lille, 77 av. Denfert-Rochereau, 75014 Paris,
France3737institutetext: Serco Gestión de Negocios for European Space Agency
(ESA), Camino bajo del Castillo, s/n, Urbanizacion Villafranca del Castillo,
Villanueva de la Cañada, 28692 Madrid, Spain3838institutetext: Institut
d’Astrophysique et de Géophysique, Université de Liège, 19c, Allée du 6 Août,
B-4000 Liège, Belgium3939institutetext: CRAAG - Centre de Recherche en
Astronomie, Astrophysique et Géophysique, Route de l’Observatoire Bp 63
Bouzareah 16340 Algiers, Algeria4040institutetext: Institute for Astronomy,
University of Edinburgh, Royal Observatory, Blackford Hill, Edinburgh EH9 3HJ,
United Kingdom4141institutetext: RHEA for European Space Agency (ESA), Camino
bajo del Castillo, s/n, Urbanizacion Villafranca del Castillo, Villanueva de
la Cañada, 28692 Madrid, Spain4242institutetext: ATG Europe for European Space
Agency (ESA), Camino bajo del Castillo, s/n, Urbanizacion Villafranca del
Castillo, Villanueva de la Cañada, 28692 Madrid, Spain4343institutetext: CIGUS
CITIC - Department of Computer Science and Information Technologies,
University of A Coruña, Campus de Elviña s/n, A Coruña, 15071,
Spain4444institutetext: Université de Strasbourg, CNRS, Observatoire
astronomique de Strasbourg, UMR 7550, 11 rue de l’Université, 67000
Strasbourg, France4545institutetext: Kavli Institute for Cosmology Cambridge,
Institute of Astronomy, Madingley Road, Cambridge, CB3 0HA4646institutetext:
Leibniz Institute for Astrophysics Potsdam (AIP), An der Sternwarte 16, 14482
Potsdam, Germany4747institutetext: CENTRA, Faculdade de Ciências, Universidade
de Lisboa, Edif. C8, Campo Grande, 1749-016 Lisboa, Portugal4848institutetext:
Department of Informatics, Donald Bren School of Information and Computer
Sciences, University of California, Irvine, 5226 Donald Bren Hall, 92697-3440
CA Irvine, United States4949institutetext: INAF - Osservatorio Astrofisico di
Catania, via S. Sofia 78, 95123 Catania, Italy5050institutetext: Dipartimento
di Fisica e Astronomia ””Ettore Majorana””, Università di Catania, Via S.
Sofia 64, 95123 Catania, Italy5151institutetext: INAF - Osservatorio
Astronomico di Roma, Via Frascati 33, 00078 Monte Porzio Catone (Roma),
Italy5252institutetext: Space Science Data Center - ASI, Via del Politecnico
SNC, 00133 Roma, Italy5353institutetext: Department of Physics, University of
Helsinki, P.O. Box 64, 00014 Helsinki, Finland5454institutetext: Finnish
Geospatial Research Institute FGI, Geodeetinrinne 2, 02430 Masala,
Finland5555institutetext: Institut UTINAM CNRS UMR6213, Université Bourgogne
Franche-Comté, OSU THETA Franche-Comté Bourgogne, Observatoire de Besançon,
BP1615, 25010 Besançon Cedex, France5656institutetext: HE Space Operations BV
for European Space Agency (ESA), Keplerlaan 1, 2201AZ, Noordwijk, The
Netherlands5757institutetext: Dpto. de Inteligencia Artificial, UNED, c/ Juan
del Rosal 16, 28040 Madrid, Spain5858institutetext: Konkoly Observatory,
Research Centre for Astronomy and Earth Sciences, E ̈otv ̈os Loránd Research
Network (ELKH), MTA Centre of Excellence, Konkoly Thege Miklós út 15-17, 1121
Budapest, Hungary5959institutetext: ELTE E ̈otv ̈os Loránd University,
Institute of Physics, 1117, Pázmány Péter sétány 1A, Budapest,
Hungary6060institutetext: Instituut voor Sterrenkunde, KU Leuven,
Celestijnenlaan 200D, 3001 Leuven, Belgium6161institutetext: Department of
Astrophysics/IMAPP, Radboud University, P.O.Box 9010, 6500 GL Nijmegen, The
Netherlands6262institutetext: University of Vienna, Department of
Astrophysics, T ̈urkenschanzstraße 17, A1180 Vienna, Austria6363institutetext:
Institute of Physics, Laboratory of Astrophysics, Ecole Polytechnique Fédérale
de Lausanne (EPFL), Observatoire de Sauverny, 1290 Versoix,
Switzerland6464institutetext: Kapteyn Astronomical Institute, University of
Groningen, Landleven 12, 9747 AD Groningen, The Netherlands6565institutetext:
School of Physics and Astronomy / Space Park Leicester, University of
Leicester, University Road, Leicester LE1 7RH, United
Kingdom6666institutetext: Thales Services for CNES Centre Spatial de Toulouse,
18 avenue Edouard Belin, 31401 Toulouse Cedex 9, France6767institutetext:
Depto. Estadística e Investigación Operativa. Universidad de Cádiz, Avda.
República Saharaui s/n, 11510 Puerto Real, Cádiz, Spain6868institutetext:
Center for Research and Exploration in Space Science and Technology,
University of Maryland Baltimore County, 1000 Hilltop Circle, Baltimore MD,
USA6969institutetext: GSFC - Goddard Space Flight Center, Code 698, 8800
Greenbelt Rd, 20771 MD Greenbelt, United States7070institutetext: EURIX
S.r.l., Corso Vittorio Emanuele II 61, 10128, Torino, Italy7171institutetext:
Porter School of the Environment and Earth Sciences, Tel Aviv University, Tel
Aviv 6997801, Israel7272institutetext: Harvard-Smithsonian Center for
Astrophysics, 60 Garden St., MS 15, Cambridge, MA 02138, USA7373institutetext:
HE Space Operations BV for European Space Agency (ESA), Camino bajo del
Castillo, s/n, Urbanizacion Villafranca del Castillo, Villanueva de la Cañada,
28692 Madrid, Spain7474institutetext: Instituto de Astrofísica e Ciências do
Espaço, Universidade do Porto, CAUP, Rua das Estrelas, PT4150-762 Porto,
Portugal7575institutetext: LFCA/DAS,Universidad de Chile,CNRS,Casilla 36-D,
Santiago, Chile7676institutetext: SISSA - Scuola Internazionale Superiore di
Studi Avanzati, via Bonomea 265, 34136 Trieste, Italy7777institutetext:
Telespazio for CNES Centre Spatial de Toulouse, 18 avenue Edouard Belin, 31401
Toulouse Cedex 9, France7878institutetext: University of Turin, Department of
Computer Sciences, Corso Svizzera 185, 10149 Torino, Italy7979institutetext:
Dpto. de Matemática Aplicada y Ciencias de la Computación, Univ. de Cantabria,
ETS Ingenieros de Caminos, Canales y Puertos, Avda. de los Castros s/n, 39005
Santander, Spain8080institutetext: Centro de Astronomía - CITEVA, Universidad
de Antofagasta, Avenida Angamos 601, Antofagasta 1270300,
Chile8181institutetext: DLR Gesellschaft f ̈ur Raumfahrtanwendungen (GfR) mbH
M ̈unchener Straße 20 , 82234 Weßling8282institutetext: Centre for
Astrophysics Research, University of Hertfordshire, College Lane, AL10 9AB,
Hatfield, United Kingdom8383institutetext: University of Turin, Mathematical
Department ””G.Peano””, Via Carlo Alberto 10, 10123 Torino,
Italy8484institutetext: INAF - Osservatorio Astronomico d’Abruzzo, Via Mentore
Maggini, 64100 Teramo, Italy8585institutetext: Instituto de Astronomia,
Geofìsica e Ciências Atmosféricas, Universidade de São Paulo, Rua do Matão,
1226, Cidade Universitaria, 05508-900 São Paulo, SP, Brazil8686institutetext:
APAVE SUDEUROPE SAS for CNES Centre Spatial de Toulouse, 18 avenue Edouard
Belin, 31401 Toulouse Cedex 9, France8787institutetext: Mésocentre de calcul
de Franche-Comté, Université de Franche-Comté, 16 route de Gray, 25030
Besançon Cedex, France8888institutetext: Theoretical Astrophysics, Division of
Astronomy and Space Physics, Department of Physics and Astronomy, Uppsala
University, Box 516, 751 20 Uppsala, Sweden8989institutetext: ATOS for CNES
Centre Spatial de Toulouse, 18 avenue Edouard Belin, 31401 Toulouse Cedex 9,
France9090institutetext: School of Physics and Astronomy, Tel Aviv University,
Tel Aviv 6997801, Israel9191institutetext: Astrophysics Research Centre,
School of Mathematics and Physics, Queen’s University Belfast, Belfast BT7
1NN, UK9292institutetext: Centre de Données Astronomique de Strasbourg,
Strasbourg, France9393institutetext: Institute for Computational Cosmology,
Department of Physics, Durham University, Durham DH1 3LE, UK9494institutetext:
European Southern Observatory, Karl-Schwarzschild-Str. 2, 85748 Garching,
Germany9595institutetext: Max-Planck-Institut f ̈ur Astrophysik, Karl-
Schwarzschild-Straße 1, 85748 Garching, Germany9696institutetext: Data Science
and Big Data Lab, Pablo de Olavide University, 41013, Seville,
Spain9797institutetext: Barcelona Supercomputing Center (BSC), Plaça Eusebi G
̈uell 1-3, 08034-Barcelona, Spain9898institutetext: ETSE Telecomunicación,
Universidade de Vigo, Campus Lagoas-Marcosende, 36310 Vigo, Galicia,
Spain9999institutetext: Asteroid Engineering Laboratory, Space Systems, Luleå
University of Technology, Box 848, S-981 28 Kiruna, Sweden100100institutetext:
Vera C Rubin Observatory, 950 N. Cherry Avenue, Tucson, AZ 85719,
USA101101institutetext: Department of Astrophysics, Astronomy and Mechanics,
National and Kapodistrian University of Athens, Panepistimiopolis, Zografos,
15783 Athens, Greece102102institutetext: TRUMPF Photonic Components GmbH,
Lise-Meitner-Straße 13, 89081 Ulm, Germany103103institutetext: IAC - Instituto
de Astrofisica de Canarias, Via Láctea s/n, 38200 La Laguna S.C., Tenerife,
Spain104104institutetext: Department of Astrophysics, University of La Laguna,
Via Láctea s/n, 38200 La Laguna S.C., Tenerife, Spain105105institutetext:
Faculty of Aerospace Engineering, Delft University of Technology, Kluyverweg
1, 2629 HS Delft, The Netherlands106106institutetext: Radagast
Solutions107107institutetext: Laboratoire Univers et Particules de
Montpellier, CNRS Université Montpellier, Place Eugène Bataillon, CC72, 34095
Montpellier Cedex 05, France108108institutetext: Université de Caen Normandie,
Côte de Nacre Boulevard Maréchal Juin, 14032 Caen, France109109institutetext:
LESIA, Observatoire de Paris, Université PSL, CNRS, Sorbonne Université,
Université de Paris, 5 Place Jules Janssen, 92190 Meudon,
France110110institutetext: SRON Netherlands Institute for Space Research,
Niels Bohrweg 4, 2333 CA Leiden, The Netherlands111111institutetext:
Astronomical Observatory, University of Warsaw, Al. Ujazdowskie 4, 00-478
Warszawa, Poland112112institutetext: Scalian for CNES Centre Spatial de
Toulouse, 18 avenue Edouard Belin, 31401 Toulouse Cedex 9,
France113113institutetext: Université Rennes, CNRS, IPR (Institut de Physique
de Rennes) - UMR 6251, 35000 Rennes, France114114institutetext: INAF -
Osservatorio Astronomico di Capodimonte, Via Moiariello 16, 80131, Napoli,
Italy115115institutetext: Shanghai Astronomical Observatory, Chinese Academy
of Sciences, 80 Nandan Road, Shanghai 200030, People’s Republic of
China116116institutetext: University of Chinese Academy of Sciences, No.19(A)
Yuquan Road, Shijingshan District, Beijing 100049, People’s Republic of
China117117institutetext: Niels Bohr Institute, University of Copenhagen,
Juliane Maries Vej 30, 2100 Copenhagen Ø, Denmark118118institutetext: DXC
Technology, Retortvej 8, 2500 Valby, Denmark119119institutetext: Las Cumbres
Observatory, 6740 Cortona Drive Suite 102, Goleta, CA 93117,
USA120120institutetext: CIGUS CITIC, Department of Nautical Sciences and
Marine Engineering, University of A Coruña, Paseo de Ronda 51, 15071, A
Coruña, Spain121121institutetext: Astrophysics Research Institute, Liverpool
John Moores University, 146 Brownlow Hill, Liverpool L3 5RF, United
Kingdom122122institutetext: IPAC, Mail Code 100-22, California Institute of
Technology, 1200 E. California Blvd., Pasadena, CA 91125,
USA123123institutetext: IRAP, Université de Toulouse, CNRS, UPS, CNES, 9 Av.
colonel Roche, BP 44346, 31028 Toulouse Cedex 4, France124124institutetext:
MTA CSFK Lend ̈ulet Near-Field Cosmology Research Group, Konkoly Observatory,
MTA Research Centre for Astronomy and Earth Sciences, Konkoly Thege Miklós út
15-17, 1121 Budapest, Hungary125125institutetext: Departmento de Física de la
Tierra y Astrofísica, Universidad Complutense de Madrid, 28040 Madrid,
Spain126126institutetext: Ruđer Bošković Institute, Bijenička cesta 54, 10000
Zagreb, Croatia127127institutetext: Villanova University, Department of
Astrophysics and Planetary Science, 800 E Lancaster Avenue, Villanova PA
19085, USA128128institutetext: INAF - Osservatorio Astronomico di Brera, via
E. Bianchi, 46, 23807 Merate (LC), Italy129129institutetext: STFC, Rutherford
Appleton Laboratory, Harwell, Didcot, OX11 0QX, United
Kingdom130130institutetext: Charles University, Faculty of Mathematics and
Physics, Astronomical Institute of Charles University, V Holesovickach 2,
18000 Prague, Czech Republic131131institutetext: Department of Particle
Physics and Astrophysics, Weizmann Institute of Science, Rehovot 7610001,
Israel132132institutetext: Department of Astrophysical Sciences, 4 Ivy Lane,
Princeton University, Princeton NJ 08544, USA133133institutetext: Departamento
de Astrofísica, Centro de Astrobiología (CSIC-INTA), ESA-ESAC. Camino Bajo del
Castillo s/n. 28692 Villanueva de la Cañada, Madrid, Spain134134institutetext:
naXys, University of Namur, Rempart de la Vierge, 5000 Namur,
Belgium135135institutetext: CGI Deutschland B.V. & Co. KG, Mornewegstr. 30,
64293 Darmstadt, Germany136136institutetext: Institute of Global Health,
University of Geneva137137institutetext: Astronomical Observatory Institute,
Faculty of Physics, Adam Mickiewicz University, Poznań,
Poland138138institutetext: H H Wills Physics Laboratory, University of
Bristol, Tyndall Avenue, Bristol BS8 1TL, United Kingdom139139institutetext:
Department of Physics and Astronomy G. Galilei, University of Padova, Vicolo
dell’Osservatorio 3, 35122, Padova, Italy140140institutetext: CERN, Geneva,
Switzerland141141institutetext: Applied Physics Department, Universidade de
Vigo, 36310 Vigo, Spain142142institutetext: Association of Universities for
Research in Astronomy, 1331 Pennsylvania Ave. NW, Washington, DC 20004,
USA143143institutetext: European Southern Observatory, Alonso de Córdova 3107,
Casilla 19, Santiago, Chile144144institutetext: Sorbonne Université, CNRS,
UMR7095, Institut d’Astrophysique de Paris, 98bis bd. Arago, 75014 Paris,
France145145institutetext: Faculty of Mathematics and Physics, University of
Ljubljana, Jadranska ulica 19, 1000 Ljubljana, Slovenia

#  Gaia Data Release 3: Chemical cartography of the Milky Way

Gaia Collaboration  A. Recio-Blanco Gaia Data Release 3: Chemical cartography
of the Milky WayGaia Data Release 3: Chemical cartography of the Milky Way G.
Kordopatis Gaia Data Release 3: Chemical cartography of the Milky WayGaia Data
Release 3: Chemical cartography of the Milky Way P. de Laverny Gaia Data
Release 3: Chemical cartography of the Milky WayGaia Data Release 3: Chemical
cartography of the Milky Way P.A. Palicio Gaia Data Release 3: Chemical
cartography of the Milky WayGaia Data Release 3: Chemical cartography of the
Milky Way A. Spagna Gaia Data Release 3: Chemical cartography of the Milky
WayGaia Data Release 3: Chemical cartography of the Milky Way L. Spina Gaia
Data Release 3: Chemical cartography of the Milky WayGaia Data Release 3:
Chemical cartography of the Milky Way D. Katz Gaia Data Release 3: Chemical
cartography of the Milky WayGaia Data Release 3: Chemical cartography of the
Milky Way P. Re Fiorentin Gaia Data Release 3: Chemical cartography of the
Milky WayGaia Data Release 3: Chemical cartography of the Milky Way E. Poggio
Gaia Data Release 3: Chemical cartography of the Milky WayGaia Data Release 3:
Chemical cartography of the Milky WayGaia Data Release 3: Chemical cartography
of the Milky WayGaia Data Release 3: Chemical cartography of the Milky Way
P.J. McMillan Gaia Data Release 3: Chemical cartography of the Milky WayGaia
Data Release 3: Chemical cartography of the Milky Way A. Vallenari Gaia Data
Release 3: Chemical cartography of the Milky WayGaia Data Release 3: Chemical
cartography of the Milky Way M.G. Lattanzi Gaia Data Release 3: Chemical
cartography of the Milky WayGaia Data Release 3: Chemical cartography of the
Milky WayGaia Data Release 3: Chemical cartography of the Milky WayGaia Data
Release 3: Chemical cartography of the Milky Way G.M. Seabroke Gaia Data
Release 3: Chemical cartography of the Milky WayGaia Data Release 3: Chemical
cartography of the Milky Way L. Casamiquela Gaia Data Release 3: Chemical
cartography of the Milky WayGaia Data Release 3: Chemical cartography of the
Milky WayGaia Data Release 3: Chemical cartography of the Milky WayGaia Data
Release 3: Chemical cartography of the Milky Way A. Bragaglia Gaia Data
Release 3: Chemical cartography of the Milky WayGaia Data Release 3: Chemical
cartography of the Milky Way T. Antoja Gaia Data Release 3: Chemical
cartography of the Milky WayGaia Data Release 3: Chemical cartography of the
Milky Way C.A.L. Bailer-Jones Gaia Data Release 3: Chemical cartography of the
Milky WayGaia Data Release 3: Chemical cartography of the Milky Way M.
Schultheis Gaia Data Release 3: Chemical cartography of the Milky WayGaia Data
Release 3: Chemical cartography of the Milky Way R. Andrae Gaia Data Release
3: Chemical cartography of the Milky WayGaia Data Release 3: Chemical
cartography of the Milky Way M. Fouesneau Gaia Data Release 3: Chemical
cartography of the Milky WayGaia Data Release 3: Chemical cartography of the
Milky Way M. Cropper Gaia Data Release 3: Chemical cartography of the Milky
WayGaia Data Release 3: Chemical cartography of the Milky Way T. Cantat-Gaudin
Gaia Data Release 3: Chemical cartography of the Milky WayGaia Data Release 3:
Chemical cartography of the Milky WayGaia Data Release 3: Chemical cartography
of the Milky WayGaia Data Release 3: Chemical cartography of the Milky Way A.
Bijaoui Gaia Data Release 3: Chemical cartography of the Milky WayGaia Data
Release 3: Chemical cartography of the Milky Way U. Heiter Gaia Data Release
3: Chemical cartography of the Milky WayGaia Data Release 3: Chemical
cartography of the Milky Way A.G.A. Brown Gaia Data Release 3: Chemical
cartography of the Milky WayGaia Data Release 3: Chemical cartography of the
Milky Way T. Prusti Gaia Data Release 3: Chemical cartography of the Milky
WayGaia Data Release 3: Chemical cartography of the Milky Way J.H.J. de
Bruijne Gaia Data Release 3: Chemical cartography of the Milky WayGaia Data
Release 3: Chemical cartography of the Milky Way F. Arenou Gaia Data Release
3: Chemical cartography of the Milky WayGaia Data Release 3: Chemical
cartography of the Milky Way C. Babusiaux Gaia Data Release 3: Chemical
cartography of the Milky WayGaia Data Release 3: Chemical cartography of the
Milky WayGaia Data Release 3: Chemical cartography of the Milky WayGaia Data
Release 3: Chemical cartography of the Milky Way M. Biermann Gaia Data Release
3: Chemical cartography of the Milky WayGaia Data Release 3: Chemical
cartography of the Milky Way O.L. Creevey Gaia Data Release 3: Chemical
cartography of the Milky WayGaia Data Release 3: Chemical cartography of the
Milky Way C. Ducourant Gaia Data Release 3: Chemical cartography of the Milky
WayGaia Data Release 3: Chemical cartography of the Milky Way D.W. Evans Gaia
Data Release 3: Chemical cartography of the Milky WayGaia Data Release 3:
Chemical cartography of the Milky Way L. Eyer Gaia Data Release 3: Chemical
cartography of the Milky WayGaia Data Release 3: Chemical cartography of the
Milky Way R. Guerra Gaia Data Release 3: Chemical cartography of the Milky
WayGaia Data Release 3: Chemical cartography of the Milky Way A. Hutton Gaia
Data Release 3: Chemical cartography of the Milky WayGaia Data Release 3:
Chemical cartography of the Milky Way C. Jordi Gaia Data Release 3: Chemical
cartography of the Milky WayGaia Data Release 3: Chemical cartography of the
Milky Way S.A. Klioner Gaia Data Release 3: Chemical cartography of the Milky
WayGaia Data Release 3: Chemical cartography of the Milky Way U.L. Lammers
Gaia Data Release 3: Chemical cartography of the Milky WayGaia Data Release 3:
Chemical cartography of the Milky Way L. Lindegren Gaia Data Release 3:
Chemical cartography of the Milky WayGaia Data Release 3: Chemical cartography
of the Milky Way X. Luri Gaia Data Release 3: Chemical cartography of the
Milky WayGaia Data Release 3: Chemical cartography of the Milky Way F. Mignard
Gaia Data Release 3: Chemical cartography of the Milky WayGaia Data Release 3:
Chemical cartography of the Milky Way C. Panem Gaia Data Release 3: Chemical
cartography of the Milky WayGaia Data Release 3: Chemical cartography of the
Milky Way D. Pourbaix† Gaia Data Release 3: Chemical cartography of the Milky
WayGaia Data Release 3: Chemical cartography of the Milky WayGaia Data Release
3: Chemical cartography of the Milky WayGaia Data Release 3: Chemical
cartography of the Milky Way S. Randich Gaia Data Release 3: Chemical
cartography of the Milky WayGaia Data Release 3: Chemical cartography of the
Milky Way P. Sartoretti Gaia Data Release 3: Chemical cartography of the Milky
WayGaia Data Release 3: Chemical cartography of the Milky Way C. Soubiran Gaia
Data Release 3: Chemical cartography of the Milky WayGaia Data Release 3:
Chemical cartography of the Milky Way P. Tanga Gaia Data Release 3: Chemical
cartography of the Milky WayGaia Data Release 3: Chemical cartography of the
Milky Way N.A. Walton Gaia Data Release 3: Chemical cartography of the Milky
WayGaia Data Release 3: Chemical cartography of the Milky Way U. Bastian Gaia
Data Release 3: Chemical cartography of the Milky WayGaia Data Release 3:
Chemical cartography of the Milky Way R. Drimmel Gaia Data Release 3: Chemical
cartography of the Milky WayGaia Data Release 3: Chemical cartography of the
Milky Way F. Jansen Gaia Data Release 3: Chemical cartography of the Milky
WayGaia Data Release 3: Chemical cartography of the Milky Way F. van Leeuwen
Gaia Data Release 3: Chemical cartography of the Milky WayGaia Data Release 3:
Chemical cartography of the Milky Way J. Bakker Gaia Data Release 3: Chemical
cartography of the Milky WayGaia Data Release 3: Chemical cartography of the
Milky Way C. Cacciari Gaia Data Release 3: Chemical cartography of the Milky
WayGaia Data Release 3: Chemical cartography of the Milky Way J. Castañeda
Gaia Data Release 3: Chemical cartography of the Milky WayGaia Data Release 3:
Chemical cartography of the Milky Way F. De Angeli Gaia Data Release 3:
Chemical cartography of the Milky WayGaia Data Release 3: Chemical cartography
of the Milky Way C. Fabricius Gaia Data Release 3: Chemical cartography of the
Milky WayGaia Data Release 3: Chemical cartography of the Milky Way Y. Frémat
Gaia Data Release 3: Chemical cartography of the Milky WayGaia Data Release 3:
Chemical cartography of the Milky Way L. Galluccio Gaia Data Release 3:
Chemical cartography of the Milky WayGaia Data Release 3: Chemical cartography
of the Milky Way A. Guerrier Gaia Data Release 3: Chemical cartography of the
Milky WayGaia Data Release 3: Chemical cartography of the Milky Way E. Masana
Gaia Data Release 3: Chemical cartography of the Milky WayGaia Data Release 3:
Chemical cartography of the Milky Way R. Messineo Gaia Data Release 3:
Chemical cartography of the Milky WayGaia Data Release 3: Chemical cartography
of the Milky Way N. Mowlavi Gaia Data Release 3: Chemical cartography of the
Milky WayGaia Data Release 3: Chemical cartography of the Milky Way C. Nicolas
Gaia Data Release 3: Chemical cartography of the Milky WayGaia Data Release 3:
Chemical cartography of the Milky Way K. Nienartowicz Gaia Data Release 3:
Chemical cartography of the Milky WayGaia Data Release 3: Chemical cartography
of the Milky WayGaia Data Release 3: Chemical cartography of the Milky WayGaia
Data Release 3: Chemical cartography of the Milky Way F. Pailler Gaia Data
Release 3: Chemical cartography of the Milky WayGaia Data Release 3: Chemical
cartography of the Milky Way P. Panuzzo Gaia Data Release 3: Chemical
cartography of the Milky WayGaia Data Release 3: Chemical cartography of the
Milky Way F. Riclet Gaia Data Release 3: Chemical cartography of the Milky
WayGaia Data Release 3: Chemical cartography of the Milky Way W. Roux Gaia
Data Release 3: Chemical cartography of the Milky WayGaia Data Release 3:
Chemical cartography of the Milky Way R. Sordo Gaia Data Release 3: Chemical
cartography of the Milky WayGaia Data Release 3: Chemical cartography of the
Milky Way F. Thévenin Gaia Data Release 3: Chemical cartography of the Milky
WayGaia Data Release 3: Chemical cartography of the Milky Way G. Gracia-Abril
Gaia Data Release 3: Chemical cartography of the Milky WayGaia Data Release 3:
Chemical cartography of the Milky WayGaia Data Release 3: Chemical cartography
of the Milky WayGaia Data Release 3: Chemical cartography of the Milky Way J.
Portell Gaia Data Release 3: Chemical cartography of the Milky WayGaia Data
Release 3: Chemical cartography of the Milky Way D. Teyssier Gaia Data Release
3: Chemical cartography of the Milky WayGaia Data Release 3: Chemical
cartography of the Milky Way M. Altmann Gaia Data Release 3: Chemical
cartography of the Milky WayGaia Data Release 3: Chemical cartography of the
Milky WayGaia Data Release 3: Chemical cartography of the Milky WayGaia Data
Release 3: Chemical cartography of the Milky Way M. Audard Gaia Data Release
3: Chemical cartography of the Milky WayGaia Data Release 3: Chemical
cartography of the Milky WayGaia Data Release 3: Chemical cartography of the
Milky WayGaia Data Release 3: Chemical cartography of the Milky Way I. Bellas-
Velidis Gaia Data Release 3: Chemical cartography of the Milky WayGaia Data
Release 3: Chemical cartography of the Milky Way K. Benson Gaia Data Release
3: Chemical cartography of the Milky WayGaia Data Release 3: Chemical
cartography of the Milky Way J. Berthier Gaia Data Release 3: Chemical
cartography of the Milky WayGaia Data Release 3: Chemical cartography of the
Milky Way R. Blomme Gaia Data Release 3: Chemical cartography of the Milky
WayGaia Data Release 3: Chemical cartography of the Milky Way P.W. Burgess
Gaia Data Release 3: Chemical cartography of the Milky WayGaia Data Release 3:
Chemical cartography of the Milky Way D. Busonero Gaia Data Release 3:
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of the Milky Way G. Busso Gaia Data Release 3: Chemical cartography of the
Milky WayGaia Data Release 3: Chemical cartography of the Milky Way H. Cánovas
Gaia Data Release 3: Chemical cartography of the Milky WayGaia Data Release 3:
Chemical cartography of the Milky Way B. Carry Gaia Data Release 3: Chemical
cartography of the Milky WayGaia Data Release 3: Chemical cartography of the
Milky Way A. Cellino Gaia Data Release 3: Chemical cartography of the Milky
WayGaia Data Release 3: Chemical cartography of the Milky Way N. Cheek Gaia
Data Release 3: Chemical cartography of the Milky WayGaia Data Release 3:
Chemical cartography of the Milky Way G. Clementini Gaia Data Release 3:
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of the Milky Way Y. Damerdji Gaia Data Release 3: Chemical cartography of the
Milky WayGaia Data Release 3: Chemical cartography of the Milky WayGaia Data
Release 3: Chemical cartography of the Milky WayGaia Data Release 3: Chemical
cartography of the Milky Way M. Davidson Gaia Data Release 3: Chemical
cartography of the Milky WayGaia Data Release 3: Chemical cartography of the
Milky Way P. de Teodoro Gaia Data Release 3: Chemical cartography of the Milky
WayGaia Data Release 3: Chemical cartography of the Milky Way M. Nuñez Campos
Gaia Data Release 3: Chemical cartography of the Milky WayGaia Data Release 3:
Chemical cartography of the Milky Way L. Delchambre Gaia Data Release 3:
Chemical cartography of the Milky WayGaia Data Release 3: Chemical cartography
of the Milky Way A. Dell’Oro Gaia Data Release 3: Chemical cartography of the
Milky WayGaia Data Release 3: Chemical cartography of the Milky Way P. Esquej
Gaia Data Release 3: Chemical cartography of the Milky WayGaia Data Release 3:
Chemical cartography of the Milky Way J. Fernández-Hernández Gaia Data Release
3: Chemical cartography of the Milky WayGaia Data Release 3: Chemical
cartography of the Milky Way E. Fraile Gaia Data Release 3: Chemical
cartography of the Milky WayGaia Data Release 3: Chemical cartography of the
Milky Way D. Garabato Gaia Data Release 3: Chemical cartography of the Milky
WayGaia Data Release 3: Chemical cartography of the Milky Way P. García-Lario
Gaia Data Release 3: Chemical cartography of the Milky WayGaia Data Release 3:
Chemical cartography of the Milky Way E. Gosset Gaia Data Release 3: Chemical
cartography of the Milky WayGaia Data Release 3: Chemical cartography of the
Milky WayGaia Data Release 3: Chemical cartography of the Milky WayGaia Data
Release 3: Chemical cartography of the Milky Way R. Haigron Gaia Data Release
3: Chemical cartography of the Milky WayGaia Data Release 3: Chemical
cartography of the Milky Way J.-L. Halbwachs Gaia Data Release 3: Chemical
cartography of the Milky WayGaia Data Release 3: Chemical cartography of the
Milky Way N.C. Hambly Gaia Data Release 3: Chemical cartography of the Milky
WayGaia Data Release 3: Chemical cartography of the Milky Way D.L. Harrison
Gaia Data Release 3: Chemical cartography of the Milky WayGaia Data Release 3:
Chemical cartography of the Milky WayGaia Data Release 3: Chemical cartography
of the Milky WayGaia Data Release 3: Chemical cartography of the Milky Way J.
Hernández Gaia Data Release 3: Chemical cartography of the Milky WayGaia Data
Release 3: Chemical cartography of the Milky Way D. Hestroffer Gaia Data
Release 3: Chemical cartography of the Milky WayGaia Data Release 3: Chemical
cartography of the Milky Way S.T. Hodgkin Gaia Data Release 3: Chemical
cartography of the Milky WayGaia Data Release 3: Chemical cartography of the
Milky Way B. Holl Gaia Data Release 3: Chemical cartography of the Milky
WayGaia Data Release 3: Chemical cartography of the Milky WayGaia Data Release
3: Chemical cartography of the Milky WayGaia Data Release 3: Chemical
cartography of the Milky Way K. Janßen Gaia Data Release 3: Chemical
cartography of the Milky WayGaia Data Release 3: Chemical cartography of the
Milky Way G. Jevardat de Fombelle Gaia Data Release 3: Chemical cartography of
the Milky WayGaia Data Release 3: Chemical cartography of the Milky Way S.
Jordan Gaia Data Release 3: Chemical cartography of the Milky WayGaia Data
Release 3: Chemical cartography of the Milky Way A. Krone-Martins Gaia Data
Release 3: Chemical cartography of the Milky WayGaia Data Release 3: Chemical
cartography of the Milky WayGaia Data Release 3: Chemical cartography of the
Milky WayGaia Data Release 3: Chemical cartography of the Milky Way A.C.
Lanzafame Gaia Data Release 3: Chemical cartography of the Milky WayGaia Data
Release 3: Chemical cartography of the Milky WayGaia Data Release 3: Chemical
cartography of the Milky WayGaia Data Release 3: Chemical cartography of the
Milky Way W. L ̈offler Gaia Data Release 3: Chemical cartography of the Milky
WayGaia Data Release 3: Chemical cartography of the Milky Way O. Marchal Gaia
Data Release 3: Chemical cartography of the Milky WayGaia Data Release 3:
Chemical cartography of the Milky Way P.M. Marrese Gaia Data Release 3:
Chemical cartography of the Milky WayGaia Data Release 3: Chemical cartography
of the Milky WayGaia Data Release 3: Chemical cartography of the Milky WayGaia
Data Release 3: Chemical cartography of the Milky Way A. Moitinho Gaia Data
Release 3: Chemical cartography of the Milky WayGaia Data Release 3: Chemical
cartography of the Milky Way K. Muinonen Gaia Data Release 3: Chemical
cartography of the Milky WayGaia Data Release 3: Chemical cartography of the
Milky WayGaia Data Release 3: Chemical cartography of the Milky WayGaia Data
Release 3: Chemical cartography of the Milky Way P. Osborne Gaia Data Release
3: Chemical cartography of the Milky WayGaia Data Release 3: Chemical
cartography of the Milky Way E. Pancino Gaia Data Release 3: Chemical
cartography of the Milky WayGaia Data Release 3: Chemical cartography of the
Milky WayGaia Data Release 3: Chemical cartography of the Milky WayGaia Data
Release 3: Chemical cartography of the Milky Way T. Pauwels Gaia Data Release
3: Chemical cartography of the Milky WayGaia Data Release 3: Chemical
cartography of the Milky Way C. Reylé Gaia Data Release 3: Chemical
cartography of the Milky WayGaia Data Release 3: Chemical cartography of the
Milky Way M. Riello Gaia Data Release 3: Chemical cartography of the Milky
WayGaia Data Release 3: Chemical cartography of the Milky Way L. Rimoldini
Gaia Data Release 3: Chemical cartography of the Milky WayGaia Data Release 3:
Chemical cartography of the Milky Way T. Roegiers Gaia Data Release 3:
Chemical cartography of the Milky WayGaia Data Release 3: Chemical cartography
of the Milky Way J. Rybizki Gaia Data Release 3: Chemical cartography of the
Milky WayGaia Data Release 3: Chemical cartography of the Milky Way L.M. Sarro
Gaia Data Release 3: Chemical cartography of the Milky WayGaia Data Release 3:
Chemical cartography of the Milky Way C. Siopis Gaia Data Release 3: Chemical
cartography of the Milky WayGaia Data Release 3: Chemical cartography of the
Milky Way M. Smith Gaia Data Release 3: Chemical cartography of the Milky
WayGaia Data Release 3: Chemical cartography of the Milky Way A. Sozzetti Gaia
Data Release 3: Chemical cartography of the Milky WayGaia Data Release 3:
Chemical cartography of the Milky Way E. Utrilla Gaia Data Release 3: Chemical
cartography of the Milky WayGaia Data Release 3: Chemical cartography of the
Milky Way M. van Leeuwen Gaia Data Release 3: Chemical cartography of the
Milky WayGaia Data Release 3: Chemical cartography of the Milky Way U. Abbas
Gaia Data Release 3: Chemical cartography of the Milky WayGaia Data Release 3:
Chemical cartography of the Milky Way P. Ábrahám Gaia Data Release 3: Chemical
cartography of the Milky WayGaia Data Release 3: Chemical cartography of the
Milky WayGaia Data Release 3: Chemical cartography of the Milky WayGaia Data
Release 3: Chemical cartography of the Milky Way A. Abreu Aramburu Gaia Data
Release 3: Chemical cartography of the Milky WayGaia Data Release 3: Chemical
cartography of the Milky Way C. Aerts Gaia Data Release 3: Chemical
cartography of the Milky WayGaia Data Release 3: Chemical cartography of the
Milky WayGaia Data Release 3: Chemical cartography of the Milky WayGaia Data
Release 3: Chemical cartography of the Milky WayGaia Data Release 3: Chemical
cartography of the Milky WayGaia Data Release 3: Chemical cartography of the
Milky Way J.J. Aguado Gaia Data Release 3: Chemical cartography of the Milky
WayGaia Data Release 3: Chemical cartography of the Milky Way M. Ajaj Gaia
Data Release 3: Chemical cartography of the Milky WayGaia Data Release 3:
Chemical cartography of the Milky Way F. Aldea-Montero Gaia Data Release 3:
Chemical cartography of the Milky WayGaia Data Release 3: Chemical cartography
of the Milky Way G. Altavilla Gaia Data Release 3: Chemical cartography of the
Milky WayGaia Data Release 3: Chemical cartography of the Milky WayGaia Data
Release 3: Chemical cartography of the Milky WayGaia Data Release 3: Chemical
cartography of the Milky Way M.A. Álvarez Gaia Data Release 3: Chemical
cartography of the Milky WayGaia Data Release 3: Chemical cartography of the
Milky Way J. Alves Gaia Data Release 3: Chemical cartography of the Milky
WayGaia Data Release 3: Chemical cartography of the Milky Way F. Anders Gaia
Data Release 3: Chemical cartography of the Milky WayGaia Data Release 3:
Chemical cartography of the Milky Way R.I. Anderson Gaia Data Release 3:
Chemical cartography of the Milky WayGaia Data Release 3: Chemical cartography
of the Milky Way E. Anglada Varela Gaia Data Release 3: Chemical cartography
of the Milky WayGaia Data Release 3: Chemical cartography of the Milky Way D.
Baines Gaia Data Release 3: Chemical cartography of the Milky WayGaia Data
Release 3: Chemical cartography of the Milky Way S.G. Baker Gaia Data Release
3: Chemical cartography of the Milky WayGaia Data Release 3: Chemical
cartography of the Milky Way L. Balaguer-Núñez Gaia Data Release 3: Chemical
cartography of the Milky WayGaia Data Release 3: Chemical cartography of the
Milky Way E. Balbinot Gaia Data Release 3: Chemical cartography of the Milky
WayGaia Data Release 3: Chemical cartography of the Milky Way Z. Balog Gaia
Data Release 3: Chemical cartography of the Milky WayGaia Data Release 3:
Chemical cartography of the Milky WayGaia Data Release 3: Chemical cartography
of the Milky WayGaia Data Release 3: Chemical cartography of the Milky Way C.
Barache Gaia Data Release 3: Chemical cartography of the Milky WayGaia Data
Release 3: Chemical cartography of the Milky Way D. Barbato Gaia Data Release
3: Chemical cartography of the Milky WayGaia Data Release 3: Chemical
cartography of the Milky WayGaia Data Release 3: Chemical cartography of the
Milky WayGaia Data Release 3: Chemical cartography of the Milky Way M. Barros
Gaia Data Release 3: Chemical cartography of the Milky WayGaia Data Release 3:
Chemical cartography of the Milky Way M.A. Barstow Gaia Data Release 3:
Chemical cartography of the Milky WayGaia Data Release 3: Chemical cartography
of the Milky Way S. Bartolomé Gaia Data Release 3: Chemical cartography of the
Milky WayGaia Data Release 3: Chemical cartography of the Milky Way J.-L.
Bassilana Gaia Data Release 3: Chemical cartography of the Milky WayGaia Data
Release 3: Chemical cartography of the Milky Way N. Bauchet Gaia Data Release
3: Chemical cartography of the Milky WayGaia Data Release 3: Chemical
cartography of the Milky Way U. Becciani Gaia Data Release 3: Chemical
cartography of the Milky WayGaia Data Release 3: Chemical cartography of the
Milky Way M. Bellazzini Gaia Data Release 3: Chemical cartography of the Milky
WayGaia Data Release 3: Chemical cartography of the Milky Way A. Berihuete
Gaia Data Release 3: Chemical cartography of the Milky WayGaia Data Release 3:
Chemical cartography of the Milky Way M. Bernet Gaia Data Release 3: Chemical
cartography of the Milky WayGaia Data Release 3: Chemical cartography of the
Milky Way S. Bertone Gaia Data Release 3: Chemical cartography of the Milky
WayGaia Data Release 3: Chemical cartography of the Milky WayGaia Data Release
3: Chemical cartography of the Milky WayGaia Data Release 3: Chemical
cartography of the Milky WayGaia Data Release 3: Chemical cartography of the
Milky WayGaia Data Release 3: Chemical cartography of the Milky Way L. Bianchi
Gaia Data Release 3: Chemical cartography of the Milky WayGaia Data Release 3:
Chemical cartography of the Milky Way A. Binnenfeld Gaia Data Release 3:
Chemical cartography of the Milky WayGaia Data Release 3: Chemical cartography
of the Milky Way S. Blanco-Cuaresma Gaia Data Release 3: Chemical cartography
of the Milky WayGaia Data Release 3: Chemical cartography of the Milky Way T.
Boch Gaia Data Release 3: Chemical cartography of the Milky WayGaia Data
Release 3: Chemical cartography of the Milky Way A. Bombrun Gaia Data Release
3: Chemical cartography of the Milky WayGaia Data Release 3: Chemical
cartography of the Milky Way D. Bossini Gaia Data Release 3: Chemical
cartography of the Milky WayGaia Data Release 3: Chemical cartography of the
Milky Way S. Bouquillon Gaia Data Release 3: Chemical cartography of the Milky
WayGaia Data Release 3: Chemical cartography of the Milky WayGaia Data Release
3: Chemical cartography of the Milky WayGaia Data Release 3: Chemical
cartography of the Milky Way L. Bramante Gaia Data Release 3: Chemical
cartography of the Milky WayGaia Data Release 3: Chemical cartography of the
Milky Way E. Breedt Gaia Data Release 3: Chemical cartography of the Milky
WayGaia Data Release 3: Chemical cartography of the Milky Way A. Bressan Gaia
Data Release 3: Chemical cartography of the Milky WayGaia Data Release 3:
Chemical cartography of the Milky Way N. Brouillet Gaia Data Release 3:
Chemical cartography of the Milky WayGaia Data Release 3: Chemical cartography
of the Milky Way E. Brugaletta Gaia Data Release 3: Chemical cartography of
the Milky WayGaia Data Release 3: Chemical cartography of the Milky Way B.
Bucciarelli Gaia Data Release 3: Chemical cartography of the Milky WayGaia
Data Release 3: Chemical cartography of the Milky WayGaia Data Release 3:
Chemical cartography of the Milky WayGaia Data Release 3: Chemical cartography
of the Milky Way A. Burlacu Gaia Data Release 3: Chemical cartography of the
Milky WayGaia Data Release 3: Chemical cartography of the Milky Way A.G.
Butkevich Gaia Data Release 3: Chemical cartography of the Milky WayGaia Data
Release 3: Chemical cartography of the Milky Way R. Buzzi Gaia Data Release 3:
Chemical cartography of the Milky WayGaia Data Release 3: Chemical cartography
of the Milky Way E. Caffau Gaia Data Release 3: Chemical cartography of the
Milky WayGaia Data Release 3: Chemical cartography of the Milky Way R.
Cancelliere Gaia Data Release 3: Chemical cartography of the Milky WayGaia
Data Release 3: Chemical cartography of the Milky Way R. Carballo Gaia Data
Release 3: Chemical cartography of the Milky WayGaia Data Release 3: Chemical
cartography of the Milky Way T. Carlucci Gaia Data Release 3: Chemical
cartography of the Milky WayGaia Data Release 3: Chemical cartography of the
Milky Way M.I. Carnerero Gaia Data Release 3: Chemical cartography of the
Milky WayGaia Data Release 3: Chemical cartography of the Milky Way J.M.
Carrasco Gaia Data Release 3: Chemical cartography of the Milky WayGaia Data
Release 3: Chemical cartography of the Milky Way M. Castellani Gaia Data
Release 3: Chemical cartography of the Milky WayGaia Data Release 3: Chemical
cartography of the Milky Way A. Castro-Ginard Gaia Data Release 3: Chemical
cartography of the Milky WayGaia Data Release 3: Chemical cartography of the
Milky Way L. Chaoul Gaia Data Release 3: Chemical cartography of the Milky
WayGaia Data Release 3: Chemical cartography of the Milky Way P. Charlot Gaia
Data Release 3: Chemical cartography of the Milky WayGaia Data Release 3:
Chemical cartography of the Milky Way L. Chemin Gaia Data Release 3: Chemical
cartography of the Milky WayGaia Data Release 3: Chemical cartography of the
Milky Way V. Chiaramida Gaia Data Release 3: Chemical cartography of the Milky
WayGaia Data Release 3: Chemical cartography of the Milky Way A. Chiavassa
Gaia Data Release 3: Chemical cartography of the Milky WayGaia Data Release 3:
Chemical cartography of the Milky Way N. Chornay Gaia Data Release 3: Chemical
cartography of the Milky WayGaia Data Release 3: Chemical cartography of the
Milky Way G. Comoretto Gaia Data Release 3: Chemical cartography of the Milky
WayGaia Data Release 3: Chemical cartography of the Milky WayGaia Data Release
3: Chemical cartography of the Milky WayGaia Data Release 3: Chemical
cartography of the Milky Way G. Contursi Gaia Data Release 3: Chemical
cartography of the Milky WayGaia Data Release 3: Chemical cartography of the
Milky Way W.J. Cooper Gaia Data Release 3: Chemical cartography of the Milky
WayGaia Data Release 3: Chemical cartography of the Milky WayGaia Data Release
3: Chemical cartography of the Milky WayGaia Data Release 3: Chemical
cartography of the Milky Way T. Cornez Gaia Data Release 3: Chemical
cartography of the Milky WayGaia Data Release 3: Chemical cartography of the
Milky Way S. Cowell Gaia Data Release 3: Chemical cartography of the Milky
WayGaia Data Release 3: Chemical cartography of the Milky Way F. Crifo Gaia
Data Release 3: Chemical cartography of the Milky WayGaia Data Release 3:
Chemical cartography of the Milky Way M. Crosta Gaia Data Release 3: Chemical
cartography of the Milky WayGaia Data Release 3: Chemical cartography of the
Milky WayGaia Data Release 3: Chemical cartography of the Milky WayGaia Data
Release 3: Chemical cartography of the Milky Way C. Crowley Gaia Data Release
3: Chemical cartography of the Milky WayGaia Data Release 3: Chemical
cartography of the Milky Way C. Dafonte Gaia Data Release 3: Chemical
cartography of the Milky WayGaia Data Release 3: Chemical cartography of the
Milky Way A. Dapergolas Gaia Data Release 3: Chemical cartography of the Milky
WayGaia Data Release 3: Chemical cartography of the Milky Way P. David Gaia
Data Release 3: Chemical cartography of the Milky WayGaia Data Release 3:
Chemical cartography of the Milky Way F. De Luise Gaia Data Release 3:
Chemical cartography of the Milky WayGaia Data Release 3: Chemical cartography
of the Milky Way R. De March Gaia Data Release 3: Chemical cartography of the
Milky WayGaia Data Release 3: Chemical cartography of the Milky Way J. De
Ridder Gaia Data Release 3: Chemical cartography of the Milky WayGaia Data
Release 3: Chemical cartography of the Milky Way R. de Souza Gaia Data Release
3: Chemical cartography of the Milky WayGaia Data Release 3: Chemical
cartography of the Milky Way A. de Torres Gaia Data Release 3: Chemical
cartography of the Milky WayGaia Data Release 3: Chemical cartography of the
Milky Way E.F. del Peloso Gaia Data Release 3: Chemical cartography of the
Milky WayGaia Data Release 3: Chemical cartography of the Milky Way E. del
Pozo Gaia Data Release 3: Chemical cartography of the Milky WayGaia Data
Release 3: Chemical cartography of the Milky Way M. Delbo Gaia Data Release 3:
Chemical cartography of the Milky WayGaia Data Release 3: Chemical cartography
of the Milky Way A. Delgado Gaia Data Release 3: Chemical cartography of the
Milky WayGaia Data Release 3: Chemical cartography of the Milky Way J.-B.
Delisle Gaia Data Release 3: Chemical cartography of the Milky WayGaia Data
Release 3: Chemical cartography of the Milky Way C. Demouchy Gaia Data Release
3: Chemical cartography of the Milky WayGaia Data Release 3: Chemical
cartography of the Milky Way T.E. Dharmawardena Gaia Data Release 3: Chemical
cartography of the Milky WayGaia Data Release 3: Chemical cartography of the
Milky Way P. Di Matteo Gaia Data Release 3: Chemical cartography of the Milky
WayGaia Data Release 3: Chemical cartography of the Milky Way S. Diakite Gaia
Data Release 3: Chemical cartography of the Milky WayGaia Data Release 3:
Chemical cartography of the Milky Way C. Diener Gaia Data Release 3: Chemical
cartography of the Milky WayGaia Data Release 3: Chemical cartography of the
Milky Way E. Distefano Gaia Data Release 3: Chemical cartography of the Milky
WayGaia Data Release 3: Chemical cartography of the Milky Way C. Dolding Gaia
Data Release 3: Chemical cartography of the Milky WayGaia Data Release 3:
Chemical cartography of the Milky Way B. Edvardsson Gaia Data Release 3:
Chemical cartography of the Milky WayGaia Data Release 3: Chemical cartography
of the Milky Way H. Enke Gaia Data Release 3: Chemical cartography of the
Milky WayGaia Data Release 3: Chemical cartography of the Milky Way C. Fabre
Gaia Data Release 3: Chemical cartography of the Milky WayGaia Data Release 3:
Chemical cartography of the Milky Way M. Fabrizio Gaia Data Release 3:
Chemical cartography of the Milky WayGaia Data Release 3: Chemical cartography
of the Milky WayGaia Data Release 3: Chemical cartography of the Milky WayGaia
Data Release 3: Chemical cartography of the Milky Way S. Faigler Gaia Data
Release 3: Chemical cartography of the Milky WayGaia Data Release 3: Chemical
cartography of the Milky Way G. Fedorets Gaia Data Release 3: Chemical
cartography of the Milky WayGaia Data Release 3: Chemical cartography of the
Milky WayGaia Data Release 3: Chemical cartography of the Milky WayGaia Data
Release 3: Chemical cartography of the Milky Way P. Fernique Gaia Data Release
3: Chemical cartography of the Milky WayGaia Data Release 3: Chemical
cartography of the Milky WayGaia Data Release 3: Chemical cartography of the
Milky WayGaia Data Release 3: Chemical cartography of the Milky Way F.
Figueras Gaia Data Release 3: Chemical cartography of the Milky WayGaia Data
Release 3: Chemical cartography of the Milky Way Y. Fournier Gaia Data Release
3: Chemical cartography of the Milky WayGaia Data Release 3: Chemical
cartography of the Milky Way C. Fouron Gaia Data Release 3: Chemical
cartography of the Milky WayGaia Data Release 3: Chemical cartography of the
Milky Way F. Fragkoudi Gaia Data Release 3: Chemical cartography of the Milky
WayGaia Data Release 3: Chemical cartography of the Milky WayGaia Data Release
3: Chemical cartography of the Milky WayGaia Data Release 3: Chemical
cartography of the Milky WayGaia Data Release 3: Chemical cartography of the
Milky WayGaia Data Release 3: Chemical cartography of the Milky Way M. Gai
Gaia Data Release 3: Chemical cartography of the Milky WayGaia Data Release 3:
Chemical cartography of the Milky Way A. Garcia-Gutierrez Gaia Data Release 3:
Chemical cartography of the Milky WayGaia Data Release 3: Chemical cartography
of the Milky Way M. Garcia-Reinaldos Gaia Data Release 3: Chemical cartography
of the Milky WayGaia Data Release 3: Chemical cartography of the Milky Way M.
García-Torres Gaia Data Release 3: Chemical cartography of the Milky WayGaia
Data Release 3: Chemical cartography of the Milky Way A. Garofalo Gaia Data
Release 3: Chemical cartography of the Milky WayGaia Data Release 3: Chemical
cartography of the Milky Way A. Gavel Gaia Data Release 3: Chemical
cartography of the Milky WayGaia Data Release 3: Chemical cartography of the
Milky Way P. Gavras Gaia Data Release 3: Chemical cartography of the Milky
WayGaia Data Release 3: Chemical cartography of the Milky Way E. Gerlach Gaia
Data Release 3: Chemical cartography of the Milky WayGaia Data Release 3:
Chemical cartography of the Milky Way R. Geyer Gaia Data Release 3: Chemical
cartography of the Milky WayGaia Data Release 3: Chemical cartography of the
Milky Way P. Giacobbe Gaia Data Release 3: Chemical cartography of the Milky
WayGaia Data Release 3: Chemical cartography of the Milky Way G. Gilmore Gaia
Data Release 3: Chemical cartography of the Milky WayGaia Data Release 3:
Chemical cartography of the Milky Way S. Girona Gaia Data Release 3: Chemical
cartography of the Milky WayGaia Data Release 3: Chemical cartography of the
Milky Way G. Giuffrida Gaia Data Release 3: Chemical cartography of the Milky
WayGaia Data Release 3: Chemical cartography of the Milky Way R. Gomel Gaia
Data Release 3: Chemical cartography of the Milky WayGaia Data Release 3:
Chemical cartography of the Milky Way A. Gomez Gaia Data Release 3: Chemical
cartography of the Milky WayGaia Data Release 3: Chemical cartography of the
Milky Way J. González-Núñez Gaia Data Release 3: Chemical cartography of the
Milky WayGaia Data Release 3: Chemical cartography of the Milky WayGaia Data
Release 3: Chemical cartography of the Milky WayGaia Data Release 3: Chemical
cartography of the Milky Way I. González-Santamaría Gaia Data Release 3:
Chemical cartography of the Milky WayGaia Data Release 3: Chemical cartography
of the Milky Way J.J. González-Vidal Gaia Data Release 3: Chemical cartography
of the Milky WayGaia Data Release 3: Chemical cartography of the Milky Way M.
Granvik Gaia Data Release 3: Chemical cartography of the Milky WayGaia Data
Release 3: Chemical cartography of the Milky WayGaia Data Release 3: Chemical
cartography of the Milky WayGaia Data Release 3: Chemical cartography of the
Milky Way P. Guillout Gaia Data Release 3: Chemical cartography of the Milky
WayGaia Data Release 3: Chemical cartography of the Milky Way J. Guiraud Gaia
Data Release 3: Chemical cartography of the Milky WayGaia Data Release 3:
Chemical cartography of the Milky Way R. Gutiérrez-Sánchez Gaia Data Release
3: Chemical cartography of the Milky WayGaia Data Release 3: Chemical
cartography of the Milky Way L.P. Guy Gaia Data Release 3: Chemical
cartography of the Milky WayGaia Data Release 3: Chemical cartography of the
Milky WayGaia Data Release 3: Chemical cartography of the Milky WayGaia Data
Release 3: Chemical cartography of the Milky Way D. Hatzidimitriou Gaia Data
Release 3: Chemical cartography of the Milky WayGaia Data Release 3: Chemical
cartography of the Milky WayGaia Data Release 3: Chemical cartography of the
Milky WayGaia Data Release 3: Chemical cartography of the Milky Way M. Hauser
Gaia Data Release 3: Chemical cartography of the Milky WayGaia Data Release 3:
Chemical cartography of the Milky WayGaia Data Release 3: Chemical cartography
of the Milky WayGaia Data Release 3: Chemical cartography of the Milky Way M.
Haywood Gaia Data Release 3: Chemical cartography of the Milky WayGaia Data
Release 3: Chemical cartography of the Milky Way A. Helmer Gaia Data Release
3: Chemical cartography of the Milky WayGaia Data Release 3: Chemical
cartography of the Milky Way A. Helmi Gaia Data Release 3: Chemical
cartography of the Milky WayGaia Data Release 3: Chemical cartography of the
Milky Way M.H. Sarmiento Gaia Data Release 3: Chemical cartography of the
Milky WayGaia Data Release 3: Chemical cartography of the Milky Way S.L.
Hidalgo Gaia Data Release 3: Chemical cartography of the Milky WayGaia Data
Release 3: Chemical cartography of the Milky WayGaia Data Release 3: Chemical
cartography of the Milky WayGaia Data Release 3: Chemical cartography of the
Milky Way N. Hładczuk Gaia Data Release 3: Chemical cartography of the Milky
WayGaia Data Release 3: Chemical cartography of the Milky WayGaia Data Release
3: Chemical cartography of the Milky WayGaia Data Release 3: Chemical
cartography of the Milky Way D. Hobbs Gaia Data Release 3: Chemical
cartography of the Milky WayGaia Data Release 3: Chemical cartography of the
Milky Way G. Holland Gaia Data Release 3: Chemical cartography of the Milky
WayGaia Data Release 3: Chemical cartography of the Milky Way H.E. Huckle Gaia
Data Release 3: Chemical cartography of the Milky WayGaia Data Release 3:
Chemical cartography of the Milky Way K. Jardine Gaia Data Release 3: Chemical
cartography of the Milky WayGaia Data Release 3: Chemical cartography of the
Milky Way G. Jasniewicz Gaia Data Release 3: Chemical cartography of the Milky
WayGaia Data Release 3: Chemical cartography of the Milky Way A. Jean-Antoine
Piccolo Gaia Data Release 3: Chemical cartography of the Milky WayGaia Data
Release 3: Chemical cartography of the Milky Way Ó. Jiménez-Arranz Gaia Data
Release 3: Chemical cartography of the Milky WayGaia Data Release 3: Chemical
cartography of the Milky Way J. Juaristi Campillo Gaia Data Release 3:
Chemical cartography of the Milky WayGaia Data Release 3: Chemical cartography
of the Milky Way F. Julbe Gaia Data Release 3: Chemical cartography of the
Milky WayGaia Data Release 3: Chemical cartography of the Milky Way L.
Karbevska Gaia Data Release 3: Chemical cartography of the Milky WayGaia Data
Release 3: Chemical cartography of the Milky WayGaia Data Release 3: Chemical
cartography of the Milky WayGaia Data Release 3: Chemical cartography of the
Milky Way P. Kervella Gaia Data Release 3: Chemical cartography of the Milky
WayGaia Data Release 3: Chemical cartography of the Milky Way S. Khanna Gaia
Data Release 3: Chemical cartography of the Milky WayGaia Data Release 3:
Chemical cartography of the Milky WayGaia Data Release 3: Chemical cartography
of the Milky WayGaia Data Release 3: Chemical cartography of the Milky Way
A.J. Korn Gaia Data Release 3: Chemical cartography of the Milky WayGaia Data
Release 3: Chemical cartography of the Milky Way Á Kóspál Gaia Data Release 3:
Chemical cartography of the Milky WayGaia Data Release 3: Chemical cartography
of the Milky WayGaia Data Release 3: Chemical cartography of the Milky WayGaia
Data Release 3: Chemical cartography of the Milky WayGaia Data Release 3:
Chemical cartography of the Milky WayGaia Data Release 3: Chemical cartography
of the Milky Way Z. Kostrzewa-Rutkowska Gaia Data Release 3: Chemical
cartography of the Milky WayGaia Data Release 3: Chemical cartography of the
Milky WayGaia Data Release 3: Chemical cartography of the Milky WayGaia Data
Release 3: Chemical cartography of the Milky Way K. Kruszyńska Gaia Data
Release 3: Chemical cartography of the Milky WayGaia Data Release 3: Chemical
cartography of the Milky Way M. Kun Gaia Data Release 3: Chemical cartography
of the Milky WayGaia Data Release 3: Chemical cartography of the Milky Way P.
Laizeau Gaia Data Release 3: Chemical cartography of the Milky WayGaia Data
Release 3: Chemical cartography of the Milky Way S. Lambert Gaia Data Release
3: Chemical cartography of the Milky WayGaia Data Release 3: Chemical
cartography of the Milky Way A.F. Lanza Gaia Data Release 3: Chemical
cartography of the Milky WayGaia Data Release 3: Chemical cartography of the
Milky Way Y. Lasne Gaia Data Release 3: Chemical cartography of the Milky
WayGaia Data Release 3: Chemical cartography of the Milky Way J.-F. Le Campion
Gaia Data Release 3: Chemical cartography of the Milky WayGaia Data Release 3:
Chemical cartography of the Milky Way Y. Lebreton Gaia Data Release 3:
Chemical cartography of the Milky WayGaia Data Release 3: Chemical cartography
of the Milky WayGaia Data Release 3: Chemical cartography of the Milky WayGaia
Data Release 3: Chemical cartography of the Milky Way T. Lebzelter Gaia Data
Release 3: Chemical cartography of the Milky WayGaia Data Release 3: Chemical
cartography of the Milky Way S. Leccia Gaia Data Release 3: Chemical
cartography of the Milky WayGaia Data Release 3: Chemical cartography of the
Milky Way N. Leclerc Gaia Data Release 3: Chemical cartography of the Milky
WayGaia Data Release 3: Chemical cartography of the Milky Way I. Lecoeur-Taibi
Gaia Data Release 3: Chemical cartography of the Milky WayGaia Data Release 3:
Chemical cartography of the Milky Way S. Liao Gaia Data Release 3: Chemical
cartography of the Milky WayGaia Data Release 3: Chemical cartography of the
Milky WayGaia Data Release 3: Chemical cartography of the Milky WayGaia Data
Release 3: Chemical cartography of the Milky WayGaia Data Release 3: Chemical
cartography of the Milky WayGaia Data Release 3: Chemical cartography of the
Milky Way E.L. Licata Gaia Data Release 3: Chemical cartography of the Milky
WayGaia Data Release 3: Chemical cartography of the Milky Way H.E.P. Lindstrøm
Gaia Data Release 3: Chemical cartography of the Milky WayGaia Data Release 3:
Chemical cartography of the Milky WayGaia Data Release 3: Chemical cartography
of the Milky WayGaia Data Release 3: Chemical cartography of the Milky WayGaia
Data Release 3: Chemical cartography of the Milky WayGaia Data Release 3:
Chemical cartography of the Milky Way T.A. Lister Gaia Data Release 3:
Chemical cartography of the Milky WayGaia Data Release 3: Chemical cartography
of the Milky Way E. Livanou Gaia Data Release 3: Chemical cartography of the
Milky WayGaia Data Release 3: Chemical cartography of the Milky Way A. Lobel
Gaia Data Release 3: Chemical cartography of the Milky WayGaia Data Release 3:
Chemical cartography of the Milky Way A. Lorca Gaia Data Release 3: Chemical
cartography of the Milky WayGaia Data Release 3: Chemical cartography of the
Milky Way C. Loup Gaia Data Release 3: Chemical cartography of the Milky
WayGaia Data Release 3: Chemical cartography of the Milky Way P. Madrero Pardo
Gaia Data Release 3: Chemical cartography of the Milky WayGaia Data Release 3:
Chemical cartography of the Milky Way A. Magdaleno Romeo Gaia Data Release 3:
Chemical cartography of the Milky WayGaia Data Release 3: Chemical cartography
of the Milky Way S. Managau Gaia Data Release 3: Chemical cartography of the
Milky WayGaia Data Release 3: Chemical cartography of the Milky Way R.G. Mann
Gaia Data Release 3: Chemical cartography of the Milky WayGaia Data Release 3:
Chemical cartography of the Milky Way M. Manteiga Gaia Data Release 3:
Chemical cartography of the Milky WayGaia Data Release 3: Chemical cartography
of the Milky Way J.M. Marchant Gaia Data Release 3: Chemical cartography of
the Milky WayGaia Data Release 3: Chemical cartography of the Milky Way M.
Marconi Gaia Data Release 3: Chemical cartography of the Milky WayGaia Data
Release 3: Chemical cartography of the Milky Way J. Marcos Gaia Data Release
3: Chemical cartography of the Milky WayGaia Data Release 3: Chemical
cartography of the Milky Way M.M.S. Marcos Santos Gaia Data Release 3:
Chemical cartography of the Milky WayGaia Data Release 3: Chemical cartography
of the Milky Way D. Marín Pina Gaia Data Release 3: Chemical cartography of
the Milky WayGaia Data Release 3: Chemical cartography of the Milky Way S.
Marinoni Gaia Data Release 3: Chemical cartography of the Milky WayGaia Data
Release 3: Chemical cartography of the Milky WayGaia Data Release 3: Chemical
cartography of the Milky WayGaia Data Release 3: Chemical cartography of the
Milky Way F. Marocco Gaia Data Release 3: Chemical cartography of the Milky
WayGaia Data Release 3: Chemical cartography of the Milky Way D.J. Marshall
Gaia Data Release 3: Chemical cartography of the Milky WayGaia Data Release 3:
Chemical cartography of the Milky Way L. Martin Polo Gaia Data Release 3:
Chemical cartography of the Milky WayGaia Data Release 3: Chemical cartography
of the Milky Way J.M. Martín-Fleitas Gaia Data Release 3: Chemical cartography
of the Milky WayGaia Data Release 3: Chemical cartography of the Milky Way G.
Marton Gaia Data Release 3: Chemical cartography of the Milky WayGaia Data
Release 3: Chemical cartography of the Milky Way N. Mary Gaia Data Release 3:
Chemical cartography of the Milky WayGaia Data Release 3: Chemical cartography
of the Milky Way A. Masip Gaia Data Release 3: Chemical cartography of the
Milky WayGaia Data Release 3: Chemical cartography of the Milky Way D. Massari
Gaia Data Release 3: Chemical cartography of the Milky WayGaia Data Release 3:
Chemical cartography of the Milky Way A. Mastrobuono-Battisti Gaia Data
Release 3: Chemical cartography of the Milky WayGaia Data Release 3: Chemical
cartography of the Milky Way T. Mazeh Gaia Data Release 3: Chemical
cartography of the Milky WayGaia Data Release 3: Chemical cartography of the
Milky Way S. Messina Gaia Data Release 3: Chemical cartography of the Milky
WayGaia Data Release 3: Chemical cartography of the Milky Way D. Michalik Gaia
Data Release 3: Chemical cartography of the Milky WayGaia Data Release 3:
Chemical cartography of the Milky Way N.R. Millar Gaia Data Release 3:
Chemical cartography of the Milky WayGaia Data Release 3: Chemical cartography
of the Milky Way A. Mints Gaia Data Release 3: Chemical cartography of the
Milky WayGaia Data Release 3: Chemical cartography of the Milky Way D. Molina
Gaia Data Release 3: Chemical cartography of the Milky WayGaia Data Release 3:
Chemical cartography of the Milky Way R. Molinaro Gaia Data Release 3:
Chemical cartography of the Milky WayGaia Data Release 3: Chemical cartography
of the Milky Way L. Molnár Gaia Data Release 3: Chemical cartography of the
Milky WayGaia Data Release 3: Chemical cartography of the Milky WayGaia Data
Release 3: Chemical cartography of the Milky WayGaia Data Release 3: Chemical
cartography of the Milky WayGaia Data Release 3: Chemical cartography of the
Milky WayGaia Data Release 3: Chemical cartography of the Milky Way G. Monari
Gaia Data Release 3: Chemical cartography of the Milky WayGaia Data Release 3:
Chemical cartography of the Milky Way M. Monguió Gaia Data Release 3: Chemical
cartography of the Milky WayGaia Data Release 3: Chemical cartography of the
Milky Way P. Montegriffo Gaia Data Release 3: Chemical cartography of the
Milky WayGaia Data Release 3: Chemical cartography of the Milky Way A. Montero
Gaia Data Release 3: Chemical cartography of the Milky WayGaia Data Release 3:
Chemical cartography of the Milky Way R. Mor Gaia Data Release 3: Chemical
cartography of the Milky WayGaia Data Release 3: Chemical cartography of the
Milky Way A. Mora Gaia Data Release 3: Chemical cartography of the Milky
WayGaia Data Release 3: Chemical cartography of the Milky Way R. Morbidelli
Gaia Data Release 3: Chemical cartography of the Milky WayGaia Data Release 3:
Chemical cartography of the Milky Way T. Morel Gaia Data Release 3: Chemical
cartography of the Milky WayGaia Data Release 3: Chemical cartography of the
Milky Way D. Morris Gaia Data Release 3: Chemical cartography of the Milky
WayGaia Data Release 3: Chemical cartography of the Milky Way T. Muraveva Gaia
Data Release 3: Chemical cartography of the Milky WayGaia Data Release 3:
Chemical cartography of the Milky Way C.P. Murphy Gaia Data Release 3:
Chemical cartography of the Milky WayGaia Data Release 3: Chemical cartography
of the Milky Way I. Musella Gaia Data Release 3: Chemical cartography of the
Milky WayGaia Data Release 3: Chemical cartography of the Milky Way Z. Nagy
Gaia Data Release 3: Chemical cartography of the Milky WayGaia Data Release 3:
Chemical cartography of the Milky Way L. Noval Gaia Data Release 3: Chemical
cartography of the Milky WayGaia Data Release 3: Chemical cartography of the
Milky Way F. Ocaña Gaia Data Release 3: Chemical cartography of the Milky
WayGaia Data Release 3: Chemical cartography of the Milky WayGaia Data Release
3: Chemical cartography of the Milky WayGaia Data Release 3: Chemical
cartography of the Milky Way A. Ogden Gaia Data Release 3: Chemical
cartography of the Milky WayGaia Data Release 3: Chemical cartography of the
Milky Way C. Ordenovic Gaia Data Release 3: Chemical cartography of the Milky
WayGaia Data Release 3: Chemical cartography of the Milky Way J.O. Osinde Gaia
Data Release 3: Chemical cartography of the Milky WayGaia Data Release 3:
Chemical cartography of the Milky Way C. Pagani Gaia Data Release 3: Chemical
cartography of the Milky WayGaia Data Release 3: Chemical cartography of the
Milky Way I. Pagano Gaia Data Release 3: Chemical cartography of the Milky
WayGaia Data Release 3: Chemical cartography of the Milky Way L. Palaversa
Gaia Data Release 3: Chemical cartography of the Milky WayGaia Data Release 3:
Chemical cartography of the Milky WayGaia Data Release 3: Chemical cartography
of the Milky WayGaia Data Release 3: Chemical cartography of the Milky Way L.
Pallas-Quintela Gaia Data Release 3: Chemical cartography of the Milky WayGaia
Data Release 3: Chemical cartography of the Milky Way A. Panahi Gaia Data
Release 3: Chemical cartography of the Milky WayGaia Data Release 3: Chemical
cartography of the Milky Way S. Payne-Wardenaar Gaia Data Release 3: Chemical
cartography of the Milky WayGaia Data Release 3: Chemical cartography of the
Milky Way X. Peñalosa Esteller Gaia Data Release 3: Chemical cartography of
the Milky WayGaia Data Release 3: Chemical cartography of the Milky Way A.
Penttil ̈a Gaia Data Release 3: Chemical cartography of the Milky WayGaia Data
Release 3: Chemical cartography of the Milky Way B. Pichon Gaia Data Release
3: Chemical cartography of the Milky WayGaia Data Release 3: Chemical
cartography of the Milky Way A.M. Piersimoni Gaia Data Release 3: Chemical
cartography of the Milky WayGaia Data Release 3: Chemical cartography of the
Milky Way F.-X. Pineau Gaia Data Release 3: Chemical cartography of the Milky
WayGaia Data Release 3: Chemical cartography of the Milky Way E. Plachy Gaia
Data Release 3: Chemical cartography of the Milky WayGaia Data Release 3:
Chemical cartography of the Milky WayGaia Data Release 3: Chemical cartography
of the Milky WayGaia Data Release 3: Chemical cartography of the Milky WayGaia
Data Release 3: Chemical cartography of the Milky WayGaia Data Release 3:
Chemical cartography of the Milky Way G. Plum Gaia Data Release 3: Chemical
cartography of the Milky WayGaia Data Release 3: Chemical cartography of the
Milky Way A. Prša Gaia Data Release 3: Chemical cartography of the Milky
WayGaia Data Release 3: Chemical cartography of the Milky Way L. Pulone Gaia
Data Release 3: Chemical cartography of the Milky WayGaia Data Release 3:
Chemical cartography of the Milky Way E. Racero Gaia Data Release 3: Chemical
cartography of the Milky WayGaia Data Release 3: Chemical cartography of the
Milky WayGaia Data Release 3: Chemical cartography of the Milky WayGaia Data
Release 3: Chemical cartography of the Milky Way S. Ragaini Gaia Data Release
3: Chemical cartography of the Milky WayGaia Data Release 3: Chemical
cartography of the Milky Way M. Rainer Gaia Data Release 3: Chemical
cartography of the Milky WayGaia Data Release 3: Chemical cartography of the
Milky WayGaia Data Release 3: Chemical cartography of the Milky WayGaia Data
Release 3: Chemical cartography of the Milky Way C.M. Raiteri Gaia Data
Release 3: Chemical cartography of the Milky WayGaia Data Release 3: Chemical
cartography of the Milky Way P. Ramos Gaia Data Release 3: Chemical
cartography of the Milky WayGaia Data Release 3: Chemical cartography of the
Milky WayGaia Data Release 3: Chemical cartography of the Milky WayGaia Data
Release 3: Chemical cartography of the Milky Way M. Ramos-Lerate Gaia Data
Release 3: Chemical cartography of the Milky WayGaia Data Release 3: Chemical
cartography of the Milky Way S. Regibo Gaia Data Release 3: Chemical
cartography of the Milky WayGaia Data Release 3: Chemical cartography of the
Milky Way P.J. Richards Gaia Data Release 3: Chemical cartography of the Milky
WayGaia Data Release 3: Chemical cartography of the Milky Way C. Rios Diaz
Gaia Data Release 3: Chemical cartography of the Milky WayGaia Data Release 3:
Chemical cartography of the Milky Way V. Ripepi Gaia Data Release 3: Chemical
cartography of the Milky WayGaia Data Release 3: Chemical cartography of the
Milky Way A. Riva Gaia Data Release 3: Chemical cartography of the Milky
WayGaia Data Release 3: Chemical cartography of the Milky Way H.-W. Rix Gaia
Data Release 3: Chemical cartography of the Milky WayGaia Data Release 3:
Chemical cartography of the Milky Way G. Rixon Gaia Data Release 3: Chemical
cartography of the Milky WayGaia Data Release 3: Chemical cartography of the
Milky Way N. Robichon Gaia Data Release 3: Chemical cartography of the Milky
WayGaia Data Release 3: Chemical cartography of the Milky Way A.C. Robin Gaia
Data Release 3: Chemical cartography of the Milky WayGaia Data Release 3:
Chemical cartography of the Milky Way C. Robin Gaia Data Release 3: Chemical
cartography of the Milky WayGaia Data Release 3: Chemical cartography of the
Milky Way M. Roelens Gaia Data Release 3: Chemical cartography of the Milky
WayGaia Data Release 3: Chemical cartography of the Milky Way H.R.O. Rogues
Gaia Data Release 3: Chemical cartography of the Milky WayGaia Data Release 3:
Chemical cartography of the Milky Way L. Rohrbasser Gaia Data Release 3:
Chemical cartography of the Milky WayGaia Data Release 3: Chemical cartography
of the Milky Way M. Romero-Gómez Gaia Data Release 3: Chemical cartography of
the Milky WayGaia Data Release 3: Chemical cartography of the Milky Way N.
Rowell Gaia Data Release 3: Chemical cartography of the Milky WayGaia Data
Release 3: Chemical cartography of the Milky Way F. Royer Gaia Data Release 3:
Chemical cartography of the Milky WayGaia Data Release 3: Chemical cartography
of the Milky Way D. Ruz Mieres Gaia Data Release 3: Chemical cartography of
the Milky WayGaia Data Release 3: Chemical cartography of the Milky Way K.A.
Rybicki Gaia Data Release 3: Chemical cartography of the Milky WayGaia Data
Release 3: Chemical cartography of the Milky Way G. Sadowski Gaia Data Release
3: Chemical cartography of the Milky WayGaia Data Release 3: Chemical
cartography of the Milky Way A. Sáez Núñez Gaia Data Release 3: Chemical
cartography of the Milky WayGaia Data Release 3: Chemical cartography of the
Milky Way A. Sagristà Sellés Gaia Data Release 3: Chemical cartography of the
Milky WayGaia Data Release 3: Chemical cartography of the Milky Way J.
Sahlmann Gaia Data Release 3: Chemical cartography of the Milky WayGaia Data
Release 3: Chemical cartography of the Milky Way E. Salguero Gaia Data Release
3: Chemical cartography of the Milky WayGaia Data Release 3: Chemical
cartography of the Milky Way N. Samaras Gaia Data Release 3: Chemical
cartography of the Milky WayGaia Data Release 3: Chemical cartography of the
Milky WayGaia Data Release 3: Chemical cartography of the Milky WayGaia Data
Release 3: Chemical cartography of the Milky Way V. Sanchez Gimenez Gaia Data
Release 3: Chemical cartography of the Milky WayGaia Data Release 3: Chemical
cartography of the Milky Way N. Sanna Gaia Data Release 3: Chemical
cartography of the Milky WayGaia Data Release 3: Chemical cartography of the
Milky Way R. Santoveña Gaia Data Release 3: Chemical cartography of the Milky
WayGaia Data Release 3: Chemical cartography of the Milky Way M. Sarasso Gaia
Data Release 3: Chemical cartography of the Milky WayGaia Data Release 3:
Chemical cartography of the Milky Way E. Sciacca Gaia Data Release 3: Chemical
cartography of the Milky WayGaia Data Release 3: Chemical cartography of the
Milky Way M. Segol Gaia Data Release 3: Chemical cartography of the Milky
WayGaia Data Release 3: Chemical cartography of the Milky Way J.C. Segovia
Gaia Data Release 3: Chemical cartography of the Milky WayGaia Data Release 3:
Chemical cartography of the Milky Way D. Ségransan Gaia Data Release 3:
Chemical cartography of the Milky WayGaia Data Release 3: Chemical cartography
of the Milky Way D. Semeux Gaia Data Release 3: Chemical cartography of the
Milky WayGaia Data Release 3: Chemical cartography of the Milky Way S. Shahaf
Gaia Data Release 3: Chemical cartography of the Milky WayGaia Data Release 3:
Chemical cartography of the Milky Way H.I. Siddiqui Gaia Data Release 3:
Chemical cartography of the Milky WayGaia Data Release 3: Chemical cartography
of the Milky Way A. Siebert Gaia Data Release 3: Chemical cartography of the
Milky WayGaia Data Release 3: Chemical cartography of the Milky WayGaia Data
Release 3: Chemical cartography of the Milky WayGaia Data Release 3: Chemical
cartography of the Milky Way L. Siltala Gaia Data Release 3: Chemical
cartography of the Milky WayGaia Data Release 3: Chemical cartography of the
Milky Way A. Silvelo Gaia Data Release 3: Chemical cartography of the Milky
WayGaia Data Release 3: Chemical cartography of the Milky Way E. Slezak Gaia
Data Release 3: Chemical cartography of the Milky WayGaia Data Release 3:
Chemical cartography of the Milky Way I. Slezak Gaia Data Release 3: Chemical
cartography of the Milky WayGaia Data Release 3: Chemical cartography of the
Milky Way R.L. Smart Gaia Data Release 3: Chemical cartography of the Milky
WayGaia Data Release 3: Chemical cartography of the Milky Way O.N. Snaith Gaia
Data Release 3: Chemical cartography of the Milky WayGaia Data Release 3:
Chemical cartography of the Milky Way E. Solano Gaia Data Release 3: Chemical
cartography of the Milky WayGaia Data Release 3: Chemical cartography of the
Milky Way F. Solitro Gaia Data Release 3: Chemical cartography of the Milky
WayGaia Data Release 3: Chemical cartography of the Milky Way D. Souami Gaia
Data Release 3: Chemical cartography of the Milky WayGaia Data Release 3:
Chemical cartography of the Milky WayGaia Data Release 3: Chemical cartography
of the Milky WayGaia Data Release 3: Chemical cartography of the Milky Way J.
Souchay Gaia Data Release 3: Chemical cartography of the Milky WayGaia Data
Release 3: Chemical cartography of the Milky Way F. Spoto Gaia Data Release 3:
Chemical cartography of the Milky WayGaia Data Release 3: Chemical cartography
of the Milky Way I.A. Steele Gaia Data Release 3: Chemical cartography of the
Milky WayGaia Data Release 3: Chemical cartography of the Milky Way H.
Steidelm ̈uller Gaia Data Release 3: Chemical cartography of the Milky WayGaia
Data Release 3: Chemical cartography of the Milky Way C.A. Stephenson Gaia
Data Release 3: Chemical cartography of the Milky WayGaia Data Release 3:
Chemical cartography of the Milky WayGaia Data Release 3: Chemical cartography
of the Milky WayGaia Data Release 3: Chemical cartography of the Milky Way M.
S ̈uveges Gaia Data Release 3: Chemical cartography of the Milky WayGaia Data
Release 3: Chemical cartography of the Milky Way J. Surdej Gaia Data Release
3: Chemical cartography of the Milky WayGaia Data Release 3: Chemical
cartography of the Milky WayGaia Data Release 3: Chemical cartography of the
Milky WayGaia Data Release 3: Chemical cartography of the Milky Way L.
Szabados Gaia Data Release 3: Chemical cartography of the Milky WayGaia Data
Release 3: Chemical cartography of the Milky Way E. Szegedi-Elek Gaia Data
Release 3: Chemical cartography of the Milky WayGaia Data Release 3: Chemical
cartography of the Milky Way F. Taris Gaia Data Release 3: Chemical
cartography of the Milky WayGaia Data Release 3: Chemical cartography of the
Milky Way M.B. Taylor Gaia Data Release 3: Chemical cartography of the Milky
WayGaia Data Release 3: Chemical cartography of the Milky Way R. Teixeira Gaia
Data Release 3: Chemical cartography of the Milky WayGaia Data Release 3:
Chemical cartography of the Milky Way L. Tolomei Gaia Data Release 3: Chemical
cartography of the Milky WayGaia Data Release 3: Chemical cartography of the
Milky Way N. Tonello Gaia Data Release 3: Chemical cartography of the Milky
WayGaia Data Release 3: Chemical cartography of the Milky Way F. Torra Gaia
Data Release 3: Chemical cartography of the Milky WayGaia Data Release 3:
Chemical cartography of the Milky Way J. Torra† Gaia Data Release 3: Chemical
cartography of the Milky WayGaia Data Release 3: Chemical cartography of the
Milky Way G. Torralba Elipe Gaia Data Release 3: Chemical cartography of the
Milky WayGaia Data Release 3: Chemical cartography of the Milky Way M.
Trabucchi Gaia Data Release 3: Chemical cartography of the Milky WayGaia Data
Release 3: Chemical cartography of the Milky WayGaia Data Release 3: Chemical
cartography of the Milky WayGaia Data Release 3: Chemical cartography of the
Milky Way A.T. Tsounis Gaia Data Release 3: Chemical cartography of the Milky
WayGaia Data Release 3: Chemical cartography of the Milky Way C. Turon Gaia
Data Release 3: Chemical cartography of the Milky WayGaia Data Release 3:
Chemical cartography of the Milky Way A. Ulla Gaia Data Release 3: Chemical
cartography of the Milky WayGaia Data Release 3: Chemical cartography of the
Milky Way N. Unger Gaia Data Release 3: Chemical cartography of the Milky
WayGaia Data Release 3: Chemical cartography of the Milky Way M.V. Vaillant
Gaia Data Release 3: Chemical cartography of the Milky WayGaia Data Release 3:
Chemical cartography of the Milky Way E. van Dillen Gaia Data Release 3:
Chemical cartography of the Milky WayGaia Data Release 3: Chemical cartography
of the Milky Way W. van Reeven Gaia Data Release 3: Chemical cartography of
the Milky WayGaia Data Release 3: Chemical cartography of the Milky Way O.
Vanel Gaia Data Release 3: Chemical cartography of the Milky WayGaia Data
Release 3: Chemical cartography of the Milky Way A. Vecchiato Gaia Data
Release 3: Chemical cartography of the Milky WayGaia Data Release 3: Chemical
cartography of the Milky Way Y. Viala Gaia Data Release 3: Chemical
cartography of the Milky WayGaia Data Release 3: Chemical cartography of the
Milky Way D. Vicente Gaia Data Release 3: Chemical cartography of the Milky
WayGaia Data Release 3: Chemical cartography of the Milky Way S. Voutsinas
Gaia Data Release 3: Chemical cartography of the Milky WayGaia Data Release 3:
Chemical cartography of the Milky Way M. Weiler Gaia Data Release 3: Chemical
cartography of the Milky WayGaia Data Release 3: Chemical cartography of the
Milky Way T. Wevers Gaia Data Release 3: Chemical cartography of the Milky
WayGaia Data Release 3: Chemical cartography of the Milky WayGaia Data Release
3: Chemical cartography of the Milky WayGaia Data Release 3: Chemical
cartography of the Milky Way Ł. Wyrzykowski Gaia Data Release 3: Chemical
cartography of the Milky WayGaia Data Release 3: Chemical cartography of the
Milky Way A. Yoldas Gaia Data Release 3: Chemical cartography of the Milky
WayGaia Data Release 3: Chemical cartography of the Milky Way P. Yvard Gaia
Data Release 3: Chemical cartography of the Milky WayGaia Data Release 3:
Chemical cartography of the Milky Way H. Zhao Gaia Data Release 3: Chemical
cartography of the Milky WayGaia Data Release 3: Chemical cartography of the
Milky Way J. Zorec Gaia Data Release 3: Chemical cartography of the Milky
WayGaia Data Release 3: Chemical cartography of the Milky Way S. Zucker Gaia
Data Release 3: Chemical cartography of the Milky WayGaia Data Release 3:
Chemical cartography of the Milky Way T. Zwitter Gaia Data Release 3: Chemical
cartography of the Milky WayGaia Data Release 3: Chemical cartography of the
Milky Way

(Received February ??, 2022; accepted ?? ??, 2022)

###### Abstract

Context. The motion of stars has been used to reveal details of the complex
history of the Milky Way, in constant interaction with its environment.
Nevertheless, to reconstruct the Galactic history puzzle in its entirety, the
chemo-physical characterisation of stars is essential. Previous Gaia data
releases were supported by a smaller, heterogeneous, and spatially biased
mixture of chemical data from ground-based observations.

Aims. Gaia Data Release 3 opens a new era of all-sky spectral analysis of
stellar populations thanks to the nearly 5.6 million stars observed by the
Radial Velocity Spectrometer (RVS) and parametrised by the GSP-Spec module. In
this work, we aim to demonstrate the scientific quality of Gaia’s Milky Way
chemical cartography through a chemo-dynamical analysis of disc and halo
populations.

Methods. Stellar atmospheric parameters and chemical abundances provided by
Gaia DR3 spectroscopy are combined with DR3 radial velocities and EDR3
astrometry to analyse the relationships between chemistry and Milky Way
structure, stellar kinematics, and orbital parameters.

Results. The all-sky Gaia chemical cartography allows a powerful and precise
chemo-dynamical view of the Milky Way with unprecedented spatial coverage and
statistical robustness. First, it reveals the strong vertical symmetry of the
Galaxy and the flared structure of the disc. Second, the observed kinematic
disturbances of the disc —seen as phase space correlations— and kinematic or
orbital substructures are associated with chemical patterns that favour stars
with enhanced metallicities and lower [$\alpha$/Fe] abundance ratios compared
to the median values in the radial distributions. This is detected both for
young objects that trace the spiral arms and older populations. Several
$\alpha$, iron-peak elements and at least one heavy element trace the thin and
thick disc properties in the solar cylinder. Third, young disc stars show a
recent chemical impoverishment in several elements. Fourth, the largest chemo-
dynamical sample of open clusters analysed so far shows a steepening of the
radial metallicity gradient with age, which is also observed in the young
field population. Finally, the Gaia chemical data have the required coverage
and precision to unveil galaxy accretion debris and heated disc stars on halo
orbits through their [$\alpha$/Fe] ratio, and to allow the study of the chemo-
dynamical properties of globular clusters.

Conclusions. Gaia DR3 chemo-dynamical diagnostics open new horizons before the
era of ground-based wide-field spectroscopic surveys. They unveil a complex
Milky Way that is the outcome of an eventful evolution, shaping it to the
present day.

###### Key Words.:

Galaxy: abundances, Stars: abundances, Galaxy: evolution, Galaxy: kinematics
and dynamics, open clusters and associations, Galaxy:structure, Galaxy: disc,
Galaxy: halo

##  1 Introduction

The European Space Agency Gaia mission has transformed our understanding of
the Milky Way, thanks to its ability to trace the motion of stars in the sky
(Gaia Collaboration, Brown, A. G. A. et al., 2021). The observation of these
movements has allowed us to see the Galaxy as an evolving system. Components
that were previously thought to be distinct (the thin disc in the Galactic
plane with ongoing star formation, the more diffuse and older thick disc, the
central bulge, and the extended stellar halo) now appear to be interlinked
formation phases of a system in clear interaction with its environment. In
particular, studies of stellar orbits and kinematics have uncovered a
considerable proportion of merger debris in the halo (e.g. Helmi et al., 2018;
Belokurov et al., 2018a; Malhan et al., 2018; Myeong et al., 2019; Helmi,
2020, and references therein) and the Galactic disc (e.g. Sestito et al.,
2020; Re Fiorentin et al., 2021). Additionally, investigations of stellar
motions have revealed the Galactic disc phase mixing process, which is
subsequent to a mildly disturbed state (Antoja et al., 2018). A massive disc-
crossing perturber (e.g. Binney & Schönrich, 2018) —possibly akin to the
Sagittarius dwarf galaxy (Laporte et al., 2019b; Bland-Hawthorn et al., 2019)—
or a strong buckling of the stellar bar (e.g. Khoperskov et al., 2020) are the
most likely interpretations of this phenomenon. A recent or ongoing encounter
with a satellite galaxy seems also to be responsible for the rapidly
precessing disc warp (Poggio et al., 2020, 2021b). In summary, the picture of
a ‘living and breathing Galaxy’ has emerged thanks to Gaia data (Belokurov,
2019; Brown, 2021).

Despite the above-mentioned transformational results, stellar motions alone do
not allow a complete reconstruction of the intricate puzzle of Galactic
history. The orbit of a star evolves in response to fluctuations in the
Galaxy’s gravitational field (e.g. Sellwood & Binney, 2002). As a consequence,
the reconstruction of the history of the Milky Way based on the interpretation
of stellar motions in terms of evolutionary processes is hampered by
degenerate explanations and the complex interplay of different physical
mechanisms.

Indeed, understanding how galaxies like the Milky Way form and evolve remains
a challenge. In the cold dark matter Universe, galaxies grow through a
sequence of merger and accretion events. However, the impact of these events
on the evolution of a galaxy is extremely difficult to predict because of the
complex physics of baryons. As a consequence, studying the chemo-physical
properties of matter is essential to comprehend the Galaxy in which we live.
Fortunately, we have a powerful tool at our disposal: stellar spectroscopy.

The study of stellar spectra gave rise to the science of astrophysics in the
19th century (e.g. Huggins & Miller, 1864; Huggins & Huggins, 1899) and, since
then, the varying characteristics of spectral absorption lines have been used
by researchers to decipher the physical properties of stars (Maury &
Pickering, 1897; Cannon & Pickering, 1918). Stellar parametrisation became a
powerful decryption tool, allowing us to unveil the chemical composition of
stellar atmospheres (Payne, 1925b, a), and to provide observational evidence
of the stellar nucleosynthesis theory (Burbidge et al., 1957). Stars form
during the collapse of molecular clouds of gas and dust. Like alchemists,
stars of different masses synthesise all chemical elements except
hydrogen111More particularly, the Big Bang nucleosynthesis produced H, He and
Li, cosmic rays contribute to Li, Be and B production and stellar
nucleosynthesis concerns all chemical elements except H.; they partially
return them in the later stages of their life into the interstellar medium,
from which new stars are born. As a consequence, the stellar chemical
composition evolves from one generation to the next, and reflects the gas
conditions at the time and place of the formation of a star. Moreover,
contrary to stellar motions, the chemical abundances of a star’s atmosphere
are conserved222With the exception of some chemical species whose surface
abundance can be modified in certain stellar evolution phases. from its birth,
and can therefore be used to trace its origin. Chemical abundances break
degenerated dynamical scenarios with a variety of conserved parameters (e.g.
they play a key role in merger debris studies; e.g. Helmi, 2020). Therefore,
stellar atmospheres record the past in their chemical abundances, allowing a
look-back time that varies between a few hundred million years and the age of
the first stars in the Universe.

In this framework, previous intermediate Gaia data releases had to be
complemented with chemical data from ground-based observations. However,
ground-based spectroscopic surveys like GALAH (e.g. Buder et al., 2021),
APOGEE (Abdurro’uf et al., 2021), Gaia-ESO Survey (Gilmore et al., 2022;
Randich et al., 2022), and RAVE (Steinmetz et al., 2020), despite the recent
improvement of multiplex capabilities, are still hampered by spatially biased
samples. In addition, the inhomogeneity induced by different analysis
procedures, targeted stellar types, and spectral configurations blur the
collected chemical information. Moreover, ground-based spectroscopy suffers
from time-dependent effects such as the Earth’s atmospheric absorption and
instrumental systematic effects, which are difficult to model with
discontinuous data collections.

Fortunately, the context is now evolving favourably. Gaia Data Release 3 (DR3;
Gaia Collaboration, Vallenari et al., 2022) opens a new era of all-sky
spectroscopy and chemo-physical characterisation of Galactic stellar
populations, and includes a new transformational data set that confirms Gaia’s
leading role in the golden age of Galactic archaeology: the largest
homogeneous spectral analysis performed so far with a total of 5 594 205 stars
observed by the Radial Velocity Spectrometer (RVS; Cropper et al., 2018; Katz
et al., 2022) and parametrised by the General Stellar Parametriser -
spectroscopy (GSP-Spec; Recio-Blanco et al., 2022). With continuous data
collection for 34 months outside the Earth’s atmosphere, and a large volume
coverage reaching distances of about 8 kpc from the Sun (thanks to the
population of giant stars), the Gaia DR3 spectroscopic survey provides stellar
parameters and chemical abundances in all major Galactic populations,
sharpening our global view of the Milky Way. In addition to the sky coverage
advantage, it is worth comparing this Gaia DR3 GSP-Spec catalogue with high-
resolution ground-based surveys in other crucial characteristics for Milky Way
studies, as the number of analysed stars, the limiting magnitude, and the
explored chemical diagnostics. For magnitudes brighter than G$=$13.6333In DR3,
99% of the GSP-Spec catalogue has Gmag$<$13.6. This will strongly evolve in
future releases, reaching much fainter magnitudes thanks to the continuous and
on-going Gaia observations, there are more stars in the Gaia DR3 GSP-Spec
catalogue than in any other ground-based survey (with both GALAH and APOGEE
representing only $\sim$8% of Gaia GSP-Spec). For magnitudes fainter than
13.6, Gaia GSP-Spec has about 61 000 stars (reaching G$=$16.1 mag), GALAH has
about 130 000 stars (20% of the survey, reaching G$=$18 mag) and APOGEE about
314 000 stars (43% of the survey, reaching G$\simeq$20 mag). Concerning the
nucleosynthesis diagnostics444The following general nucleosynthetic channels
are considered: (i) cosmic rays spallation, (ii) nuclear burning in low- and
intermediate-mass stars, (iii) $\alpha$-process in core collapse supernovae
(massive stars), (iv) neutrino process in core collapse supernovae, (v)
explosions of Type Ia supernovae (C+O white dwarfs in binary systems), (vi)
slow neutron capture (s-process), and (vii) rapid neutron capture (r-process).
through individual abundance estimates, Gaia DR3 GSP-Spec explores five
different nucleosynthetic channels with 13 chemical elements, while GALAH
covers seven nucleosynthetic channels with 21 elements, and APOGEE six
channels with 24 elements.

The goal of this paper is to demonstrate the scientific quality of Gaia’s
chemical cartography through a chemo-dynamical analysis of disc and halo
populations. To this purpose, Sect. 2 presents the data that are used,
including (i) DR3 atmospheric parameters and chemical abundances (Sect. 2.1),
(ii) DR3 radial velocities (Sect. 2.2), (iii) EDR3 astrometric data and
distances (Sect. 2.3), (iv) a set of stellar velocities and orbits
specifically derived for this work (Sect. 2.4), and (v) the definition of
working subsamples (Sect. 2.5) allowing us to optimise the scientific
analysis, and illustrating the use of quality flags defined in Recio-Blanco et
al. (2022).

In Sect. 3 we present the global chemical properties of the Milky Way through
sky and Galactic maps (Sect. 3.1) and explore selection function effects
(Sect. 3.2). Section 4 presents the radial and vertical chemical gradients of
field stellar populations. In Sect. 5 we present our analysis of large-scale
chemo-kinematical correlations, while in Sect. 6 we explore the relation
between the orbital parameters and stellar chemistry. Subsequently, Sect. 7 is
dedicated to chemo-dynamical relations in solar cylinder populations using
individual element abundances, and in Section 8 we use the open clusters
population to study chemo-kinematical correlations and the temporal evolution
of disc radial chemical gradients.

Finally, Sect. 9 summarises the results of our Galactic chemo-dynamical
analysis using the Gaia RVS GSP-Spec database. In particular, we discuss the
observed chemical markers of Milky Way structure (Sect. 9.1), disc kinematic
disturbances (Sect. 9.2), and satellite accretion (Sect. 9.3). This is
completed with the examination of the detected chemo-dynamical trends of the
last billion years (Sect. 9.4) and, finally, with a discussion of the Sun’s
chemo-dynamical properties in the context of its Galactic environment (Sect.
9.5). Our overall conclusions are presented in Sect. 10.

##  2 Data

###  2.1 Stellar atmospheric parameters and chemical data

This work makes use of the stellar physical parameters and chemical abundances
derived from the Gaia RVS spectra by the GSP-Spec module and available through
the astrophysical_parameters table of Gaia DR3. It is worth mentioning that
the present work does not use the global metallicity [M/H] derived from BPRP
spectra by the General Stellar Parametrizer from Photometry (GSP-Phot) and
published in the GaiaSource and AstrophysicalParameters tables (`mh_gspphot`
field). Although GSP-Phot metallicities are suitable for different scientific
purposes, their application to large-scale Galactic chemo-dynamical studies
requires a calibration that at the time of writing this paper was not
available.

GSP-Spec estimates the main atmospheric parameters (effective temperature
$T_{\rm eff}$, stellar surface gravity log($g$)555$g$ being expressed in
cm.s-2, global metallicity [M/H]666We adopt the standard abundance notation
for a given element $X$: [X/H] $=\log{({\rm X/H})_{\star}}-\log{({\rm
X/H})_{\odot}}$, where (X/H) is the abundance by number, and
$\log\epsilon(X)\equiv\log{({\rm X/H})}+12$., and the global abundance of
$\alpha$-elements777$\alpha$-elements are O, Ne, Mg, Si, S, Ar, Ca, and Ti.
with respect to iron [$\alpha$/Fe]), together with the individual abundances
of 12 different chemical elements from RVS spectra of single stars. The RVS
wavelength range is $[845-872]$ nm, and its medium resolving power is
$R=\lambda/\Delta\lambda\sim 11\,500$ (Cropper et al., 2018). This spectral
parametrisation is based on the MatisseGauguin GSP-Spec workflow and is
described in detail in the GSP-Spec processing paper (Recio-Blanco et al.,
2022). It is worth recalling that the GSP-Spec [M/H] estimation considers all
the non-$\alpha$ metallicity indicators in the observed spectra thanks to a
four-dimensional synthetic spectra grid including not only the [M/H] dimension
but also the [$\alpha$/Fe] one. Non-$\alpha$ indicators are dominated by Fe
lines in the RVS domain. As a consequence, the estimated [M/H] value follows
the [Fe/H] abundance with a tight correlation.

In the following sections, $T_{\rm eff}$ is taken from the `teff_gspspec`
field; log($g$) comes from the `logg_gspspec` field; [M/H] is taken from
`mh_gspspec`; and [$\alpha$/Fe] corresponds to `alphafe_gspspec` with a
calibration888It is important to note that Gaia DR3 catalogue values are not
calibrated. imposed that requires a zero average value for [$\alpha$/Fe] in
the solar neighbourhood for any gravity (see Recio-Blanco et al., 2022, Table
16).

In a similar way, all the stellar individual chemical abundances come from the
GSP-Spec estimates. In particular, this paper makes use of [N/Fe]
(`nfe_gspspec`), [Mg/Fe] (`mgfe_gspspec`), [Si/Fe] (`sife_gspspec`), [S/Fe]
(`sfe_gspspec`), [Ca/Fe] (`cafe_gspspec`), [Ti/Fe] (`tife_gspspec`), [Cr/Fe]
(`crfe_gspspec`), [Fe/M] (`fem_gspspec`), [Ni/Fe] (`nife_gspspec`), and
[Ce/Fe] (`cefe_gspspec`). As for the [$\alpha$/Fe] estimates, these individual
abundances were calibrated following the prescriptions indicated in Table 16
of Recio-Blanco et al. (2022). It is important to note here that GSP-spec
assumes the reference solar abundances of Grevesse et al. (2007).

In addition, we make use of the GSP-Spec quality flags reported in the
`flags_gspspec` string chain (which consists of 41 characters) defined in
Recio-Blanco et al. (2022). For example, we make use of the first three
characters in this chain (that is, `flags_gspspec[0]`, `flags_gspspec[1]`, and
`flags_gspspec[2]`, reporting on the degree of parameter biases from line
broadening) and called `vbroadT`, `vbroadG,` and `vbroadM,` respectively (see
naming convention in Recio-Blanco et al., 2022).

Finally, the uncertainty on any derived parameter (`Param_unc`) or abundance
(`[X/Fe]_unc`) is defined as half of the difference between its upper and
lower confidence levels (e.g. `Teff_unc` $=$ [`teff_gspspec_upper` $-$
`teff_gspspec_lower`]/2).

###  2.2 Radial velocities

The complete GSP-Spec sample contains 5 594 205 stars in total (based on the
query `flags_gspspec` is not null). DR3 provides radial velocities
(`radial_velocity`, $V_{\rm Rad}$) for 33 834 834 stars (Katz et al., 2022)
through the gaia_source table. The GSP-Spec sample is a subset of the $V_{\rm
Rad}$ sample because the GSP-Spec sample was selected based on the signal-to-
noise ratio (S/N) of the mean RVS spectra. An unpublished GSP-Spec S/N $>20$
was used (Recio-Blanco et al., 2022). This was found to be very similar to
`rv_expected_sig_to_noise`999rv_expected_sig_to_noise propagates median noise
properties, whereas rv_spec_sig_to_noise calculates the noise from the scatter
on the signal in each wavelength bin and provides the median of these. in the
gaia_source table. $V_{\rm Rad}$ is used to Doppler shift RVS CCD spectra to
rest before combining them into a mean RVS spectrum (Seabroke et al., 2022).
The sensitivity of GSP-Spec parametrisation to spectra that are not perfectly
corrected for their radial velocity shift is flagged in the GSP-Spec
`flags_gspspec` string. In particular, characters 3 to 5 (`flags_gspspec[3]`,
`flags_gspspec[4]` and `flags_gspspec[5]`), called `vradT`, `vradG,` and
`vradM` respectively, report on the degree of parameter biases from $V_{\rm
Rad}$ uncertainties (see Recio-Blanco et al., 2022, for more details on these
flags).

Figure 1: Milky Way stars in the GSP-Spec database (General sample). This
HEALPix map in Galactic coordinates has a resolution of 0.46∘. The colour code
corresponds to the median of the stellar distance from the Sun. This colour
code enhances thin and thick disc populations in the Galactic plane, far from
the solar neighbourhood. The Galactic bulge stars are also visible in the
central region. Finally, the higher distance of the Magellanic Clouds and of
several globular clusters reveal their presence in the regions far from the
Galactic plane otherwise dominated by foreground stars of the solar
neighbourhood.  Figure 2: Same as Fig.1 but colour coded with the median of
the stellar metallicity [M/H] in each pixel. In the Galactic plane, the higher
metallicity values of the thin disc are visible. In the central Galactic
regions, a more metal-poor mix of bulge and thick disc populations is present.
Far from the disc plane, high-metallicity thin disc stars at low distances
from the Sun and more distant metal-poor halo stars are present. Figure 3:
Same as Fig.2 but colour-coded with the median of [$\alpha$/Fe] in each pixel.
The large structures close to the ecliptic poles are artifacts caused by the
Gaia scanning law (see text). Thin disc stars are visible in the plane thanks
to their low [$\alpha$/Fe] values.

Figure 4: Same as Fig. 2 but for different distance intervals shown from the
closest (top panel of left column) to the most distant (bottom panel of right
column). The distance ranges adopted in each panel are indicated in their
lower right corner together with the number of stars in their bottom left
corner. The colour code corresponds to the median of the metallicity and is
continuous between the first four subpanels showing rather metal-rich stars,
and the two last panels dominated by metal-poor populations.

Figure 5: Galactic maps for the General sample stars colour coded according to
stellar count, the median of [M/H], and the median of [$\alpha$/Fe] (from left
to right, respectively). The top row shows the maps in Cartesian coordinates
(X,Y), with the background image being the Milky Way sketch from Churchwell et
al. (2009). In the bottom row, $R$ and $Z$ are the distances from the Galactic
centre and plane, respectively.

###  2.3 Astrometric data and distances

High-precision astrometric parameters
$(\alpha,\delta,\mu_{\alpha*},\mu_{\delta},\varpi)$ from Gaia EDR3 (Gaia
Collaboration, Brown, A. G. A. et al., 2021) complement the above-described
radial velocities, allowing three-dimensional study of stellar velocity.
Thanks to the bright magnitude limit of the spectroscopic sample, the median
parallax uncertainty is better than 20 $\mu$as for most of our targets and the
median uncertainty increases up to a maximum of $\sim 40$ $\mu$as for the
faintest stars with magnitude $G\simeq 14$.

Based on these Gaia EDR3 astrometric data, Bailer-Jones et al. (2021)
geometric distances, $r_{\rm Geo}$, are adopted in this study. To test the
implications on our analysis of the Galaxy prior (a 3D model of the stellar
distribution and extinction) adopted by Bailer-Jones et al. (2021), we defined
an astrometric control sample (ACS, Appendix A). This sample is composed of
stellar distances, $r_{\varpi}$, exclusively based on the observed Gaia
trigonometric parallaxes after removing the individual parallax zero points,
$\Delta_{\varpi}$, following Lindegren et al. (2021). In addition, the ACS
selection fulfills the following criteria: (i) a parallax uncertainty of less
than 20% derived from (ii) five-parameter astrometric solutions with
renormalised unit weight error (RUWE) $<1.4$, (iii) sources not flagged as
duplicated by the Gaia cross-matching algorithm (Torra et al., 2021), and (iv)
with full photometry ($G$, $G_{\rm BP}$, $G_{\rm RP}$) and radial velocity
available. To compare the two distance estimates, we consider the fractional
residual $(r_{\rm Geo}-r_{\varpi})/r_{\varpi}$ for objects in common. The
median value of the residuals is $-0.04$% and its median absolute deviation is
0.2%, showing very good overall agreement between both estimates. As shown in
Appendix A, the main discrepancy occurs in the Galactic plane, where Bayesian
distances are greater than the pure trigonometric parallax-based distances by
$\lesssim$ 4%. These very small discrepancies have a negligible impact on the
results of this work and, as a consequence, $r_{\rm Geo}$ distances are
adopted in the following.

###  2.4 Galactocentric positions, velocities, and orbits

For the computation of the stellar positions (Galactocentric Cartesian $X$,
$Y$, and $Z$ positions, and cylindrical radius $R$) and the Galactocentric
cylindrical velocities ($V_{R}$, $V_{\phi}$, and $V_{Z}$ in a right-handed
frame with positive $V_{\phi}$ for most of the disc stars), we adopted the
Sun’s Galactocentric position $(R,Z)_{\odot}=(8.249,0.0208)$ kpc (Gravity
Collaboration et al., 2021; Bennett & Bovy, 2019) and Galactocentric
cylindrical velocities $(V_{R},V_{\phi},V_{Z})_{\odot}=(-9.5,250.7,8.56)$ km
s-1 (Reid & Brunthaler, 2020; Gravity Collaboration et al., 2021), as well as
Gaia’s $\alpha$, $\delta$, line-of-sight velocity, and Bailer-Jones et al.
(2021) geometric distances for each target. The orbital parameters (actions
$J_{R},J_{\phi},J_{Z}$, apocenter and pericenter distance $R_{a}$, $R_{p}$,
maximum distance from the plane reached during the star’s orbit $Z_{\rm max}$)
are computed using the Stäckel fudge method Binney (2012) implemented in the
Galpy code (Bovy, 2015), combined with a rescaled version of the McMillan
(2017) axisymmetric Galactic potential. In this model, the Galactocentric
distance of the Sun is $R_{\odot}=8.249$ kpc while the circular velocity of
the Local Standard of Rest is set to 238.5 km s-1 (Gravity Collaboration et
al., 2021; Schönrich et al., 2010). The lower and upper confidence limits for
each of these parameters are obtained by drawing Monte Carlo realisations of
$\mu_{\alpha*},\mu_{\delta}$, $V_{\rm Rad}$, and distance, and propagating
them through the positions, velocities, and orbits. We assumed Gaussian
symmetric distributions for the proper motions and line-of-sight velocities,
and a broken Gaussian distribution for distance (based on the lower and upper
confidence limits of Bailer-Jones et al. 2021).

###  2.5 Working samples

To optimise the analysis of this work, different data selections and quality
cuts are required. To this purpose, we defined several data samples with the
following characteristics. The precise conditions used for these sample
selections are presented in Appendix B, including the corresponding catalogue
queries.

General sample (5 527 090 stars; Sects. 3 and 6): From the complete GSP-Spec
sample (containing 5 594 205 stars in total), we excluded about 56 000 stars
located near the cool end of the GSP-Spec parameter space and suffering from
biases in different parameters (Recio-Blanco et al., 2022). The remaining
objects without $r_{\rm Geo}$ distances were removed. For this sample, the
median uncertainty in [M/H] is 0.075 dex and the median uncertainty in
[$\alpha$/Fe] is 0.05 dex.

Medium quality sample (4 140 759 stars; Sect. 3, Sect. 5, Sect. 6): This
results from additional quality criteria rejecting stars with grid border
effects and large parameter uncertainties. For this sample, the median
uncertainty in [M/H] is 0.06 dex and the median uncertainty in [$\alpha$/Fe]
is 0.04 dex.

Gradient analysis sample (2 762 809 stars, Sect. 4): This optimises the
quality of the [M/H] and [$\alpha$/Fe] parameters and the astrometric quality
to ensure reliable distance estimates, with the goal of estimating radial and
vertical gradients. For this sample, the median uncertainty in [M/H] is 0.05
dex and the median uncertainty in [$\alpha$/Fe] is 0.035 dex.

High-quality sample (2 218 573 stars, Sect. 5): This selects the most precise
stellar parameters and chemical abundances. We note, in particular, that the
choice of the $fluxNoise=0$ filter flag imposes a selection of stars with very
low parameter uncertainties. For this sample, the median uncertainty in [M/H]
is 0.03 dex and the median uncertainty in [$\alpha$/Fe] is 0.015 dex.

Individual abundances samples (Sect. 3 and 7): these have been defined to
optimise the individual abundance distributions of different chemical
elements. The number of selected stars depends on the chemical element.
Specifically, as expected, the precision of abundance measurements is a
function of different conditions, such as the number of analysed lines, their
equivalent widths, and possible blends, which vary with effective temperature,
surface gravity, mean metallicity, and other individual abundances, and is
different from one element to another.

##  3 Global chemical properties of the Milky Way

Figure 6: Kiel diagrams across the Milky Way for the Medium Quality sample,
colour coded according to the median of the mean metallicity. The number of
stars in each subpanel is indicated in its upper left corner. The global ($R$,
$Z$) distribution of Fig. 5 (bottom row) is shown in the background with grey
levels. Moving away from the Sun, the sample becomes dominated by
intrinsically bright giants. Figure 7: Same as Fig. 6 but for [$\alpha$/Fe]
versus [M/H] (star counts).

The $\sim$5.5 million star database of spectroscopic stellar parameters and
chemical abundances (see Sect 2.1), as part of the Gaia all-sky data
collection, provides significant radial and vertical coverage of our Galaxy,
but also probes a considerable range in azimuth. In this section, we first
analyse the global spatial distribution of the stars in the Milky Way and
their chemical properties, and then we illustrate the selection function in
radial and vertical bins. Here, we show the chemical properties and spatial
coverage of three representative stellar populations selected from the Kiel
diagram of the near-plane objects: massive young stars, bright red giant
branch (RGB) objects and hot turn-off (TO) stars.

###  3.1 Spatial and chemical trends

Sky maps in Galactic coordinates

The distribution of all the stars in the General sample is presented in
Galactic coordinate maps colour coded according to distance (Fig. 1),
metallicity (Fig. 2), and [$\alpha$/Fe] abundance (Fig. 3).

We first note that the ecliptic pole scanning law (EPSL; Boubert & Everall,
2020) pattern is visible in Fig. 3 with slightly higher [$\alpha$/Fe] values.
Between 25 July and 21 August 2014 (the first weeks of Gaia’s nominal
mission), Gaia operated in EPSL mode (Gaia Collaboration, Prusti, T. et al.,
2016). During this period, stars close to the ecliptic poles and along great
circles connecting them were observed a greater number of times than during
Gaia’s nominal scanning law. This leads to spectra with higher S\N towards the
EPSL footprint. As Gaia continues to observe in nominal scanning law, the S/N
will homogenise over the sky for future data releases.The higher S/N of the
spectra along the EPSL pattern allows the parameterisation of fainter (and
hence more distant) stars in these regions, leading to a slightly lower mean
metallicity and especially larger mean [$\alpha$/Fe] values per pixel.

The metal-rich and relatively $\alpha$-low thin disc is easily identified in
Figs. 1, 2, and 3. In the direction of the Galactic bulge, outside the
Galactic plane, one sees a dominant metal-poor population. Indeed, due to the
fact that the bulge is more radially concentrated, many thick disc stars are
present in these regions, decreasing the median metallicity. The regions
located far from the plane are filled with a mixture of nearby metal-rich
$\alpha$-low disc stars and more distant metal-poor $\alpha$-rich halo stars
(see also Sect. 4).

To complement this first global view, we cut Fig. 2 into different distance
intervals from the Sun (see Fig. 4). Similar figures for the [$\alpha$/Fe]
distribution are provided in the Appendix (Fig. 39). The scanning law features
described above are visible in the closest distance bin (D$<$0.5 kpc, upper
left panel). Figures 4 and 39 in the Appendix show that, whereas the sky is
filled by metal-rich and $\alpha$-low thin disc stars within 500 pc of the
Sun, the Galactic discs start to progressively emerge with increasing
distance. The more metal-poor and $\alpha$-rich halo dominates beyond $\sim$4
kpc. In the more distant panel, beyond 6 kpc, the thick disc is well seen on
both sides of the Galactic centre and the thin disc has almost disappeared
because of interstellar extinction. An asymmetry can also be seen in the
metallicity map close to the Galactic centre (with the central region being
more metal-rich at positive longitudes than at negative ones), which may
result from the presence of the central bar and an inhomogeneous distance
distribution around the Galactic centre in this more distant bin due to
extinction. Finally, the Small and Large Magellanic Clouds (SMC and LMC,
respectively) are also clearly visible in this panel, both being rather
$\alpha$ poor. We note that the LMC appears rather metal rich. Our LMC sample
is indeed dominated by bright massive and young stars (referred to as blue
loop stars by Gaia Collaboration, Luri, X. et al., 2021), which likely sample
the metal-rich LMC populations.

Galactic maps in Cartesian coordinates

Figure 5 (top panels) shows three maps in (X-Y) Cartesian coordinates of all
the General sample stars superimposed on the Milky Way sketch of Hurt &
Benjamin (Churchwell et al., 2009). From left to right, the maps are colour
coded according to stellar counts, mean metallicity, and enrichment in
$\alpha$-elements with respect to iron. We note that, in the panels colour
coded according to [M/H] and [$\alpha$/Fe], the apparent bulge asymmetry
described in Figs. 4 and 39 is again seen between the Sun and the Bar.

The bottom row of Fig. 5 shows the distribution of the same stars in the ($R$,
$Z$) plane, where $R$ is the Galactic centre distance and $Z$ the distance
from the Galactic plane. It can be seen that the spatial coverage of this
sample with measured [M/H] and [$\alpha$/Fe] is very large, spanning several
kiloparsec. Close to the Galactic plane and towards the inner regions, a thin
stripe of metal-rich low-$\alpha$ stars is clearly seen. Its vertical
extension is about 300 pc below and above the plane, which is the typical
scale height of the thin disc. This stripe is therefore the thin disc seen
edge-on. It is not detected for $R\la$ 3.5 kpc because of interstellar
extinction and the resultant lack of sufficiently bright stars for analysis by
GSP-Spec at smaller Galactic radii. Towards the external regions near the
plane, this thin disc is also seen up to $\sim$14 kpc from the Galactic
centre. Its flare in the outer regions is traced by the progressive increase
of high-metallicity low-[$\alpha$/Fe] stars farther away from the plane, as we
move towards higher $R$ values (see Sect. 5 for a chemo-kinematical
perspective of the disc flare). Moreover, the stars located close to the
Galactic plane but in the external parts of the disc appear more metal poor
and slightly more $\alpha$ rich: a clear gradient in [M/H] and [$\alpha$/Fe]
versus $R$ is thus revealed (see also Sect.4). As a consequence, at large
heights from the Galactic plane, internal regions are dominated by low-
metallicity thick disc and halo stars, while for R$>$12 kpc, flared disc stars
of higher metallicity and lower [$\alpha$/Fe] values dominate.

Figure 8: Kiel diagram of all the Medium Quality stars located within 1 kpc of
the Galactic plane. The location of the HotTO, RGB, and Massive subsamples is
illustrated. Their spatial distribution and chemical properties are detailed
in Figs. 9, 10, and 11, respectively.

Figure 9: HotTO stars of the Medium Quality sample located within 1 kpc of the
Galactic plane. Their XY spatial distribution is shown within $\pm$4 kpc of
the Sun, colour coded according to stellar count and the median of the mean
metallicity (left and central panels, respectively). The solar position is
indicated by a filled star coloured according to solar metallicity ([M/H]=0.0
dex). The right panel shows the evolution of calcium (top) and sulfur (bottom)
abundances with respect to iron abundances versus the mean metallicity.

Figure 10: Same as Fig. 9 but for RGB stars within 1 kpc of the Galactic plane

and over a more extended XY domain ($\pm$6 kpc from the Sun). Nickel
abundances are shown in the bottom-right panel.

Figure 11: Same as Fig. 9 but for Massive stars located within 400 pc of the
Galactic plane, thus focusing attention on the thin disc. The spiral arm
structure is visible in the left and central panels. Calcium and nitrogen
abundance distributions are shown in the right top and bottom panels,
respectively. For comparison, the distribution of the RGB stars in terms of
calcium abundance is shown in grey in the top panel

.

Figure 12: Cerium abundances for the coolest Massive and RGB stars of the
Medium Quality sample located close to the Galactic plane and colour coded
according to stellar density and the median of [Ca/Fe] (top and bottom panel,
respectively).

###  3.2 Exploration of the selection function

The large spatial coverage of the Gaia chemical database requires a global
presentation of the underlying parameter distribution across the Galaxy. In
addition, the large variety of stellar types included in the catalogue demands
that we understand the underlying spatial distribution across the Kiel
diagram. Without entering into a detailed characterisation of the selection
function, in this section we explore its impact so as to help DR3 users and to
support the chemo-dynamical analysis of this paper.

####  3.2.1 Stellar parameter distribution across the Galaxy

To dissect the covered spatial volume, we divided the ($R$, $Z$) plane into
bins of 2x2 kpc2. The resulting [$R$, $Z$] grid of Kiel diagrams colour coded
according to [M/H] is shown in Fig. 6, and that of [$\alpha$/Fe] versus [M/H]
distributions is presented in Fig. 7. In both figures, the global ($R$, $Z$)
density contour plot is shown in the background. For the purpose of clarity,
only the stars in the Medium Quality sample (4 140 759 objects) are included.
As anticipated from the previous section, about 90% of this sample is found
between 6 and 10 kpc in $R$ and $|Z|<2$ kpc.

The majority of the stars are metal-rich and alpha-poor dwarfs on the main
sequence and belonging to the thin disc. Close to the Sun, all evolutionary
stellar stages from main sequence stars up to the tip of the asymptotic giant
branch (AGB) are encountered with a large mixture of [M/H] and [$\alpha$/Fe]
combinations. Moving away from the solar location in both directions, the
selection function progressively favours intrinsically brighter stars with
lower log($g$) values. The radial and vertical metallicity gradients can also
be qualitatively appreciated (see Sect. 4 for quantification of the
gradients). For $|Z|>4$ kpc, only metal-poor RGB and AGB stars are observed
and most of them have metallicities of between $\sim$-2.5 and $\sim$-0.5 dex
with high $\alpha$-enrichment. Nevertheless, a few more metal-rich stars from
the flared disc are visible in the outer regions. We also note a high symmetry
with respect to the Galactic plane for the Kiel and [$\alpha$/Fe] versus [M/H]
diagrams. As illustrated in Fig. 7, the global standard decreasing trend of
[$\alpha$/Fe] with metallicity can be seen across the Galaxy.

####  3.2.2 Kiel diagram selections near the Galactic plane

To further illustrate the selection function close to the Galactic plane,
where stellar type variations are more important, we first show in Fig. 8 the
Kiel diagram of the Medium Quality stars with $|Z|<1$ kpc. We then define
three subsamples by selecting: (i) the hottest dwarfs of the main sequence
around the turn-off, (ii) the bright part of the RGB above the clump, and
(iii) the massive bright stars hotter than the RGB, including blue loop stars
and variables such as Cepheids. This last selection, which is biased towards
young stars, is indeed dominated by stars located very close to the Galactic
plane and an additional filter keeping stars at $|Z|<$ 400 pc is applied to
avoid contaminants (mainly from the RGB population that is nearby in the Kiel
diagram). Hereafter, these subsamples are respectively labelled hot turn-off
(HotTO), RGB, and Massive as indicated in Fig. 8.

The (X,Y) spatial distribution and chemical properties of the three
populations are shown in the left and central panels of Figures 9, 10, and 11,
respectively. The metallicity colour scale is the same in the three figures
for comparison purposes. In addition, the right top panels in the three
figures show the evolution of the calcium abundance ratio with respect to
iron, [Ca/Fe], as a function of metallicity for the three populations selected
in the Kiel diagram of Fig. 8. The abundance of this chemical element is the
easiest to derive from RVS spectra thanks to the presence of the strong
absorption Ca ii IR triplet lines. Finally, the abundance trends of additional
elements are shown in the right bottom panels as a function of stellar type
and therefore the presence or absence of the lines of an element in the
related spectra. Sulfur lines are only detected for hot dwarfs (because of its
rather high excitation energy) and its abundance is illustrated in Fig. 9. The
only nickel line selected in the RVS range provides reliable estimates for
bright cool giants and its corresponding abundance is shown in Fig. 10.
Finally, nitrogen abundances are nicely illustrated using the hot massive
population in Fig. 11.

To optimise the individual chemical abundance plots, the Individual abundance
sample defined in Sect. 2.5 is used. We note that, even after applying rather
strict selection criteria (c.f. Sect. 2.5), the number of reported abundances
is huge (from $\sim 10^{4}$ to a couple of $\sim 10^{6}$, depending on the
chemical species) and generally much larger than any other published abundance
catalogue. As shown below, the behaviour of these chemical species is in
perfect agreement with previously published catalogues of stellar abundances
and with Galactic chemical evolution models (see e.g. Prantzos et al., 2018;
Kobayashi et al., 2020; Matteucci, 2021, and references therein for
observational datasets), confirming their high quality. Finally, we note here
that the individual abundance calibrations proposed by Recio-Blanco et al.
(2022) have been applied.

Spatial distributions in the disc plane

First, the left panels of Figs. 9-11 reveal that almost 680 000 HotTO stars
are found within about 1 kpc of the Sun, because they are not bright enough to
sample more distant regions. In contrast, the RGB sample contains somewhat
fewer stars (about 580 000) but allows us to explore much more extended
regions up to 5-6 kpc from the Sun. Similarly, Massive stars are distributed
up to about 3 kpc from the Sun. Their spatial distribution is not homogeneous
and nicely reveals the closest spiral arms, that is, the Sagittarius/Carina,
Local, and Persus arms, in agreement with the spatial maps derived by Poggio
et al. (2021a) from Gaia EDR3 astrometry and photometry. These massive stars
also show the enhanced equivalent width of the diffuse interstellar band at
862 nm, confirming their nature as tracers of the spiral arms (Gaia
Collaboration, Schultheis et al. 2022).

Metallicity distributions in the Galactic plane

The metallicity distributions in the (X,Y) plane of the three samples are
shown in the central panels of Figs. 9-11. Most strikingly, we see that a
large fraction of the HotTO stars are metal rich (up to [M/H]$\sim$+0.5 dex).
Indeed, the selection of the HotTO sample favours the younger and therefore
more chemically enriched TO stars because of the temperature cut at $T_{\rm
eff}$$>$6000 K. Finally, the slightly more metal-poor yellowish feature
centred on the solar position comes from an inhomogeneous $Z$ distribution of
these stars. In fact, near the Sun, the sample reaches slightly greater
distances from the plane, with median values of around 0.2 kpc, while outside
the solar vicinity, and probably driven by the younger objects in the sample,
most of the HotTO stars are slightly hotter (in order to be brighter) and
therefore closer to the plane at $|Z|\la$0.1 kpc. Therefore, the vertical
metallicity gradient (see also Sect.4) seems to explain the central
metallicity feature. Nevertheless, the solar metallicity (represented by the
colour of the central starred marker) is in agreement with the global [M/H]
distribution of HotTO stars, as expected.

Regarding the RGB sample (cf. Fig 10), stars are on average more metal-poor
than the HotTO ones, with values around [M/H]$<-0.4$ dex in most parts of the
(X,Y) plane. However, there is a metallicity gradient that is visible for
$X\gtrsim$5 kpc, with [M/H] values decreasing with distance from the Galactic