TY - JOUR A1 - Anders, Friedrich ED - Ambühl, Annemarie ED - Carlà-Uhink, Filippo ED - Rollinger, Christian ED - Walde, Christine T1 - Rezension von Erich Claßen u. a. (Hrsgg.): Roms fließende Grenzen. Archäologische Landesausstellung Nordrhein- Westfalen 2021/2022 BT - wbg Theiss (Darmstadt 2021) (= Schriften zur Bodendenkmalpf lege in Nordrhein-Westfalen Band 12), 584 S., 410 farb. Abb. ISBN: 978-3-8062-4428-1, 40,00 € JF - thersites 16 Y1 - 2023 U6 - https://doi.org/10.34679/thersites.vol16.212 SN - 2364-7612 VL - 2023 IS - 16 SP - 145 EP - 153 ER - TY - JOUR A1 - Sanchez Sanz, Arturo A1 - Laudenbach, Benoît A1 - Weiß, Adrian A1 - Werner, Eva A1 - Stachon, Markus A1 - Anders, Friedrich A1 - Barthel, Christian A1 - Berrens, Dominik A1 - Avalli, Andrea A1 - Vandewalle, Alexander A1 - Ferrara, Pasquale A1 - Pohl, Patrik ED - Ambühl, Annemarie ED - Carlà-Uhink, Filippo ED - Rollinger, Christian ED - Walde, Christine T1 - Spring Issue T2 - thersites Y1 - 2023 U6 - https://doi.org/10.34679/thersites.vol16 SN - 2364-7612 VL - 2023 IS - 16 ER - TY - THES A1 - Anders, Friedrich T1 - Disentangling the chemodynamical history of the Milky Way disc with asteroseismology and spectroscopy T1 - Die chemodynamische Entwicklung der Milchstraßenscheibe im Lichte asteroseismischer und spektroskopischer Himmelsdurchmusterungen N2 - Galaxies are among the most complex systems that can currently be modelled with a computer. A realistic simulation must take into account cosmology and gravitation as well as effects of plasma, nuclear, and particle physics that occur on very different time, length, and energy scales. The Milky Way is the ideal test bench for such simulations, because we can observe millions of its individual stars whose kinematics and chemical composition are records of the evolution of our Galaxy. Thanks to the advent of multi-object spectroscopic surveys, we can systematically study stellar populations in a much larger volume of the Milky Way. While the wealth of new data will certainly revolutionise our picture of the formation and evolution of our Galaxy and galaxies in general, the big-data era of Galactic astronomy also confronts us with new observational, theoretical, and computational challenges. This thesis aims at finding new observational constraints to test Milky-Way models, primarily based on infra-red spectroscopy from the Apache Point Observatory Galactic Evolution Experiment (APOGEE) and asteroseismic data from the CoRoT mission. We compare our findings with chemical-evolution models and more sophisticated chemodynamical simulations. In particular we use the new powerful technique of combining asteroseismic and spectroscopic observations that allows us to test the time dimension of such models for the first time. With CoRoT and APOGEE (CoRoGEE) we can infer much more precise ages for distant field red-giant stars, opening up a new window for Galactic archaeology. Another important aspect of this work is the forward-simulation approach that we pursued when interpreting these complex datasets and comparing them to chemodynamical models. The first part of the thesis contains the first chemodynamical study conducted with the APOGEE survey. Our sample comprises more than 20,000 red-giant stars located within 6 kpc from the Sun, and thus greatly enlarges the Galactic volume covered with high-resolution spectroscopic observations. Because APOGEE is much less affected by interstellar dust extinction, the sample covers the disc regions very close to the Galactic plane that are typically avoided by optical surveys. This allows us to investigate the chemo-kinematic properties of the Milky Way's thin disc outside the solar vicinity. We measure, for the first time with high-resolution data, the radial metallicity gradient of the disc as a function of distance from the Galactic plane, demonstrating that the gradient flattens and even changes its sign for mid-plane distances greater than 1 kpc. Furthermore, we detect a gap between the high- and low-[$\alpha$/Fe] sequences in the chemical-abundance diagram (associated with the thin and thick disc) that unlike in previous surveys can hardly be explained by selection effects. Using 6D kinematic information, we also present chemical-abundance diagrams cleaned from stars on kinematically hot orbits. The data allow us to confirm without doubt that the scale length of the (chemically-defined) thick disc is significantly shorter than that of the thin disc. In the second part, we present our results of the first combination of asteroseismic and spectroscopic data in the context of Galactic Archaeology. We analyse APOGEE follow-up observations of 606 solar-like oscillating red giants in two CoRoT fields close to the Galactic plane. These stars cover a large radial range of the Galactic disc (4.5 kpc $\lesssim R_{\rm Gal}\lesssim15$ kpc) and a large age baseline (0.5 Gyr $\lesssim \tau\lesssim$ 13 Gyr), allowing us to study the age- and radius-dependence of the [$\alpha$/Fe] vs. [Fe/H] distributions. We find that the age distribution of the high-[$\alpha$/Fe] sequence appears to be broader than expected from a monolithically-formed old thick disc that stopped to form stars 10 Gyr ago. In particular, we discover a significant population of apparently young, [$\alpha$/Fe]-rich stars in the CoRoGEE data whose existence cannot be explained by standard chemical-evolution models. These peculiar stars are much more abundant in the inner CoRoT field LRc01 than in the outer-disc field LRc01, suggesting that at least part of this population has a chemical-evolution rather than a stellar-evolution origin, possibly due to a peculiar chemical-enrichment history of the inner disc. We also find that strong radial migration is needed to explain the abundance of super-metal-rich stars in the outer disc. Finally, we use the CoRoGEE sample to study the time evolution of the radial metallicity gradient in the thin disc, an observable that has been the subject of observational and theoretical debate for more than 20 years. By dividing the CoRoGEE dataset into six age bins, performing a careful statistical analysis of the radial [Fe/H], [O/H], and [Mg/Fe] distributions, and accounting for the biases introduced by the observation strategy, we obtain reliable gradient measurements. The slope of the radial [Fe/H] gradient of the young red-giant population ($-0.058\pm0.008$ [stat.] $\pm0.003$ [syst.] dex/kpc) is consistent with recent Cepheid data. For the age range of $1-4$ Gyr, the gradient steepens slightly ($-0.066\pm0.007\pm0.002$ dex/kpc), before flattening again to reach a value of $\sim-0.03$ dex/kpc for stars with ages between 6 and 10 Gyr. This age dependence of the [Fe/H] gradient can be explained by a nearly constant negative [Fe/H] gradient of $\sim-0.07$ dex/kpc in the interstellar medium over the past 10 Gyr, together with stellar heating and migration. Radial migration also offers a new explanation for the puzzling observation that intermediate-age open clusters in the solar vicinity (unlike field stars) tend to have higher metallicities than their younger counterparts. We suggest that non-migrating clusters are more likely to be kinematically disrupted, which creates a bias towards high-metallicity migrators from the inner disc and may even steepen the intermediate-age cluster abundance gradient. N2 - Galaxien gehören zu den komplexesten physikalischen Systemen, die derzeit mit Computern modelliert werden können. Eine realistische Galaxiensimulation muss kosmologische Effekte genauso berücksichtigen wie die Gesetze der Plasma-, Kern-, und Teilchenphysik. Die Milchstraße ist ein ideales Labor für die Überprüfung solcher Simulationen, da moderne Teleskope die Kinematik und chemische Zusammensetzung von Millionen von Milchstraßensternen einzeln analysieren können und uns so einen Einblick in die Entstehungsgeschichte unserer Galaxie geben. Dank groß angelegter spektroskopischer Himmelsdurchmusterungen lassen sich seit Neuestem auch stellare Populationen in fernen Regionen der Milchstraße systematisch studieren. Dieser Datenreichtum hat das Potential, unseren Blick auf die Entstehung unserer kosmischen Heimat zu revolutionieren, konfrontiert die Forschung aber auch mit neuen beobachtungstechnischen, theoretischen und numerischen Herausforderungen. Das Ziel dieser Arbeit ist es, moderne numerische Modelle der Milchstraße mittels neuer Beobachtungen zu testen. Hierbei benutzen wir vor Allem Infrarotspektroskopiedaten des Apache Point Observatory Galactic Evolution Experiment (APOGEE), sowie asteroseismische Daten der europäischen Exoplanetenmission CoRoT. Wir vergleichen unsere Resultate mit semianalytischen chemischen Entwicklungsmodellen und komplexeren chemodynamischen Simulationen, wobei uns die Kombination von asteroseismischen und spektroskopischen Daten erlaubt, zum ersten Mal die Zeitdimension solcher Modelle zu testen. Mit den CoRoT-APOGEE-Beobachtungen (kurz: CoRoGEE) lassen sich viel präzisere Altersbestimmungen für entfernte Riesensterne berechnen. Ein weiterer wichtiger Bestandteil dieser Arbeit ist die Verwendung sogenannter Mock-Beobachtungen, bei denen ein chemodynamisches Milchstraßenmodell so ``beobachtet'' wird wie die Milchstraße selbst, unter möglichst realistischer Berücksichtigung aller Beobachtungseffekte. Dies erlaubt uns akkuratere Vergleiche von Modellen und Daten, und ermöglicht eine einfachere Interpretation. Der erste Teil dieser Arbeit enthält eine chemodynamische Untersuchung von mehr als 20,000 roten Riesensternen, die sich bis zu 6 kpc (20,000 Lichtjahre) entfernt befinden. Diese Studie, die mit den ersten APOGEE-Daten gemacht wurde, konnte so das galaktische Volumen, das mit hochauflösender Spektroskopie je beobachtet wurde, dramatisch vergrößern. Weil die Sensitivität von APOGEE als Infrarotexperiment weit weniger durch interstellare Extinktion behindert wird, dringt unsere Stichprobe außerdem in die Regionen nahe der galaktischen Ebene vor, die typischerweise von optischen Durchmusterungen vermieden werden. Das erlaubt es uns, die chemodynamischen Eigenschaften der dünnen Milchstraßenscheibe außerhalb der unmittelbaren Sonnenumgebung zu studieren. Wir können beispielsweise zum ersten Mal mit hochauflösender Spektroskopie den radialen Metallizitätsgradienten der Scheibe als Funktion des Abstands von der Scheibenebene messen und zeigen, dass dieser Gradient oberhalb von 1 kpc positiv ist. Außerdem detektieren wir eine Lücke zwischen den Populationen I und II im chemischen [$\alpha$/Fe]-[Fe/H]-Häufigkeitsdiagramm, die im Gegensatz zur früheren Datenerhebungen schwerlich durch Selektionseffekte erklärt werden kann. Da für viele Sterne zudem 6-dimensionale Phasenrauminformationen vorliegen, können wir außerdem chemische Häufigkeitsdiagramme analysieren, in denen stellare Passanten aus anderen galaktischen Regionen ausgeblendet werden. Unsere Daten bestätigen zweifelsfrei die kurze Skalenlänge der dicken Milchstraßenscheibe (Population II). Im zweiten Teil der Arbeit nutzen wir zum ersten Mal kombinierte seismisch-spektroskopische Beobachtungen zum Zwecke der Galaktischen Archäologie. Wir analysieren dabei APOGEE-Beobachtungen von 606 roten Riesensternen in zwei CoRoT-Himmelsfeldern nahe der Galaktischen Ebene. Die Sterne sind über einen weiten Bereich der Galaktischen Scheibe verteilt (4.5 kpc $\lesssim R_{\rm Gal}\lesssim15$ kpc) und decken eine große Altersspanne ab (0.5 Gyr $\lesssim \tau\lesssim$ 13 Gyr), was es uns erlaubt, sowohl die Alters- als auch die radiale Abhängigkeit der [$\alpha$/Fe]-[Fe/H]-Verteilungen zu untersuchen. Dabei konstatieren wir, dass die Altersverteilung der Population-II-Sterne breiter ist als man es für ein monolithisches Kollaps-Szenario der dicken Scheibe erwarten würde. Vor Allem liegt das an einer vorher nicht bekannten, aber signifikanten Population scheinbar junger [$\alpha$/Fe]-reicher Sterne, deren Existenz mit Standardmodellen für die chemische Evolution der Galaktischen Scheibe nicht erklärbar ist. Diese eigentümlichen Objekte sind viel häufiger in der inneren Scheibe zu finden als in der äußeren, was darauf hindeutet, dass zumindest ein Teil dieser Population tatsächlich einen physikalischen Ursprung hat (etwa eine besondere chemische Entwicklung nahe des Galaktischen Balkens) und nicht etwa auf systematische Fehler in der Altersbestimmung zurückzuführen ist. Ein weiteres Resultat ergibt sich aus der Fülle von super-metallreichen Sternen in der äußeren Scheibe: der Effekt radialer Sternmigration scheint dort eine größere Rolle zu spielen als bisher angenommen. Im letzten Teil nutzen wir die CoRoGEE-Stichprobe, um die Zeitentwicklung des radialen Metallizitätsgradienten der dünnen Scheibe zu studieren; eine Unbekannte, die sowohl unter Theoretikern als auch unter Beobachtern in den letzten zwanzig Jahren immer wieder für Diskussionen sorgte. Wir teilen dazu die CoRoGEE-Daten in sechs Altersgruppen ein und erhalten durch eine sorgfältige statistische Analyse der radialen [Fe/H] Verteilungen unter Berücksichtigung systematischer Unsicherheiten verlässliche Werte für den Metallizitätsgradienten. Dessen Anstieg für die junge Population der roten Riesen ($-0.058\pm0.008$ [stat.] $\pm0.003$ [syst.] dex/kpc) ist konsistent mit den neuesten Messungen an Cepheiden. Im Altersbereich $1-4$ Gyr verzeichnen wir einen leicht steileren Gradienten ($-0.066\pm0.007\pm0.002$ dex/kpc), der für ältere Sterne (6--10 Gyr) wieder flacher ausfällt ($\sim-0.03$ dex/kpc). Diese Altersabhängigkeit des Metallizitätsgradienten lässt sich unter anderem durch ein Modell erklären, in dem der Metallizitätsgradient des interstellaren Medium etwa konstant bei $~-0.07$ dex/kpc liegt und in alten stellaren Populationen durch kinematische Effekte wie stellare Migration verwaschen wird. Stellare radiale Migration eröffnet uns außerdem eine elegante Erklärung für die verwundernde Tatsche, dass Sternhaufen mittleren Alters in der Sonnenumgebung oft höhere Metallizitäten aufweisen als junge Haufen. Um das zu erklären, schlagen wir ein Szenario vor, in dem nichtmigrierende Haufen eher durch gravitative Wechselwirkungen in der Scheibe zersöort werden als migrierende, was in der Sonnenumgebung eine Verzerrung zu Gunsten metallreicherer Haufen aus der inneren Scheibe nach sich zöge und, wie ebenfalls beobachtet, zur Folge hätte, dass der Metallizitätsgradient der mittelalten Haufenpopulation viel steiler wäre als der der jungen Haufen. KW - galactic astronomy KW - Milky Way evolution KW - Milky Way chemodynamics KW - red giant stars KW - asteroseismology KW - spectroscopy KW - galaktische Astrophysik KW - Entstehung der Milchstraße KW - Chemodynamik der Milchstraße KW - rote Riesensterne KW - Asteroseismologie KW - Spektroskopie Y1 - 2017 U6 - http://nbn-resolving.de/urn/resolver.pl?urn:nbn:de:kobv:517-opus4-396681 ER - TY - JOUR A1 - Schleussner, Carl-Friedrich A1 - Frieler, Katja A1 - Meinshausen, Malte A1 - Yin, J. A1 - Levermann, Anders T1 - Emulating Atlantic overturning strength for low emission scenarios consequences for sea-level rise along the North American east coast JF - Earth system dynamics N2 - In order to provide probabilistic projections of the future evolution of the Atlantic Meridional Overturning Circulation (AMOC), we calibrated a simple Stommel-type box model to emulate the output of fully coupled three-dimensional atmosphere-ocean general circulation models (AOGCMs) of the Coupled Model Intercomparison Project (CMIP). Based on this calibration to idealised global warming scenarios with and without interactive atmosphere-ocean fluxes and freshwater perturbation simulations, we project the future evolution of the AMOC mean strength within the covered calibration range for the lower two Representative Concentration Pathways (RCPs) until 2100 obtained from the reduced complexity carbon cycle-climate model MAGICC 6. For RCP3-PD with a global mean temperature median below 1.0 degrees C warming relative to the year 2000, we project an ensemble median weakening of up to 11% compared to 22% under RCP4.5 with a warming median up to 1.9 degrees C over the 21st century. Additional Greenland meltwater of 10 and 20 cm of global sea-level rise equivalent further weakens the AMOC by about 4.5 and 10 %, respectively. By combining our outcome with a multi-model sea-level rise study we project a dynamic sea-level rise along the New York City coastline of 4 cm for the RCP3-PD and of 8 cm for the RCP4.5 scenario over the 21st century. We estimate the total steric and dynamic sea-level rise for New York City to be about 24 cm until 2100 for the RCP3-PD scenario, which can hold as a lower bound for sea-level rise projections in this region, as it does not include ice sheet and mountain glacier contributions. Y1 - 2011 U6 - https://doi.org/10.5194/esd-2-191-2011 SN - 2190-4979 SN - 2190-4987 VL - 2 IS - 2 SP - 191 EP - 200 PB - Copernicus CY - Göttingen ER - TY - JOUR A1 - Mengel, Matthias A1 - Levermann, Anders A1 - Schleussner, Carl-Friedrich A1 - Born, Andreas T1 - Enhanced Atlantic subpolar gyre variability through baroclinic threshold in a coarse resolution model JF - Earth system dynamics N2 - Direct observations, satellite measurements and paleo records reveal strong variability in the Atlantic subpolar gyre on various time scales. Here we show that variations of comparable amplitude can only be simulated in a coupled climate model in the proximity of a dynamical threshold. The threshold and the associated dynamic response is due to a positive feedback involving increased salt transport in the subpolar gyre and enhanced deep convection in its centre. A series of sensitivity experiments is performed with a coarse resolution ocean general circulation model coupled to a statistical-dynamical atmosphere model which in itself does not produce atmospheric variability. To simulate the impact of atmospheric variability, the model system is perturbed with freshwater forcing of varying, but small amplitude and multi-decadal to centennial periodicities and observational variations in wind stress. While both freshwater and wind-stress-forcing have a small direct effect on the strength of the subpolar gyre, the magnitude of the gyre's response is strongly increased in the vicinity of the threshold. Our results indicate that baroclinic self-amplification in the North Atlantic ocean can play an important role in presently observed SPG variability and thereby North Atlantic climate variability on multi-decadal scales. Y1 - 2012 U6 - https://doi.org/10.5194/esd-3-189-2012 SN - 2190-4979 SN - 2190-4987 VL - 3 IS - 2 SP - 189 EP - 197 PB - Copernicus CY - Göttingen ER - TY - JOUR A1 - Schleussner, Carl-Friedrich A1 - Levermann, Anders A1 - Meinshausen, Malte T1 - Probabilistic projections of the Atlantic overturning JF - Climatic change : an interdisciplinary, intern. journal devoted to the description, causes and implications of climatic change N2 - Changes in the Atlantic overturning circulation have a strong influence on European temperatures, North American sea level and other climate phenomena worldwide. A meaningful assessment of associated societal impacts needs to be based on the full range of its possible future evolution. This requires capturing both the uncertainty in future warming pathways and the inherently long-term response of the ocean circulation. While probabilistic projections of the global mean and regional temperatures exist, process-based probabilistic assessments of large-scale dynamical systems such as the Atlantic overturning are still missing. Here we present such an assessment and find that a reduction of more than 50 % in Atlantic overturning strength by the end of the 21 (s t) century is within the likely range under an unmitigated climate change scenario (RCP8.5). By combining linear response functions derived from comprehensive climate simulations with the full range of possible future warming pathways, we provide probability estimates of overturning changes by the year 2100. A weakening of more than 25 % is found to be very unlikely under a climate protection scenario (RCP2.6), but likely for unmitigated climate change. The method is able to reproduce the modelled recovery caused by climatic equilibration under climate protection scenarios which provides confidence in the approach. Within this century, a reduction of the Atlantic overturning is a robust climatic phenomena that intensifies with global warming and needs to be accounted for in global adaptation strategies. Y1 - 2014 U6 - https://doi.org/10.1007/s10584-014-1265-2 SN - 0165-0009 SN - 1573-1480 VL - 127 IS - 3-4 SP - 579 EP - 586 PB - Springer CY - Dordrecht ER - TY - JOUR A1 - Schleussner, Carl-Friedrich A1 - Runge, Jakob A1 - Lehmann, Jasvcha A1 - Levermann, Anders T1 - The role of the North Atlantic overturning and deep ocean for multi-decadal global-mean-temperature variability JF - Earth system dynamics Y1 - 2014 U6 - https://doi.org/10.5194/esd-5-103-2014 SN - 2190-4979 SN - 2190-4987 VL - 5 IS - 1 SP - 103 EP - 115 PB - Copernicus CY - Göttingen ER - TY - JOUR A1 - Schleussner, Carl-Friedrich A1 - Rogelj, Joeri A1 - Schaeffer, Michiel A1 - Lissner, Tabea A1 - Licker, Rachel A1 - Fischer, Erich M. A1 - Knutti, Reto A1 - Levermann, Anders A1 - Frieler, Katja A1 - Hare, William T1 - Science and policy characteristics of the Paris Agreement temperature goal JF - Nature climate change Y1 - 2016 U6 - https://doi.org/10.1038/NCLIMATE3096 SN - 1758-678X SN - 1758-6798 VL - 6 SP - 827 EP - 835 PB - Nature Publ. Group CY - London ER - TY - JOUR A1 - Schleussner, Carl-Friedrich A1 - Donges, Jonathan A1 - Engemann, Denis A. A1 - Levermann, Anders T1 - Clustered marginalization of minorities during social transitions induced by co-evolution of behaviour and network structure JF - Scientific reports N2 - Large-scale transitions in societies are associated with both individual behavioural change and restructuring of the social network. These two factors have often been considered independently, yet recent advances in social network research challenge this view. Here we show that common features of societal marginalization and clustering emerge naturally during transitions in a co-evolutionary adaptive network model. This is achieved by explicitly considering the interplay between individual interaction and a dynamic network structure in behavioural selection. We exemplify this mechanism by simulating how smoking behaviour and the network structure get reconfigured by changing social norms. Our results are consistent with empirical findings: The prevalence of smoking was reduced, remaining smokers were preferentially connected among each other and formed increasingly marginalized clusters. We propose that self-amplifying feedbacks between individual behaviour and dynamic restructuring of the network are main drivers of the transition. This generative mechanism for co-evolution of individual behaviour and social network structure may apply to a wide range of examples beyond smoking. Y1 - 2016 U6 - https://doi.org/10.1038/srep30790 SN - 2045-2322 VL - 6 SP - 3407 EP - 3417 PB - Nature Publ. Group CY - London ER - TY - JOUR A1 - Anders, Friedrich A1 - Khalatyan, Arman A1 - Queiroz, Anna B. A. A1 - Chiappini, Cristina A1 - Ardèvol, Judith A1 - Casamiquela, Laia A1 - Figueras, Francesca A1 - Jiménez-Arranz, Óscar A1 - Jordi, Carme A1 - Monguio, Maria A1 - Romero-Gómez, Merce A1 - Altamirano, Diego A1 - Antoja, Teresa A1 - Assaad, R. A1 - Cantat-Gaudin, Tristan A1 - Castro-Ginard, Alfred A1 - Enke, Harry A1 - Girardi, Léo A1 - Guiglion, Guillaume A1 - Khan, Saniya A1 - Luri, Xavier A1 - Miglio, Andrea A1 - Minchev, Ivan A1 - Ramos, Pau A1 - Santiago, Basillio Xavier A1 - Steinmetz, Matthias T1 - Photo-astrometric distances, extinctions, and astrophysical parameters for Gaia EDR3 stars brighter than G=18.5 JF - Astronomy and astrophysics N2 - We present a catalogue of 362 million stellar parameters, distances, and extinctions derived from Gaia's Early Data Release (EDR3) cross-matched with the photometric catalogues of Pan-STARRS1, SkyMapper, 2MASS, and All WISE. The higher precision of the Gaia EDR3 data, combined with the broad wavelength coverage of the additional photometric surveys and the new stellar-density priors of the StarHorse code, allows us to substantially improve the accuracy and precision over previous photo-astrometric stellar-parameter estimates. At magnitude G = 14 (17), our typical precisions amount to 3% (15%) in distance, 0.13 mag (0.15 mag) in V-band extinction, and 140 K (180 K) in effective temperature. Our results are validated by comparisons with open clusters, as well as with asteroseismic and spectroscopic measurements, indicating systematic errors smaller than the nominal uncertainties for the vast majority of objects. We also provide distance- and extinction-corrected colour-magnitude diagrams, extinction maps, and extensive stellar density maps that reveal detailed substructures in the Milky Way and beyond. The new density maps now probe a much greater volume, extending to regions beyond the Galactic bar and to Local Group galaxies, with a larger total number density. We publish our results through an ADQL query interface (gaia . aip . de) as well as via tables containing approximations of the full posterior distributions. Our multi-wavelength approach and the deep magnitude limit render our results useful also beyond the next Gaia release, DR3. KW - stars: distances KW - stars: fundamental parameters KW - Galaxy: general KW - Galaxy: stellar content KW - Galaxy: structure Y1 - 2022 U6 - https://doi.org/10.1051/0004-6361/202142369 SN - 0004-6361 SN - 1432-0746 VL - 658 PB - EDP Sciences CY - Les Ulis ER -