Download - RC3: La Vía Láctea y sus componentesRC3: Vía Láctea y sus componentes Milky Way’s Formation and evolution (a) VL026 - Gallart et al. Uncovering the birth of the Milky Way through

XIV.0ReuniónCientífica 13-15julio2020

RC3:LaVíaLácteaysuscomponentes

15:30-16:15hTuesday,July14th 2020

82contributions

SEAVirtualScienceMeeting2020

20’Summaryofmainresultsinthepresentedcontributions

25’Opendiscussiononhottopics inthestudyoftheMWanditscomponents

SantiRoca-Fàbrega,SergioSimón-Díaz,EvaVillaver


RC3:VíaLácteaysuscomponentes

MilkyWay’sFormationandevolution

(a)VL026- Gallart etal.UncoveringthebirthoftheMilkyWaythroughaccuratestellarageswithGaia

(b)VL058-Mor etal.Gaiamissiondatarevealsare-ignitionofstarformationintheMilkyWay’sdiscabout5billionyearsago

(c)VL069- Roca-Fàbrega etal.ThebimodalA(Li)distributionofMilkyWay’sthindiskstarsandtheGalacticscaleevents

(d)VL074- Ruiz-Laraetal.TherecurrentimpactoftheSagittariusdwarfontheMilkyWaystarformationhistory

(e)VL078- Sotillo-Ramosetal.ThediverseevolutionarypathwaysofMilkyWay-likegalaxieswithTNG50

- High quality data from Gaia, combined withchemistry from APOGEE and GALAH surveys, andwith theory/simulations, allowed the communityto study the mass accretion history of the MW.

- Several groups are reporting new findings on theformation of the thin and thick disks structures,and also of the stellar halo.

- Events that drove to the formation of the currentGalaxy components are well detected as imprintsin the MW’s stars chemistry and kinematics.

- Cosmological simulations are playing animportant role when trying to understand theeffects of Galactic scale events on the MW starformation history.

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MilkyWay’schemistry

(f)VL008- Arellano-Córdova etal.UnderstandingthechemicalevolutionofC,O,N,Ne,S,ClandAr intheMilkyWayusingHIIregions

(g)VL013- Carbajo-Hijarrubia etal.StatusoftheOCCASOsurveyfortheanalysisofthechemistryoftheGalacticdisc

(h)VL082- Viscasillas VázquezChemicalabundancesofs- andr-processelementsintheSolarVicinity3

- Radial profiles and temporal evolutionof metal abundances, both inindividual and cluster stars, are beingused by many researchers to differentscenarios of formation and evolutionof the MW components.

- Comparison with external galaxiesshow that the MW behaves similarly toother spiral galaxies.

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KinematicsofMWstars

(i)VL004- Andersetal.Stellarradialmigrationasasubdiffusiveprocess

(j)VL005- AnguianoTheStellarVelocityDistributionFunction intheMilkyWayGalaxy

(k)VL018-Miret-Roig etal.Dynamicaltraceback ageoftheBetaPictorismovinggroup

(l)VL027- García-Conde etal.Phasespiralsincosmologicalsimulations

- High precision Gaia DR2 kinematics areused by several groups to get a bettermodelling of the thin-thick diskcomponents and its evolution in time(e.g. radial migration).

- Cosmological simulations have shownto be good tools to better understandformation and evolution of kinematicstructures in the MW thin disk.

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Stellarstructures- Disk

(m)VL016- Andersetal.Reanalysing theGalacticopen-clusterpopulation inlightofGaiaDR2

(n)VL017- Chrobakova etal.StructureoftheoutergalacticdiskwithGaiaDR2

(o)VL062- Pardo-Araujoetal.Probingtheprecessing barmodelfortheGalacticwarporigin

(p)VL073- Romero-Gómez etal.DissectingtheGalacticbarusingGaiaobservablesandstatisticaltechniques

- Several colleagues are analyzing theMW disk. They compared Gaia datawith theoretical models to betterunderstand the formation and natureof the Warp.

- The galactic bar is also deeplyanalyzed by applying statisticaltechniques on the Gaia DR2 data.

- A new OC’s catalogue from Gaia DR2has been obtained. OC’s stellar agefunction needs to be revised.

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Stellarstructures– haloandouterdisk

(q)VL006- Antoja etal.TheSagittariusstreamwithGaiadata

(r)VL055-Miró-Carretero etal.TracinginstellartidalstreamsintheMilkyWayhalowiththeJ-PLUSphotometry

(s)VL066- Ramosetal.TheHalo-Discdynamicalcoupling.GaiablinddetectionoftheMonocerosandACSstructures

- Many research groups are working onthe analysis of the halo substructureembedded in GaiaDR2, using noveltechniques. In particular, results fromthe analysis of the Sagittarius and itsstream are a clear example of how halostellar structures give us information onthe formation and evolution of ourGalaxy.

- Some groups study the presence of newstructures in the outer disk, that may bea consequence of strong perturbationsover the MW’s disk.

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Somequestions/hottopicstobediscussed

- MW formation history with Gaia DR3 + RAVE + APOGEE + … will new data begood enough to finally solve some of the still open key/fundamental questions(bar formation and properties, spiral arms, recent perturbers)?

- Is there a flattening of the O/H in the inner disk? What about metallicitygradients in general? Can old/new radial migration scenarios predict/fit newobservations?

- The MW’s bar: Old, young, long, short, metal rich, metal poor?

- How to break degeneracies on the identification of disk structures caused byexternal perturbations (streams, warp, stripped stars from the outer MW disk, …)
