Show simple item record

dc.contributor.authorDomínguez Tenreiro, Rosa María 
dc.contributor.authorOñorbe, J.
dc.contributor.authorMartínez-Serrano, F.
dc.contributor.authorSerna, A.
dc.contributor.otherUAM. Departamento de Física Teóricaes_ES
dc.date.accessioned2015-06-15T17:57:27Z
dc.date.available2015-06-15T17:57:27Z
dc.date.issued2011-06-01
dc.identifier.citationMonthly Notices of the Royal Astronomical Society 413.4 (2011): 3022-3038en_US
dc.identifier.issn0035-8711 (print)es_ES
dc.identifier.issn1365-2966 (online)es_ES
dc.identifier.urihttp://hdl.handle.net/10486/666805
dc.descriptionThis article has been accepted for publication in Monthly Notices of the Royal Astronomical Society ©: 2011 RAS © 2011 The AuthorsPublished by Oxford University Press on behalf of the Royal Astronomical Society. All rights reserveden_US
dc.description.abstractWe have studied the mass assembly and star formation histories of massive galaxies identified at low redshift in different cosmological hydrodynamical simulations. To this end, we have carried out a detailed follow-up backwards in time of their constituent mass elements (sampled by particles) of different types. After that, the configurations they depict at progressively higher zs were carefully analysed. The analyses show that these histories share common generic patterns, irrespective of particular circumstances. In any case, however, the results we have found are different depending on the particle type. The most outstanding differences follow. We have found that by z∼ 3.5-6, mass elements identified as stellar particles at z= 0 exhibit a gaseous cosmic-web-like morphology with scales of ∼1 physical Mpc, where the densest mass elements have already turned into stars by z∼ 6. These settings are in fact the densest pieces of the cosmic web, where no hot particles show up, and dynamically organized as a hierarchy of flow convergence regions (FCRs), that is, attraction basins for mass flows. At high z FCRs undergo fast contractive deformations with very low angular momentum, shrinking them violently. Indeed, by z∼ 1 most of the gaseous or stellar mass they contain shows up as bound to a massive elliptical-like object at their centres, with typical half-mass radii of rmass star∼ 2-3kpc. After this, a second phase comes about where the mass assembly rate is much slower and characterized by mergers involving angular momentum. On the other hand, mass elements identified at the diffuse hot coronae surrounding massive galaxies at z= 0 do not display a clear web-like morphology at any z. Diffuse gas is heated when FCRs go through contractive deformations. Most of this gas remains hot and with low density throughout the evolution. To shed light on the physical foundations of the behaviour revealed by our analyses (i.e. a two-phase formation process with different implications for diffuse or shocked mass elements), as well as on their possible observational implications, these patterns have been confronted with some generic properties of singular flows as described by the adhesion model (i.e. potential character of the velocity field, singular versus regular points, dressing, locality when a spectrum of perturbations is implemented). We have found that the common patterns the simulations show can be interpreted as a natural consequence of flow properties that, moreover, could explain different generic observational results from massive galaxies or their samples. We briefly discuss some of themen_US
dc.description.sponsorshipThis work was partially supported by the DGES (Spain) through the grants AYA2009-12792-C03-02 and AYA2009-12792- C03-03 from the PNAyA, as well as by the regional Madrid V PRICIT programme through the ASTROMADRID network (CAM S2009/ESP-1496)en_US
dc.format.extent17 pag.es_ES
dc.format.mimetypeapplication/pdfen
dc.language.isoengen
dc.publisherRASen_US
dc.relation.ispartofMonthly Notices of the Royal Astronomical Societyen_US
dc.rights© 2011 RASen_US
dc.rights© 2011 The Authorsen_US
dc.subject.otherCosmology: miscellaneouses_ES
dc.subject.otherCosmology: theoryes_ES
dc.subject.otherGalaxies: formationes_ES
dc.subject.otherGalaxies: high-redshiftes_ES
dc.subject.otherGalaxies: star formationes_ES
dc.subject.otherHydrodynamicses_ES
dc.titleLarge-scale gas dynamics in the adhesion model: Implications for the two-phase massive galaxy formation scenarioes_ES
dc.typearticlees_ES
dc.subject.ecienciaFísicaes_ES
dc.relation.publisherversionhttp://dx.doi.org/10.1111/j.1365-2966.2011.18379.xes_ES
dc.identifier.doi10.1111/j.1365-2966.2011.18379.xes_ES
dc.identifier.publicationfirstpage3022es_ES
dc.identifier.publicationissue4es_ES
dc.identifier.publicationlastpage3038es_ES
dc.identifier.publicationvolume413es_ES
dc.relation.projectIDComunidad de Madrid. S2009/ESP-1496/ ASTROMADRIDes_ES
dc.type.versioninfo:eu-repo/semantics/publishedVersionen
dc.rights.accessRightsopenAccesses_ES
dc.facultadUAMFacultad de Ciencias


Files in this item

Thumbnail

This item appears in the following Collection(s)

Show simple item record