Evolution induced by dry minor mergers onto fast-rotator S0 galaxies

dc.contributor.authorTapia, Trinidad
dc.contributor.authorEliche Moral, María del Carmen
dc.contributor.authorQuerejeta, Miguel
dc.contributor.authorBalcells, Marc
dc.contributor.authorGonzález García, A. César
dc.contributor.authorPrieto, Mercedes
dc.contributor.authorAguerri, J. Alfonso L.
dc.contributor.authorGallego Maestro, Jesús
dc.contributor.authorZamorano Calvo, Jaime
dc.contributor.authorRodríguez Pérez, Cristina
dc.contributor.authorBorlaff, Alejandro
dc.date.accessioned2023-06-19T14:57:28Z
dc.date.available2023-06-19T14:57:28Z
dc.date.issued2014-05
dc.description© ESO, 2014. The authors thank the anonymous referee for the provided input that helped to improve this publication significantly, and to Frederic Bournaud for his interesting and useful comments. Supported by the Spanish Ministry of Economy and Competitiveness (MINECO) under projects AYA2006-12955, AYA2009-10368, AYA2009-11137, AYA2012-30717, AYA2010-21322-C03-02, AYA2010-21887-C04-04, and by the Madrid Regional Government through the AstroMadrid Project (CAM S2009/ESP-1496, http://www.laeff.cab.inta-csic.es/projects/astromadrid/main/index.php). Funded by the Spanish MICINN under the Consolider-Ingenio 2010 Program grant CSD2006-0070: "First Science with the GTC" (http://www.iac.es/consolider-ingenio-gtc/), and by the Spanish programme of International Campus of Excellence Moncloa (CEI). A.C.G.G. is a Ramón y Cajal Fellow of the Spanish MINECO. TT. gratefully acknowledged the computer resources, technical expertise and assistance provided by the LaPalma (IAC/RES, Spain) supercomputer installations.
dc.description.abstractContext. Numerical studies have shown that the properties of the S0 galaxies with kinematics intermediate between fast and slow rotators are difficult to explain by a scenario of major mergers. Aims. We investigate whether the smoother perturbation induced by minor mergers can reproduce these systems. Methods. We analysed collisionless N-body simulations of intermediate and minor dry mergers onto S0s to determine the structural and kinematic evolution induced by the encounters. The original primary galaxies represent gas-poor fast-rotator S0b and S0c galaxies with high intrinsic ellipticities. The original bulges are intrinsically spherical and have low rotation. Different mass ratios, parent bulges, density ratios, and orbits were studied. Results. Minor mergers induce a lower decrease of the global rotational support (as provided by λ_e) than encounters of lower mass ratios, which results in S0s with properties intermediate between fast and slow rotators. The resulting remnants are intrinsically more triaxial, less flattened, and span the whole range of apparent ellipticities up to ϵ_e ~ 0.8. They do not show lower apparent ellipticities in random projections than initially; on the contrary, the formation of oval distortions and the disc thickening increase the percentage of projections at 0.4 < ϵ_e < 0.7. In the experiments with S0b progenitor galaxies, minor mergers tend to spin up the bulge and to slightly decrease its intrinsic ellipticity, whereas in the cases of primary S0c galaxies they keep the rotational support of the bulge nearly constant and significantly decrease its intrinsic ellipticity. The remnant bulges remain nearly spherical (B/A ~ C/A> 0.9), but exhibit a wide range of triaxialities (0.20 < T < 1.00). In the plane of global anisotropy of velocities (δ) vs. intrinsic ellipticity (ϵ_e,intr), some of our models extend the linear trend found in previous major merger simulations towards higher ϵ_e,intr values, while others clearly depart from it (depending on the progenitor S0). This is consistent with the wide dispersion exhibited by real S0s in this diagram compared with ellipticals, which follow the linear trend drawn by major merger simulations. Conclusions. The smoother changes induced by minor mergers can explain the existence of S0s with intermediate kinematic properties between fast and slow rotators that are difficult to explain with major mergers. The different trends exhibited by ellipticals and S0 galaxies in the δ – ϵ_e diagram may be pointing to the different role played by major mergers in the build-up of each morphological type.
dc.description.departmentDepto. de Física de la Tierra y Astrofísica
dc.description.facultyFac. de Ciencias Físicas
dc.description.refereedTRUE
dc.description.sponsorshipMinisterio de Economía y Competitividad (MINECO), España
dc.description.sponsorshipAstroMadrid Project
dc.description.sponsorshipConsolider-Ingenio Program
dc.description.sponsorshipCampus de Excelencia Internacional (CEI), Campus Moncloa
dc.description.sponsorshipComunidad de Madrid
dc.description.sponsorshipMinisterio de Ciencia e Innovación (MCINN), España
dc.description.statuspub
dc.eprint.idhttps://eprints.ucm.es/id/eprint/34385
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dc.identifier.doi10.1051/0004-6361/201321386
dc.identifier.issn0004-6361
dc.identifier.officialurlhttp://arxiv.org/ct?url=http%3A%2F%2Fdx.doi.org%2F10%252E1051%2F0004-6361%2F201321386&v=9a071eb6
dc.identifier.relatedurlhttp://www.aanda.org/
dc.identifier.urihttps://hdl.handle.net/20.500.14352/34947
dc.journal.titleAstronomy & Astrophysics
dc.language.isoeng
dc.publisherEDP Sciencies
dc.relation.projectIDAYA2006-12955
dc.relation.projectIDAYA2009-10368
dc.relation.projectIDAYA2009-11137
dc.relation.projectIDAYA2012-30717
dc.relation.projectIDAYA2010-21322-C03-02
dc.relation.projectIDAYA2010-21887-C04-04
dc.relation.projectIDCAM S2009/ESP-1496
dc.relation.projectIDCSD2006-0070
dc.rights.accessRightsopen access
dc.subject.cdu52
dc.subject.keywordLess-than 1.5
dc.subject.keywordDigital sky survey
dc.subject.keywordTo-light ratio
dc.subject.keywordelliptic galaxies
dc.subject.keywordDisk galaxies
dc.subject.keywordAtlas(3D) project
dc.subject.keywordSecular evolution
dc.subject.keywordCluster galaxies
dc.subject.keywordStar-formation
dc.subject.keywordE/S0 galaxies
dc.subject.ucmAstrofísica
dc.subject.ucmAstronomía (Física)
dc.titleEvolution induced by dry minor mergers onto fast-rotator S0 galaxies
dc.typejournal article
dc.volume.number565
dspace.entity.typePublication
relation.isAuthorOfPublication303794a4-e4bf-4262-9a94-11bc46167d8e
relation.isAuthorOfPublication949589a4-3398-4ac6-805c-5dcf70d066f2
relation.isAuthorOfPublication.latestForDiscovery303794a4-e4bf-4262-9a94-11bc46167d8e
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