English   español  
Please use this identifier to cite or link to this item: http://hdl.handle.net/10261/213528
Share/Impact:
Statistics
logo share SHARE logo core CORE   Add this article to your Mendeley library MendeleyBASE

Visualizar otros formatos: MARC | Dublin Core | RDF | ORE | MODS | METS | DIDL | DATACITE
Exportar a otros formatos:

DC FieldValueLanguage
dc.contributor.authorBreda, Irises_ES
dc.contributor.authorPapaderos, Polychronises_ES
dc.contributor.authorGomes, Jean Micheles_ES
dc.contributor.authorVílchez Medina, José Manueles_ES
dc.contributor.authorZiegler, Bodo L.es_ES
dc.contributor.authorHirschmann, Michaelaes_ES
dc.contributor.authorCardoso, Leandro S. M.es_ES
dc.contributor.authorLagos, Patricioes_ES
dc.contributor.authorBuitrago, Fernandoes_ES
dc.date.accessioned2020-06-05T09:48:25Z-
dc.date.available2020-06-05T09:48:25Z-
dc.date.issued2020-
dc.identifier.citationAstronomy and Astrophysics - Les Ulis 635: A177 (2020)es_ES
dc.identifier.issn0004-6361-
dc.identifier.urihttp://hdl.handle.net/10261/213528-
dc.description.abstractRadial age gradients hold the cumulative record for the multitude of physical processes driving the build-up of stellar populations and the ensuing star formation (SF) quenching process in galaxy bulges and, therefore, potentially sensitive discriminators between competing theoretical concepts on bulge formation and evolution. Based on spectral modeling of integral field spectroscopy (IFS) data from the CALIFA survey, we derived mass- and light-weighted stellar age gradients (δ(t∗B)L,M) within the photometrically determined bulge radius (RB) of a representative sample of local face-on late-type galaxies that span 2.6 dex in stellar mass (8.9 ≤ logM∗T ≤ 11.5). Our analysis documents a trend of decreasing δ(t∗B)L,M with increasing M∗T, with high-mass bulges predominantly showing negative age gradients and vice versa. The inversion from positive to negative δ(t∗B)L,M occurs at logM∗T ' 10, which roughly coincides with the transition from lower-mass bulges whose gas excitation is powered by SF to bulges classified as composite, LINER, or Seyfert. We discuss two simple limiting cases for the origin of radial age gradients in massive late-type galaxy bulges. The first one assumes that the stellar age in the bulge is initially spatially uniform (δ(t∗B)L,M ≈ 0), thus the observed age gradients (~-3 Gyr/RB) arise from an inside-out SF quenching (ioSFQ) front that is radially expanding with a mean velocity vq. In this case, the age gradients for massive bulges translate into a slow (vq ~1-2 km s-1) ioSFQ that lasts until z ~ 2, suggesting mild negative feedback by SF or an active galactic nucleus (AGN). If, on the other hand, negative age gradients in massive bulges are not due to ioSFQ but primarily due to their inside-out formation process, then the standard hypothesis of quasi-monolithic bulge formation has to be discarded in favor of another scenario. This would involve a gradual buildup of stellar mass over 2-3 Gyr through, for instance, inside-out SF and inward migration of SF clumps from the disk. In this case, rapid (≪1 Gyr) AGN-driven ioSFQ cannot be ruled out. While theM∗T versus δ(t∗B)L,M relation suggests that the assembly history of bulges is primarily regulated by galaxy mass, its large scatter (~1.7 Gyr/RB) reflects a considerable diversity. This calls for an in-depth examination of the role of various processes (e.g., negative and positive AGN feedback, bar-driven gas inflows) with higher-quality IFS data in conjunction with advanced spectral modeling codes. © 2020 EDP Sciences. All rights reserved.es_ES
dc.description.sponsorshipWe thank the anonymous referee for valuable comments and suggestions. Additionally, we thank the EU for providing to Portugal a substantial fraction of the financial resources that allowed it to sustain a research infrastructure in astrophysics. Specifically, this work was carried out at an institute whose funding is provided to 85% by th e EU via the FCT (Fundacao para a Ciencia e a Tecnologia) apparatus, through European and national funding via FEDER through COMPETE by the grants UID/FIS/04434/2013 & POCI-01-0145-FEDER-007672 and PTDC/FIS-AST/3214/2012 & FCOMP01-0124-FEDER-029170. Additionally, this work was supported through FCT grants UID/FIS/04434/2019, UIDB/04434/2020 and UIDP/04434/2020. We further acknowledge support by European Community Programme (FP7/20072013) under grant agreement No. PIRSES-GA-2013-612701 (SELGIFS). We are grateful to Dr. Dimitri Gadotti, Prof. Daniel Schaerer and Dr. Andrew Humphrey for valuable comments. I. B. was supported by the FCT PhD::SPACE Doctoral Network (PD/00040/2012) through the fellowship PD/BD/52707/2014 funded by FCT (Portugal) and POPH/FSE (EC) and by the fellowship CAUP07/2014-BI in the context of the FCT project PTDC/FIS-AST/3214/2012 & FCOMP-01-0124-FEDER-029170. P. P. was supported through Investigador FCT contract IF/01220/2013/CP1191/CT0002 and by a contract that is supported by FCT/MCTES through national funds (PIDDAC) and by grant PTDC/FIS-AST/29245/2017. J. M. G. is supported by the fellowship CIAAUP-04/2016-BPD in the context of the FCT project UID/FIS/04434/2013 & POCI01-0145-FEDER-007672 and acknowledges the previous support by the fellowships SFRH/BPD/66958/2009 funded by FCT and POPH/FSE (EC) and DL 57/2016/CP1364/CT0003. L. S. M. C. acknowledges support by the project "Enabling Green E-science for the SKA Research Infrastructure (ENGAGE SKA)" (reference POCI-01-0145-FEDER-022217), funded by COMPETE 2020 and FCT. P.L. acknowledges support by DL57/2016/CP1364/CT0010. F. B. acknowledges the support by FCT via the postdoctoral fellowship SFRH/BPD/103958/2014. This study uses data provided by the Calar Alto Legacy Integral Field Area (CALIFA) survey (califa.caha.es), funded by the Spanish Ministry of Science under grant ICTS-2009-10, and the Centro Astronomico Hispano-Aleman. It is based on observations collected at the Centro Astronomico Hispano Aleman (CAHA) at Calar Alto, operated jointly by the Max-Planck-Institut fur Astronomie and the Instituto de Astrofisica de Andalucia (CSIC). This research has made use of the NASA/IPAC Extragalactic Database (NED) which is operated by the Jet Propulsion Laboratory, California Institute of Technology, under contract with the National Aeronautics and Space Administration.es_ES
dc.language.isoenges_ES
dc.publisherEDP Scienceses_ES
dc.relation.isversionofPublisher's versiones_ES
dc.rightsopenAccesses_ES
dc.subjectGalaxies: spirales_ES
dc.subjectGalaxies: bulgeses_ES
dc.subjectGalaxies: evolutiones_ES
dc.titleStellar age gradients and inside-out star formation quenching in galaxy bulgeses_ES
dc.typeartículoes_ES
dc.identifier.doihttp://dx.doi.org/10.1051/0004-6361/201937193-
dc.description.peerreviewedPeer reviewedes_ES
dc.relation.publisherversionhttp://dx.doi.org/10.1051/0004-6361/201937193es_ES
dc.contributor.funderFundação para a Ciência e a Tecnologia (Portugal)es_ES
dc.contributor.funderEuropean Commissiones_ES
dc.relation.csices_ES
oprm.item.hasRevisionno ko 0 false*
dc.identifier.funderhttp://dx.doi.org/10.13039/501100001871es_ES
dc.identifier.funderhttp://dx.doi.org/10.13039/501100000780es_ES
Appears in Collections:(IAA) Artículos
Files in This Item:
File Description SizeFormat 
IAA_2020aa37193.pdf1,13 MBAdobe PDFThumbnail
View/Open
Show simple item record
 


WARNING: Items in Digital.CSIC are protected by copyright, with all rights reserved, unless otherwise indicated.