English   español  
Please use this identifier to cite or link to this item: http://hdl.handle.net/10261/140572
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
Exportar a otros formatos:
Title

Outer-disk reddening and gas-phase metallicities: The CALIFA connection

AuthorsMarino, R. A.; Sánchez, Sebastián F. ; Cardiel, Nicolás; Vílchez Medina, José Manuel ; Kehrig, C. ; González Delgado, Rosa M. ; García-Benito, Rubén ; Mast, Damián ; Iglesias-Páramo, J. ; Bland-Hawthorn, J.
KeywordsGalaxies: ISM
Galaxies: photometry
Galaxies: evolution
Galaxies: abundances
ISM: abundances
Issue Date2016
PublisherEDP Sciences
CitationAstronomy and Astrophysics 585: A47 (2016)
AbstractWe study, for the first time in a statistically significant and well-defined sample, the relation between the outer-disk ionized-gas metallicity gradients and the presence of breaks in the surface brightness profiles of disk galaxies. Sloan Digital Sky Survey (SDSS) g′- and r′-band surface brightness, (g′ - r′) color, and ionized-gas oxygen abundance profiles for 324 galaxies within the Calar Alto Legacy Integral Field Area (CALIFA) survey are used for this purpose. We perform a detailed light-profile classification, finding that 84% of our disks show down- or up-bending profiles (Type II and Type III, respectively), while the remaining 16% are well fitted by one single exponential (Type I). The analysis of the color gradients at both sides of this break shows a U-shaped profile for most Type II galaxies with an average minimum (g′ - r′) color of ∼ 0.5mag and an ionized-gas metallicity flattening associated with it only in the case of low-mass galaxies. Comparatively, more massive systems show a rather uniform negative metallicity gradient. The correlation between metallicity flattening and stellar mass for these systems results in p-values as low as 0.01. Independent of the mechanism having shaped the outer light profiles of these galaxies, stellar migration or a previous episode of star formation in a shrinking star-forming disk, it is clear that the imprint in their ionized-gas metallicity was different for low- and high-mass Type II galaxies. In the case of Type III disks, a positive correlation between the change in color and abundance gradient is found (the null hypothesis is ruled out with a p-value of 0.02), with the outer disks of Type III galaxies with masses ≤10 M′ showing a weak color reddening or even a bluing. This is interpreted as primarily due to a mass downsizing effect on the population of Type III galaxies that recently experienced an enhanced inside-out growth.
DescriptionBased on observations collected at the German-Spanish Astronomical Center, Calar Alto, jointly operated by the Max-Planck-Institut für Astronomie Heidelberg and the Instituto de Astrofísica de Andalucía (CSIC ).
CALIFA Team: et al.
Publisher version (URL)http://dx.doi.org/10.1051/0004-6361/201526986
URIhttp://hdl.handle.net/10261/140572
DOI10.1051/0004-6361/201526986
Identifiersdoi: 10.1051/0004-6361/201526986
e-issn: 1432-0746
issn: 0004-6361
Appears in Collections:(EEZA) Artículos
(IFCA) Artículos
(IAA) Artículos
Files in This Item:
File Description SizeFormat 
gas-phase metallicities.pdf8,08 MBAdobe PDFThumbnail
View/Open
Show full item record
 

Related articles:


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