Mass-metallicity relation explored with CALIFA I. Is there a dependence on the star-formation rate?
By Sebastián F. Sánchez, F. Rosales-Ortega, B. Jungwiert, J. Iglesias-Páramo, J. Vílchez, R. Marino, C. Walcher, B. Husemann, D. Mast, A. Monreal-Ibero and 32 more. 2013
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We studied the global and local ℳ-Z relation based on the first data available from the CALIFA survey (150 galaxies). This survey provides integral field spectroscopy of the complete optical extent of each galaxy (up to 2−3 effective radii), with a resolution high enough to separate individual H II regions and/or aggregations. About 3000 individual H II regions have been detected. The spectra cover the wavelength range between [OII]3727 and [SII]6731, with a sufficient signal-to-noise ratio to derive the oxygen abundance and star-formation rate associated with each region. In addition, we computed the integrated and spatially resolved stellar masses (and surface densities) based on SDSS photometric data. We explore the relations between the stellar mass, oxygen abundance and star-formation rate using this dataset. We derive a tight relation between the integrated stellar mass and the gas-phase abundance, with a dispersion lower than the one already reported in the literature (σ_Δlog (O/H) = 0.07 dex). Indeed, this dispersion is only slightly higher than the typical error derived for our oxygen abundances. However, we found no secondary relation with the star-formation rate other than the one induced by the primary relation of this quantity with the stellar mass. The analysis for our sample of ~3000 individual H II regions confirms (i) a local mass-metallicity relation and (ii) the lack of a secondary relation with the star-formation rate. The same analysis was performed with similar results for the specific star-formation rate. Our results agree with the scenario in which gas recycling in galaxies, both locally and globally, is much faster than other typical timescales, such like that of gas accretion by inflow and/or metal loss due to outflows. In essence, late-type/disk-dominated galaxies seem to be in a quasi-steady situation, with a behavior similar to the one expected from an instantaneous recycling/closed-box model.
Subfields: Astronomy and Astrophysics, Instrumentation
View Paper: https://www.semanticscholar.org/paper/51260de14fd80cb056a8f3724616493d6f27386d
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Citations in the corpus
- New calibrations for abundance determinations in H ii regions (2016, background): “…dependence on environment or star formation rate (e.g., Lequeux et al. 1979; Grebel et al. 2003; Tremonti et al. 2004; Erb et al. 2006; Panter et al. 2008; Zahid et al. 2012; Sánchez et al. 2013; Peng & Maiolino 2014; Zahid et al. 2014; Izotov et al. 2015, to just name a few of the many studies).”
- Metallicity evolution, metallicity gradients, and gas fractions at z ~ 3.4 (2013, result): “Recently, Sánchez et al. (2013) by using spatially resolved spectroscopy of nearby galaxies, have not confirmed the metallicity dependence on the SFR, in contrast to previous studies.”
- A characteristic oxygen abundance gradient in galaxy disks unveiled with CALIFA (2013, methodology): “Z relation (e.g., Tremonti et al. 2004; Sanchez et al. 2013).”
- The nature of LINER galaxies: Ubiquitous hot old stars and rare accreting black holes (2013, background): “The combination with the low-resolution V500 grating allows for mapping of stellar ages, metallicities, full star-formation histories, ionised-gas emission line fluxes, and chemical abundances (e.g. Pérez et al. 2013; Sánchez et al. 2013; Falcón-Barroso et al. in prep.).”
- THE UNIVERSAL RELATION OF GALACTIC CHEMICAL EVOLUTION: THE ORIGIN OF THE MASS–METALLICITY RELATION (2014, background): “However, the redshift independence of the relation between stellar mass, metallicity and SFR remains tentative (Niino 2012; Pérez-Montero et al. 2013; Sánchez et al. 2013; Zahid et al. 2013b; Ly et al. 2014).”
- The CALIFA survey across the Hubble sequence: Spatially resolved stellar population properties in galaxies (2015, background): “…how the bulge (disk) properties change with respect to those of the galaxy as a whole.3 3 Based on the exponential fit analysis developed by (Sánchez et al. 2013) and (Sánchez-Blázquez et al. 2014), we conclude that the regions between 1 and 2 HLR are dominated by the disk component; thus,…”