A New Scaling Relation for H Ii Regions in Spiral Galaxies: Unveiling the True Nature of the Mass-Metallicity Relation

Rosales-Ortega, F. F.; Sanchez, S. F.; Iglésias-Páramo, J.; Díaz, Ángeles I.; Vílchez, J. M.; Bland-Hawthorn, Joss; Husemann, B.; Mast, D.

doi:10.1088/2041-8205/756/2/l31

Cited by 132 publications

(191 citation statements)

References 48 publications

(55 reference statements)

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“…This result was derived by analyzing the individual H ii regions of a sample of 174 starforming galaxies, based on slit spectroscopy. We independently confirmed this relation (Rosales-Ortega et al 2012), using a statistically complete sample of ∼2500 H ii regions extracted from a sample of 38 galaxies, using integral field spectroscopy (IFS), described in Sánchez et al (2012b).…”

Section: Introductionmentioning

confidence: 71%

“…In Rosales-Ortega et al (2012) we presented a new scaling relation between the oxygen abundance and the surface mass density for individual H ii regions (Σ-Z relation) 7 .This relation is a local version of the global M-Z relation, and indeed, it is possible to recover this latter one from the former by integrating over a certain aperture (Rosales-Ortega et al 2012). We proposed that this relation is the real fundamental one and the M-Z relation is a natural consequence.…”

Section: Dependence Of the σ-Z Relation On The Sfrmentioning

confidence: 91%

“…Figure 5, top-left panel, shows the Σ-Z relation for the H ii regions of the CALIFA galaxies explored so far. As a first result, we reproduce the relation described in Rosales-Ortega et al (2012), using a completely different dataset (the catalog of H ii regions extracted from 38 face-on spirals, using IFS data, from Sánchez et al 2012b). Both quantities have a strong correlation, with a correlation coefficient of r = 0.98.…”

Section: Dependence Of the σ-Z Relation On The Sfrmentioning

confidence: 98%

“…The narrow-band image is properly corrected for the contamination of the adjacent continuum. (ii) The narrowband image is used as an input for HIIexplorer 5 , an automatic H ii region detection code created for this kind of analysis (Sánchez et al 2012b;Rosales-Ortega et al 2012). The code provides a segmentation map that identifies each detected ionized region.…”

Section: Oxygen Abundancementioning

confidence: 99%

“…Instead of the classical polynomial function adopted by most previous studies for this relation (e.g., T04, Kewley & Ellison 2008;Mannucci et al 2010;Rosales-Ortega et al 2012;Hughes et al 2013), we chose to adopt an asymptotic function to describe the relation between both parameters following Moustakas et al (2011):…”

Section: Mass Metallicity Relationmentioning

confidence: 99%

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Mass-metallicity relation explored with CALIFA

Sánchez¹,

Rosales-Ortega²,

Jungwiert³

et al. 2013

A&A

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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.

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Section: Introductionmentioning

confidence: 71%

Section: Dependence Of the σ-Z Relation On The Sfrmentioning

confidence: 91%

Section: Dependence Of the σ-Z Relation On The Sfrmentioning

confidence: 98%

Section: Oxygen Abundancementioning

confidence: 99%

Section: Mass Metallicity Relationmentioning

confidence: 99%

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Mass-metallicity relation explored with CALIFA

Sánchez¹,

Rosales-Ortega²,

Jungwiert³

et al. 2013

A&A

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238

184

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Outskirts of Nearby Disk Galaxies: Star Formation and Stellar Populations

Elmegreen¹,

Hunter

2017

Astrophysics and Space Science Library

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The properties and star formation processes in the far-outer disks of nearby spiral and dwarf irregular galaxies are reviewed. The origin and structure of the generally exponential profiles in stellar disks is considered to result from cosmological infall combined with a non-linear star formation law and a history of stellar migration and scattering from spirals, bars, and random collisions with interstellar clouds. In both spirals and dwarfs, the far-outer disks tend to be older, redder and thicker than the inner disks, with the overall radial profiles suggesting inside-out star formation plus stellar scattering in spirals, and outside-in star formation with a possible contribution from scattering in dwarfs. Dwarf irregulars and the far-outer parts of spirals both tend to be gas dominated, and the gas radial profile is often non-exponential although still decreasing with radius. The ratio of Hα to far-UV flux tends to decrease with lower surface brightness in these regions, suggesting either a change in the initial stellar mass function or the sampling of that function, or a possible loss of Hα photons.

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IFUs surveys, a panoramic view of galaxy evolution

Sánchez

2014

Proc. IAU

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We present here a brief summary of the currenly on-going IFU surveys of galaxies in the Local Universe, describing their main characteristics, including their sample selections, instrumental setups, wavelength ranges, and area of the galaxies covered. Finally, we make an emphasis on the main characteristics of the CALIFA survey and the more recent results that has been recently publishedComment: 8 Pages, 2 Figures, S.F.Sanchez et al. 2014, in IAU Symp. 309, "Galaxy in 3D across the Universe", B. L. Ziegler, F. Combes, H. Dannerbauer, M. Verdugo, Eds. (Cambridge: Cambridge Univ. Press), in pres

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A New Scaling Relation for H Ii Regions in Spiral Galaxies: Unveiling the True Nature of the Mass-Metallicity Relation

Cited by 132 publications

References 48 publications

Mass-metallicity relation explored with CALIFA

Mass-metallicity relation explored with CALIFA

Outskirts of Nearby Disk Galaxies: Star Formation and Stellar Populations

IFUs surveys, a panoramic view of galaxy evolution

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