Oxygen and nitrogen abundances in nearby galaxies

Pilyugin, L. S.; Vı́lchez, J. M.; Contini, T.

doi:10.1051/0004-6361:20034522

Cited by 306 publications

(458 citation statements)

References 186 publications

(124 reference statements)

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“…This dependence, initially obtained for irregular galaxies, was later confirmed for galaxies of different morphological types (e.g. Vila-Costas & Edmunds 1992; Kobulnicky & Zaritsky 1999;Melbourne & Salzer 2002;Lee et al 2004;Pilyugin et al 2004; Lee et al 2006). …”

Section: Introductionmentioning

confidence: 54%

An investigation of the luminosity-metallicity relation for a large sample of low-metallicity emission-line galaxies

Гусева

Papaderos

Meyer

et al. 2009

A&A

103

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Context. We present 8.2 m VLT spectroscopic observations of 28 H ii regions in 16 emission-line galaxies and 3.6 m ESO telescope spectroscopic observations of 38 H ii regions in 28 emission-line galaxies. These emission-line galaxies were selected mainly from the data release 6 (DR6) of the Sloan digital sky survey (SDSS) as metal-deficient galaxy candidates. Aims. We collect photometric and high-quality spectroscopic data for a large uniform sample of star forming galaxies including new observations. Our aim is to study the luminosity-metallicity (L − Z) relation for nearby galaxies, especially at its low-metallicity end and compare it with that for higher-redshift galaxies.Methods. Physical conditions and element abundances in the new sample are derived with the T e -method, excluding six H ii regions from the VLT observations and nearly two third of the H ii regions from the 3.6 m observations. Element abundances for the latter galaxies were derived with the semiempirical strong-line method.Results. From our new observations we find that the oxygen abundance in 61 out of the 66 H ii regions of our sample ranges from 12 + log O/H = 7.05 to 8.22. Our sample includes 27 new galaxies with 12 + log O/H < 7.6 which qualify as extremely metal-poor star-forming galaxies (XBCDs). Among them are 10 H ii regions with 12 + log O/H < 7.3. The new sample is combined with a further 93 low-metallicity galaxies with accurate oxygen abundance determinations from our previous studies, yielding in total a high-quality spectroscopic data set of 154 H ii regions. 9000 more galaxies with oxygen abundances, based mainly on the T e -method, are compiled from the SDSS. Photometric data for all galaxies of our combined sample are taken from the SDSS database while distances are from the NED. Our data set spans a range of 8 mag with respect to its absolute magnitude in SDSS g (-12 > ∼ M g > ∼ −20) and nearly 2 dex in its oxygen abundance (7.0 < ∼ 12 + log O/H < ∼ 8.8), allowing us to probe the L − Z relation in the nearby universe down to the lowest currently studied metallicity level. The L − Z relation established on the basis of the present sample is consistent with previous ones obtained for emission-line galaxies.

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Section: Introductionmentioning

confidence: 54%

An investigation of the luminosity-metallicity relation for a large sample of low-metallicity emission-line galaxies

Гусева

Papaderos

Meyer

et al. 2009

A&A

103

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“…To estimate the Z at the location of our SNe within their hosts, we can correct the global Z of their hosts for the metallicity gradient that is known to characterize galaxies (e.g., Pilyugin et al 2004;Taddia et al 2013Taddia et al , 2015, where the nucleus is typically more metal-rich than the outer parts. We used the derived global Z as a proxy of the central Z, and then adopted an average Z gradient of −0.47 R −1 25 (see Pilyugin et al 2004).…”

Section: Analysis and Resultsmentioning

confidence: 99%

“…We used the derived global Z as a proxy of the central Z, and then adopted an average Z gradient of −0.47 R −1 25 (see Pilyugin et al 2004). The deprojected and radius-normalized distance for each SN from its host center (see Table A.2) was estimated using the SN and the host-galaxy coordinates, the host-galaxy radius, the host-galaxy axis ratio, and the position angle as obtained from SDSS (Ahn et al 2014).…”

Section: Analysis and Resultsmentioning

confidence: 99%

Metallicity from Type II supernovae from the (i)PTF

Taddia

Moquist

Sollerman

et al. 2016

A&A

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Type IIP supernovae (SNe IIP) have recently been proposed as metallicity (Z) probes. The spectral models of Dessart et al. (2014, MNRAS, 440, 1856 showed that the pseudo-equivalent width of Fe ii λ5018 (pEW 5018 ) during the plateau phase depends on the primordial Z, but there was a paucity of SNe IIP exhibiting pEW 5018 that were compatible with Z < 0.4 Z . This lack might be due to some physical property of the SN II population or to the fact that those SNe have been discovered in luminous, metal-rich targeted galaxies. Here we use SN II observations from the untargeted (intermediate) Palomar Transient Factory [(i)PTF] survey, aiming to investigate the pEW 5018 distribution of this SN population and, in particular, to look for the presence of SNe II at lower Z. We perform pEW 5018 measurements on the spectra of a sample of 39 (i)PTF SNe II, selected to have well-constrained explosion epochs and light-curve properties. Based on the comparison with the pEW 5018 spectral models, we subgrouped our SNe into four Z bins from Z ≈ 0.1 Z up to Z ≈ 2 Z . We also independently investigated the Z of the hosts by using their absolute magnitudes and colors and, in a few cases, using strong-line diagnostics from spectra. We searched for possible correlations between SN observables, such as their peak magnitudes and the Z inferred from pEW 5018 . We found 11 events with pEW 5018 that were small enough to indicate Z ≈ 0.1 Z . The trend of pEW 5018 with Z matches the Z estimates obtained from the host-galaxy photometry, although the significance of the correlation is weak. We also found that SNe with brighter peak magnitudes have smaller pEW 5018 and occur at lower Z.

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“…Peimbert 1979;Shaver et al 1983;Vila-Costas & Edmunds 1992;Zaritsky et al 1994;Kennicutt et al 2003;Pilyugin et al 2004;Bresolin et al 2009b;Rosales-Ortega et al 2011;Marino et al 2012;Sánchez et al 2012b;Pilyugin et al 2014;Sánchez et al 2014;Sánchez-Menguiano et al 2016b;Zinchenko et al 2016;Belfiore et al 2017). However, recently it has been found that some spiral galaxies show lower (higher) oxygen abundance val-ues in the inner (outer) regions than that expected according to the observed negative gradients.…”

Section: The Shape Of the Abundance Profilesmentioning

confidence: 99%

The shape of oxygen abundance profiles explored with MUSE: evidence for widespread deviations from single gradients

Sánchez-Menguiano

Sanchez

Pérez

et al. 2018

A&A

150

146

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We characterised the oxygen abundance radial distribution of a sample of 102 spiral galaxies observed with VLT/MUSE using the O3N2 calibrator. The high spatial resolution of the data allowed us to detect 14345 H ii regions with the same image quality as with photometric data, avoiding any dilution effect. We developed a new methodology to automatically fit the abundance radial profiles, finding that 55 galaxies of the sample exhibit a single negative gradient. The remaining 47 galaxies also display, as well as this negative trend, either an inner drop in the abundances (21), an outer flattening (10), or both (16), which suggests that these features are a common property of disc galaxies. The presence and depth of the inner drop depends on the stellar mass of the galaxies with the most massive systems presenting the deepest abundance drops, while there is no such dependence in the case of the outer flattening. We find that the inner drop appears always around 0.5 r e , while the position of the outer flattening varies over a wide range of galactocentric distances. Regarding the main negative gradient, we find a characteristic slope in the sample of α O/H = − 0.10 ± 0.03 dex/r e . This slope is independent of the presence of bars and the density of the environment. However, when inner drops or outer flattenings are detected, slightly steeper gradients are observed. This suggests that radial motions might play an important role in shaping the abundance profiles. We define a new normalisation scale ('the abundance scale length', r O/H ) for the radial profiles based on the characteristic abundance gradient, with which all the galaxies show a similar position for the inner drop (∼ 0.5 r O/H ) and the outer flattening (∼ 1.5 r O/H ). Finally, we find no significant dependence of the dispersion around the negative gradient with any property of the galaxies, with values compatible with the uncertainties associated with the derivation of the abundances.

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Oxygen and nitrogen abundances in nearby galaxies

Cited by 306 publications

References 186 publications

An investigation of the luminosity-metallicity relation for a large sample of low-metallicity emission-line galaxies

An investigation of the luminosity-metallicity relation for a large sample of low-metallicity emission-line galaxies

Metallicity from Type II supernovae from the (i)PTF

The shape of oxygen abundance profiles explored with MUSE: evidence for widespread deviations from single gradients

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