The Abundance Properties of Nearby Late-Type Galaxies. I. The Data

Pilyugin, L. S.; Grebel, Eva K.; Kniazev, A. Y.

doi:10.1088/0004-6256/147/6/131

Cited by 159 publications

(262 citation statements)

References 216 publications

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“…In this context, it would be useful to check whether the deviations are correlated with the airmass during the observation, but none of the papers whose spectra we use provides the airmass values of their observations. The new calibration of the P method of Pilyugin et al (2014), which we have called P ′ above, is less sensitive to the [O ii] λ3727/Hβ line ratio and performs much better when used to derive the oxygen abundance gradient, implying a slope of −0.008 dex kpc −1 and a dispersion around the gradient of 0.09 dex. However, the calibration sample of the P ′ method includes regions with abundances determined using the C method.…”

Section: Discussionmentioning

confidence: 99%

“…Besides two old determinations based on the R23 method calibrated with photoionization models by Pagel et al (1979), we have chosen to present the results that are based on methods similar to the ones we use. The most recent determination, that of Pilyugin et al (2014), is based on abundances calculated with the P and C methods slightly modified, which we label as P ′ and C ′ . Pilyugin et al (2014) also derived the gradient for N/H with their C ′ method for regions with galactocentric distances in the range 4-13 kpc, finding a slope of −0.033, steeper than the one we find with the C method for the range of 3-33 kpc, −0.020.…”

Section: Comparison With Other Workmentioning

confidence: 99%

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The oxygen abundance gradient in M81 and the robustness of abundance determinations in H ii regions

Arellano-Córdova

Rodríguez

Mayya

et al. 2015

Mon. Not. R. Astron. Soc.

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We study the sensitivity of the methods available for abundance determinations in H ii regions to potential observational problems. We compare the dispersions they introduce around the oxygen and nitrogen abundance gradients when applied to five different sets of spectra of H ii regions in the galaxy M81. Our sample contains 116 H ii regions with galactocentric distances of 3 to 33 kpc, including 48 regions observed by us with the OSIRIS long-slit spectrograph at the 10.4-m Gran Telescopio Canarias telescope. The direct method can be applied to 31 regions, where we can get estimates of the electron temperature. The different methods imply oxygen abundance gradients with slopes of −0.010 to −0.002 dex kpc −1 , and dispersions in the range 0.06-0.25 dex. The direct method produces the shallowest slope and the largest dispersion, illustrating the difficulty of obtaining good estimates of the electron temperature. Three of the strong-line methods, C, ONS, and N2, are remarkably robust, with dispersions of ∼ 0.06 dex, and slopes in the range −0.008 to −0.006 dex kpc −1 . The robustness of each method can be directly related to its sensitivity to the line intensity ratios that are more difficult to measure properly. Since the results of the N2 method depend strongly on the N/O abundance ratio and on the ionization parameter, we recommend the use of the C and ONS methods when no temperature estimates are available or when they have poor quality, although the behaviour of these methods when confronted with regions that have different properties and different values of N/O should be explored.

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Section: Discussionmentioning

confidence: 99%

Section: Comparison With Other Workmentioning

confidence: 99%

The oxygen abundance gradient in M81 and the robustness of abundance determinations in H ii regions

Arellano-Córdova

Rodríguez

Mayya

et al. 2015

Mon. Not. R. Astron. Soc.

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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

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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“…The observed oxygen References. abundance profiles of the NGC 300 disk used to constrain the gas-phase oxygen predicted by our model are those of Bresolin et al (2009) and Pilyugin et al (2014), since these two papers enlarged the number of the Hii regions in whose spectra [Oiii]λ4363 can be detected. At the same time, the characteristic oxygen abundance, which is defined as the oxygen value 12 + log(O/H) at the effective radius r eff , is representative of the average value of the young component across the galaxy (Garnett 2002;Sánchez et al 2013).…”

Section: Chemical Abundancementioning

confidence: 99%

The star formation history of low-mass disk galaxies: A case study of NGC 300

Kang

Zhang

Chang

et al. 2015

A&A

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Context. Since NGC 300 is a bulgeless, isolated low-mass galaxy and it has not experienced radial migration during its evolution history, it can be treated as an ideal laboratory to test the simple galactic chemical evolution model. Aims. Our main aim is to investigate the main properties of the star formation history (SFH) of NGC 300 and compare its SFH with that of M 33 to explore the common properties and differences between these two nearby low-mass systems. Methods. We construct a simple chemical evolution model for NGC 300, assuming its disk forms gradually from continuous accretion of primordial gas and including the gas-outflow process. The model allows us to build a bridge between the SFH and observed data of NGC 300, in particular, the present-day radial profiles and global observed properties (e.g., cold gas mass, star formation rate, and metallicity). By means of comparing the model predictions with the corresponding observations, we adopt the classical χ 2 methodology to find out the best combination of free parameters a, b, and b out . Results. Our results show that by assuming an inside-out formation scenario and an appropriate outflow rate, our model reproduces well most of the present-day observational values. The model not only reproduces well the radial profiles, but also the global observational data for the NGC 300 disk. Our results suggest that NGC 300 may experience a rapid growth of its disk. Through comparing the best-fitting, model-predicted SFH of NGC 300 with that of M 33, we find that the mean stellar age of NGC 300 is older than that of M 33 and there is a recent lack of primordial gas infall onto the disk of NGC 300. Our results also imply that the local environment may play a key role in the secular evolution of galaxy disks.

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The Abundance Properties of Nearby Late-Type Galaxies. I. The Data

Cited by 159 publications

References 216 publications

The oxygen abundance gradient in M81 and the robustness of abundance determinations in H ii regions

The oxygen abundance gradient in M81 and the robustness of abundance determinations in H ii regions

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

The star formation history of low-mass disk galaxies: A case study of NGC 300

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