The Galactic chemical evolution of oxygen inferred from 3D non-LTE spectral-line-formation calculations

Amarsi, A. M.; Asplund, Martin; Collet, Remo; Leenaarts, J.

doi:10.1093/mnrasl/slv122

Cited by 58 publications

(66 citation statements)

References 53 publications

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“…In all the distributions of Fig. 3 The values of Z from pEW 5018 cover a wider range than those from LZ and LCZ (see Amarsi et al 2015). Therefore, SNe with low pEW 5018 will be found at higher hostgalaxy Z (based on O abundance) than expected from the models based on Fe abundance, and vice versa.…”

Section: Analysis and Resultsmentioning

confidence: 84%

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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Section: Analysis and Resultsmentioning

confidence: 84%

Metallicity from Type II supernovae from the (i)PTF

Taddia

Moquist

Sollerman

et al. 2016

A&A

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“…If the trend of increasing [O/Fe] with decreasing [Fe/H] that has been found for metal-poor field stars in the Galaxy (e.g., Amarsi et al 2015;Dobrovolskas et al 2015) is applicable to GCs, then stars in a GC with low …”

Section: Fobe Effmentioning

confidence: 95%

Constraints on the Distance Moduli, Helium, and Metal Abundances, and Ages of Globular Clusters from Their RR Lyrae and Non-variable Horizontal Branch Stars. II. Multiple Stellar Populations in 47 Tuc, M3, and M13

Denissenkov

VandenBerg

Kopacki

et al. 2017

ApJ

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We present a new set of horizontal-branch (HB) models computed with the MESA stellar evolution code. The models adopt α-enhanced Asplund et al. (2009) 6 Gyr, whereas M 13 has ∆Y 0 ∼ 0.08 and (m − M ) V = 14.42, implying an age of 12.9 Gyr. Mass loss during giant-branch evolution and ∆Y 0 appear to be the primary second parameters for M 3 and M 13. New observations for 7 of the 9 known RR Lyrae in M 13 are also reported. Surprisingly, periods predicted for the c-type variables tend to be too high (by up to ∼ 0.1 d).

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“…The existence of primary nitrogen has been questioned for stellar spectra (Asplund 2005), but the nebular data consistently appear to follow the primary/secondary trend (see Vila Costas & Edmunds (1993); Amarsi et al (2015), the most carefully and consistently reduced stellar oxygen data available. The adopted piece-wise linear fit is shown as a red line, and the standard (GC) metallicity (fiducial point) as a yellow circle.…”

Section: Carbon and Nitrogenmentioning

confidence: 99%

“…Mid-and right panels show the stellar data for Mg and Si. Sources: (Amarsi et al 2015, O, blue and black points) (Ruchti et al 2011, Mg, Si, dark green), (Adibekyan et al 2012, Mg, Si, grey), (González Hernández et al 2013, Mg, Si, orange), (Bensby et al 2014, Mg, Si, blue discs), (Hinkel et al 2014, Mg, Si, purple), (Howes et al 2015, Mg, Si, red circles) , Si, blue circles) Dopita et al (2000); Groves et al (2004); Dopita et al (2013), and Izotov & Thuan (1999)), so we accept this model as a useful description of the scaling behaviour of nitrogen. The observed dispersion in the values of log(N/O), especially at low metallicity, are discussed in Gavilán et al (2006).…”

Section: Carbon and Nitrogenmentioning

confidence: 99%

Abundance scaling in stars, nebulae and galaxies

Nicholls¹,

Sutherland²,

Dopita³

et al. 2016

Mon. Not. R. Astron. Soc.

116

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We present a new basis for scaling abundances with total metallicity in nebular photoionisation models, based on extensive Milky Way stellar abundance data, to replace the uniform scaling normally used in the analysis of H ii regions. Our goal is to provide a single scaling method and local abundance reference standard for use in nebular modelling and its key inputs, the stellar atmosphere and evolutionary track models. We introduce a parametric enrichment factor, ζ, to describe how atomic abundances scale with total abundance, and which allows for a simple conversion between scales based on different reference elements (usually oxygen or iron) . The models and parametric description provide a more physically realistic approach than simple uniform abundance scaling. With appropriate parameters, the methods described here may be applied to H ii regions in the Milky Way, large and dwarf galaxies in the local universe, Active Galactic Nuclei (AGNs), and to star forming regions at high redshift.

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The Galactic chemical evolution of oxygen inferred from 3D non-LTE spectral-line-formation calculations

Cited by 58 publications

References 53 publications

Metallicity from Type II supernovae from the (i)PTF

Metallicity from Type II supernovae from the (i)PTF

Constraints on the Distance Moduli, Helium, and Metal Abundances, and Ages of Globular Clusters from Their RR Lyrae and Non-variable Horizontal Branch Stars. II. Multiple Stellar Populations in 47 Tuc, M3, and M13

Abundance scaling in stars, nebulae and galaxies

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