The<i>Gaia</i>-ESO Survey: Galactic evolution of sulphur and zinc

Duffau, S.; Caffau, E.; Sbordone, L.; Bonifacio, P.; Andrievsky, S. M.; Коротин, С. А.; Babusiaux, C.; Salvadori, Stefania; Monaco, L.; François, P.; Skúladóttir, Ása; Bragaglia, A.; Donati, P.; Spina, L.; Gallagher, A. J.; Ludwig, H.‐G.; Christlieb, N.; Hansen, C. J.; Mott, A.; Steffen, M.; Zaggia, S.; Blanco-Cuaresma, S.; Calura, F.; Friel, Eileen D.; Jiménez-Esteban, F. M.; Koch, Andreas; Magrini, L.; Pancino, E.; Bin, Tang; Tautvaišienė, G.; Vallenari, A.; Hawkins, Keith; Gilmore, G.; Randich, S.; Feltzing, Sofia; Bensby, T.; Flaccomio, E.; Smiljanić, R.; Bayo, A.; Carraro, G.; Casey, Andrew R.; Costado, M. T.; Damiani, F.; Franciosini, E.; Hourihane, A.; Jofré, P.; Lardo, C.; Lewis, Jim; Morbidelli, L.; Sousa, S.; Worley, C. C.

doi:10.1051/0004-6361/201730477

Cited by 44 publications

(22 citation statements)

References 133 publications

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“…As previously said, there are no S abundance determination from GALAH and we assume that it scales as Si as shown in Chen et al (2002). The same trend is present in several studies (Caffau et al 2005;Jönsson et al 2011;Takeda et al 2016;Duffau et al 2017) regarding dwarfs and giants, reassuring us to scale S with the Si abundance trends.…”

Section: Stellar Abundancessupporting

confidence: 81%

Influence of sub- and super-solar metallicities on the composition of solid planetary building blocks

Bitsch

Battistini

2019

A&A

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The composition of the protoplanetary disc is thought to be linked to the composition of the host star, where a higher overall metallicity of the host star provides more building blocks for planets. However, most of the planet formation simulations only link the stellar iron abundance [Fe/H] to planet formation and the iron abundance in itself is used as a proxy to scale all elements. On the other hand, large surveys of stellar abundances show that this is not true. We use here stellar abundances from the GALAH surveys to determine the average detailed abundances of Fe, Si, Mg, O, and C for a broad range of host star metallicities with [Fe/H] spanning from -0.4 to +0.4. Using an equilibrium chemical model that features the most important rock forming molecules as well as volatile contributions of H 2 O, CO 2 , CH 4 and CO, we calculate the chemical composition of solid planetary building blocks around stars with different metallicities. Solid building blocks that are formed entirely interior to the water ice line (T>150K) only show an increase in Mg 2 SiO 4 and a decrease in MgSiO 3 for increasing host star metallicity, related to the increase of Mg/Si for higher [Fe/H]. Solid planetary building blocks forming exterior to the water ice line (T<150K), on the other hand, show dramatic changes in their composition. In particular the water ice content decreases from around ∼50% at [Fe/H]=-0.4 to ∼6% at [Fe/H]=0.4 in our chemical model. This is mainly caused by the increasing C/O ratio with increasing [Fe/H], which binds most of the oxygen in gaseous CO and CO 2 , resulting in a small water ice fraction. Planet formation simulations coupled with the chemical model confirm these results by showing that the water ice content of super-Earths decreases with increasing host star metallicity due to the increased C/O ratio. This decrease of the water ice fraction has important consequences for planet formation, planetary composition and the eventual habitability of planetary systems formed around these high metallicity stars.

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Section: Stellar Abundancessupporting

confidence: 81%

Influence of sub- and super-solar metallicities on the composition of solid planetary building blocks

Bitsch

Battistini

2019

A&A

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“…Recent measurements of zinc and iron abundances for individual red giant branch stars in the Milky Way (Duffau et al 2017;Barbuy et al 2015) and in nearby dwarf galaxies (Skúladóttir et al 2017(Skúladóttir et al , 2018 The analytical calculations presented in the above papers to explain the observed trends, suggest that supernovae Ia (SNIa) can be responsible of such unusual low [Zn/Fe] ratio. Indeed, SNIa produce large amount of iron with respect to zinc.…”

Section: Is There a Degeneracy With The Snia Imprint?mentioning

confidence: 96%

“…To address these issues we estimate the possible chemical enrichment paths of an ISM imprinted by normal Pop II stars exploding as both core-collapse SN (SNII) and supernovae Ia (SNIa), thus adopting a very similar approach of that developed by Duffau et al (2017) and Skúladóttir et al (2017). To avoid including the unknown contribution from primordial stars to the chemical enrichment, we assume an initial ISM composition equal to the average abundance pattern of "normal" Galactic halo stars at [Fe/H] ≈ −3 (Cayrel et al 2004;Yong et al 2013).…”

Section: Is There a Degeneracy With The Snia Imprint?mentioning

confidence: 99%

Probing the existence of very massive first stars

Salvadori

Bonifacio

Caffau

et al. 2019

Monthly Notices of the Royal Astronomical Society

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We present a novel approach aimed at identifying the key chemical elements to search for the (missing) descendants of very massive first stars exploding as Pair Instability Supernovae (PISN). Our simple and general method consists in a parametric study accounting for the unknowns related to early cosmic star-formation and metalenrichment. Our approach allow us to define the most likely [Fe/H] and abundance ratios of long-lived stars born in inter-stellar media polluted by the nucleosynthetic products of PISN at a > 90%, 70%, and 50% level. In agreement with previous works, we show that the descendants of very massive first stars can be most likely found at [Fe/H]≈ −2. Further, we demonstrate that to search for an under-abundance of [(N, Cu, Zn)/Fe]< 0 is the key to identify these rare descendants. The "killing elements" N, Zn, and Cu are not produced by PISN, so that their sub-Solar abundance with respect to iron persists in environments polluted by further generations of normal core-collapse supernovae up to a 50% level. We show that the star BD +80 • 245, which has [Fe/H]= −2.2, [N/Fe]= −0.79, [Cu/Fe]= −0.75, and [Zn/Fe]= −0.12 can be the smoking gun of the chemical imprint from very massive first stars. To this end we acquired new spectra for BD +80 • 245 and re-analysed those available from the literature accounting for Non-Local Thermodynamic Equilibrium corrections for Cu. We discuss how to find more of these missing descendants in ongoing and future surveys to tightly constrain the mass distribution of the first stars.

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“…In fact, in a broad range of the metallicity down to [Fe/H] ≃ −2 dex, Zn in stars in the solar neighborhood shows a concentration around [Zn/Fe]= 0 and thus seems to be created along with Fe and other iron peak elements (Sneden et al 1991). However, it has become clear that systematic differences in the [Zn/Fe] trends are found in different systems (thin and thick disks, bulge, halo, and dwarf galaxies) thanks to the efforts of various authors (Duffau et al 2017;Ji & Frebel 2018;Hirai et al 2018, and references therein). The origins of Zn remain still elusive and its implication to the Galactic chemical evolution may be unique compared with other betterunderstood elements (see, e.g., Tsujimoto & Nishimura 2018).…”

Section: Astronomical Implicationsmentioning

confidence: 99%

Identification of Absorption Lines of Heavy Metals in the Wavelength Range 0.97–1.32 μm

Matsunaga

Taniguchi

Jian

et al. 2020

ApJS

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Stellar absorption lines of heavy elements can give us various insights into the chemical evolution of the Galaxy and nearby galaxies. Recently developed spectrographs for the near-infrared wavelengths are becoming more and more powerful for producing a large number of high-quality spectra, but identification and characterization of the absorption lines in the infrared range remain to be fulfilled. We searched for lines of the elements heavier than the iron group, i.e., those heavier than Ni, in the Y (9760-11100Å) and J (11600-13200Å) bands. We considered the lines in three catalogs, i.e., Vienna Atomic Line Database (VALD), the compilation by R. Kurucz, and the list published in 1999 by Meléndez & Barbuy. Candidate lines were selected based on synthetic spectra and the confirmation was done by using WINERED spectra of 13 supergiants and giants within FGK spectral types (spanning 4000-7200 K in the effective temperature). We have detected lines of Zn I, Sr II, Y II, Zr I, Ba II, Sm II, Eu II, and Dy II, in the order of atomic number. Although the number of the lines is small, 23 in total, they are potentially useful diagnostic lines of the Galactic chemical evolution, especially in the regions for which interstellar extinction hampers detailed chemical analyses with spectra in shorter wavelengths. We also report the detection of lines whose presence was not predicted by the synthetic spectra created with the above three line lists.

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TheGaia-ESO Survey: Galactic evolution of sulphur and zinc

Cited by 44 publications

References 133 publications

Influence of sub- and super-solar metallicities on the composition of solid planetary building blocks

Influence of sub- and super-solar metallicities on the composition of solid planetary building blocks

Probing the existence of very massive first stars

Identification of Absorption Lines of Heavy Metals in the Wavelength Range 0.97–1.32 μm

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