Galactic chemical abundance evolution in the solar neighborhood up to the iron peak

Alibés, Andreu; Labay, J.; Canal, R.

doi:10.1051/0004-6361:20010296

Cited by 103 publications

(187 citation statements)

References 87 publications

(146 reference statements)

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“…Although this model is not the only one capable of reproducing the data, it does reproduce the majority of the Milky Way properties, and most of its assumptions are shared by other authors (e.g. Prantzos & Boissier 2000a;Alibés et al 2001;Chang et al 1999). By adopting this model for other spiral galaxies, most of the parameters are fixed by the observational constraints of the Milky Way.…”

Section: Models Of Spiral Galaxiesmentioning

confidence: 96%

Silicon depletion in damped Ly αsystems

Vladilo

Abate²,

Yin

et al. 2011

A&A

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Silicates are an important component of interstellar dust that has been poorly investigated in high redshift galaxies. As a preliminary step to studying silicates at high redshift, we survey silicon depletions in damped Ly α (DLA) systems. Silicon depletion is mild in the Galactic interstellar medium (ISM) and is expected to be weaker in most DLA systems, so we introduce a method for improving the accuracy of DLA depletion measurements. We compare abundance ratios measured in the gas with calculations of total abundance ratios of gas and dust predicted by models of galactic chemical evolution tailored for DLA systems. To tune the model parameters, we use the dust-free observational diagram S/Zn versus Zn/H, and we also compare the look back time estimated from the absorption redshift with the evolutionary time predicted by the model. By applying our method to a large set of DLA column densities, we succeeded in measuring the depletion of silicon in 74 systems. For comparison, we also measure iron and magnesium depletions (105 and 10 systems, respectively) with the same method. The mean depletion of silicon that we derive, δ Si −0.27 ± 0.16 dex, is surprisingly close to that of iron, δ Fe −0.42 ± 0.28 dex, despite iron being much more depleted than silicon in the Galactic ISM. Silicon depletion in DLA systems does not correlate with metallicity, at variance with iron depletion, for which we confirm a rise with [Fe/H] found in previous work. Magnesium depletion seems to behave more in accordance with silicon than with iron. The different behaviors of the silicon and iron depletions suggests a complex history of dust production at the early stages of galactic chemical evolution.

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Section: Models Of Spiral Galaxiesmentioning

confidence: 96%

Silicon depletion in damped Ly αsystems

Vladilo

Abate²,

Yin

et al. 2011

A&A

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“…That suggests the metallicity of the gas should be somewhat higher than solar. Using the Galactic abundance gradient values given by Alibés et al (2001), one may estimate the oxygen abundance as [O/H] 0.1 ÷ 0.2 (relative to the Solar value). For nitrogen the enrichment may be as high as [N/H] 0.2 ÷ 0.3 because its abundance scales non-linearly with metallicity and its gradients are generally steeper at higher metallicities (van Zee 1998).…”

Section: Abundancesmentioning

confidence: 99%

The Eastern filament of W50

Abolmasov¹,

Maryeva²,

Burenkov³

2010

Astron Nachr

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The dates of receipt and acceptance should be inserted later Key words ISM: individual (W50) -ISM: kinematics and dynamics -stars: individuals (SS433)We present new spectral (FPI and long-slit) data on the Eastern optical filament of the well known radionebula W50 associated with SS433. We find that on sub-parsec scales different emission lines are emitted by different regions with evidently different physical conditions. Kinematical properties of the ionized gas show evidence for moderately high (V ∼ 100 km s −1 ) supersonic motions. [O III]λ5007 emission is found to be multi-component and differs from lowerexcitation [S II]λ6717 line both in spatial and kinematical properties. Indirect evidence for very low characteristic densities of the gas (n ∼ 0.1 cm −3 ) is found. We propose radiative (possibly incomplete) shock waves in low-density, moderately high metallicity gas as the most probable candidate for the power source of the optical filament. Apparent nitrogen overabundance is better understood if the location of W50 in the Galaxy is taken into account.

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“…For the region covered by the Chandra observation, the abundances are close to solar for these elements. The nucleosynthetic studies of Timmes, Woosley, & Weaver (1995) and Alibés, Labay, & Canal (2001), which contain compendia of Galactic abundance data in the form of X/Fe as a function of Fe/H, can be used to link the observed species to those of interest for X-ray spectroscopy, e.g., Ca, Si, Fe, and Ni.…”

Section: Spectroscopymentioning

confidence: 99%

Diffuse X‐Ray Emission from M101

Küntz

Snowden

Pence

et al. 2003

ApJ

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The total 0.45-1.0 keV luminosity of M101 is 3:2 Â 10 39 ergs s À1 , of which 2:3 Â 10 39 ergs s À1 is due to diffuse emission. (Chandra observes only $60% of the diffuse emission observed by ROSAT because of its superior point-source detection.) Of the diffuse emission seen by Chandra, no more than 6% can be due to luminous unresolved point sources, such as X-ray binaries, and $10% is likely due to dwarf stars. The diffuse emission traces the spiral arms and is roughly correlated with the H and far-UV emission. The radial distribution closely follows the optical profile. The bulk of the diffuse emission is characterized by a two-thermal component spectrum with kT ¼ 0:20 and 0.75 keV, and the ratio of the emission measures of the two components is roughly constant as a function of both radius and surface brightness. The softer component has a sufficiently large covering factor that the bulk of the emission is likely extraplanar. We find no evidence of an extended axisymmetric X-ray halo, suggesting that any such halo has a strength much smaller than current predictions.

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Galactic chemical abundance evolution in the solar neighborhood up to the iron peak

Cited by 103 publications

References 87 publications

Silicon depletion in damped Ly αsystems

Silicon depletion in damped Ly αsystems

The Eastern filament of W50

Diffuse X‐Ray Emission from M101

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