Elemental Depletions in the Magellanic Clouds and the Evolution of Depletions With Metallicity

Tchernyshyov, Kirill; Meixner, Margaret; Seale, Jonathan; Fox, Andrew; Friedman, S. D.; Dwek, Eli; Galliano, F.

doi:10.1088/0004-637x/811/2/78

Cited by 56 publications

(120 citation statements)

References 78 publications

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“…The values derived from latertype giants and supergiants may be slightly higher than those obtained from H II regions and earlier-type stars, however. Our adopted values (7.95 dex for the LMC and 7.45 dex for the SMC) are consistent with several other recent estimates also based on values compiled from studies of different kinds of objects (e.g., Hunter et al 2007;Salmon et al 2012;Tchernyshyov et al 2015). Those adopted values are about 0.2 dex lower, relative to solar abundances, than the values obtained for most heavier elements-which are typically about −0.3 dex for the LMC and about −0.7 dex for the SMC (largely from the same references).…”

Section: Appendix C Galactic Column Densitiessupporting

confidence: 91%

“…All seven sight lines have been observed with both HST/STIS and FUSE in the UV-yielding column densities for both H and H 2 Cartledge et al 2005;Welty et al 2012;R. Xue et al 2016, in preparation) and for various atomic and molecular species (Friedman et al 2000;Welty et al , 2004André et al 2004;Sofia et al 2006;Tchernyshyov et al 2015;D. E. Welty et al 2016, in preparation).…”

Section: Sight Linesmentioning

confidence: 96%

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Thermal Pressures in the Interstellar Medium of the Magellanic Clouds*

Welty

Lauroesch

Wong

et al. 2016

ApJ

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We discuss the thermal pressures (n H T) in predominantly cold, neutral interstellar gas in the Magellanic Clouds, derived from analyses of the fine-structure excitation of neutral carbon, as seen in high-resolution Hubble Space Telescope/Space Telescope Imaging Spectrograph spectra of seven diverse sight lines in the LMC and SMC. Detailed fits to the line profiles of the absorption from C I, C I * , and C I ** yield consistent column densities for the three to six C I multiplets detected in each sight line. In the LMC and SMC, N(C I tot ) is consistent with Galactic trends versus N(Na I) and N(CH), but is slightly lower versus N(K I) and N(H 2 ). As for N(Na I) and N(K I), N(C I tot ) is generally significantly lower, for a given N(H tot ), in the LMC and (especially) in the SMC, compared to the local Galactic relationship. For the LMC and SMC components with well-determined column densities for C I, C I * , and C I ** , the derived thermal pressures are typically factors of a few higher than the values found for most cold, neutral clouds in the Galactic ISM. Such differences are consistent with the predictions of models for clouds in systems (like the LMC and SMC) that are characterized by lower metallicities, lower dust-to-gas ratios, and enhanced radiation fields-where higher pressures are required for stable cold, neutral clouds. The pressures may be further enhanced by energetic activity (e.g., due to stellar winds, star formation, and/or supernova remnants) in several of the regions probed by these sight lines. Comparisons are made with the C I observed in some quasar absorption-line systems.

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Section: Appendix C Galactic Column Densitiessupporting

confidence: 91%

Section: Sight Linesmentioning

confidence: 96%

Thermal Pressures in the Interstellar Medium of the Magellanic Clouds*

Welty

Lauroesch

Wong

et al. 2016

ApJ

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“…We compare some of our results with the recent work of Tchernyshyov et al (2015) on the abundances and dust depletion in the Small Magellanic Cloud (SMC) and Large Magellanic Cloud (LMC). We test whether the observed relative abundances in the SMC and LMC are consistent with our sequences of relative abundances.…”

Section: Appendix D: Comparison With the Depletion In The Magellanic mentioning

confidence: 66%

“…We compare our results with the abundances and depletion δ X derived by Tchernyshyov et al (2015) for the Magellanic Clouds (MC; see Appendix D). We find that the relative abundances in the MC are consistent with the sequences of relative abundances that we found for DLAs and the Galaxy.…”

Section: Dust Depletionmentioning

confidence: 92%

“…Thus, a first possible interpretation of the mere existence of the sequences of relative abundances, from DLAs to the Galaxy, is that grain growth in the ISM must be an important process of dust formation. The dust fraction and the level of depletion varies significantly even within a galaxy, and this is likely because of dust condensation in the ISM (Jenkins 2009;Mattsson et al 2014b;Tchernyshyov et al 2015). Furthermore, the sequences of observed relative abundances are continuous in [Zn/Fe] all the way from DLAs to Galactic absorbers.…”

Section: Dust Depletionmentioning

confidence: 99%

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Dust-depletion sequences in damped Lyman-αabsorbers

Ledoux

Mattsson

et al. 2016

A&A

160

186

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We study metal depletion due to dust in the interstellar medium (ISM) to infer the properties of dust grains and characterize the metal and dust content of galaxies down to low metallicity and intermediate redshift z. We provide metal column densities and abundances of a sample of 70 damped Lyman-α absorbers (DLAs) towards quasars, observed at high spectral resolution with the Very Large Telescope (VLT) Ultraviolet and Visual Echelle Spectrograph (UVES). This is the largest sample of phosphorus abundances measured in DLAs so far. We use literature measurements for Galactic clouds to cover the high-metallicity end. We discover tight (scatter 0.2 dex) correlations between [Zn/Fe] and the observed relative abundances from dust depletion. This implies that grain growth in the ISM is an important process of dust production. These sequences are continuous in [Zn/Fe] from dust-free to dusty DLAs, and to Galactic clouds, suggesting that the availability of refractory metals in the ISM is crucial for dust production, regardless of the star formation history. We observe [S/Zn] up to ∼ 0.25 dex in DLAs, which is broadly consistent with Galactic stellar abundances. Furthermore, we find a good agreement between the nucleosynthetic pattern of Galactic halo stars and our observations of the least dusty DLAs. This supports recent star formation in low-metallicity DLAs. The derived depletions of Zn, O, P, S, Si, Mg, Mn, Cr, and Fe correlate with [Zn/Fe], with steeper slopes for more refractory elements. P is mostly not affected by dust depletion. We present canonical depletion patterns to be used as reference in future studies of relative abundances and depletion. We derive the total (dust-corrected) metallicity, typically −2 [M/H] tot 0 for DLAs, and scattered around solar metallicity for the Galactic ISM. The dust-to-metal ratio (DTM) increases with metallicity, again supporting the importance of grain growth for dust production. The dust extinction A V derived from the depletion is typically < 0.2 mag in DLAs. Finally, we derive elemental abundances in dust, which is key to understanding the dust composition and its evolution. We observe similar abundances of Mg, Si, and Fe in dust; this suggests that grain species such as pyroxenes and iron oxides are more important than olivine, but this needs to be confirmed by more detailed analysis. Overall, we characterize dust depletion, nucleosynthesis, and dust-corrected metallicity in DLAs, providing a unified picture from low-metallicity systems to the Galactic ISM.

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The formation and cosmic evolution of dust in the early Universe: I. Dust sources

Schneider,

Maiolino

2024

Astron Astrophys Rev

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Dust-obscured star formation has dominated the cosmic history of star formation, since $$z \simeq 4$$ z ≃ 4 . However, the recent finding of significant amount of dust in galaxies out to $$z \simeq 8$$ z ≃ 8 has opened the new frontier of investigating the origin of dust also in the earliest phases of galaxy formation, within the first 1.5 billion years from the Big Bang. This is a key and rapid transition phase for the evolution of dust, as galaxy evolutionary timescales become comparable with the formation timescales of dust. It is also an area of research that is experiencing an impressive growth, especially thanks to the recent results from cutting edge observing facilities, ground-based, and in space. Our aim is to provide an overview of the several findings on dust formation and evolution at $$z > 4$$ z > 4 , and of the theoretical efforts to explain the observational results. We have organized the review in two parts. In the first part, presented here, we focus on dust sources, primarily supernovae and asymptotic giant branch stars, and the subsequent reprocessing of dust in the interstellar medium, through grain destruction and growth. We also discuss other dust production mechanisms, such as Red Super Giants, Wolf–Rayet stars, Classical Novae, Type Ia Supernovae, and dust formation in quasar winds. The focus of this first part is on theoretical models of dust production sources, although we also discuss the comparison with observations in the nearby Universe, which are key to put constraints on individual sources and processes. While the description has a general applicability at any redshift, we emphasize the relative role of different sources in the dust build-up in the early Universe. In the second part, which will be published later on, we will focus on the recent observational results at $$z > 4$$ z > 4 , discussing the theoretical models that have been proposed to interpret those results, as well as the profound implications for galaxy formation.

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Elemental Depletions in the Magellanic Clouds and the Evolution of Depletions With Metallicity

Cited by 56 publications

References 78 publications

Thermal Pressures in the Interstellar Medium of the Magellanic Clouds*

Thermal Pressures in the Interstellar Medium of the Magellanic Clouds*

Dust-depletion sequences in damped Lyman-αabsorbers

The formation and cosmic evolution of dust in the early Universe: I. Dust sources

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