A UNIFIED REPRESENTATION OF GAS-PHASE ELEMENT DEPLETIONS IN THE INTERSTELLAR MEDIUM

By E. Jenkins. 2009

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A study of gas-phase element abundances reported in the literature for 17 different elements sampled over 243 sight lines in the local part of our Galaxy reveals that the depletions into solid form (dust grains) are extremely well characterized by trends that employ only three kinds of parameters. One is an index that describes the overall level of depletion applicable to the gas in any particular sight line, and the other two represent linear coefficients that describe how to derive each element's depletion from this sight-line parameter. The information from this study reveals the relative proportions of different elements that are incorporated into dust at different stages of grain growth. An extremely simple scheme is proposed for deriving the dust contents and metallicities of absorption-line systems that are seen in the spectra of distant quasars or the optical afterglows of gamma-ray bursts. Contrary to presently accepted thinking, the elements sulfur and krypton appear to show measurable changes in their depletions as the general levels of depletions of other elements increase, although more data are needed to ascertain whether or not these findings are truly compelling. Nitrogen appears to show no such increase. The incorporation of oxygen into solid form in the densest gas regions far exceeds the amounts that can take the form of silicates or metallic oxides; this conclusion is based on differential measurements of depletion and thus is unaffected by uncertainties in the solar abundance reference scale.

Subfields: Astronomy and Astrophysics, Instrumentation

View Paper: https://www.semanticscholar.org/paper/d0b91821977b5709e1b634ff27fb24a85ec5d8ae

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Citations in the corpus

On the reservoir of sulphur in dark clouds : chemistry and elemental abundance reconciled (2017, background): “…desorption of species from the grain surface into the gas-phase, and the surface-bulk and bulk-surface ex- (1) Wakelam & Herbst (2008), (2) Jenkins (2009), (3) Hincelin et al. (2011), (4) Low-metal abundances from Graedel et al. (1982), (5) Depleted value from Neufeld et al.…”
RECONCILING THE STELLAR AND NEBULAR SPECTRA OF HIGH-REDSHIFT GALAXIES (2016, background): “Assuming gas-phase depletion [Si/H]gas = −0.63, the depletion expected for the other elements can be calculated from the fits given by Jenkins (2009) with the parameter F∗ = 0.36± 0.09 (see his equation 10 and Table 4) determined from Si: [O/H]gas ' −0.09, [C/H]gas ' −0.15, [N/H]gas ' −0.11, and…”
De re metallica: the cosmic chemical evolution of galaxies (2018, background): “Cosmic chemical evolution of galaxies 37 Extensive studies and reviews on the dust depletion patterns and dust properties have been published (e.g., Savage & Sembach, 1996; Draine, 2003; Jenkins, 2009; De Cia et al., 2016; Galliano et al., 2018) and an extensive discussion goes beyond this paper.”
A BUDGET AND ACCOUNTING OF METALS AT z ∼ 0: RESULTS FROM THE COS-HALOS SURVEY (2013, background): “We note that observational constraints on the oxygen mass fraction of dust from oxygen dust depletions are difficult to reconcile with chemical models (Sofia & Meyer 2001; Draine 2003; Jenkins 2009; Whittet 2010).”
THE PERSISTENCE OF COOL GALACTIC WINDS IN HIGH STELLAR MASS GALAXIES BETWEEN z ∼ 1.4 AND ∼1 (2009, background): “Assuming solar abundance, no ionization correction and a factor of −2.3 dex depletion onto dust (Jenkins 2009), we obtain log N (H) ∼ 20.3–20.7, which is nearly a factor of 10 higher than our constraint on the column from analysis of Mg ii.”
Gas and grain chemical composition in cold cores as predicted by the Nautilus three-phase model (2016, background): “MNRAS 000, 1–14 (2015) The Nautilus 3-phase model 5 (1) see discussion in Wakelam & Herbst (2008), (2) Jenkins (2009), (3) see discussion in Hincelin et al. (2011), (4) low metal abundance from Graedel et al. (1982), (5) Depleted value from Neufeld et al. (2005). as Hama et al. (2012) for H atoms…”
THE MASS–METALLICITY RELATION WITH THE DIRECT METHOD ON STACKED SPECTRA OF SDSS GALAXIES (2012, background): “Second, the fraction of metals depleted onto dust grains is poorly constrained by observations (see Draine 2003; Jenkins 2009) but is a required parameter of the photoionization models.”
Chemical abundances in high-redshift galaxies: a powerful new emission line diagnostic (2016, methodology): “The depletion factors of the heavy elements onto dust are derived from the formulae of Jenkins (2009), extended to the other elements on the basis of condensation temperatures and/or position on the periodic table.”
THE CO-TO-H2 CONVERSION FACTOR FROM INFRARED DUST EMISSION ACROSS THE LOCAL GROUP (2011, background): “The depletion of heavy elements from the gas phase increases with increasing density (Jenkins 2009), though absorption measurements cannot probe to very high densities.”
EVIDENCE FOR UBIQUITOUS COLLIMATED GALACTIC-SCALE OUTFLOWS ALONG THE STAR-FORMING SEQUENCE AT z ∼ 0.5 (2013, methodology): “Adopting conservative dust depletion factors consistent with those measured in the local Galactic ISM (+0.5 dex for Mg and +1.0 dex for Fe; Jenkins 2009), and assuming solar abundance ratios and no ionization correction, this limit implies Nflow(Fe II)< 1017.5 cm−2 and Nflow(Mg II)< 10 18.0 cm−2.”
Cool outflows in galaxies and their implications (2020, background): “…and Susanne Aalto6 HI 21-cm observations have a finite beam and the UV observations are effectively infinitesimal, beam-smearing corrections must be applied to take into account potential small-scale structure in the H I beam (e.g., Walter et al. 2017; Jenkins 2009; Bordoloi et al. 2017b).”
Observations of the Icy Universe (2015, background): “Even larger grains have been suggested as a source of the “missing” oxygen (§6.6; Jenkins 2009), because their infrared absorption profiles become too wide and shallow to be detected.”
Sulphur-bearing species in the coma of comet 67P/Churyumov–Gerasimenko (2016, background): “…of 1000 relative to its cosmic abundance (Penzias et al. 1971; Tieftrunk et al. 1994) whereas in the diffuse interstellar medium (ISM) it is present with its cosmic abundance relative to oxygen of ∼1/37 (Savage & Sembach 1996; Garcı́a-Rojas et al. 2006; Howk, Sembach & Savage 2006; Jenkins 2009).”
Interstellar Mapping and Acceleration Probe (IMAP): A New NASA Mission (2018, background): “The D/H ratio provides input on stellar evolution, and its contribution to the local matter inventory and the Ne/O ratio has ramifications on the balance between volatile and refractory elements (e.g., Jenkins 2009), which requires observation of gas phase and dust composition in the LISM.”