Metals, depletion and dimming: decrypting dust

Tayyaba Zafar, Palle Møller

Research output: Contribution to journalArticleResearchpeer-review

Abstract

Dust plays a pivotal role in the chemical enrichment of the interstellar medium. In the era of mid-/high-resolution spectra and multiband spectral energy distributions, testing extinctions against gas and dust-phase properties is becoming possible. In order to test relations between metals, dust, and depletions, and comparing those to the Local Group (LG) relations, we build a sample of 93 γ-ray bursts and quasar absorbers (the largest sample so far) which have extinction and elemental column density measurements available. We find that extinctions and total column density of the volatile elements (Zn, S) are correlated [with a best fit of dust-to-metals (DTM) 4.05 × 10¯²² mag cm²] and consistent with the LG DTM relation. The refractory elements (Fe, Si) follow a similar, but less significant, relation offset about 1 dex from the LG relation. On the assumption that depletion on to dust grains is the cause, we compute the total (gas+dust-phase) column density and find a remarkable agreement with the LG DTM relation: a best fit of 4.91 × 10¯²² mag cm². We then use our results to compute the amount of ‘intervening metal from unknown sources’ in random sightlines out to redshifts of z = 5. Those metals implicate the presence of dust and give rise to an average ‘cosmic dust dimming’ effect that we express as a function of redshift, CDD(⁠z⁠). The CDD is unimportant out to redshifts of about 3, but because it is cumulative it becomes significant at redshifts z = 3–5. Our results in this paper are based on a minimum of assumptions and effectively relying on observations.
LanguageEnglish
Pages2731–2738
Number of pages8
JournalMonthly Notices of the Royal Astronomical Society
Volume482
Issue number2
DOIs
Publication statusPublished - Jan 2019

Fingerprint

dimming
depletion
dust
metal
metals
extinction
cosmic dust
volatile element
refractories
spectral energy distribution
gamma ray bursts
gases
quasars
gas
absorbers

Keywords

  • ISM: abundances
  • dust, extinction
  • galaxies: high-redshift
  • quasars: general

Cite this

Zafar, Tayyaba ; Møller, Palle. / Metals, depletion and dimming : decrypting dust. In: Monthly Notices of the Royal Astronomical Society. 2019 ; Vol. 482, No. 2. pp. 2731–2738.
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Metals, depletion and dimming : decrypting dust. / Zafar, Tayyaba; Møller, Palle.

In: Monthly Notices of the Royal Astronomical Society, Vol. 482, No. 2, 01.2019, p. 2731–2738.

Research output: Contribution to journalArticleResearchpeer-review

TY - JOUR

T1 - Metals, depletion and dimming

T2 - Monthly Notices of the Royal Astronomical Society

AU - Zafar, Tayyaba

AU - Møller, Palle

PY - 2019/1

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N2 - Dust plays a pivotal role in the chemical enrichment of the interstellar medium. In the era of mid-/high-resolution spectra and multiband spectral energy distributions, testing extinctions against gas and dust-phase properties is becoming possible. In order to test relations between metals, dust, and depletions, and comparing those to the Local Group (LG) relations, we build a sample of 93 γ-ray bursts and quasar absorbers (the largest sample so far) which have extinction and elemental column density measurements available. We find that extinctions and total column density of the volatile elements (Zn, S) are correlated [with a best fit of dust-to-metals (DTM) 4.05 × 10¯²² mag cm²] and consistent with the LG DTM relation. The refractory elements (Fe, Si) follow a similar, but less significant, relation offset about 1 dex from the LG relation. On the assumption that depletion on to dust grains is the cause, we compute the total (gas+dust-phase) column density and find a remarkable agreement with the LG DTM relation: a best fit of 4.91 × 10¯²² mag cm². We then use our results to compute the amount of ‘intervening metal from unknown sources’ in random sightlines out to redshifts of z = 5. Those metals implicate the presence of dust and give rise to an average ‘cosmic dust dimming’ effect that we express as a function of redshift, CDD(⁠z⁠). The CDD is unimportant out to redshifts of about 3, but because it is cumulative it becomes significant at redshifts z = 3–5. Our results in this paper are based on a minimum of assumptions and effectively relying on observations.

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KW - ISM: abundances

KW - dust, extinction

KW - galaxies: high-redshift

KW - quasars: general

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JO - Monthly Notices of the Royal Astronomical Society

JF - Monthly Notices of the Royal Astronomical Society

SN - 0035-8711

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ER -