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From the same journal

By the same authors

The relationship between dust and [C I] at z = 1 and beyond

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The relationship between dust and [C I] at z = 1 and beyond. / Bourne, N.; Dunlop, J.~S.; Simpson, J.~M.; Rowlands, K.~E.; Geach, J.~E.; McLeod, D.~J.

In: Monthly Notices of the Royal Astronomical Society, Vol. 482, No. 3, 01.01.2019, p. 3135-3161.

Research output: Contribution to journalArticle

Harvard

Bourne, N, Dunlop, JS, Simpson, JM, Rowlands, KE, Geach, JE & McLeod, DJ 2019, 'The relationship between dust and [C I] at z = 1 and beyond', Monthly Notices of the Royal Astronomical Society, vol. 482, no. 3, pp. 3135-3161. https://doi.org/10.1093/mnras/sty2773

APA

Bourne, N., Dunlop, J. S., Simpson, J. M., Rowlands, K. E., Geach, J. E., & McLeod, D. J. (2019). The relationship between dust and [C I] at z = 1 and beyond. Monthly Notices of the Royal Astronomical Society, 482(3), 3135-3161. https://doi.org/10.1093/mnras/sty2773

Vancouver

Author

Bourne, N. ; Dunlop, J.~S. ; Simpson, J.~M. ; Rowlands, K.~E. ; Geach, J.~E. ; McLeod, D.~J. / The relationship between dust and [C I] at z = 1 and beyond. In: Monthly Notices of the Royal Astronomical Society. 2019 ; Vol. 482, No. 3. pp. 3135-3161.

Bibtex

@article{6eb6c3f786d243d3a554ec4c4b7b0635,
title = "The relationship between dust and [C I] at z = 1 and beyond",
abstract = "Measuring molecular gas mass is vital for understanding the evolution of galaxies at high redshifts (z ≳ 1). Most measurements rely on CO as a tracer, but dependencies on metallicity, dynamics, and surface density lead to systematic uncertainties in high-z galaxies, where these physical properties are difficult to observe, and where the physical environments can differ systematically from those at z = 0. Dust continuum emission provides a potential alternative assuming a known dust/gas ratio, but this must be calibrated on a direct gas tracer at z ≳ 1. In this paper, we consider the [C I] 492-GHz emission line, which has been shown to trace molecular gas closely throughout Galactic clouds and has the advantages of being optically thin in typical conditions (unlike CO), and being observable at accessible frequencies at high redshifts (in contrast to the low-excitation lines of CO). We use the Atacama Large Millimetre/submillimetre Array to measure [C I], CO(4–3), and dust emission in a representative sample of star-forming galaxies at z = 1, and combine these data with multiwavelength spectral energy distributions to study relationships between dust and gas components of galaxies. We uncover a strong [C I]–dust correlation, suggesting that both trace similar phases of the gas. By incorporating other samples from the literature, we show that this correlation persists over a wide range of luminosities and redshifts up to z ∼ 4. Finally, we explore the implications of our results as an independent test of literature calibrations for dust as a tracer of gas mass, and for predicting the C I abundance.",
keywords = "Galaxies: evolution, Galaxies: ISM, Submillimetre: galaxies",
author = "N. Bourne and J.~S. Dunlop and J.~M. Simpson and K.~E. Rowlands and J.~E. Geach and D.~J. McLeod",
note = "{\textcopyright} 2018 The Author(s) Published by Oxford University Press on behalf of the Royal Astronomical Society.",
year = "2019",
month = jan,
day = "1",
doi = "10.1093/mnras/sty2773",
language = "English",
volume = "482",
pages = "3135--3161",
journal = "Monthly Notices of the Royal Astronomical Society",
issn = "0035-8711",
publisher = "Oxford University Press",
number = "3",

}

RIS

TY - JOUR

T1 - The relationship between dust and [C I] at z = 1 and beyond

AU - Bourne, N.

AU - Dunlop, J.~S.

AU - Simpson, J.~M.

AU - Rowlands, K.~E.

AU - Geach, J.~E.

AU - McLeod, D.~J.

N1 - © 2018 The Author(s) Published by Oxford University Press on behalf of the Royal Astronomical Society.

PY - 2019/1/1

Y1 - 2019/1/1

N2 - Measuring molecular gas mass is vital for understanding the evolution of galaxies at high redshifts (z ≳ 1). Most measurements rely on CO as a tracer, but dependencies on metallicity, dynamics, and surface density lead to systematic uncertainties in high-z galaxies, where these physical properties are difficult to observe, and where the physical environments can differ systematically from those at z = 0. Dust continuum emission provides a potential alternative assuming a known dust/gas ratio, but this must be calibrated on a direct gas tracer at z ≳ 1. In this paper, we consider the [C I] 492-GHz emission line, which has been shown to trace molecular gas closely throughout Galactic clouds and has the advantages of being optically thin in typical conditions (unlike CO), and being observable at accessible frequencies at high redshifts (in contrast to the low-excitation lines of CO). We use the Atacama Large Millimetre/submillimetre Array to measure [C I], CO(4–3), and dust emission in a representative sample of star-forming galaxies at z = 1, and combine these data with multiwavelength spectral energy distributions to study relationships between dust and gas components of galaxies. We uncover a strong [C I]–dust correlation, suggesting that both trace similar phases of the gas. By incorporating other samples from the literature, we show that this correlation persists over a wide range of luminosities and redshifts up to z ∼ 4. Finally, we explore the implications of our results as an independent test of literature calibrations for dust as a tracer of gas mass, and for predicting the C I abundance.

AB - Measuring molecular gas mass is vital for understanding the evolution of galaxies at high redshifts (z ≳ 1). Most measurements rely on CO as a tracer, but dependencies on metallicity, dynamics, and surface density lead to systematic uncertainties in high-z galaxies, where these physical properties are difficult to observe, and where the physical environments can differ systematically from those at z = 0. Dust continuum emission provides a potential alternative assuming a known dust/gas ratio, but this must be calibrated on a direct gas tracer at z ≳ 1. In this paper, we consider the [C I] 492-GHz emission line, which has been shown to trace molecular gas closely throughout Galactic clouds and has the advantages of being optically thin in typical conditions (unlike CO), and being observable at accessible frequencies at high redshifts (in contrast to the low-excitation lines of CO). We use the Atacama Large Millimetre/submillimetre Array to measure [C I], CO(4–3), and dust emission in a representative sample of star-forming galaxies at z = 1, and combine these data with multiwavelength spectral energy distributions to study relationships between dust and gas components of galaxies. We uncover a strong [C I]–dust correlation, suggesting that both trace similar phases of the gas. By incorporating other samples from the literature, we show that this correlation persists over a wide range of luminosities and redshifts up to z ∼ 4. Finally, we explore the implications of our results as an independent test of literature calibrations for dust as a tracer of gas mass, and for predicting the C I abundance.

KW - Galaxies: evolution

KW - Galaxies: ISM

KW - Submillimetre: galaxies

UR - http://www.scopus.com/inward/record.url?scp=85066952181&partnerID=8YFLogxK

U2 - 10.1093/mnras/sty2773

DO - 10.1093/mnras/sty2773

M3 - Article

VL - 482

SP - 3135

EP - 3161

JO - Monthly Notices of the Royal Astronomical Society

JF - Monthly Notices of the Royal Astronomical Society

SN - 0035-8711

IS - 3

ER -