Probing cosmic dawn with emission lines: predicting infrared and nebular line emission for ALMA and JWST

Harley Katz, Thomas P. Galligan, Taysun Kimm, Joakim Rosdahl, Martin G. Haehnelt, Jeremy Blaizot, Julien Devriendt, Adrianne Slyz, Nicolas Laporte, Richard Ellis

Research output: Contribution to journalArticle

1 Citation (Scopus)

Abstract

Infrared and nebular lines provide some of our best probes of the physics regulating the properties of the interstellar medium (ISM) at high redshift. However, interpreting the physical conditions of high-redshift galaxies directly from emission lines remains complicated due to inhomogeneities in temperature, density, metallicity, ionization parameter, and spectral hardness. We present a new suite of cosmological, radiation-hydrodynamics simulations, each centred on a massive Lyman-break galaxy that resolves such properties in an inhomogeneous ISM. Many of the simulated systems exhibit transient but well-defined gaseous discs that appear as velocity gradients in [C ii] 157.6 μ m emission. Spatial and spectral offsets between [C ii] 157.6 μ m and [O iii] 88.33 μ m are common, but not ubiquitous, as each line probes a different phase of the ISM. These systems fall on the local [C ii]-SFR relation, consistent with newer observations that question previously observed [C ii] 157.6 μ m deficits. Our galaxies are consistent with the nebular line properties of observed z ∼2-3 galaxies and reproduce offsets on the BPT and mass-excitation diagrams compared to local galaxies due to higher star formation rate (SFR), excitation, and specific-SFR, as well as harder spectra from young, metal-poor binaries. We predict that local calibrations between H α and [O ii] 3727 A luminosity and galaxy SFR apply up to z > 10, as do the local relations between certain strong line diagnostics (R23 and [O iii] 5007 A /H β) and galaxy metallicity. Our new simulations are well suited to interpret the observations of line emission from current (ALMA and HST) and upcoming facilities (JWST and ngVLA).

Original languageEnglish
Pages (from-to)5902-5921
Number of pages20
JournalMonthly Notices of the Royal Astronomical Society
Volume487
Issue number4
DOIs
Publication statusPublished - 2019 Jun 25

Fingerprint

James Webb Space Telescope
galaxies
star formation rate
probe
metallicity
inhomogeneity
hardness
simulation
ionization
physics
hydrodynamics
diagram
calibration
probes
rate
metal
excitation
diagrams
luminosity
temperature

All Science Journal Classification (ASJC) codes

  • Astronomy and Astrophysics
  • Space and Planetary Science

Cite this

Katz, Harley ; Galligan, Thomas P. ; Kimm, Taysun ; Rosdahl, Joakim ; Haehnelt, Martin G. ; Blaizot, Jeremy ; Devriendt, Julien ; Slyz, Adrianne ; Laporte, Nicolas ; Ellis, Richard. / Probing cosmic dawn with emission lines : predicting infrared and nebular line emission for ALMA and JWST. In: Monthly Notices of the Royal Astronomical Society. 2019 ; Vol. 487, No. 4. pp. 5902-5921.
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title = "Probing cosmic dawn with emission lines: predicting infrared and nebular line emission for ALMA and JWST",
abstract = "Infrared and nebular lines provide some of our best probes of the physics regulating the properties of the interstellar medium (ISM) at high redshift. However, interpreting the physical conditions of high-redshift galaxies directly from emission lines remains complicated due to inhomogeneities in temperature, density, metallicity, ionization parameter, and spectral hardness. We present a new suite of cosmological, radiation-hydrodynamics simulations, each centred on a massive Lyman-break galaxy that resolves such properties in an inhomogeneous ISM. Many of the simulated systems exhibit transient but well-defined gaseous discs that appear as velocity gradients in [C ii] 157.6 μ m emission. Spatial and spectral offsets between [C ii] 157.6 μ m and [O iii] 88.33 μ m are common, but not ubiquitous, as each line probes a different phase of the ISM. These systems fall on the local [C ii]-SFR relation, consistent with newer observations that question previously observed [C ii] 157.6 μ m deficits. Our galaxies are consistent with the nebular line properties of observed z ∼2-3 galaxies and reproduce offsets on the BPT and mass-excitation diagrams compared to local galaxies due to higher star formation rate (SFR), excitation, and specific-SFR, as well as harder spectra from young, metal-poor binaries. We predict that local calibrations between H α and [O ii] 3727 A luminosity and galaxy SFR apply up to z > 10, as do the local relations between certain strong line diagnostics (R23 and [O iii] 5007 A /H β) and galaxy metallicity. Our new simulations are well suited to interpret the observations of line emission from current (ALMA and HST) and upcoming facilities (JWST and ngVLA).",
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Katz, H, Galligan, TP, Kimm, T, Rosdahl, J, Haehnelt, MG, Blaizot, J, Devriendt, J, Slyz, A, Laporte, N & Ellis, R 2019, 'Probing cosmic dawn with emission lines: predicting infrared and nebular line emission for ALMA and JWST', Monthly Notices of the Royal Astronomical Society, vol. 487, no. 4, pp. 5902-5921. https://doi.org/10.1093/mnras/stz1672

Probing cosmic dawn with emission lines : predicting infrared and nebular line emission for ALMA and JWST. / Katz, Harley; Galligan, Thomas P.; Kimm, Taysun; Rosdahl, Joakim; Haehnelt, Martin G.; Blaizot, Jeremy; Devriendt, Julien; Slyz, Adrianne; Laporte, Nicolas; Ellis, Richard.

In: Monthly Notices of the Royal Astronomical Society, Vol. 487, No. 4, 25.06.2019, p. 5902-5921.

Research output: Contribution to journalArticle

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T1 - Probing cosmic dawn with emission lines

T2 - predicting infrared and nebular line emission for ALMA and JWST

AU - Katz, Harley

AU - Galligan, Thomas P.

AU - Kimm, Taysun

AU - Rosdahl, Joakim

AU - Haehnelt, Martin G.

AU - Blaizot, Jeremy

AU - Devriendt, Julien

AU - Slyz, Adrianne

AU - Laporte, Nicolas

AU - Ellis, Richard

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Y1 - 2019/6/25

N2 - Infrared and nebular lines provide some of our best probes of the physics regulating the properties of the interstellar medium (ISM) at high redshift. However, interpreting the physical conditions of high-redshift galaxies directly from emission lines remains complicated due to inhomogeneities in temperature, density, metallicity, ionization parameter, and spectral hardness. We present a new suite of cosmological, radiation-hydrodynamics simulations, each centred on a massive Lyman-break galaxy that resolves such properties in an inhomogeneous ISM. Many of the simulated systems exhibit transient but well-defined gaseous discs that appear as velocity gradients in [C ii] 157.6 μ m emission. Spatial and spectral offsets between [C ii] 157.6 μ m and [O iii] 88.33 μ m are common, but not ubiquitous, as each line probes a different phase of the ISM. These systems fall on the local [C ii]-SFR relation, consistent with newer observations that question previously observed [C ii] 157.6 μ m deficits. Our galaxies are consistent with the nebular line properties of observed z ∼2-3 galaxies and reproduce offsets on the BPT and mass-excitation diagrams compared to local galaxies due to higher star formation rate (SFR), excitation, and specific-SFR, as well as harder spectra from young, metal-poor binaries. We predict that local calibrations between H α and [O ii] 3727 A luminosity and galaxy SFR apply up to z > 10, as do the local relations between certain strong line diagnostics (R23 and [O iii] 5007 A /H β) and galaxy metallicity. Our new simulations are well suited to interpret the observations of line emission from current (ALMA and HST) and upcoming facilities (JWST and ngVLA).

AB - Infrared and nebular lines provide some of our best probes of the physics regulating the properties of the interstellar medium (ISM) at high redshift. However, interpreting the physical conditions of high-redshift galaxies directly from emission lines remains complicated due to inhomogeneities in temperature, density, metallicity, ionization parameter, and spectral hardness. We present a new suite of cosmological, radiation-hydrodynamics simulations, each centred on a massive Lyman-break galaxy that resolves such properties in an inhomogeneous ISM. Many of the simulated systems exhibit transient but well-defined gaseous discs that appear as velocity gradients in [C ii] 157.6 μ m emission. Spatial and spectral offsets between [C ii] 157.6 μ m and [O iii] 88.33 μ m are common, but not ubiquitous, as each line probes a different phase of the ISM. These systems fall on the local [C ii]-SFR relation, consistent with newer observations that question previously observed [C ii] 157.6 μ m deficits. Our galaxies are consistent with the nebular line properties of observed z ∼2-3 galaxies and reproduce offsets on the BPT and mass-excitation diagrams compared to local galaxies due to higher star formation rate (SFR), excitation, and specific-SFR, as well as harder spectra from young, metal-poor binaries. We predict that local calibrations between H α and [O ii] 3727 A luminosity and galaxy SFR apply up to z > 10, as do the local relations between certain strong line diagnostics (R23 and [O iii] 5007 A /H β) and galaxy metallicity. Our new simulations are well suited to interpret the observations of line emission from current (ALMA and HST) and upcoming facilities (JWST and ngVLA).

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