UCL Discovery
UCL home » Library Services » Electronic resources » UCL Discovery

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

Katz, H; Galligan, TP; Kimm, T; Rosdahl, J; Haehnelt, MG; Blaizot, J; Devriendt, J; ... Ellis, R; + view all (2019) Probing cosmic dawn with emission lines: predicting infrared and nebular line emission for ALMA and JWST. Monthly Notices of the Royal Astronomical Society , 487 (4) pp. 5902-5921. 10.1093/mnras/stz1672. Green open access

[thumbnail of Ellis_Probing cosmic dawn with emission lines. Predicting infrared and nebular line emission for ALMA and JWST_VoR.pdf]
Preview
Text
Ellis_Probing cosmic dawn with emission lines. Predicting infrared and nebular line emission for ALMA and JWST_VoR.pdf - Published version

Download (5MB) | Preview

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 μm emission. Spatial and spectral offsets between [C II] 157.6 μm and [O III] 88.33 μm 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 μm 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] 3727A˚ luminosity and galaxy SFR apply up to z > 10, as do the local relations between certain strong line diagnostics (R23 and [O III] 5007A˚/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).

Type: Article
Title: Probing cosmic dawn with emission lines: predicting infrared and nebular line emission for ALMA and JWST
Open access status: An open access version is available from UCL Discovery
DOI: 10.1093/mnras/stz1672
Publisher version: https://doi.org/10.1093/mnras/stz1672
Language: English
Additional information: This version is the version of record. For information on re-use, please refer to the publisher’s terms and conditions.
Keywords: ISM: kinematics and dynamics, ISM: lines and bands, galaxies: high-redshift, galaxies: star formation
UCL classification: UCL
UCL > Provost and Vice Provost Offices
UCL > Provost and Vice Provost Offices > UCL BEAMS
UCL > Provost and Vice Provost Offices > UCL BEAMS > Faculty of Maths and Physical Sciences
UCL > Provost and Vice Provost Offices > UCL BEAMS > Faculty of Maths and Physical Sciences > Dept of Physics and Astronomy
URI: https://discovery.ucl.ac.uk/id/eprint/10076241
Downloads since deposit
30Downloads
Download activity - last month
Download activity - last 12 months
Downloads by country - last 12 months

Archive Staff Only

View Item View Item