Rest-frame ultraviolet-to-optical spectral characteristics of extremely metal-poor and metal-free galaxies

By A. Inoue. 2011

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Finding the first generation of galaxies in the early Universe is the greatest step forward towards understanding galaxy formation and evolution. For a strategic survey of such galaxies and the interpretation of the obtained data, this paper presents an ultraviolet-to-optical spectral model of galaxies with a great care of the nebular emission. In particular, we present a machine-readable table of intensities of 119 nebular emission lines from Lyα to the rest-frame 1 m as a function of metallicity from zero to the solar one. Based on the spectral model, we present criteria of equivalent widths of Lyα, He iiλ1640, Hα, Hβ and [O iii]λ5007 to select extremely metal-poor and metal-free galaxies although these criteria have uncertainty caused by the Lyman continuum escape fraction and the star formation duration. We also present criteria of broad-band colours which will be useful to select candidates for spectroscopic follow-up from drop-out galaxies. We propose the line intensity ratio of [O iii]λ5007 to Hβ < 0.1 as the most robust criterion for <1/1000 of the solar metallicity. This ratio of a galaxy with a few M⊙ yr−1 at z∼ 8 is detectable by spectroscopy with the James Webb Space Telescope within a reasonable exposure time.

Subfields: Astronomy and Astrophysics, Instrumentation

View Paper: https://www.semanticscholar.org/paper/ff0070bdfef48dc7dc63417e8907de5112b42c34

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Citations in the corpus

Detection of the Far-infrared [O iii] and Dust Emission in a Galaxy at Redshift 8.312: Early Metal Enrichment in the Heart of the Reionization Era (2018, methodology): “In addition, we take into account the [O III] 88 μm line (Inoue et al. 2014b) and nebular continuum in the UV-to-optical wavelengths (Inoue 2011a).”
THE EVOLUTION OF THE GALAXY STELLAR MASS FUNCTION AT z = 4–8: A STEEPENING LOW-MASS-END SLOPE WITH INCREASING REDSHIFT (2015, background): “In this prescription, the strengths of H and He recombination lines (including Hβ) are set by the number of non-escaping ionizing photons, and the strengths of metal lines relative to Hβ are given by Inoue (2011).”
CIGALE: a python Code Investigating GALaxy Emission (2018, methodology): “…into account flexible SFH and stellar populations (Bruzual & Charlot 2003; Maraston 2005), ionised A103, page 16 of 33 A103, page 17 of 33 gas (Inoue 2011), attenuation by dust (Calzetti et al. 2000; Charlot & Fall 2000) and re-emission of the energy at longer wavelengths (Draine & Li 2007;…”
Spectroscopy of superluminous supernova host galaxies. A preference of hydrogen-poor events for extreme emission line galaxies (2014, background): “Inoue (2011) finds that the highest EWs are attained at ∼0.2 Z , exactly the metallicity regime where most of our SLSNe are found.”
Big Three Dragons: A z = 7.15 Lyman-break galaxy detected in [O iii] 88 μm, [C ii] 158 μm, and dust continuum with ALMA (2018, background): “The nebular continuum and emission lines of Inoue (2011a) are included.”
Dust Attenuation Curves in the Local Universe: Demographics and New Laws for Star-forming Galaxies and High-redshift Analogs (2018, methodology): “The nebular templates expand upon Inoue (2011) and have been computed using Cloudy 08.00 (Ferland et al. 1998).”
JWST Census for the Mass–Metallicity Star Formation Relations at z = 4–10 with Self-consistent Flux Calibration and Proper Metallicity Calibrators (2023, background): “…diagnosing the presence of accreting black holes in the system, and detecting galaxies hosting the very ﬁ rst generation of stars in the early Universe ( e.g., Schaerer 2003; Inoue 2011; Kewley et al. 2013; Bouwens et al. 2016; Nakajima & Maiolino 2022; Trussler et al. 2022; Katz et al. 2023a ) .”
An updated analytic model for attenuation by the intergalactic medium (2014, methodology): “…(Z = 0.02, 0.008, and 0.004), the Chabrier initial mass function between 0.1 and 100 M⊙ (Chabrier 2003), exponentially declining star formation history, the Calzetti attenuation law (Calzetti et al. 2000), and the emission line model by Inoue (2011) with the Lyman continuum escape fraction of zero.”
Photometric Redshifts for Hyper Suprime-Cam Subaru Strategic Program Data Release 1 (2017, background): “Emission lines are added to the templates assuming solar metallicity (Inoue 2011).”
VERY STRONG EMISSION-LINE GALAXIES IN THE WFC3 INFRARED SPECTROSCOPIC PARALLEL SURVEY AND IMPLICATIONS FOR HIGH-REDSHIFT GALAXIES, (2011, background): “Ono et al. 2010; Watson et al. 2010; Raiter et al. 2010; Finlator et al. 2011; McLure et al. 2011; Inoue 2011) dealing with SED modeling.”
THE RELATION BETWEEN STAR FORMATION RATE AND STELLAR MASS FOR GALAXIES AT 3.5 ⩽ z ⩽ 6.5 IN CANDELS (2014, methodology): “Following Inoue (2011), we relate the Hβ line luminosity to the incident number of Lyman-continuum photons as LHβ = 4.78 × 10 −13 1 − fesc 1 + 0.6fesc NLyC [erg s −1], (1) where fesc is the fraction of ionizing Lyman continuum (LyC) photons escaping the galaxy into the IGM and NLyC is the…”
THE EVOLUTION OF THE GALAXY REST-FRAME ULTRAVIOLET LUMINOSITY FUNCTION OVER THE FIRST TWO BILLION YEARS (2014, methodology): “We also included nebular emission lines using the prescription of Salmon et al. (2015)—which uses the line ratios from Inoue (2011), based on the number of ionizing photons from a given model—and assuming the ionizing photon escape fraction is ≈ zero.”