ABSTRACT The nebular recombination line H α is widely used as a star formation rate (SFR) indicator in the local and high-redshift Universe. We present a detailed H α radiative transfer study of high-resolution isolated Milky-Way and Large Magellanic Cloud simulations that include radiative transfer, non-equilibrium thermochemistry, and dust evolution. We focus on the spatial morphology and temporal variability of the H α emission, and its connection to the underlying gas and star formation properties. The H α and H β radial and vertical surface brightness profiles are in excellent agreement with observations of nearby galaxies. We find that the fraction of H α emission from collisional excitation amounts to fcol ∼ 5–$$10{{\ \rm per\ cent}}$$, only weakly dependent on radius and vertical height, and that scattering boosts the H α luminosity by $$\sim 40{{\ \rm per\ cent}}$$. The dust correction via the Balmer decrement works well (intrinsic H α emission recoverable within 25 per cent), though the dust attenuation law depends on the amount of attenuation itself both on spatially resolved and integrated scales. Important for the understanding of the H α–SFR connection is the dust and helium absorption of ionizing radiation (Lyman continuum [LyC] photons), which are about $$f_{\rm abs}\approx 28{{\ \rm per\ cent}}$$ and $$f_{\rm He}\approx 9{{\ \rm per\ cent}}$$, respectively. Together with an escape fraction of $$f_{\rm esc}\approx 6{{\ \rm per\ cent}}$$, this reduces the available budget for hydrogen line emission by nearly half ($$f_{\rm H}\approx 57{{\ \rm per\ cent}}$$). We discuss the impact of the diffuse ionized gas, showing – among other things – that the extraplanar H α emission is powered by LyC photons escaping the disc. Future applications of this framework to cosmological (zoom-in) simulations will assist in the interpretation of spectroscopy of high-redshift galaxies with the upcoming James Webb Space Telescope. 
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                            Lyman continuum escape fraction in Ly α emitters at z ≃ 3.1
                        
                    
    
            ABSTRACT We measure the Lyman continuum (LyC) escape fraction in 54 faint Lyman-alpha emitters (LAEs) at $$z$$ ≃ 3.1 in the GOODS-South field. With the average magnitude of R = 26.7 AB (MUV = −18.8 and L ≃ 0.1L*), these galaxies represent a population of compact young dwarf galaxies. Their properties are likely to resemble those in the galaxies responsible for reionizing the Universe at $$z$$ > 6. We do not detect LyC emission in any individual LAEs in the deep HST F336W images, which covers the rest-frame 820 Å. We do not detect the LyC emission of these LAEs in the stacked F336W images either. The 3σ upper limit of LyC escape fractions is $$f_{\rm esc}\lt 14\!-\!32{{\ \rm per\ cent}}$$. However, the high Ly α rest-frame equivalent width (EW), low stellar mass, and UV luminosity of these LAEs suggest that they should have $$f_{\rm esc}\gt 50{{\ \rm per\ cent}}$$. The low LyC escape fraction from this work and other stacking analyses suggests that the LyC-leaking galaxies with $$f_{\rm esc}\gt 50{{\ \rm per\ cent}}$$ at $$z$$ = 2–3 do not follow the relation between fesc and UV luminosity and Ly α EW derived from typical galaxies at similar redshifts. Therefore, the UV luminosity and Ly α EW are not the best indicators for the LyC escape fraction. 
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                            - Award ID(s):
- 1908284
- PAR ID:
- 10194935
- Date Published:
- Journal Name:
- Monthly Notices of the Royal Astronomical Society: Letters
- Volume:
- 493
- Issue:
- 1
- ISSN:
- 1745-3925
- Page Range / eLocation ID:
- L65 to L69
- Format(s):
- Medium: X
- Sponsoring Org:
- National Science Foundation
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