Journal
MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY
Volume 489, Issue 2, Pages 2417-2438Publisher
OXFORD UNIV PRESS
DOI: 10.1093/mnras/stz2238
Keywords
galaxies: evolution; galaxies: formation; intergalactic medium
Categories
Funding
- CNRS
- CNES (Centre National d'Etudes Spatiales)
- ESO
- ESO science visitor programme
- DFG cluster of excellence 'Origin and Structure of the Universe'
- Alexander von Humboldt Foundation
- Science and Technology Facilities Council as part of the UK E-ELT Programme at the University of Oxford [ST/N002717/1, ST/M007650/1]
- STFC [ST/S001409/1, ST/M007650/1, ST/N002717/1] Funding Source: UKRI
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We simulate the flux emitted from galaxy haloes in order to quantify the brightness of the circumgalactic medium (CGM). We use dedicated zoom-in cosmological simulations with the hydrodynamical adaptive mesh refinement code RAMSES, which are evolved down to z = 0 and reach a maximum spatial resolution of 380 h(-1) pc and a gas mass resolution up to 1.8 x 10(5) h(-1) M-circle dot in the densest regions. We compute the expected emission from the gas in the CGM using CLOUDY emissivity models for different lines (e.g. Ly alpha, CIV, OVI, CVI, OVIII) considering UV background fluorescence, gravitational cooling and continuum emission. In the case of Lya, we additionally consider the scattering of continuum photons. We compare our predictions to current observations and find them to be in good agreement at any redshift after adjusting the Ly alpha escape fraction. We combine our mock observations with instrument models for Faint Intergalactic Redshifted Emission Balloon-2 (FIREBall-2; UV balloon spectrograph) and HARMONI (visible and NIR IFU on the ELT) to predict CGM observations with either instrument and optimize target selections and observing strategies. Our results show that Lya emission from the CGM at a redshift of 0.7 will be observable with FIREBall-2 for bright galaxies (NUV similar to 18 mag), while metal lines like OVI and C IV will remain challenging to detect. HARMONI is found to be well suited to study the CGM at different redshifts with various tracers.
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