Konstantinos Migkas

/Konstantinos Migkas

Konstantinos Migkas

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Anisotropy of the X-ray galaxy cluster luminosity-temperature relation

The ionic [CII] fine structure line at 158 micron is the brightest emission line in the spectrum of star-forming galaxies and as a result a reliable star formation tracer. It is an excellent target for unresolved spectral line intensity mapping observations at redshifts 5 to 9, providing an integral, unbiased tomographic view of the star formation activity and galaxy distribution throughout the epoch of reionization. CCAT-p, a high altitude (5600 m) 6-meters diameter telescope, equipped with state-of-the-art (sub)mm spectrometers with large field of view, will be the ideal instrument to map the [CII] intensity distribution. To test the feasibility and help optimize the survey strategy of CCAT-p, there is a need for high-redshift mock [CII] line intensity maps. Implementing machine learning algorithms trained by N-body-hydrodynamical simulations, I populate dark matter halo catalogues, coming from larger dark matter only N-body simulations, with galaxies. By making use of semi-analytical relations and the physical properties of these galaxies I calculate the intensity of the [CII] line and its contaminants, such as CO lines emission coming from lower redshifts and FIR foreground radiation, for several redshift slices. Based on these calculations I will present techniques and strategies for efficiently subtracting the contamination and statistically analyzing the targeted signal