This method was thus potentially biased against the highest redshift objects and galaxies in the 1.4 1 ( Sargent et al. Their precise position was determined by radio interferometry, and their redshift were measured using optical spectroscopy. However, identifying the optical counterparts was not trivial because of the large beam of single-dish submillimeter telescopes ( ~15– 20′′). (2005) find that the median redshift of these submillimeter galaxies (SMGs) is 2.3. This showed the importance of submillimeter observations in drawing a complete picture of the star formation activity in the high-redshift Universe. 1997), which were missed by optical surveys. Two decades ago, the first deep submillimeter surveys (850 μm) revealed a population of dusty, strongly star-forming galaxies (e.g., Smail et al. Key words: submillimeter: galaxies / infrared: galaxies / galaxies: evolution / galaxies: high-redshift / galaxies: star formation / gravitational lensing: strongĭetermining the star formation history in the Universe is a key challenge to understand the evolution of galaxies ( Madau & Dickinson 2014). This SPT sample is expected to be dominated by a population of lensed main-sequence galaxies and a minor contribution ( ~10%) of unlensed extreme starbursts. We found that the higher redshift of 1.4 mm-selected South Pole Telescope (SPT) sources compared to other SMG surveys is caused not only by the lensing selection, but also by the longer wavelength. Paradoxically, at a fixed wavelength and flux limit, the lensed sources are not always at higher redshift. This median redshift also varies significantly with the depth of the surveys, and deeper surveys do not necessarily probe higher redshifts. This model reproduces the observed redshift distributions from 100 μm to 1.4 mm and, especially, the increase in the median redshift with survey wavelength without any new parameter tuning. ![]() We interpret the wide variety of redshift distributions for galaxies found by far-infrared and (sub) millimeter deep surveys depending on their depth and wavelength using our phenomenological model of galaxy evolution. 2, 85748 Garching, GermanyĮ-mail: Astronomy Centre, Department of Physics and Astronomy, University of Sussex, Brighton, BN1 9QH, UKģ Laboratoire AIM-Paris-Saclay, CEA/DSM/Irfu – CNRS – Université Paris Diderot, CEA-Saclay, Pt courrier 131, 91191 Gif-sur-Yvette, France Matthieu Béthermin 1, Carlos De Breuck 1, Mark Sargent 2 and Emanuele Daddi 3ġ European Southern Observatory, Karl-Schwarzschild-Str. ![]()
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