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  • 2102.07779v1

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The X-SHOOTER Lyman-$α$ survey at z=2 (XLS-z2) I: the panchromatic spectrum of typical Lyman-$α$ emitters

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Forthcoming
  • Jorryt Matthee
  • David Sobral
  • Matthew Hayes
  • Gabriele Pezzulli
  • Max Gronke
  • Daniel Schaerer
  • Rohan P. Naidu
  • Huub Röttgering
  • João Calhau
  • Ana Paulino-Afonso
  • Sérgio Santos
  • Ricardo Amorín
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<mark>Journal publication date</mark>4/05/2021
<mark>Journal</mark>Monthly Notices of the Royal Astronomical Society
Publication StatusAccepted/In press
<mark>Original language</mark>English

Abstract

We present the first results from the X-SHOOTER Lyman-$\alpha$ survey at $z=2$ (XLS-$z2$). XLS-$z2$ is a deep spectroscopic survey of 35 Lyman-$\alpha$ emitters (LAEs) utilising $\approx90$ hours of exposure time with VLT/X-SHOOTER and covers rest-frame Ly$\alpha$ to H$\alpha$ emission with R$\approx4000$. We present the sample selection, the observations and the data reduction. Systemic redshifts are measured from rest-frame optical lines for 33/35 sources. In the stacked spectrum, our LAEs are characterised by an interstellar medium with little dust, a low metallicity and a high ionisation state. The ionising sources are young hot stars that power strong emission-lines in the optical and high ionisation lines in the UV. The LAEs exhibit clumpy UV morphologies and have outflowing kinematics with blue-shifted SiII absorption, a broad [OIII] component and a red-skewed Ly$\alpha$ line. Typically 30 % of the Ly$\alpha$ photons escape, of which one quarter on the blue side of the systemic velocity. A fraction of Ly$\alpha$ photons escapes directly at the systemic suggesting clear channels enabling a $\approx10$ % escape of ionising photons, consistent with an inference based on MgII. A combination of a low effective HI column density, a low dust content and young star-burst determine whether a star forming galaxy is observed as a LAE. The first is possibly related to outflows and/or a fortunate viewing angle, while we find that the latter two in LAEs are typical for their stellar mass of 10$^9$ M$_{\odot}$.