We present deep spectroscopic follow-up observations of the Bremer Deep Field (BDF), where the two z ∼ 7 bright Lyα emitters (LAE) BDF521 and BDF3299 were previously discovered by Vanzella et al. and where a factor of ∼3-4 overdensity of faint LBGs has been found by Castellano et al. We confirm a new bright Lyα emitter, BDF2195, at the same redshift of BDF521, z = 7.008 and at only ∼90 kpc physical distance from it, confirming that the BDF area is likely an overdense, reionized region. A quantitative assessment of the Lyα fraction shows that the number of detected bright emitters is much higher than the average found at z ∼ 7, suggesting a high Lyα transmission through the intergalactic medium. However, the line visibility from fainter galaxies is at odds with this finding, as no Lyα emission is found in any of the observed candidates with M UV > -20.25. This discrepancy can be understood either if some mechanism prevents Lyα emission from fainter galaxies within the ionized bubbles from reaching the observer, or if faint galaxies are located outside the reionized area and bright LAEs are solely responsible for the creation of their own H ii regions. A thorough assessment of the nature of the BDF region and of its sources of re-ionizing radiation will be made possible by James Webb Space Telescope spectroscopic capabilities.

Spectroscopic Investigation of a Reionized Galaxy Overdensity at z = 7

Pentericci, L.;VANZELLA, Eros;Ferrara, A.;Carniani, S.;Gallerani, S.;Maiolino, R.;
2018

Abstract

We present deep spectroscopic follow-up observations of the Bremer Deep Field (BDF), where the two z ∼ 7 bright Lyα emitters (LAE) BDF521 and BDF3299 were previously discovered by Vanzella et al. and where a factor of ∼3-4 overdensity of faint LBGs has been found by Castellano et al. We confirm a new bright Lyα emitter, BDF2195, at the same redshift of BDF521, z = 7.008 and at only ∼90 kpc physical distance from it, confirming that the BDF area is likely an overdense, reionized region. A quantitative assessment of the Lyα fraction shows that the number of detected bright emitters is much higher than the average found at z ∼ 7, suggesting a high Lyα transmission through the intergalactic medium. However, the line visibility from fainter galaxies is at odds with this finding, as no Lyα emission is found in any of the observed candidates with M UV > -20.25. This discrepancy can be understood either if some mechanism prevents Lyα emission from fainter galaxies within the ionized bubbles from reaching the observer, or if faint galaxies are located outside the reionized area and bright LAEs are solely responsible for the creation of their own H ii regions. A thorough assessment of the nature of the BDF region and of its sources of re-ionizing radiation will be made possible by James Webb Space Telescope spectroscopic capabilities.
2018
dark ages, reionization, first stars; galaxies: evolution; galaxies: high-redshift; astro-ph.GA; astro-ph.GA; astro-ph.CO; Astronomy and Astrophysics; Space and Planetary Science
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Utilizza questo identificativo per citare o creare un link a questo documento: https://hdl.handle.net/11384/76409
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