Large scale structure at z=5.7 near the Hubble and Chandra deep fields

Details Large scale structure at z=5.7 near the Hubble and Chandra deep fields Large scale structure at z=5.7 near the Hubble and Chandra deep fields

Aug 2005

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2005noao.prop..521m&link_type=abstract

NOAO Proposal ID #2005B-0521

Physics

Scientific paper

The formation of galaxies and the reionization of the intergalactic medium are major milestones in cosmic history that are only now becoming accessible to observation. The two basic questions about reionization are (1) when did reionization happen and (2) what was responsible for the UV photons that ionized the intergalactic medium. From the deepest imaging and spectroscopic data we have in the Hubble Ultra Deep field (HUDF), it seems that the answer to both the questions may well depend on the clustering of galaxies at z 6. Narrow-band imaging corresponding to Lyα at z 5.8 shows a factor of 3-4 overdensity of Lyα galaxies at spatial scale of at least 40 comoving Mpc (cMpc), and the HUDF is situated at the edge. Spectroscopy with the ACS grism reveals a corresponding peak in the redshift distibution extending to 150 cMpc along the line of sight, making this the largest scale structure seen at these redshifts. Because of the factor of four overdensity in galaxies locally there are sufficient photons to ionize the IGM. We wish to determine the transverse size of this region. By extending the area of the survey by three MOSAIC fields we will map out this overdense region at z 5.8 to 180x180 cMpc. The sizes and abundances of such overdense regions will tell us a lot about where star-formation happened in the early universe, i.e. the bias factor of early galaxy formation ; and the possible size and topology of ionized bubbles. This information cannot be had even with N-body simulations since none can simultaneously represent such a large volume and sufficient resolution to study galaxy formation. We can also test to see if the properties of galaxies in the overdense regions are different from "field" galaxies, for e.g. more older stars, since star-formation happened early here.

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